FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Wehrle, AE Marscher, AP Jorstad, SG Gurwell, MA Joshi, M MacDonald, NR Williamson, KE Agudo, I Grupe, D AF Wehrle, Ann E. Marscher, Alan P. Jorstad, Svetlana G. Gurwell, Mark A. Joshi, Manasvita MacDonald, Nicholas R. Williamson, Karen E. Agudo, Ivan Grupe, Dirk TI MULTIWAVELENGTH VARIATIONS OF 3C 454.3 DURING THE 2010 NOVEMBER TO 2011 JANUARY OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: general; quasars: individual (3C 454.3) ID ACTIVE GALACTIC NUCLEI; SYNCHROTRON EMISSION; HOT DUST; VARIABILITY; BLAZARS; JET; RADIATION; TELESCOPE; QUASARS; SPECTRA AB We present multiwavelength data of the blazar 3C 454.3 obtained during an extremely bright outburst from 2010 November through 2011 January. These include flux density measurements with the Herschel Space Observatory at five submillimeter-wave and far-infrared bands, the Fermi Large Area Telescope at gamma-ray energies, Swift at X-ray, ultraviolet (UV), and optical frequencies, and the Submillimeter Array at 1.3 mm. From this data set, we form a series of 52 spectral energy distributions (SEDs) spanning nearly two months that are unprecedented in time coverage and breadth of frequency. Discrete correlation analysis of the millimeter, far-infrared, and gamma-ray light curves show that the variations were essentially simultaneous, indicative of cospatiality of the emission, at these wavebands. In contrast, differences in short-term fluctuations at various wavelengths imply the presence of inhomogeneities in physical conditions across the source. We locate the site of the outburst in the parsec-scale "core," whose flux density as measured on 7 mm Very Long Baseline Array images increased by 70% during the first five weeks of the outburst. Based on these considerations and guided by the SEDs, we propose a model in which turbulent plasma crosses a conical standing shock in the parsec-scale region of the jet. Here, the high-energy emission in the model is produced by inverse Compton scattering of seed photons supplied by either nonthermal radiation from a Mach disk, thermal emission from hot dust, or (for X-rays) synchrotron radiation from plasma that crosses the standing shock. For the two dates on which we fitted the model SED to the data, the model corresponds very well to the observations at all bands except at X-ray energies, where the spectrum is flatter than observed. C1 [Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA. [Marscher, Alan P.; Jorstad, Svetlana G.; Joshi, Manasvita; MacDonald, Nicholas R.; Williamson, Karen E.; Agudo, Ivan] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Jorstad, Svetlana G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Gurwell, Mark A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Agudo, Ivan] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Grupe, Dirk] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Wehrle, AE (reprint author), Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA. EM awehrle@spacescience.org RI Agudo, Ivan/G-1701-2015; Jorstad, Svetlana/H-6913-2013 OI Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453 FU Guest Investigator support from NASA via Herschel [RSA 1427799]; Fermi Guest Investigator [NNX11AAO85G]; NASA under Fermi Guest Investigator [NNX08AV65G, NNX10AO59G, NNX10AU15G, NNX11AQ03G]; Swift Guest Investigator [NNX10AF88G]; Smithsonian Institution; Academia Sinica; regional government of Andalucia [P09-FQM-4784]; "Ministerio de Ciencia e Innovacion" of Spain [AYA2010-14844] FX We are grateful to the Herschel Director Goran Pilbratt, Swift Principal Investigator Neil Gehrels, Herschel ESA staff astronomers Mark Kidger, Pedro Garcia-Lario, and Herschel NASA staff astronomers Babar Ali, Nicolas Billot, Phil Appleton, and Bernhard Schulz. We also thank the Herschel spacecraft schedulers in Munich for setting up our monitoring program. A. Wehrle acknowledges Guest Investigator support from NASA via Herschel RSA 1427799 and Fermi Guest Investigator grant NNX11AAO85G. The BU group acknowledges support by NASA under Fermi Guest Investigator grants NNX08AV65G, NNX10AO59G, NNX10AU15G, and NNX11AQ03G and Swift Guest Investigator grant NNX10AF88G. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The VLBA is an instrument of 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. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. Swift at PSU is supported by NASA contract NAS5-00136. I. Agudo acknowledges funding support from the regional government of Andalucia and the "Ministerio de Ciencia e Innovacion" of Spain through grants P09-FQM-4784 and AYA2010-14844, respectively. NR 41 TC 48 Z9 48 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 20 PY 2012 VL 758 IS 2 AR 72 DI 10.1088/0004-637X/758/2/72 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 030HO UT WOS:000310562000001 ER PT J AU Brown, JM Rosenfeld, KA Andrews, SM Wilner, DJ van Dishoeck, EF AF Brown, J. M. Rosenfeld, K. A. Andrews, S. M. Wilner, D. J. van Dishoeck, E. F. TI MATRYOSHKA HOLES: NESTED EMISSION RINGS IN THE TRANSITIONAL DISK OPH IRS 48 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; protoplanetary disks; stars: individual (Oph IRS 48); stars: pre-main sequence; submillimeter: general ID PROTOPLANETARY DISK; RHO-OPHIUCHI; STAR-FORMATION; DUST EMISSION; GIANT PLANET; INNER HOLE; GAP; EVOLUTION; SPECTROSCOPY; MIGRATION AB The processes that form transition disks-disks with depleted inner regions-are not well understood; possible scenarios include planet formation, grain growth, and photoevaporation. Disks with spatially resolved dust holes are rare, but, in general, even less is known about the gas structure. The disk surrounding the A0 star Oph IRS 48 in the nearby rho Ophiuchus region has a 30 AU radius hole previously detected in the 18.7 mu m dust continuum and in warm CO in the 5 mu m fundamental rovibrational band. We present here Submillimeter Array 880 mu m continuum imaging resolving an inner hole. However, the radius of the hole in the millimeter dust is only 13 AU, significantly smaller than measured at otherwavelengths. The nesting structure of the disk is counter intuitive, with increasingly large radius rings of emission seen in the millimeter dust (12.9(-3.4)(+1.7) AU), 5 mu m CO (30 AU), and 18.7 mu m dust (peaking at 55 AU). We discuss possible explanations for this structure, including self-shadowing that cools the disk surface layers, photodissociation of CO, and photoevaporation. However, understanding this unusual disk within the stringent multi-wavelength spatial constraints will require further observations to search for cold atomic and molecular gas. C1 [Brown, J. M.; Rosenfeld, K. A.; Andrews, S. M.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Brown, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM joannabrown@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica; Smithsonian Astrophysical Observatory from an SMA fellowship; Spinoza grant from the Netherlands Organization for Scientific Research (NWO); EU A-ERC grant [291141] 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. The authors thank Jes Jorgenesen for providing the earlier 230 GHz data and Vincent Geers for the reduced VISIR data. J. M. Brown acknowledges the Smithsonian Astrophysical Observatory for support from an SMA fellowship. Astrochemistry at Leiden is supported by a Spinoza grant from the Netherlands Organization for Scientific Research (NWO) and by EU A-ERC grant 291141 CHEMPLAN. NR 36 TC 12 Z9 12 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2012 VL 758 IS 2 AR L30 DI 10.1088/2041-8205/758/2/L30 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018RH UT WOS:000309679300006 ER PT J AU Godfrey, LEH Lovell, JEJ Burke-Spolaor, S Ekers, R Bicknell, GV Birkinshaw, M Worrall, DM Jauncey, DL Schwartz, DA Marshall, HL Gelbord, J Perlman, ES Georganopoulos, M AF Godfrey, L. E. H. Lovell, J. E. J. Burke-Spolaor, S. Ekers, R. Bicknell, G. V. Birkinshaw, M. Worrall, D. M. Jauncey, D. L. Schwartz, D. A. Marshall, H. L. Gelbord, J. Perlman, E. S. Georganopoulos, M. TI PERIODIC STRUCTURE IN THE MEGAPARSEC-SCALE JET OF PKS 0637-752 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (PKS0637-752) ID ACTIVE GALACTIC NUCLEI; BINARY BLACK-HOLE; II RADIO-SOURCES; HUBBLE-SPACE-TELESCOPE; X-RAY-EMISSION; ACCRETION DISK; RELATIVISTIC JETS; GALAXY; INSTABILITY; CHANDRA AB We present 18 GHz Australia Telescope Compact Array imaging of the megaparsec-scale quasar jet PKS 0637-752 with angular resolution similar to 0 ''.58. We draw attention to a spectacular train of quasi-periodic knots along the inner 11 '' of the jet, with average separation similar to 1.1 arcsec (7.6 kpc projected). We consider two classes of model to explain the periodic knots: those that involve a static pattern through which the jet plasma travels (e.g., stationary shocks) and those that involve modulation of the jet engine. Interpreting the knots as re-confinement shocks implies the jet kinetic power Q(jet) similar to 10(46) erg s(-1), but the constant knot separation along the jet is not expected in a realistic external density profile. For models involving modulation of the jet engine, we find that the required modulation period is 2 x 10(3) yr < tau < 3 x 10(5) yr. The lower end of this range is applicable if the jet remains highly relativistic on kiloparsec scales, as implied by the IC/CMB model of jet X-ray emission. We suggest that the periodic jet structure in PKS 0637-752 may be analogous to the quasi-periodic jet modulation seen in the microquasar GRS 1915+105, believed to result from limit cycle behavior in an unstable accretion disk. If variations in the accretion rate are driven by a binary black hole, the predicted orbital radius is 0.7 pc less than or similar to a less than or similar to 30 pc, which corresponds to a maximum angular separation of similar to 0.1-5 mas. C1 [Godfrey, L. E. H.; Ekers, R.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6102, Australia. [Godfrey, L. E. H.; Bicknell, G. V.; Jauncey, D. L.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Lovell, J. E. J.; Ekers, R.; Jauncey, D. L.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Hobart, Tas 2121, Australia. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001`, Australia. [Burke-Spolaor, S.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Birkinshaw, M.; Worrall, D. M.; Schwartz, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gelbord, J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Perlman, E. S.] Florida Inst Technol, Phys & Space Sci Dept, Melbourne, FL 32901 USA. [Georganopoulos, M.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. RP Godfrey, LEH (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6102, Australia. EM L.Godfrey@curtin.edu.au RI Godfrey, Leith/B-5283-2013 FU Commonwealth of Australia; NASA [NAS8-03060]; CXC [GO9-0121B] FX The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. D.A.S. is supported by NASA contract NAS8-03060 and CXC grant GO9-0121B. NR 48 TC 13 Z9 13 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 20 PY 2012 VL 758 IS 2 AR L27 DI 10.1088/2041-8205/758/2/L27 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 018RH UT WOS:000309679300003 ER PT J AU Sosdian, SM Lear, CH Tao, K Grossman, EL O'Dea, A Rosenthal, Y AF Sosdian, Sindia M. Lear, Caroline H. Tao, Kai Grossman, Ethan L. O'Dea, Aaron Rosenthal, Yair TI Cenozoic seawater Sr/Ca evolution SO GEOCHEMISTRY GEOPHYSICS GEOSYSTEMS LA English DT Article DE gastropods; seawater chemistry; strontium ID CULTURED BENTHIC FORAMINIFERA; ATMOSPHERIC CARBON-DIOXIDE; PLANKTONIC-FORAMINIFERA; HYDROTHERMAL FLUXES; WEATHERING FLUXES; CALCIUM-CARBONATE; SATURATION STATE; TRACE-ELEMENTS; DEGREES C; STRONTIUM AB Records of seawater chemistry help constrain temporal variations in geochemical processes that impact the global carbon cycle and climate through Earth's history. Here we reconstruct Cenozoic seawater Sr/Ca (Sr/Ca-sw) using fossil Conus and turritellid gastropod Sr/Ca. Combined with an oxygen isotope paleotemperature record from the same samples, the gastropod record suggests that Sr/Ca-sw was slightly higher in the Eocene (similar to 11.4 +/- 3 mmol/mol) than today (similar to 8.54 mmol/mol) and remained relatively stable from the mid- to late Cenozoic. We compare our gastropod Cenozoic Sr/Ca-sw record with a published turritellid gastropod Sr/Ca-sw record and other published biogenic (benthic foraminifera, fossil fish teeth) and inorganic precipitate (calcite veins) Sr/Ca-sw records. Once the uncertainties with our gastropod-derived Sr/Ca-sw are taken into account the Sr/Ca-sw record agrees reasonably well with biogenic Sr/Ca-sw records. Assuming a seawater [Ca] history derived from marine evaporite inclusions, all biogenic-based Sr/Ca-sw reconstructions imply decreasing seawater [Sr] through the Cenozoic, whereas the calcite vein Sr/Ca-sw reconstruction implies increasing [Sr] through the Cenozoic. We apply a simple geochemical model to examine the implications of divergence among these seawater [Sr] reconstructions and suggest that the interpretation and uncertainties associated with the gastropod and calcite vein proxies need to be revisited. Used in conjunction with records of carbonate depositional fluxes, our favored seawater Sr/Ca scenarios point to a significant increase in the proportion of aragonite versus calcite deposition in shelf sediments from the Middle Miocene, coincident with the proliferation of coral reefs. We propose that this occurred at least 10 million years after the seawater Mg/Ca threshold was passed, and was instead aided by declining levels of atmospheric carbon dioxide. C1 [Sosdian, Sindia M.; Lear, Caroline H.] Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AT, S Glam, Wales. [Sosdian, Sindia M.; Rosenthal, Yair] Rutgers State Univ, Inst Marine & Coastal Sci, New Brunswick, NJ 08901 USA. [Sosdian, Sindia M.; Rosenthal, Yair] Rutgers State Univ, Dept Earth & Planetary Sci, New Brunswick, NJ 08901 USA. [Tao, Kai; Grossman, Ethan L.] Texas A&M Univ, Dept Geol & Geophys, College Stn, TX 77843 USA. [O'Dea, Aaron] Smithsonian Trop Res Inst, Balboa, Panama. RP Sosdian, SM (reprint author), Cardiff Univ, Sch Earth & Ocean Sci, Cardiff CF10 3AT, S Glam, Wales. EM sosdians@cardiff.ac.uk; learc@cardiff.ac.uk; taokai@gmail.com; e-grossman@tamu.edu; aaronodea@gmail.com; rosentha@imcs.rutgers.edu RI Lear, Caroline/D-2582-2009; O'Dea, Aaron/D-4114-2011; OI Lear, Caroline/0000-0002-7533-4430 FU NSF [EAR-0126311, EAR-0126173, EAR03-45471]; National Geographic Society; U.S.-UK Fulbright Fellowship; Michel T. Halbouty Chair in Geology (TAMU); National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) FX We thank T. Kobashi, who helped launch this study through his isotopic study of paleoclimates and B. N. Opdyke and J. Caves for helpful discussions. Samples were provided by T. Kobashi, D. Dockery and the Mississippi Office of Environmental Quality. We thank Anthony Coates, Helena Fortunato, Jeremy Jackson, Jill Leonard Pingel and Felix Rodriguez for helping collect sample material and Recursos Minerales for granting permits for Panama specimen collection. We acknowledge support from the NSF (EAR-0126311 to ELG, EAR-0126173 to YR and CHL, and EAR03-45471 to AO), the National Geographic Society to AO, the U.S.-UK Fulbright Fellowship to SMS, the Michel T. Halbouty Chair in Geology (TAMU), and the National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) to AO. NR 91 TC 5 Z9 5 U1 5 U2 53 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1525-2027 J9 GEOCHEM GEOPHY GEOSY JI Geochem. Geophys. Geosyst. PD OCT 19 PY 2012 VL 13 AR Q10014 DI 10.1029/2012GC004240 PG 23 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 023XN UT WOS:000310071100001 ER PT J AU Doeleman, SS Fish, VL Schenck, DE Beaudoin, C Blundell, R Bower, GC Broderick, AE Chamberlin, R Freund, R Friberg, P Gurwell, MA Ho, PTP Honma, M Inoue, M Krichbaum, TP Lamb, J Loeb, A Lonsdale, C Marrone, DP Moran, JM Oyama, T Plambeck, R Primiani, RA Rogers, AEE Smythe, DL SooHoo, J Strittmatter, P Tilanus, RPJ Titus, M Weintroub, J Wright, M Young, KH Ziurys, LM AF Doeleman, Sheperd S. Fish, Vincent L. Schenck, David E. Beaudoin, Christopher Blundell, Ray Bower, Geoffrey C. Broderick, Avery E. Chamberlin, Richard Freund, Robert Friberg, Per Gurwell, Mark A. Ho, Paul T. P. Honma, Mareki Inoue, Makoto Krichbaum, Thomas P. Lamb, James Loeb, Abraham Lonsdale, Colin Marrone, Daniel P. Moran, James M. Oyama, Tomoaki Plambeck, Richard Primiani, Rurik A. Rogers, Alan E. E. Smythe, Daniel L. SooHoo, Jason Strittmatter, Peter Tilanus, Remo P. J. Titus, Michael Weintroub, Jonathan Wright, Melvyn Young, Ken H. Ziurys, Lucy M. TI Jet-Launching Structure Resolved Near the Supermassive Black Hole in M87 SO SCIENCE LA English DT Article ID RADIO GALAXY M87; SGR-A-ASTERISK; RELATIVISTIC JETS; MAGNETOHYDRODYNAMIC SIMULATIONS; INNER JET; ACCRETION; EVOLUTION; SPIN; PROPAGATION; STABILITY AB Approximately 10% of active galactic nuclei exhibit relativistic jets, which are powered by the accretion of matter onto supermassive black holes. Although the measured width profiles of such jets on large scales agree with theories of magnetic collimation, the predicted structure on accretion disk scales at the jet launch point has not been detected. We report radio interferometry observations, at a wavelength of 1.3 millimeters, of the elliptical galaxy M87 that spatially resolve the base of the jet in this source. The derived size of 5.5 +/- 0.4 Schwarzschild radii is significantly smaller than the innermost edge of a retrograde accretion disk, suggesting that the M87 jet is powered by an accretion disk in a prograde orbit around a spinning black hole. C1 [Doeleman, Sheperd S.; Fish, Vincent L.; Schenck, David E.; Beaudoin, Christopher; Lonsdale, Colin; Rogers, Alan E. E.; Smythe, Daniel L.; SooHoo, Jason; Titus, Michael] MIT, Haystack Observ, Westford, MA 01886 USA. [Doeleman, Sheperd S.; Blundell, Ray; Gurwell, Mark A.; Loeb, Abraham; Moran, James M.; Primiani, Rurik A.; Weintroub, Jonathan; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schenck, David E.; Freund, Robert; Marrone, Daniel P.; Strittmatter, Peter; Ziurys, Lucy M.] Univ Arizona, Arizona Radio Observ, Steward Observ, Tucson, AZ 85721 USA. [Bower, Geoffrey C.; Plambeck, Richard; Wright, Melvyn] Univ Calif Berkeley, Dept Astron, Hearst Field Annex, Berkeley, CA 94720 USA. [Broderick, Avery E.] Perimeter Inst, N Waterloo, ON N2L 2Y5, Canada. [Broderick, Avery E.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Chamberlin, Richard] Caltech Submillimeter Observ, Hilo, HI 96720 USA. [Friberg, Per; Tilanus, Remo P. J.] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Ho, Paul T. P.; Inoue, Makoto] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Honma, Mareki] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. [Honma, Mareki] Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Krichbaum, Thomas P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Lamb, James] CALTECH, Owens Valley Radio Observ, Big Pine, CA 93513 USA. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. RP Doeleman, SS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM sdoeleman@haystack.mit.edu OI Marrone, Daniel/0000-0002-2367-1080; Moran, James/0000-0002-3882-4414 FU NSF; NSF University Radio Observatories (URO) [AST-1140030]; ATI [AST-0905844]; CARMA partner universities FX High-frequency VLBI work at the MIT Haystack Observatory is supported by grants from NSF. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics. The Submillimeter Telescope is operated by the Arizona Radio Observatory (ARO). ARO is partially supported through the NSF University Radio Observatories (URO: grant AST-1140030) and ATI (grant AST-0905844) programs. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. Funding for ongoing CARMA development and operations is supported by NSF and the CARMA partner universities. We thank the NASA Geodesy Program for loan of the CARMA Hydrogen Maser; J. Test, P. Yamaguchi, G. Reiland, J. Hoge, and M. Hodges for technical assistance; the staff at all participating facilities; J. Gracia and J. McKinney for providing jet simulation data used in this work; and Xilinx, Inc., for equipment donations. Data used in this paper are available in the supplementary materials. NR 34 TC 128 Z9 127 U1 1 U2 18 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 OCT 19 PY 2012 VL 338 IS 6105 BP 355 EP 358 DI 10.1126/science.1224768 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 022JS UT WOS:000309955800034 PM 23019611 ER PT J AU Ceron-Souza, I Bermingham, E McMillan, WO Jones, FA AF Ceron-Souza, Ivania Bermingham, Eldredge McMillan, William Owen Jones, Frank Andrew TI Comparative genetic structure of two mangrove species in Caribbean and Pacific estuaries of Panama SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Rhizophora mangle; Avicennia germinans; Pollen dispersal; Seed dispersal; Spatial genetic structure ID MULTILOCUS GENOTYPE DATA; MICROSATELLITE NULL ALLELES; POPULATION-STRUCTURE; RHIZOPHORA-MANGLE; PLANT-POPULATIONS; AVICENNIA-GERMINANS; LANDSCAPE GENETICS; WIND POLLINATION; FOREST STRUCTURE; RELATIVE RATES AB Background: Mangroves are ecologically important and highly threatened forest communities. Observational and genetic evidence has confirmed the long distance dispersal capacity of water-dispersed mangrove seeds, but less is known about the relative importance of pollen vs. seed gene flow in connecting populations. We analyzed 980 Avicennia germinans for 11 microsatellite loci and 940 Rhizophora mangle for six microsatellite loci and subsampled two non-coding cpDNA regions in order to understand population structure, and gene flow within and among four major estuaries on the Caribbean and Pacific coasts of Panama. Results: Both species showed similar rates of outcrossing (t= 0.7 in A. germinans and 0.8 in R. mangle) and strong patterns of spatial genetic structure within estuaries, although A. germinans had greater genetic structure in nuclear and cpDNA markers (7 demes > 4 demes and Sp= 0.02 > 0.002), and much greater cpDNA diversity (H-d= 0.8 > 0.2) than R. mangle. The Central American Isthmus serves as an exceptionally strong barrier to gene flow, with high levels nuclear (F-ST= 0.3-0.5) and plastid (T-FS= 0.5-0.8) genetic differentiation observed within each species between coasts and no shared cpDNA haplotypes between species on each coast. Finally, evidence of low ratios of pollen to seed dispersal (r = -0.6 in A. germinans and 7.7 in R. mangle), coupled with the strong observed structure in nuclear and plastid DNA among most estuaries, suggests low levels of gene flow in these mangrove species. Conclusions: We conclude that gene dispersal in mangroves is usually limited within estuaries and that coastal geomorphology and rare long distance dispersal events could also influence levels of structure. C1 [Ceron-Souza, Ivania; Bermingham, Eldredge; McMillan, William Owen; Jones, Frank Andrew] Smithsonian Trop Res Inst, Panama City, Panama. [Ceron-Souza, Ivania] Univ Puerto Rico, San Juan, PR 00931 USA. [Jones, Frank Andrew] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP Ceron-Souza, I (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM iviceron@gmail.com FU STRI (short-term fellowship); University of Puerto Rico (CREST fellowship); University of Puerto Rico (DEGI fellowship); University of Puerto Rico (NSF-EPSCor fellowship) FX This work had the financial support of STRI (short-term fellowship) and University of Puerto Rico (CREST, DEGI and NSF-EPSCor fellowships) as part of ICS's PhD thesis. Thanks to ANAM in Panama for collections permits. We are grateful to E. Diaz, L. M. Garcia, N. Giraldo and G. Thomas for fieldwork support in Panama. Finally, thanks to F. Alda, L. Geyer, A. Nordine, K. Rosas, K. Saltonstall and the two anonymous reviewers for their invaluable comments to previous version of this manuscript. NR 93 TC 16 Z9 16 U1 2 U2 68 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD OCT 18 PY 2012 VL 12 AR 205 DI 10.1186/1471-2148-12-205 PG 15 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 070LS UT WOS:000313508200001 PM 23078287 ER PT J AU Mccoy, MW Touchon, JC Landberg, T Warkentin, KM Vonesh, JR AF McCoy, Michael W. Touchon, Justin C. Landberg, Tobias Warkentin, Karen M. Vonesh, James R. TI Prey Responses to Predator Chemical Cues: Disentangling the Importance of the Number and Biomass of Prey Consumed SO PLOS ONE LA English DT Article ID TRAIT-MEDIATED INTERACTIONS; PHENOTYPIC PLASTICITY; ANTIPREDATOR BEHAVIOR; CONSPECIFIC DENSITY; TEMPORAL VARIATION; DOSAGE RESPONSE; OPPOSITE SHIFTS; INDUCED DEFENSE; LARVAL ANURANS; ALARM CUES AB To effectively balance investment in predator defenses versus other traits, organisms must accurately assess predation risk. Chemical cues caused by predation events are indicators of risk for prey in a wide variety of systems, but the relationship between how prey perceive risk in relation to the amount of prey consumed by predators is poorly understood. While per capita predation rate is often used as the metric of relative risk, studies aimed at quantifying predator-induced defenses commonly control biomass of prey consumed as the metric of risk. However, biomass consumed can change by altering either the number or size of prey consumed. In this study we determine whether phenotypic plasticity to predator chemical cues depends upon prey biomass consumed, prey number consumed, or both. We examine the growth response of red-eyed treefrog tadpoles (Agalychnis callidryas) to cues from a larval dragonfly (Anax amazili). Biomass consumed was manipulated by either increasing the number of prey while holding individual prey size constant, or by holding the number of prey constant and varying individual prey size. We address two questions. (i) Do prey reduce growth rate in response to chemical cues in a dose dependent manner? (ii) Does the magnitude of the response depend on whether prey consumption increases via number or size of prey? We find that the phenotypic response of prey is an asymptotic function of prey biomass consumed. However, the asymptotic response is higher when more prey are consumed. Our findings have important implications for evaluating past studies and how future experiments should be designed. A stronger response to predation cues generated by more individual prey deaths is consistent with models that predict prey sensitivity to per capita risk, providing a more direct link between empirical and theoretical studies which are often focused on changes in population sizes not individual biomass. C1 [McCoy, Michael W.] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. [McCoy, Michael W.; Vonesh, James R.] Virginia Commonwealth Univ, Dept Biol, Richmond, VA 23284 USA. [Touchon, Justin C.; Warkentin, Karen M.] Smithsonian Trop Res Inst, Balboa, Panama. [Touchon, Justin C.; Landberg, Tobias; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. RP Mccoy, MW (reprint author), E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. EM mccoym@ecu.edu RI Vonesh, James/I-1573-2013 OI Vonesh, James/0000-0003-2481-9988 FU U.S. National Science Foundation [DEB-0717220, DEB-0716923] FX This work was supported by the U.S. National Science Foundation (DEB-0717220 to JRV and DEB-0716923 to KMW). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 54 TC 14 Z9 14 U1 1 U2 46 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 17 PY 2012 VL 7 IS 10 AR e47495 DI 10.1371/journal.pone.0047495 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 038AF UT WOS:000311146900067 PM 23082171 ER PT J AU Freed, AM Blair, DM Watters, TR Klimczak, C Byrne, PK Solomon, SC Zuber, MT Melosh, HJ AF Freed, Andrew M. Blair, David M. Watters, Thomas R. Klimczak, Christian Byrne, Paul K. Solomon, Sean C. Zuber, Maria T. Melosh, H. J. TI On the origin of graben and ridges within and near volcanically buried craters and basins in Mercury's northern plains SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID LOBATE SCARPS; CALORIS BASIN; GLOBAL CONTRACTION; MESSENGER FLYBYS; GRAVITY-FIELD; TECTONICS; EVOLUTION; MOON; SURFACE; FLOW AB Images of Mercury's northern volcanic plains taken by the MESSENGER spacecraft reveal a large number of buried impact craters and basins discernible by wrinkle-ridge rings that overlie their rims. Many of these "ghost" craters and basins contain interior graben of diverse widths and orientations. Here we use finite element models to test a variety of mechanisms for the formation of these graben and ridges. Results show that graben are best explained by cooling of large thicknesses of flood lavas within the craters and basins; conservation of surface area during cooling induces the required extensional stress state. In contrast, the development of wrinkle-ridge rings is best explained as the result of cooling and contraction of Mercury's interior, during which a reduction in Mercury's surface area led to a compressional state of stress. The critical factor in determining where large graben form is the thickness of the youngest cooling unit, the topmost sequence of lavas that cooled coevally. A thicker cooling unit leads to a deeper initiation of normal faulting (wider graben floors). Consistent with observations, the widest graben are predicted to occur where pooled lavas were thickest, and no graben are predicted within generally thinner plains outside of major craters. Observed concentrically oriented graben can be explained by variations in the thickness of the youngest cooling unit. In contrast, none of the basin uplift mechanisms considered, including isostatic response to crater topography, inward flow of the lower crust, or exterior loading by volcanic plains, can account for concentrically oriented graben. C1 [Freed, Andrew M.; Blair, David M.; Melosh, H. J.] Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Klimczak, Christian; Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Earth Inst, Lamont Doherty Earth Observ, Palisades, NY USA. [Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. RP Freed, AM (reprint author), Purdue Univ, Dept Earth Atmospher & Planetary Sci, W Lafayette, IN 47907 USA. EM freed@purdue.edu FU NASA Discovery Program [NASW-00002, NAS5-97271]; NASA grant [PGG09-0053] FX The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. This work was also supported by NASA grant PGG09-0053 (AMF). NR 47 TC 12 Z9 12 U1 0 U2 13 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 OCT 17 PY 2012 VL 117 AR E00L06 DI 10.1029/2012JE004119 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 023ZK UT WOS:000310076400001 ER PT J AU Turner, BL Cheesman, AW Godage, HY Riley, AM Potter, BVL AF Turner, Benjamin L. Cheesman, Alexander W. Godage, H. Yasmin Riley, Andrew M. Potter, Barry V. L. TI Response to Comment on "Determination of neo- and D-chiro-Inositol Hexakisphosphate in Soils by Solution P-31 NMR Spectroscopy" SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Letter ID MUCO-INOSITOL C1 [Turner, Benjamin L.; Cheesman, Alexander W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Godage, H. Yasmin; Riley, Andrew M.; Potter, Barry V. L.] Univ Bath, Wolfson Lab Med Chem, Dept Pharm & Pharmacol, Bath BA2 7AY, Avon, England. 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; Riley, Andrew/F-3526-2013; Cheesman, Alexander/H-5918-2013 OI Turner, Benjamin/0000-0002-6585-0722; Cheesman, Alexander/0000-0003-3931-5766 NR 4 TC 1 Z9 1 U1 0 U2 16 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD OCT 16 PY 2012 VL 46 IS 20 BP 11480 EP 11481 DI 10.1021/es303737m PG 2 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 020JO UT WOS:000309805000086 ER PT J AU Denk, D Stidworthy, MF Redrobe, S Latimer, E Hayward, GS Cracknell, J Claessens, A Steinbach, F McGowan, S Dastjerdi, A AF Denk, Daniela Stidworthy, Mark F. Redrobe, Sharon Latimer, Erin Hayward, Gary S. Cracknell, Jonathan Claessens, Anais Steinbach, Falko McGowan, Sarah Dastjerdi, Akbar TI Fatal elephant endotheliotropic herpesvirus type 5 infection in a captive Asian elephant SO VETERINARY RECORD LA English DT Letter ID MAXIMUS C1 [Denk, Daniela; Stidworthy, Mark F.] IZVG Pathol, Leeds LS19 7XY, W Yorkshire, England. [Redrobe, Sharon] E Midland Zool Soc, Twycross Zoo, Atherstone CV9 3PX, Warwick, England. [Latimer, Erin] Natl Zool Pk, Natl Elephant Herpesvirus Lab, Smithsonian Conservat Biol Inst, Dept Pathol, Washington, DC 20008 USA. [Hayward, Gary S.] Johns Hopkins Sch Med, Viral Oncol Program, Baltimore, MD USA. [Cracknell, Jonathan] Longleat Safari & Adventure Pk, Longleat BA12 7NJ, Wilts, England. [Claessens, Anais; Steinbach, Falko; McGowan, Sarah; Dastjerdi, Akbar] AHVLA Weybridge, Dept Virol, New Haw, Addlestone KT15 3NB, Surrey, England. RP Denk, D (reprint author), IZVG Pathol, Gateway Dr, Leeds LS19 7XY, W Yorkshire, England. EM d.denk@izvg.co.uk RI Steinbach, Falko/C-8249-2011; Dastjerdi, Akbar/E-1803-2011; McGowan, Sarah/J-5410-2014; APHA, Staff publications/E-6082-2010 NR 9 TC 7 Z9 7 U1 2 U2 14 PU BRITISH VETERINARY ASSOC PI LONDON PA 7 MANSFIELD ST, LONDON W1M 0AT, ENGLAND SN 0042-4900 J9 VET REC JI Vet. Rec. PD OCT 13 PY 2012 VL 171 IS 15 BP 380 EP 381 DI 10.1136/vr.e6833 PG 2 WC Veterinary Sciences SC Veterinary Sciences GA 020LN UT WOS:000309810100021 PM 23065589 ER PT J AU Prettyman, TH Mittlefehldt, DW Yamashita, N Lawrence, DJ Beck, AW Feldman, WC McCoy, TJ McSween, HY Toplis, MJ Titus, TN Tricarico, P Reedy, RC Hendricks, JS Forni, O Le Corre, L Li, JY Mizzon, H Reddy, V Raymond, CA Russell, CT AF Prettyman, Thomas H. Mittlefehldt, David W. Yamashita, Naoyuki Lawrence, David J. Beck, Andrew W. Feldman, William C. McCoy, Timothy J. McSween, Harry Y. Toplis, Michael J. Titus, Timothy N. Tricarico, Pasquale Reedy, Robert C. Hendricks, John S. Forni, Olivier Le Corre, Lucille Li, Jian-Yang Mizzon, Hugau Reddy, Vishnu Raymond, Carol A. Russell, Christopher T. TI Elemental Mapping by Dawn Reveals Exogenic H in Vesta's Regolith SO SCIENCE LA English DT Article ID ASTEROID 4 VESTA; BASALTIC ACHONDRITE; GAMMA-RAY; MINERALOGY; METEORITES; MISSION; WATER AB Using Dawn's Gamma Ray and Neutron Detector, we tested models of Vesta's evolution based on studies of howardite, eucrite, and diogenite (HED) meteorites. Global Fe/O and Fe/Si ratios are consistent with HED compositions. Neutron measurements confirm that a thick, diogenitic lower crust is exposed in the Rheasilvia basin, which is consistent with global magmatic differentiation. Vesta's regolith contains substantial amounts of hydrogen. The highest hydrogen concentrations coincide with older, low-albedo regions near the equator, where water ice is unstable. The young, Rheasilvia basin contains the lowest concentrations. These observations are consistent with gradual accumulation of hydrogen by infall of carbonaceous chondrites-observed as clasts in some howardites-and subsequent removal or burial of this material by large impacts. C1 [Prettyman, Thomas H.; Yamashita, Naoyuki; Feldman, William C.; Tricarico, Pasquale; Reedy, Robert C.; Li, Jian-Yang] Planetary Sci Inst, Tucson, AZ 85719 USA. [Mittlefehldt, David W.] NASA, Johnson Space Ctr, Houston, TX 77058 USA. [Lawrence, David J.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Beck, Andrew W.; McCoy, Timothy J.] Smithsonian Inst, Washington, DC 20560 USA. [McSween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Toplis, Michael J.; Forni, Olivier; Mizzon, Hugau] Univ Toulouse, CNRS, Inst Rech Astrophys & Planetol, Toulouse, France. [Titus, Timothy N.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Hendricks, John S.] TechSource, Los Alamos, NM 87544 USA. [Le Corre, Lucille; Reddy, Vishnu] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Reddy, Vishnu] Univ N Dakota, Dept Space Studies, Grand Forks, ND USA. [Raymond, Carol A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Russell, Christopher T.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. RP Prettyman, TH (reprint author), Planetary Sci Inst, 1700 E Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM prettyman@psi.edu RI Russell, Christopher/E-7745-2012; Lujan Center, LANL/G-4896-2012; Beck, Andrew/J-7215-2015; Lawrence, David/E-7463-2015; OI Russell, Christopher/0000-0003-1639-8298; Beck, Andrew/0000-0003-4455-2299; Lawrence, David/0000-0002-7696-6667; Forni, Olivier/0000-0001-6772-9689; Reedy, Robert/0000-0002-2189-1303; Reddy, Vishnu/0000-0002-7743-3491; Prettyman, Thomas/0000-0003-0072-2831; Le Corre, Lucille/0000-0003-0349-7932 FU Jet Propulsion Laboratory (JPL), California Institute of Technology; NASA; NASA Dawn Participating Scientist Program; NASA Discovery Program Office FX We thank the Dawn team for spacecraft and instrument operations at Vesta. Portions of this work were performed by the Planetary Science Institute under contract with the Jet Propulsion Laboratory (JPL), California Institute of Technology; by JPL under contract with NASA; and by the NASA Dawn Participating Scientist Program. D. Bazell and P. Peplowski of Johns Hopkins University Applied Physics Laboratory assisted in fast-neutron data analysis. The Dawn mission is led by the University of California, Los Angeles, and managed by JPL under the auspices of the NASA Discovery Program Office. The Dawn data are archived with the NASA Planetary Data System. NR 36 TC 107 Z9 108 U1 7 U2 28 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 12 PY 2012 VL 338 IS 6104 BP 242 EP 246 DI 10.1126/science.1225354 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 019BQ UT WOS:000309712300042 PM 22997135 ER PT J AU Denevi, BW Blewett, DT Buczkowski, DL Capaccioni, F Capria, MT De Sanctis, MC Garry, WB Gaskell, RW Le Corre, L Li, JY Marchi, S McCoy, TJ Nathues, A O'Brien, DP Petro, NE Pieters, CM Preusker, F Raymond, CA Reddy, V Russell, CT Schenk, P Scully, JEC Sunshine, JM Tosi, F Williams, DA Wyrick, D AF Denevi, B. W. Blewett, D. T. Buczkowski, D. L. Capaccioni, F. Capria, M. T. De Sanctis, M. C. Garry, W. B. Gaskell, R. W. Le Corre, L. Li, J. -Y. Marchi, S. McCoy, T. J. Nathues, A. O'Brien, D. P. Petro, N. E. Pieters, C. M. Preusker, F. Raymond, C. A. Reddy, V. Russell, C. T. Schenk, P. Scully, J. E. C. Sunshine, J. M. Tosi, F. Williams, D. A. Wyrick, D. TI Pitted Terrain on Vesta and Implications for the Presence of Volatiles SO SCIENCE LA English DT Article ID CARBONACEOUS CHONDRITES; ASTEROID 4-VESTA; CERES; DAWN; MARS AB We investigated the origin of unusual pitted terrain on asteroid Vesta, revealed in images from the Dawn spacecraft. Pitted terrain is characterized by irregular rimless depressions found in and around several impact craters, with a distinct morphology not observed on other airless bodies. Similar terrain is associated with numerous martian craters, where pits are thought to form through degassing of volatile-bearing material heated by the impact. Pitted terrain on Vesta may have formed in a similar manner, which indicates that portions of the surface contain a relatively large volatile component. Exogenic materials, such as water-rich carbonaceous chondrites, may be the source of volatiles, suggesting that impactor materials are preserved locally in relatively high abundance on Vesta and that impactor composition has played an important role in shaping the asteroid's geology. C1 [Denevi, B. W.; Blewett, D. T.; Buczkowski, D. L.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Capaccioni, F.; Capria, M. T.; De Sanctis, M. C.; Tosi, F.] Ist Nazl Astrofis, Ist Astrofis & Planetol Spaziali, Rome, Italy. [Garry, W. B.; Gaskell, R. W.; Li, J. -Y.; O'Brien, D. P.] Planetary Sci Inst, Tucson, AZ USA. [Le Corre, L.; Nathues, A.; Reddy, V.] Max Planck Inst Solar Syst Res, Katlenburg Lindau, Germany. [Li, J. -Y.; Sunshine, J. M.] Univ Maryland, College Pk, MD 20742 USA. [Marchi, S.] NASA, Lunar Sci Inst, Boulder, CO USA. [McCoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Petro, N. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Pieters, C. M.] Brown Univ, Providence, RI 02912 USA. [Preusker, F.] Deutsch Zentrum Luft & Raumfahrt DLR, Inst Planetary Res, Berlin, Germany. [Raymond, C. A.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Reddy, V.] Univ N Dakota, Grand Forks, ND 58201 USA. [Russell, C. T.; Scully, J. E. C.] Univ Calif Los Angeles, Los Angeles, CA USA. [Schenk, P.] Lunar & Planetary Inst, Houston, TX 77058 USA. [Williams, D. A.] Arizona State Univ, Tempe, AZ USA. [Wyrick, D.] SW Res Inst, San Antonio, TX USA. RP Denevi, BW (reprint author), Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. EM brett.denevi@jhuapl.edu RI Denevi, Brett/I-6502-2012; Russell, Christopher/E-7745-2012; Petro, Noah/F-5340-2013; Garry, Brent/I-5920-2013; De Sanctis, Maria Cristina/G-5232-2013; Blewett, David/I-4904-2012; Buczkowski, Debra/I-7842-2015; OI Capaccioni, Fabrizio/0000-0003-1631-4314; Le Corre, Lucille/0000-0003-0349-7932; Tosi, Federico/0000-0003-4002-2434; Denevi, Brett/0000-0001-7837-6663; Russell, Christopher/0000-0003-1639-8298; De Sanctis, Maria Cristina/0000-0002-3463-4437; Blewett, David/0000-0002-9241-6358; Buczkowski, Debra/0000-0002-4729-7804; capria, maria teresa/0000-0002-9814-9588; Reddy, Vishnu/0000-0002-7743-3491 FU Dawn at Vesta Participating Scientist program; NASA; Italian Space Agency FX We thank the Dawn Science, Instrument, and Operations Teams and the Dawn at Vesta Participating Scientist program for support. A portion of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and portions were supported by the Italian Space Agency. Dawn data are archived with the NASA Planetary Data System. NR 28 TC 43 Z9 44 U1 2 U2 22 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD OCT 12 PY 2012 VL 338 IS 6104 BP 246 EP 249 DI 10.1126/science.1225374 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 019BQ UT WOS:000309712300043 PM 22997131 ER PT J AU Allevato, V Finoguenov, A Hasinger, G Miyaji, T Cappelluti, N Salvato, M Zamorani, G Gilli, R George, MR Tanaka, M Brusa, M Silverman, J Civano, F Elvis, M Shankar, F AF Allevato, V. Finoguenov, A. Hasinger, G. Miyaji, T. Cappelluti, N. Salvato, M. Zamorani, G. Gilli, R. George, M. R. Tanaka, M. Brusa, M. Silverman, J. Civano, F. Elvis, M. Shankar, F. TI OCCUPATION OF X-RAY-SELECTED GALAXY GROUPS BY X-RAY ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: active; large-scale structure of universe; quasars: general; surveys; X-rays: general ID WIDE-FIELD SURVEY; SUPERMASSIVE BLACK-HOLES; LUMINOUS RED GALAXIES; SIMILAR-TO 1; CROSS-CORRELATION FUNCTION; LARGE-SCALE STRUCTURE; DARK-MATTER HALOES; DIGITAL SKY SURVEY; COSMOS FIELD; COSMOLOGICAL EVOLUTION AB We present the first direct measurement of the mean halo occupation distribution (HOD) of X-ray-selected active galactic nuclei (AGNs) in the COSMOS field at z <= 1, based on the association of 41 XMM and 17 C-COSMOS AGNs with member galaxies of 189 X-ray-detected galaxy groups from XMM-Newton and Chandra data. We model the mean AGN occupation in the halo mass range log M-200 [M-circle dot] = 13-14.5 with a rolling-off power law with the best-fit index alpha = 0.06(-0.22; 0.36) and normalization parameter f(a) = 0.05(0.04; 0.06). We find the mean HOD of AGNs among central galaxies to be modeled by a softened step function at log M-h > log M-min = 12.75(12.10, 12.95) M-circle dot while for the satellite AGN HOD we find a preference for an increasing AGN fraction with M-h, suggesting that the average number of AGNs in satellite galaxies grows slower (alpha(s) < 0.6) than the linear proportion (alpha(s) = 1) observed for the satellite HOD of samples of galaxies. We present an estimate of the projected autocorrelation function (ACF) of galaxy groups over the range of r(p) = 0.1-40 h(-1) Mpc at < z > = 0.5. We use the large-scale clustering signal to verify the agreement between the group bias estimated by using the observed galaxy groups ACF and the value derived from the group mass estimates. We perform a measurement of the projected AGN-galaxy-group cross-correlation function, excluding from the analysis AGNs that are within galaxy groups and we model the two-halo term of the clustering signal with the mean AGN HOD based on our results. C1 [Allevato, V.] Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Allevato, V.; Salvato, M.; Brusa, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Allevato, V.; Salvato, M.] Excellence Cluster Universe, D-85748 Garching, Germany. [Finoguenov, A.] Univ Helsinki, Dept Phys, FI-00014 Helsinki, Finland. [Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Hasinger, G.; Cappelluti, N.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Miyaji, T.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Miyaji, T.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Cappelluti, N.; Zamorani, G.; Gilli, R.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [George, M. R.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [George, M. R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Tanaka, M.; Silverman, J.] Univ Tokyo, Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Civano, F.; Elvis, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Shankar, F.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92195 Meudon, France. RP Allevato, V (reprint author), Max Planck Inst Plasma Phys, Boltzmannstr 2, D-85748 Garching, Germany. RI Gilli, Roberto/P-1110-2015; OI Gilli, Roberto/0000-0001-8121-6177; Cappelluti, Nico/0000-0002-1697-186X; Zamorani, Giovanni/0000-0002-2318-301X; Brusa, Marcella/0000-0002-5059-6848 NR 94 TC 25 Z9 25 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 47 DI 10.1088/0004-637X/758/1/47 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500047 ER PT J AU Binder, B Williams, BF Eracleous, M Gaetz, TJ Plucinsky, PP Skillman, ED Dalcanton, JJ Anderson, SF Weisz, DR Kong, AKH AF Binder, B. Williams, B. F. Eracleous, M. Gaetz, T. J. Plucinsky, P. P. Skillman, E. D. Dalcanton, J. J. Anderson, S. F. Weisz, D. R. Kong, A. K. H. TI THE CHANDRA LOCAL VOLUME SURVEY: THE X-RAY POINT-SOURCE CATALOG OF NGC 300 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual: NGC 300; galaxies: spiral; X-rays: binaries; X-rays: galaxies ID NEARBY SPIRAL-GALAXIES; SMALL-MAGELLANIC-CLOUD; SCULPTOR GROUP GALAXIES; STAR-FORMATION HISTORY; LUMINOSITY FUNCTION; SUPERNOVA-REMNANTS; ACIS SURVEY; ADVANCED CAMERA; M33 CHASEM33; DARK-MATTER AB We present the source catalog of a new Chandra ACIS-I observation of NGC 300 obtained as part of the Chandra Local Volume Survey. Our 63 ks exposure covers similar to 88% of the D-25 isophote (R approximate to 6.3 kpc) and yields a catalog of 95 X-ray point sources detected at high significance to a limiting unabsorbed 0.35-8 keV luminosity of similar to 10(36) erg s(-1). Sources were cross-correlated with a previous XMM-Newton catalog, and we find 75 "X-ray transient candidate" sources that were detected by one observatory, but not the other. We derive an X-ray scale length of 1.7 +/- 0.2 kpc and a recent star formation rate of 0.12 M-circle dot yr (1) in excellent agreement with optical observations. Deep, multi-color imaging from the Hubble Space Telescope, covering similar to 32% of our Chandra field, was used to search for optical counterparts to the X-ray sources, and we have developed a new source classification scheme to determine which sources are likely X-ray binaries, supernova remnants, and background active galactic nucleus candidates. Finally, we present the X-ray luminosity functions (XLFs) at different X-ray energies, and we find the total NGC 300 X-ray point-source population to be consistent with other late-type galaxies hosting young stellar populations (less than or similar to 50 Myr). We find that XLF of sources associated with older stellar populations has a steeper slope than the XLF of X-ray sources coinciding with young stellar populations, consistent with theoretical predictions. C1 [Binder, B.; Williams, B. F.; Dalcanton, J. J.; Anderson, S. F.; Weisz, D. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Eracleous, M.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Gaetz, T. J.; Plucinsky, P. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Skillman, E. D.] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. RP Binder, B (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. FU National Aeronautics and Space Administration [G01-12118X]; Chandra X-ray Observatory Center; National Aeronautics Space Administration [NAS8-03060]; NASA [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G01-12118X 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. T.J.G. and P. P. P. acknowledge support under NASA contract NAS8-03060. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 59 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 15 DI 10.1088/0004-637X/758/1/15 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500015 ER PT J AU Bogdan, A David, LP Jones, C Forman, WR Kraft, RP AF Bogdan, Akos David, Laurence P. Jones, Christine Forman, William R. Kraft, Ralph P. TI THE DIVERSE HOT GAS CONTENT AND DYNAMICS OF OPTICALLY SIMILAR LOW-MASS ELLIPTICAL GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 821, NGC 3379, NGC 4278, NGC 4697); galaxies: ISM; X-rays: galaxies; X-rays: general; X-rays: ISM ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEUS; DIGITAL SKY SURVEY; XMM-NEWTON; STELLAR POPULATIONS; LUMINOSITY FUNCTION; M31 BULGE; NGC 3379; EMISSION; CHANDRA AB The presence of hot X-ray-emitting gas is ubiquitous in massive early-type galaxies. However, much less is known about the content and physical status of the hot X-ray gas in low-mass ellipticals. In the present paper, we study the X-ray gas content of four low-mass elliptical galaxies using archival Chandra X-ray observations. The sample galaxies, NGC 821, NGC 3379, NGC 4278, and NGC 4697, have approximately identical K-band luminosities, and hence stellar masses, yet their X-ray appearance is strikingly different. We conclude that the unresolved emission in NGC 821 and NGC 3379 is built up from a multitude of faint compact objects, such as coronally active binaries and cataclysmic variables. Despite the non-detection of X-ray gas, these galaxies may host low density, and hence low luminosity, X-ray gas components, which undergo an outflow driven by a Type Ia supernova (SN Ia). We detect hot X-ray gas with a temperature of kT similar to 0.35 keV in NGC 4278, the component of which has a steeper surface brightness distribution than the stellar light. Within the central 50 '' (similar to 3.9 kpc), the estimated gas mass is similar to 3 x 10(7) M-circle dot, implying a gas mass fraction of similar to 0.06%. We demonstrate that the X-ray gas exhibits a bipolar morphology in the northeast-southwest direction, indicating that it may be outflowing from the galaxy. The mass and energy budget of the outflow can be maintained by evolved stars and SNe Ia, respectively. The X-ray gas in NGC 4697 has an average temperature of kT similar to 0.3 keV and a significantly broader distribution than the stellar light. The total gas mass within 90 '' (similar to 5.1 kpc) is similar to 2.1 x 10(8) M-circle dot, hence the gas mass fraction is similar to 0.4%. Based on the distribution and physical parameters of the X-ray gas, we conclude that it is most likely in hydrostatic equilibrium, although a subsonic outflow may be present. C1 [Bogdan, Akos; David, Laurence P.; Jones, Christine; Forman, William R.; Kraft, Ralph P.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 FU National Aeronautics and Space Administration [NAS8-03060]; National Science Foundation; NASA through Einstein Postdoctoral Fellowship by the Chandra X-ray Center [PF1-120081]; Smithsonian Institution FX A.B. thanks Alexey Vikhlinin, Marat Gilfanov, and Junfeng Wang for helpful discussions. This research has made use of Chandra data provided by the Chandra X-ray Center. The publication makes use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. In this work, the NASA/IPAC Extragalactic Database (NED) has been used. The authors acknowledge the use of the HyperLeda database (http://leda.univ-lyon1.fr). A.B. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant No. PF1-120081 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. W.F. and C.J. acknowledge support from the Smithsonian Institution. NR 47 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 65 DI 10.1088/0004-637X/758/1/65 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500065 ER PT J AU Conroy, C AF Conroy, Charlie TI ON THE BIRTH MASSES OF THE ANCIENT GLOBULAR CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: general ID MULTIPLE STELLAR POPULATIONS; SELF-ENRICHMENT SCENARIO; ASYMPTOTIC GIANT BRANCH; LARGE-MAGELLANIC-CLOUD; NA-O ANTICORRELATION; DOUBLE MAIN-SEQUENCE; LUMINOUS STAR-CLUSTERS; OMEGA-CENTAURI; ABUNDANCE VARIATIONS; DYNAMICAL EVOLUTION AB All globular clusters (GCs) studied to date show evidence for internal (star-to-star) variation in their light-element abundances (including Li, C, N, O, F, Na, Mg, Al, and probably He). These variations have been interpreted as evidence for multiple star formation episodes within GCs, with secondary episodes fueled, at least in part, by the ejecta of asymptotic giant branch (AGB) stars from a first generation of stars. A major puzzle emerging from this otherwise plausible scenario is that the fraction of stars associated with the second episode of star formation is observed to be much larger than expected for a standard initial mass function. The present work investigates this tension by modeling the observed anti-correlation between [Na/Fe] and [O/Fe] for 20 Galactic GCs. If the abundance pattern of the retained AGB ejecta does not depend on GC mass at fixed [Fe/H], then a strong correlation is found between the fraction of current GC stellar mass composed of pure AGB ejecta, f(p), and GC mass. This fraction varies from 0.20 at low masses (10(4.5) M-circle dot) to 0.45 at high masses (10(6.5) M-circle dot). The fraction of mass associated with pure AGB ejecta is directly related to the total mass of the cluster at birth; the ratio between the initial and present mass in stars can therefore be derived. Assuming a star formation efficiency of 50%, the observed Na-O anti-correlations imply that GCs were at least 10-20 times more massive at birth, a conclusion that is in qualitative agreement with previous work. These factors are lower limits because any mass-loss mechanism that removes first- and second-generation stars equally will leave f(p) unchanged. The mass dependence of f(p) probably arises because lower mass GCs are unable to retain all of the AGB ejecta from the first stellar generation. Recent observations of elemental abundances in intermediate-age Large Magellanic Cloud clusters are re-interpreted and shown to be consistent with this basic scenario. The small scatter in f(p) at fixed GC mass argues strongly that the process responsible for the large mass loss is internal to GCs. A satisfactory explanation of these trends is currently lacking. C1 [Conroy, Charlie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Conroy, Charlie] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Conroy, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 104 TC 34 Z9 34 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 21 DI 10.1088/0004-637X/758/1/21 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500021 ER PT J AU High, FW Hoekstra, H Leethochawalit, N de Haan, T Abramson, L Aird, KA Armstrong, R Ashby, MLN Bautz, M Bayliss, M Bazin, G Benson, BA Bleem, LE Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Conroy, M Crawford, TM Crites, AT Desai, S Dobbs, MA Dudley, JP Foley, RJ Forman, WR George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McDonald, M McMahon, JJ Mehl, J Meyer, SS Mocanu, L Mohr, JJ Montroy, TE Murray, SS Natoli, T Nurgaliev, D Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Schrabback, T Shirokoff, E Song, J Spieler, HG Stalder, B Staniszewski, Z Stark, AA Story, K Stubbs, CW Suhada, R Tokarz, S van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF High, F. W. Hoekstra, H. Leethochawalit, N. de Haan, T. Abramson, L. Aird, K. A. Armstrong, R. Ashby, M. L. N. Bautz, M. Bayliss, M. Bazin, G. Benson, B. A. Bleem, L. E. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Conroy, M. Crawford, T. M. Crites, A. T. Desai, S. Dobbs, M. A. Dudley, J. P. Foley, R. J. Forman, W. R. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. 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. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McDonald, M. McMahon, J. J. Mehl, J. Meyer, S. S. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Natoli, T. Nurgaliev, D. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Schrabback, T. Shirokoff, E. Song, J. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Suhada, R. Tokarz, S. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI WEAK-LENSING MASS MEASUREMENTS OF FIVE GALAXY CLUSTERS IN THE SOUTH POLE TELESCOPE SURVEY USING MAGELLAN/MEGACAM SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: clusters: individual ID DIGITAL SKY SURVEY; X-RAY-PROPERTIES; DARK-MATTER; PHOTOMETRIC REDSHIFTS; COSMOLOGICAL CONSTRAINTS; HALO CONCENTRATIONS; SCALING RELATIONS; OBSERVED GROWTH; CATALOG; PROFILE AB We use weak gravitational lensing to measure the masses of five galaxy clusters selected from the South Pole Telescope (SPT) survey, with the primary goal of comparing these with the SPT Sunyaev-Zel'dovich (SZ) and X-ray-based mass estimates. The clusters span redshifts 0.28 < z < 0.43 and have masses M-500 > 2 x 10(14) h(-1)M(circle dot), and three of the five clusters were discovered by the SPT survey. We observed the clusters in the g'r'i' passbands with the Megacam imager on the Magellan Clay 6.5 m telescope. We measure a mean ratio of weak-lensing (WL) aperture masses to inferred aperture masses from the SZ data, both within an aperture of R-500,R-SZ derived from the SZ mass, of 1.04 +/- 0.18. We measure a mean ratio of spherical WL masses evaluated at R-500,R-SZ to spherical SZ masses of 1.07 +/- 0.18, and a mean ratio of spherical WL masses evaluated at R-500,R-WL to spherical SZ masses of 1.10 +/- 0.24. We explore potential sources of systematic error in the mass comparisons and conclude that all are subdominant to the statistical uncertainty, with dominant terms being cluster concentration uncertainty and N-body simulation calibration bias. Expanding the sample of SPT clusters with WL observations has the potential to significantly improve the SPT cluster mass calibration and the resulting cosmological constraints from the SPT cluster survey. These are the first WL detections using Megacam on the Magellan Clay telescope. C1 [High, F. W.; Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [High, F. W.; Abramson, L.; Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Hoekstra, H.] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Leethochawalit, N.; Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Armstrong, R.] Univ Illinois, Natl Ctr Supercomp Applicat, Urbana, IL 61801 USA. [Ashby, M. L. N.; Conroy, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.; Tokarz, S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bautz, M.; McDonald, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bayliss, M.; Nurgaliev, D.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; McMahon, J. J.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] 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 Phys, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Joy, M.] NASA, Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schrabback, T.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. RP High, FW (reprint author), Univ Chicago, Kavli Inst Cosmol Phys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM fwhigh@kicp.uchicago.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; OI Williamson, Ross/0000-0002-6945-2975; Stubbs, Christopher/0000-0003-0347-1724; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Hoekstra, Henk/0000-0002-0641-3231; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; Marie Curie IRG [230924]; Netherlands Organisation for Scientific Research (NWO) [639.042.814]; Excellence Cluster Universe; DFG research program [TR33]; NSF [AST-1009012, AST-1009649, MRI-0723073]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Clay fellowship; Smithsonian Astrophysical Observatory 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. H.H. acknowledges support from Marie Curie IRG grant 230924 and the Netherlands Organisation for Scientific Research (NWO) grant No. 639.042.814. The Munich group acknowledges support from the Excellence Cluster Universe and the DFG research program TR33 The Dark Universe. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012, and 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. R.J.F. is supported by a Clay fellowship.; This paper used data products produced by the OIR Telescope Data Center, supported by the Smithsonian Astrophysical Observatory. NR 80 TC 30 Z9 30 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 OCT 10 PY 2012 VL 758 IS 1 AR 68 DI 10.1088/0004-637X/758/1/68 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500068 ER PT J AU Hwang, HS Geller, MJ Kurtz, MJ Dell'Antonio, IP Fabricant, DG AF Hwang, Ho Seong Geller, Margaret J. Kurtz, Michael J. Dell'Antonio, Ian P. Fabricant, Daniel G. TI SHELS: OPTICAL SPECTRAL PROPERTIES OF WISE 22 mu m SELECTED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; galaxies: starburst; infrared: galaxies; surveys ID DIGITAL SKY SURVEY; LUMINOUS INFRARED GALAXIES; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; SIMILAR-TO 2; EMISSION-LINE GALAXIES; FIBER-FED SPECTROGRAPH; BRIGHT 10K CATALOG; DEEP LENS SURVEY; MU-M AB We use a dense, complete redshift survey, the Smithsonian Hectospec Lensing Survey (SHELS), covering a 4 deg(2) region of a deep imaging survey, the Deep Lens Survey (DLS), to study the optical spectral properties of Wide-field Infrared Survey Explorer (WISE) 22 mu m selected galaxies. Among 507 WISE 22 mu m selected sources with (S/N)(22 mu m) >= 3 (approximate to S-22 mu m greater than or similar to 2.5 mJy), we identify the optical counterparts of 481 sources (similar to 98%) at R < 25.2 in the very deep, DLS R-band source catalog. Among them, 337 galaxies at R < 21 have SHELS spectroscopic data. Most of these objects are at z < 0.8. The infrared (IR) luminosities are in the range 4.5 x 10(8)(L-circle dot) less than or similar to L-IR less than or similar to 5.4 x 10(12)(L-circle dot). Most 22 mu m selected galaxies are dusty star-forming galaxies with a small (<1.5) 4000 angstrom break. The stacked spectra of the 22 mu m selected galaxies binned in IR luminosity show that the strength of the [O III] line relative to H beta grows with increasing IR luminosity. The optical spectra of the 22 mu m selected galaxies also show that there are some (similar to 2.8%) unusual galaxies with very strong [Ne III] lambda 3869, 3968 emission lines that require hard ionizing radiation such as active galactic nuclei (AGNs) or extremely young massive stars. The specific star formation rates (sSFRs) derived from the 3.6 and 22 mu m flux densities are enhanced if the 22 mu m selected galaxies have close late-type neighbors. The sSFR distribution of the 22 mu m selected galaxies containing AGNs is similar to the distribution for star-forming galaxies without AGNs. We identify 48 dust-obscured galaxy candidates with large (greater than or similar to 1000) mid-IR to optical flux density ratio. The combination of deep photometric and spectroscopic data with WISE data suggests that WISE can probe the universe to z similar to 2. C1 [Hwang, Ho Seong; Geller, Margaret J.; Kurtz, Michael J.; Fabricant, Daniel G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dell'Antonio, Ian P.] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Hwang, HS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hhwang@cfa.harvard.edu; mgeller@cfa.harvard.edu; mkurtz@cfa.harvard.edu; ian@het.brown.edu; dfabricant@cfa.harvard.edu FU Smithsonian Institution; NSF-AST [AST-0708433]; National Aeronautics and Space Administration FX We thank the anonymous referee for his/her useful comments that improved the original manuscript. We thank Scott Kenyon for carefully reading the manuscript and Jong Chul Lee for useful discussion. H. S. H. acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. The Smithsonian Institution also supports the research of M.J.G., M.J.K., and D.G.F.. I. P. D. is supported by NSF-AST grant AST-0708433. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 117 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 25 DI 10.1088/0004-637X/758/1/25 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500025 ER PT J AU Jonker, PG Heida, M Torres, MAP Miller-Jones, JCA Fabian, AC Ratti, EM Miniutti, G Walton, DJ Roberts, TP AF Jonker, P. G. Heida, M. Torres, M. A. P. Miller-Jones, J. C. A. Fabian, A. C. Ratti, E. M. Miniutti, G. Walton, D. J. Roberts, T. P. TI THE NATURE OF THE BRIGHT ULX X-2 IN NGC 3921: A CHANDRA POSITION AND HST CANDIDATE COUNTERPART SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; X-rays: binaries ID X-RAY SOURCE; HUBBLE-SPACE-TELESCOPE; MASS BLACK-HOLE; MILLENNIUM GALAXY CATALOG; TIDAL DISRUPTION EVENTS; DIGITAL SKY SURVEY; NEARBY GALAXIES; REDSHIFT SURVEY; ESO 243-49; PHOTOMETRIC EVOLUTION AB We report on Chandra observations of the bright ultraluminous X-ray (ULX) source in NGC 3921. Previous XMM-Newton observations reported in the literature show the presence of a bright ULX at a 0.5-10 keV luminosity of 2 x 10(40) erg s(-1). Our Chandra observation finds the source at a lower luminosity of approximate to 8 x 10(39) erg s(-1); furthermore, we provide a Chandra position of the ULX accurate to 0 ''.7 at 90% confidence. The X-ray variability makes it unlikely that the high luminosity is caused by several separate X-ray sources. In three epochs of archival Hubble Space Telescope observations, we find a candidate counterpart to the ULX. There is direct evidence for variability between the two epochs of WFPC2 F814W observations with the observation obtained in 2000 showing a brighter source. Furthermore, converting the 1994 F336W and 2000 F300W WFPC2 and the 2010 F336W WFC3 observations to the Johnson U-band filter assuming a spectral type of O7I, we find evidence for a brightening of the U-band light in 2000. Using the higher resolution WFC3 observations, we resolve the candidate counterpart into two sources of similar color. We discuss the nature of the ULX and the probable association with the optical counterpart(s). Finally, we investigate a potential new explanation for some (bright) ULXs as the decaying stages of flares caused by the tidal disruption of a star by a recoiled supermassive black hole. However, we find that there should be at most only one of such systems within z = 0.08. C1 [Jonker, P. G.; Heida, M.; Torres, M. A. P.; Ratti, E. M.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Heida, M.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller-Jones, J. C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Fabian, A. C.; Walton, D. J.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Miniutti, G.] ESA, Dept Astrofis, Ctr Astrobiol CSIC INTA, E-28691 Madrid, Spain. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Jonker, PG (reprint author), SRON, Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM p.jonker@sron.nl RI Miller-Jones, James/B-2411-2013; Miniutti, Giovanni/L-2721-2014 OI Miller-Jones, James/0000-0003-3124-2814; Miniutti, Giovanni/0000-0003-0707-4531 FU Netherlands Organisation for Scientific Research; MINECO [AYA2010-21490-C02-02]; NASA/NSF; ESA; NRC; CDS FX P.G.J. and M. A. P. T. acknowledge support from the Netherlands Organisation for Scientific Research. P.G.J. acknowledges discussions with Elena Rossi, Suvi Gezari, and Luca Zampieri on tidal disruption flares. P.G.J. further acknowledges Rasmus Voss for his comments on an earlier version of the manuscript. M. H., P.G.J., and M. A. P. T. acknowledge input from Dolphin on the HST photometry. G. M. thanks the Spanish Ministry of Science and Innovation (now MINECO) for support through grant AYA2010-21490-C02-02. This research used the HST Archive facilities of the STScI, the ST-ECF, and the CADC with the support of the following granting agencies: NASA/NSF, ESA, NRC, CSA. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; of NASA's Astrophysics Data System Bibliographic Services; of SAOImage DS9, developed by Smithsonian Astrophysical Observatory; of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO; and of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. NR 67 TC 9 Z9 9 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 28 DI 10.1088/0004-637X/758/1/28 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500028 ER PT J AU Liu, MC Dupuy, TJ Bowler, BP Leggett, SK Best, WMJ AF Liu, Michael C. Dupuy, Trent J. Bowler, Brendan P. Leggett, S. K. Best, William M. J. TI TWO EXTRAORDINARY SUBSTELLAR BINARIES AT THE T/Y TRANSITION AND THE Y-BAND FLUXES OF THE COOLEST BROWN DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: general; brown dwarfs; infrared: stars; techniques: high angular resolution ID STAR ADAPTIVE OPTICS; INFRARED FILTER SET; T-DWARFS; DYNAMICAL MASS; GIANT PLANETS; UGPS J072227.51-054031.2; PHOTOMETRIC SYSTEM; L/T TRANSITION; DISCOVERY; COMPANION AB Using Keck laser guide star adaptive optics imaging, we have found that the T9 dwarf WISE J1217+1626 and T8 dwarf WISE J1711+3500 are exceptional binaries, with unusually wide separations (approximate to 0 ''.8, 8-15 AU), large near-IR flux ratios (approximate to 2-3 mag), and small mass ratios (approximate to 0.5) compared to previously known field ultracool binaries. Keck/NIRSPEC H-band spectra give a spectral type of Y0 for WISE J1217+1626B, and photometric estimates suggest T9.5 for WISE J1711+3500B. The WISE J1217+1626AB system is very similar to the T9+Y0 binary CFBDSIR J1458+1013AB; these two systems are the coldest known substellar multiples, having secondary components of approximate to 400 K and being planetary-mass binaries if their ages are <= 1 Gyr. Both WISE J1217+1626B and CFBDSIR J1458+1013B have strikingly blue Y-J colors compared to previously known T dwarfs, including their T9 primaries. Combining all available data, we find that Y-J color drops precipitously between the very latest T dwarfs and the Y dwarfs. The fact that this is seen in (coeval, mono-metallicity) binaries demonstrates that the color drop arises from a change in temperature, not surface gravity or metallicity variations among the field population. Thus, the T/Y transition established by near-IR spectra coincides with a significant change in the approximate to 1 mu m fluxes of ultracool photospheres. One explanation is the depletion of potassium, whose broad absorption wings dominate the far-red optical spectra of T dwarfs. This large color change suggests that far-red data may be valuable for classifying objects of less than or similar to 500 K. C1 [Liu, Michael C.; Bowler, Brendan P.; Best, William M. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA. RP Liu, MC (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Leggett, Sandy/0000-0002-3681-2989 FU W. M. Keck Foundation; University of Hawaii [NNX-08AE38A]; National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program; National Aeronautics and Space Administration [NAS 5-26555]; NSF [AST09-09222]; NASA through Hubble Fellowship [HF-51271.01-A]; Space Telescope Science Institute FX Most 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.; Some of the observations were obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovaci'on Productiva (Argentina).; Visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program.; We thank Scott Dahm, Terry Stickel, Jim Lyke, and the Keck Observatory staff for assistance with LGS AO observing; the Gemini Observatory staff for obtaining the NIRI photometry through queue observing; and Kimberly Aller for assistance with the IRTF/SpeX observing. We thank Andrew Stephens for providing the Gemini/NIRI cold filter profile; James R. A. Davenport for distributing his IDL implementation of the Green (2011) "cubehelix" color scheme; Caroline Morley, Jonathan Fortney and collaborators for sharing results in advance of publication; and Didier Saumon and Isabelle Baraffe for providing expanded sets of evolutionary models. This publication makes use of data products from the Wide-Field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Our research has employed the 2MASS data products; NASA's Astrophysical Data System; the SIMBAD database operated at CDS, Strasbourg, France; and the Spex Prism Spectral Libraries maintained by Adam Burgasser at http://pono.ucsd.edu/similar to adam/browndwarfs/spexprism. This research was supported by NSF grant AST09-09222 awarded to M. C. L. Support for this work to T.J.D. was provided by NASA through Hubble Fellowship grant No. HF-51271.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Finally, the authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 73 TC 33 Z9 33 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 57 DI 10.1088/0004-637X/758/1/57 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500057 ER PT J AU Lohfink, AM Reynolds, CS Miller, JM Brenneman, LW Mushotzky, RF Nowak, MA Fabian, AC AF Lohfink, Anne M. Reynolds, Christopher S. Miller, Jon M. Brenneman, Laura W. Mushotzky, Richard F. Nowak, Michael A. Fabian, Andrew C. TI THE BLACK HOLE SPIN AND SOFT X-RAY EXCESS OF THE LUMINOUS SEYFERT GALAXY FAIRALL 9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: individual (Fairall 9); galaxies: nuclei; galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; EMISSION-LINES; IRON LINES; CYGNUS X-1; NGC 3783; ABSORPTION; MODELS; VARIABILITY; MCG-6-30-15; SYSTEMS AB We present an analysis of all XMM-Newton and Suzaku X-ray spectra of the nearby luminous Seyfert galaxy Fairall 9. Confirming previous analyses, we find robust evidence for a broad iron line associated with X-ray reflection from the innermost accretion disk. By fitting a spectral model that includes a relativistically ionized reflection component, we examine the constraints on the inclination of the inner accretion disk and the black hole spin, and the complications introduced by the presence of a photoionized emission line system. Employing multi-epoch fitting, we attempt to obtain robust and concordant measures of the accretion disk parameters. We also clearly see a soft X-ray excess in Fairall 9. During certain epochs, the soft excess can be described with the same disk reflection component that produces the iron line. However, there are epochs where an additional soft component is required. This can be attributed to either an additional highly ionized, strongly blurred disk reflection component or a new X-ray continuum component. C1 [Lohfink, Anne M.; Reynolds, Christopher S.; Mushotzky, Richard F.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lohfink, Anne M.; Reynolds, Christopher S.; Mushotzky, Richard F.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brenneman, Laura W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nowak, Michael A.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Lohfink, AM (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM alohfink@astro.umd.edu RI XRAY, SUZAKU/A-1808-2009 FU ESA Member States; USA (NASA); NASA through the Suzaku Cycle-5 Guest Observer Program [NNX10AR31G]; Astrophysical Data Analysis Program [NNX12AE13G] FX We thank the Suzaku Guest Observer Facility members for their help with the newest Suzaku pointing. The authors thank the anonymous referee for comments that improved this manuscript. 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; NASA's Astrophysics Data System Bibliographic Services, observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). A.M.L. and C.S.R. acknowledge support from NASA through the Suzaku Cycle-5 Guest Observer Program (grant NNX10AR31G) and the Astrophysical Data Analysis Program (grant NNX12AE13G). NR 34 TC 30 Z9 30 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 67 DI 10.1088/0004-637X/758/1/67 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500067 ER PT J AU Testa, P De Pontieu, B Martinez-Sykora, J Hansteen, V Carlsson, M AF Testa, Paola De Pontieu, Bart Martinez-Sykora, Juan Hansteen, Viggo Carlsson, Mats TI INVESTIGATING THE RELIABILITY OF CORONAL EMISSION MEASURE DISTRIBUTION DIAGNOSTICS USING THREE-DIMENSIONAL RADIATIVE MAGNETOHYDRODYNAMIC SIMULATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); methods: numerical; Sun: activity; Sun: corona; Sun: UV radiation; techniques: spectroscopic ID EUV IMAGING SPECTROMETER; SOLAR ACTIVE REGIONS; EXTREME-ULTRAVIOLET SPECTRA; TEMPERATURE STRUCTURE; ATOMIC DATABASE; HOT PLASMA; LOOPS OBSERVATIONS; DENSITY STRUCTURE; RAY TELESCOPE; QUIET-SUN AB Determining the temperature distribution of coronal plasmas can provide stringent constraints on coronal heating. Current observations with the Extreme ultraviolet Imaging Spectrograph (EIS) on board Hinode and the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory provide diagnostics of the emission measure distribution (EMD) of the coronal plasma. Here we test the reliability of temperature diagnostics using three-dimensional radiative MHD simulations. We produce synthetic observables from the models and apply the Monte Carlo Markov chain EMD diagnostic. By comparing the derived EMDs with the "true" distributions from the model, we assess the limitations of the diagnostics as a function of the plasma parameters and the signal-to-noise ratio of the data. We find that EMDs derived from EIS synthetic data reproduce some general characteristics of the true distributions, but usually show differences from the true EMDs that are much larger than the estimated uncertainties suggest, especially when structures with significantly different density overlap along the line of sight. When using AIA synthetic data the derived EMDs reproduce the true EMDs much less accurately, especially for broad EMDs. The differences between the two instruments are due to the: (1) smaller number of constraints provided by AIA data and (2) broad temperature response function of the AIA channels which provide looser constraints to the temperature distribution. Our results suggest that EMDs derived from current observatories may often show significant discrepancies from the true EMDs, rendering their interpretation fraught with uncertainty. These inherent limitations to the method should be carefully considered when using these distributions to constrain coronal heating. C1 [Testa, Paola] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [De Pontieu, Bart; Martinez-Sykora, Juan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, Juan; Hansteen, Viggo; Carlsson, Mats] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. RP Testa, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu NR 63 TC 26 Z9 26 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 10 PY 2012 VL 758 IS 1 AR 54 DI 10.1088/0004-637X/758/1/54 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016LS UT WOS:000309520500054 ER PT J AU Holland, ND Osborn, KJ Kuhnz, LA AF Holland, Nicholas D. Osborn, Karen J. Kuhnz, Linda A. TI A new deep-sea species of harrimaniid enteropneust (Hemichordata) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE collar nerve cord; Enteropneusta; Harrimaniidae; proboscis skeleton; seamount fauna ID ACORN WORMS HEMICHORDATA; EASTERN PACIFIC; GENUS; REVISION AB Ninety-two individuals of a deep-sea harrimaniid enteropneust were imaged between 1675 m and 3225 m off the California coast. Of these, about three-fourths were positioned with their posterior regions buried in sediment or hidden by rocks, and the rest were completely exposed on the substratum. When visible, the posterior end of each worm was typically associated with a dense tangle of fecal strands. One specimen was captured and is described here as the holotype of Saxipendium implication. In life, it was 22 cm long, and the color of its dome-shaped proboscis, narrow collar, and anterior trunk was medium orange. No wing-like folds of the body wall protruded anywhere along the length of the worm. The proboscis complex included a stomochord and glomeruli, but neither a heart nor a pericardial cavity could be detected. Most of the dorsal collar nerve runs along an open invagination in the dorsal midline of the collar and is only roofed over very briefly at the posterior extremity of the collar. Another unusual feature is the exaggerated posterior extension of the horns of the proboscis skeleton, which projected into the anterior extremity of the trunk. The trunk commenced anteriorly with a pharyngeal/esophageal region that included a tract of ovaries on either side of the dorsal midline. The ripest ovaries contained a single oocyte approximately 700 pm in diameter (presumably this species is gonochoric, although no males have yet been collected). The gill skeleton lacked synapticles. More posteriorly, the trunk housed a long, darkly pigmented hepatic intestine without sacculations and a short, lightly pigmented post-hepatic intestine. The geographic range of S. implicatum appears to be restricted to the Davidson, Guide, and Taney Seamounts region in the eastern Pacific offshore of Central California. C1 [Holland, Nicholas D.] Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. [Osborn, Karen J.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Kuhnz, Linda A.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Holland, ND (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Div Marine Biol Res, La Jolla, CA 92093 USA. EM nholland@ucsd.edu FU David and Lucile Packard Foundation FX We thank David Clague and Lonny Lundsten, respectively, for collecting and shipboard processing of the holotype. We are indebted to the crew of the MBARI R/V Western Flyer and the pilots of the ROVs Tiburon and Doc Ricketts for their skill and dedication to deep-sea biology. We are also grateful to Fredrik Pleijel for photographing the fixed holotype, to Antonina Rogacheva for supplying the reference to Belichov (1971), to Horst Felbeck for unpublished photographs of Saxipendium corona turn, and to Linda Holland for criticizing our manuscript. Our work was supported in part by the David and Lucile Packard Foundation. NR 21 TC 5 Z9 5 U1 0 U2 11 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 2012 VL 125 IS 3 BP 228 EP 240 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 025HB UT WOS:000310178100002 ER PT J AU Heyer, WR Heyer, MM AF Heyer, W. Ronald Heyer, Miriam M. TI Systematics, distribution, and bibliography of the frog Leptodactylus validus Garman, 1888 (Amphibia: Leptodactylidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Amphibia; amphibian bibliography; amphibian conservation; amphibian systematics; Leptodactylus validus ID LESSER ANTILLES; PARENTAL CARE; HERPETOFAUNAL COMMUNITIES; ANTIMICROBIAL PEPTIDES; MANNOPHRYNE-OLMONAE; ANNOTATED CHECKLIST; GENUS LEPTODACTYLUS; REPRODUCTIVE MODE; NATURAL-HISTORY; CARIBBEAN FROG AB Recent molecular studies demonstrate that the species Leptodactylus pallidirostris and L. validus are conspecific. Leptodactylus pallidirostris was previously considered to occupy portions of mainland South America (Venezuela, Guyana, Suriname, and French Guiana), whereas L. validus was considered to occur only on the islands of Trinidad, Tobago, and certain Lesser Antillian islands. The purpose of this paper is to summarize information for the currently understood single species Leptodactylus validus. C1 [Heyer, W. Ronald] Smithsonian Inst, Washington, DC 20013 USA. RP Heyer, WR (reprint author), Smithsonian Inst, MRC 162,POB 37012, Washington, DC 20013 USA. EM heyerr@si.edu NR 216 TC 0 Z9 1 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD OCT 9 PY 2012 VL 125 IS 3 BP 276 EP 294 PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 025HB UT WOS:000310178100006 ER PT J AU Solari, S Pacheco, V Vivar, E Emmons, LH AF Solari, Sergio Pacheco, Victor Vivar, Elena Emmons, Louise H. TI A new species of Monodelphis (Mammalia: Didelphimorphia: Didelphidae) from the montane forests of central Peru SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE biogeography; Monodelphis gardneri; systematics; taxonomy ID MARSUPIALIA; DIVERSIFICATION; SIGMODONTINAE AB With more than 20 recognized species, Monodelphis is the most species-rich genus of living Didelphidae. Recent research on these opossums revealed additional species from Peru and Venezuela, and herein we describe a new species from the montane forests of the eastern slope of the central Andes in Peril. Monodelphis gardneri, new species, is a small taxon with three black dorsal stripes, more similar in external appearance and cranial features to taxa from eastern Brazil, such as M. theresa or M. americana, than to Andean species, like M. osgoodi. Phylogenetic analyses of cytochrome h gene sequences recovered this new species as closer to M. americana from eastern Brazil than to M. theresa (another species in our analyses with three black dorsal stripes). In spite of this external resemblance, the molecular phylogeny indicates that species with dorsal stripes, including M. americana, M. theresa, and the new species, do not form a monophyletic group. Although weakly supported, a relationship between M. americana and the new species suggests a biogeographic connection between these disjunct distributions, i.e., from eastern Brazil and the eastern versant of the Andes. C1 [Solari, Sergio] Univ Antioquia, Inst Biol, Medellin 1226, Colombia. [Pacheco, Victor; Vivar, Elena] Univ Nacl Mayor San Marcos, Museo Hist Nat, Dept Mastozool, Lima 14, Peru. [Emmons, Louise H.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Solari, S (reprint author), Univ Antioquia, Inst Biol, Medellin 1226, Colombia. EM ssolari@matematicas.udea.edu.co OI Pacheco, Victor/0000-0002-1005-135X FU Texas Tech through a J. Knox Jones Memorial Fund; Cash Family Endowment; American Society of Mammalogists; CONCYTEC FX For loan of specimens and tissues relevant to this study, we thank R. S. Voss and E. Westwig (AMNH), B. D. Patterson and W. Stanley (FMNH), M. S. Hafner (LSUMZ), J. L. Patton and C. Cicero (Museum of Vertebrate Zoology, Berkeley), and R. J. Baker and H. Garner (Natural Science Research Laboratory, Texas Tech University, Lubbock). All molecular analyses were completed during the graduate studies of Solari at Texas Tech University, under guidance of R. J. Baker; we express our gratitude for facilitating use of the molecular lab. A. L. Gardner and D. E. Wilson (USNM) supported Solari during his visit to Washington, D.C. Support was provided by Texas Tech through a J. Knox Jones Memorial Fund (2004) and a Cash Family Endowment (2006). Solari was also supported by an Albert R. and Alma Shad le Fellowship (2005) and an ASM Fellowship (2006) from the American Society of Mammalogists. Figure 4 was prepared by J. Pacheco. Additional specimens from Carpish were obtained through a grant from CONCYTEC to Pacheco; and those from Parque Nacional Yanachaga-Chemillen through a consultancy for Proteccion de Areas Naturales - PAN - II of PROFONANPE to Vivar. Reproduction of Fig. 2, originally published in Mastozoologia Neotropical, vol. 17, was facilitated by U. Pardinas. We thank R. S. Voss and R. H. Pine for critical review and comments on previous drafts. NR 36 TC 5 Z9 6 U1 1 U2 14 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 OCT 9 PY 2012 VL 125 IS 3 BP 295 EP 307 PG 13 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 025HB UT WOS:000310178100007 ER PT J AU Woodman, N AF Woodman, Neal TI This shrew is a jumping mouse (Mammalia, Dipodidae): Sorex dichrurus Rafinesque, 1833 is a synonym of Zapus hudsonius (Zimmermann, 1780) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE americanus; canadensis; dichrurus; nomenclature; Rodentia; Soricidae; Soricomorpha; taxonomy AB Constantine S. Rafinesque described Sorex dichrurus as a shrew in 1833, based on a specimen he found in a proprietary museum near Niagara Falls on the New York/Ontario border. The name subsequently has been ignored by the scientific community. By describing this specimen as a shrew and ascribing it to the genus Sorex, Rafinesque clearly indicated that his species should be considered a member of the taxonomic family now recognized as the Soricidae (Mamma ha, Eulipotyphla). Yet, the description of the animal, and its comparison to "Gerbillus," clearly identify it as a dipodid rodent, specifically Zapus hudsonius (Zimmermann, 1780); S. dichrurus should be treated as a junior subjective synonym of that taxon. Based on its type locality of Goat Island, New York, this name is also a junior synonym of the subspecies Z. hudsonius canadensis (Davies, 1798). C1 Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, Natl Museum Nat Hist, USGS Patuxent Wildlife Res Ctr, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 38 TC 3 Z9 3 U1 0 U2 4 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 OCT 9 PY 2012 VL 125 IS 3 BP 308 EP 316 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 025HB UT WOS:000310178100008 ER PT J AU Onofrio, R AF Onofrio, Roberto TI Neutrino mass variability due to nonminimal coupling to spacetime curvature in neutrinophilic two-Higgs-doublet models SO PHYSICAL REVIEW D LA English DT Article ID HIGGS DOUBLET MODEL; GRAVITATIONAL-FIELDS; VACUUM POLARIZATION; PION DECAY; OSCILLATIONS; DIMENSIONS; MILLIMETER; BOSON AB In neutrinophilic two-Higgs-doublet models, neutrinos acquire mass due to a Higgs field with vacuum expectation value of the order of similar or equal to 10(-2) eV, corresponding to a Compton wavelength in the 10 mu m range. This creates a situation in which nonminimal couplings between Higgs fields and spacetime curvature may lead to novel observable effects. Among these, we discuss the possibility of variable neutrino masses, with implications for the dependence of the neutrino oscillation frequency on the spacetime curvature, a further source of dispersion of the neutrino arrival times from supernovae events, and possibly also a mechanism leading to gravitationally-induced neutrino superluminality. Finally, we propose laboratory-scale experiments in which properly designed electroweak cavities may be used to change neutrino masses, which should be observable through time of flight experiments. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis & Astron Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis & Astron Galileo Galilei, Via Marzolo 8, I-35131 Padua, Italy. NR 40 TC 0 Z9 0 U1 0 U2 3 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 OCT 8 PY 2012 VL 86 IS 8 AR 087501 DI 10.1103/PhysRevD.86.087501 PG 4 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 017JN UT WOS:000309586300023 ER PT J AU Dong, SX Davies, SJ Ashton, PS Bunyavejchewin, S Supardi, MNN Kassim, AR Tan, S Moorcroft, PR AF Dong, Shirley Xiaobi Davies, Stuart J. Ashton, Peter S. Bunyavejchewin, Sarayudh Supardi, M. N. Nur Kassim, Abd Rahman Tan, Sylvester Moorcroft, Paul R. TI Variability in solar radiation and temperature explains observed patterns and trends in tree growth rates across four tropical forests SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE tropical forest; tree growth rates; forest demography; forest dynamics; climate variability; climate change ID AMAZON RAIN-FOREST; CLIMATE; DYNAMICS; BIOMASS; SURFACE; PLOTS AB The response of tropical forests to global climate variability and change remains poorly understood. Results from long-term studies of permanent forest plots have reported different, and in some cases opposing trends in tropical forest dynamics. In this study, we examined changes in tree growth rates at four long-term permanent tropical forest research plots in relation to variation in solar radiation, temperature and precipitation. Temporal variation in the stand-level growth rates measured at five-year intervals was found to be positively correlated with variation in incoming solar radiation and negatively related to temporal variation in night-time temperatures. Taken alone, neither solar radiation variability nor the effects of night-time temperatures can account for the observed temporal variation in tree growth rates across sites, but when considered together, these two climate variables account for most of the observed temporal variability in tree growth rates. Further analysis indicates that the stand-level response is primarily driven by the responses of smaller-sized trees (less than 20 cm in diameter). The combined temperature and radiation responses identified in this study provide a potential explanation for the conflicting patterns in tree growth rates found in previous studies. C1 [Dong, Shirley Xiaobi; Moorcroft, Paul R.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Davies, Stuart J.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, APO 34002, AA, Panama. [Ashton, Peter S.] Harvard Univ, Ctr Trop Forest Sci, Arnold Arboretum Asia Program, Cambridge, MA 02138 USA. [Bunyavejchewin, Sarayudh] Res Off, Dept Natl Pk Wildlife & Plant Conservat, Bangkok 10900, Thailand. [Supardi, M. N. Nur; Kassim, Abd Rahman] Forest Res Inst Malaysia, Div Forest Environm, Kuala Lumpur 52109, Malaysia. [Tan, Sylvester] CTFS AA 52 Ha Plot Project, Miri 98000, Sarawak, Malaysia. RP Moorcroft, PR (reprint author), Harvard Univ, Dept Organism & Evolutionary Biol, 26 Oxford St, Cambridge, MA 02138 USA. EM paul_moorcroft@harvard.edu NR 32 TC 25 Z9 27 U1 3 U2 40 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 OCT 7 PY 2012 VL 279 IS 1744 BP 3923 EP 3931 DI 10.1098/rspb.2012.1124 PG 9 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 998LC UT WOS:000308239500005 PM 22833269 ER PT J AU Ortega-Jimenez, VM Dudley, R AF Ortega-Jimenez, Victor Manuel Dudley, Robert TI Flying in the rain: hovering performance of Anna's hummingbirds under varied precipitation SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE birds; drop impact; flight performance; kinematics; rainfall ID FLIGHT; ENERGY; AERODYNAMICS; FEATHERS; IMPACT; WATER; WET AB Flight in rain represents a greater challenge for smaller animals because the relative effects of water loading and drop impact are greater at reduced scales given the increased ratios of surface area to mass. Nevertheless, it is well known that small volant taxa such as hummingbirds can continue foraging even in extreme precipitation. Here, we evaluated the effect of four rain intensities (i.e. zero, light, moderate and heavy) on the hovering performance of Anna's hummingbirds (Calypte anna) under laboratory conditions. Light-to-moderate rain had only a marginal effect on flight kinematics; wingbeat frequency of individuals in moderate rain was reduced by 7 per cent relative to control conditions. By contrast, birds hovering in heavy rain adopted more horizontal body and tail positions, and also increased wingbeat frequency substantially, while reducing stroke amplitude when compared with control conditions. The ratio between peak forces produced by single drops on a wing and on a solid surface suggests that feathers can absorb associated impact forces by up to approximately 50 per cent. Remarkably, hummingbirds hovered well even under heavy precipitation (i.e. 270 mm h(-1)) with no apparent loss of control, although mechanical power output assuming perfect and zero storage of elastic energy was estimated to be about 9 and 57 per cent higher, respectively, compared with normal hovering. C1 [Ortega-Jimenez, Victor Manuel; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Ortega-Jimenez, VM (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM vortega@berkeley.edu OI Ortega-Jimenez, Victor Manuel/0000-0003-0024-5086 FU University of California MEXUS-CONACYT FX We thank numerous members of the Dudley laboratory, especially Dennis Evangelista, and two anonymous reviewers for their valuable comments and suggestions. We also thank Sarahi Arriaga-Ramirez for helping us to write code for kinematic analyses. V.M.O.J. was supported by University of California MEXUS-CONACYT. Hummingbird care and experimental procedures were approved by the IACUC of the University of California, Berkeley. NR 29 TC 9 Z9 9 U1 2 U2 31 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 OCT 7 PY 2012 VL 279 IS 1744 BP 3996 EP 4002 DI 10.1098/rspb.2012.1285 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 998LC UT WOS:000308239500014 PM 22810431 ER PT J AU Strader, J Chomiuk, L Maccarone, TJ Miller-Jones, JCA Seth, AC AF Strader, Jay Chomiuk, Laura Maccarone, Thomas J. Miller-Jones, James C. A. Seth, Anil C. TI Two stellar-mass black holes in the globular cluster M22 SO NATURE LA English DT Article ID X-RAY BINARIES; STAR-CLUSTERS; QUIESCENCE; EMISSION; CATALOG; JETS AB Hundreds of stellar-mass black holes probably form in a typical globular star cluster, with all but one predicted to be ejected through dynamical interactions(1-3). Some observational support for this idea is provided by the lack of X-ray-emitting binary stars comprising one black hole and one other star ('black-hole/X-ray binaries') in Milky Way globular clusters, even though many neutron-star/X-ray binaries are known(4). Although a few black holes have been seen in globular clusters around other galaxies(5,6), the masses of these cannot be determined, and some may be intermediate-mass black holes that form through exotic mechanisms(7). Here we report the presence of two flat-spectrum radio sources in the Milky Way globular cluster M22, and we argue that these objects are black holes of stellar mass (each similar to 10-20 times more massive than the Sun) that are accreting matter. We find a high ratio of radio-to-X-ray flux for these black holes, consistent with the larger predicted masses of black holes in globular clusters compared to those outside(8). The identification of two black holes in one cluster shows that ejection of black holes is not as efficient as predicted by most models(1,2,4), and we argue that M22 may contain a total population of similar to 5-100 black holes. The large core radius of M22 could arise from heating produced by the black holes(9). C1 [Strader, Jay; Chomiuk, Laura] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Strader, Jay; Chomiuk, Laura] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chomiuk, Laura] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Maccarone, Thomas J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Miller-Jones, James C. A.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Strader, J (reprint author), Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. EM strader@pa.msu.edu RI Miller-Jones, James/B-2411-2013 OI Miller-Jones, James/0000-0003-3124-2814 NR 29 TC 60 Z9 61 U1 0 U2 5 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD OCT 4 PY 2012 VL 490 IS 7418 BP 71 EP 73 DI 10.1038/nature11490 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 015LG UT WOS:000309446800033 PM 23038466 ER PT J AU Gharashi, SE Daily, KM Blume, D AF Gharashi, Seyed Ebrahim Daily, K. M. Blume, D. TI Three s-wave-interacting fermions under anisotropic harmonic confinement: Dimensional crossover of energetics and virial coefficients SO PHYSICAL REVIEW A LA English DT Article ID ULTRACOLD GASES; THERMODYNAMICS; SCATTERING AB We present highly accurate solutions of the Schrodinger equation for three fermions in two different spin states with zero-range s-wave interactions under harmonic confinement. Our approach covers spherically symmetric, strictly two-dimensional, strictly one-dimensional, cigar-shaped, and pancake-shaped traps. In particular, we discuss the transition from quasi-one-dimensional to strictly one-dimensional and from quasi-two-dimensional to strictly two-dimensional geometries. We determine and interpret the eigenenergies of the system as a function of the trap geometry and the strength of the zero-range interactions. The eigenenergies are used to investigate the dependence of the second- and third-order virial coefficients, which play an important role in the virial expansion of the thermodynamic potential, on the geometry of the trap. We show that the second- and third-order virial coefficients for anisotropic confinement geometries are, for experimentally relevant temperatures, very well approximated by those for the spherically symmetric confinement for all s-wave scattering lengths. C1 [Gharashi, Seyed Ebrahim; Daily, K. M.; Blume, D.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. [Blume, D.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Gharashi, SE (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. RI Gharashi, Seyed Ebrahim/E-5378-2016 OI Gharashi, Seyed Ebrahim/0000-0002-8798-7615 FU ARO; National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University; Smithsonian Astrophysical Observatory FX We gratefully acknowledge support by the ARO and thank Krittika Goyal for contributions at the initial stage of this work. This work was additionally supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 43 TC 25 Z9 25 U1 1 U2 10 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD OCT 4 PY 2012 VL 86 IS 4 AR 042702 DI 10.1103/PhysRevA.86.042702 PG 14 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 015OP UT WOS:000309456100005 ER PT J AU Larsen, RJ Knapp, MC Genoways, HH Khan, FAA Larsen, PA Wilson, DE Baker, RJ AF Larsen, Roxanne J. Knapp, Michelle C. Genoways, Hugh H. Khan, Faisal Ali Anwarali Larsen, Peter A. Wilson, Don E. Baker, Robert J. TI Genetic Diversity of Neotropical Myotis (Chiroptera: Vespertilionidae) with an Emphasis on South American Species SO PLOS ONE LA English DT Article ID CYTOCHROME-B SEQUENCES; MORPHOLOGICAL VARIATION; MOLECULAR SYSTEMATICS; NIGRICANS SCHINZ; SIMUS THOMAS; GENUS MYOTIS; BATS; DNA; MITOCHONDRIAL; MAMMALS AB Background: Cryptic morphological variation in the Chiropteran genus Myotis limits the understanding of species boundaries and species richness within the genus. Several authors have suggested that it is likely there are unrecognized species-level lineages of Myotis in the Neotropics. This study provides an assessment of the diversity in New World Myotis by analyzing cytochrome-b gene variation from an expansive sample ranging throughout North, Central, and South America. We provide baseline genetic data for researchers investigating phylogeographic and phylogenetic patterns of Myotis in these regions, with an emphasis on South America. Methodology and Principal Findings: Cytochrome-b sequences were generated and phylogenetically analyzed from 215 specimens, providing DNA sequence data for the most species of New World Myotis to date. Based on genetic data in our sample, and on comparisons with available DNA sequence data from GenBank, we estimate the number of species-level genetic lineages in South America alone to be at least 18, rather than the 15 species currently recognized. Conclusions: Our findings provide evidence that the perception of lower species richness in South American Myotis is largely due to a combination of cryptic morphological variation and insufficient sampling coverage in genetic- based systematic studies. A more accurate assessment of the level of diversity and species richness in New World Myotis is not only helpful for delimiting species boundaries, but also for understanding evolutionary processes within this globally distributed bat genus. C1 [Larsen, Roxanne J.; Knapp, Michelle C.; Khan, Faisal Ali Anwarali; Larsen, Peter A.; Baker, Robert J.] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. [Genoways, Hugh H.] Univ Nebraska, State Museum, Lincoln, NE 68588 USA. [Wilson, Don E.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Larsen, RJ (reprint author), Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27706 USA. EM roxy.larsen@duke.edu RI Anwarali Khan, Faisal Ali/J-7670-2012; Larsen, Roxanne/I-4425-2016 OI Anwarali Khan, Faisal Ali/0000-0001-7585-4885; Larsen, Roxanne/0000-0001-8139-3261 FU Department of Biological Sciences at Texas Tech University; Biological Database; James Sowell FX This research was supported by the Department of Biological Sciences at Texas Tech University, the Biological Database, and James Sowell. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 45 TC 13 Z9 14 U1 1 U2 36 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD OCT 3 PY 2012 VL 7 IS 10 AR e46578 DI 10.1371/journal.pone.0046578 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 015NU UT WOS:000309454000058 PM 23056352 ER PT J AU Peplowski, PN Lawrence, DJ Rhodes, EA Sprague, AL McCoy, TJ Denevi, BW Evans, LG Head, JW Nittler, LR Solomon, SC Stockstill-Cahill, KR Weider, SZ AF Peplowski, Patrick N. Lawrence, David J. Rhodes, Edgar A. Sprague, Ann L. McCoy, Timothy J. Denevi, Brett W. Evans, Larry G. Head, James W. Nittler, Larry R. Solomon, Sean C. Stockstill-Cahill, Karen R. Weider, Shoshana Z. TI Variations in the abundances of potassium and thorium on the surface of Mercury: Results from the MESSENGER Gamma-Ray Spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID RADIOACTIVE ELEMENTS; LUNAR PROSPECTOR; PLANET MERCURY; CALORIS BASIN; ATMOSPHERE; MOON; PLAGIOCLASE; REDUCTION; EVOLUTION; DIFFUSION AB A technique for converting gamma-ray count rates measured by the Gamma-Ray Spectrometer on the MESSENGER spacecraft to spatially resolved maps of the gamma-ray emission from the surface of Mercury is utilized to map the surface distributions of the elements Si, O, and K over the planet's northern hemisphere. Conversion of the K gamma-ray count rates to elemental abundances on the surface reveals variations from 300 to 2400 ppm. A comparison of these abundances with models for the maximum surface temperature suggests the possibility that a temperature-related process is controlling the K abundances on the surface as well as providing K to the exosphere. The abundances of K and Th have been determined for several geologically distinct regions, including Mercury's northern smooth plains and the plains interior to the Caloris basin. The lack of a significant variation in the measured Th abundances suggests that there may be considerable variability in the K/Th abundance ratio over the mapped regions. C1 [Peplowski, Patrick N.; Lawrence, David J.; Rhodes, Edgar A.; Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Sprague, Ann L.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [McCoy, Timothy J.; Stockstill-Cahill, Karen R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Evans, Larry G.] Comp Sci Corp, Lanham, MD USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Nittler, Larry R.; Solomon, Sean C.; Weider, Shoshana Z.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. RP Peplowski, PN (reprint author), Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA. EM patrick.peplowski@jhuapl.edu RI Peplowski, Patrick/I-7254-2012; Denevi, Brett/I-6502-2012; Lawrence, David/E-7463-2015; OI Peplowski, Patrick/0000-0001-7154-8143; Denevi, Brett/0000-0001-7837-6663; Lawrence, David/0000-0002-7696-6667; Weider, Shoshana/0000-0003-1034-909X FU NASA Discovery Program [NAS5-97271, NASW-00002] FX We thank D. A. Paige for providing the modeled surface temperatures utilized in this study and G. J. Taylor for providing the Martian K and Th abundances for comparison with these results. We also thank two anonymous reviewers for thoughtful reviews that improved the clarity of the text. Finally, we are indebted to the entire MESSENGER team for their invaluable contributions to the development and operation of the MESSENGER spacecraft. The MESSENGER mission is supported by the NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. NR 52 TC 39 Z9 39 U1 0 U2 18 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 OCT 3 PY 2012 VL 117 AR E00L04 DI 10.1029/2012JE004141 PG 27 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 017TK UT WOS:000309613700001 ER PT J AU Weider, SZ Nittler, LR Starr, RD McCoy, TJ Stockstill-Cahill, KR Byrne, PK Denevi, BW Head, JW Solomon, SC AF Weider, Shoshana Z. Nittler, Larry R. Starr, Richard D. McCoy, Timothy J. Stockstill-Cahill, Karen R. Byrne, Paul K. Denevi, Brett W. Head, James W. Solomon, Sean C. TI Chemical heterogeneity on Mercury's surface revealed by the MESSENGER X-Ray Spectrometer SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ASTEROID 433 EROS; ENSTATITE CHONDRITES; ELEMENTAL COMPOSITION; FLUORESCENCE OBSERVATIONS; PHASE-RELATIONS; PARENT BODY; EMISSION; FLYBY; VOLCANISM; EXOSPHERE AB We present the analysis of 205 spatially resolved measurements of the surface composition of Mercury from MESSENGER's X-Ray Spectrometer. The surface footprints of these measurements are categorized according to geological terrain. Northern smooth plains deposits and the plains interior to the Caloris basin differ compositionally from older terrain on Mercury. The older terrain generally has higher Mg/Si, S/Si, and Ca/Si ratios, and a lower Al/Si ratio than the smooth plains. Mercury's surface mineralogy is likely dominated by high-Mg mafic minerals (e.g., enstatite), plagioclase feldspar, and lesser amounts of Ca, Mg, and/or Fe sulfides (e.g., oldhamite). The compositional difference between the volcanic smooth plains and the older terrain reflects different abundances of these minerals and points to the crystallization of the smooth plains from a more chemically evolved magma source. High-degree partial melts of enstatite chondrite material provide a generally good compositional and mineralogical match for much of the surface of Mercury. An exception is Fe, for which the low surface abundance on Mercury is still higher than that of melts from enstatite chondrites and may indicate an exogenous contribution from meteoroid impacts. C1 [Weider, Shoshana Z.; Nittler, Larry R.; Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Starr, Richard D.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Starr, Richard D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [McCoy, Timothy J.; Stockstill-Cahill, Karen R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Denevi, Brett W.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Geol Observ, Palisades, NY 10964 USA. RP Weider, SZ (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM sweider@ciw.edu RI Denevi, Brett/I-6502-2012; OI Denevi, Brett/0000-0001-7837-6663; Weider, Shoshana/0000-0003-1034-909X FU NASA Discovery Program [NAS5-97271, NASW-00002] FX The authors thank Denton Ebel and an anonymous reviewer for constructive reviews of an earlier version of this paper. We thank the MESSENGER team for the development, cruise, orbit insertion, and orbital operations of the MESSENGER spacecraft. This work is supported by the NASA Discovery Program under contract NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory and NASW-00002 to the Carnegie Institution of Washington. S.Z.W. thanks Frances E. Jenner for helpful discussions during manuscript preparation. NR 79 TC 76 Z9 76 U1 0 U2 25 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 OCT 3 PY 2012 VL 117 AR E00L05 DI 10.1029/2012JE004153 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 017TK UT WOS:000309613700002 ER PT J AU Glaetzle, AW Nath, R Zhao, B Pupillo, G Zoller, P AF Glaetzle, A. W. Nath, R. Zhao, B. Pupillo, G. Zoller, P. TI Driven-dissipative dynamics of a strongly interacting Rydberg gas SO PHYSICAL REVIEW A LA English DT Article ID DIPOLAR GASES; QUANTUM GATES; ATOMS; EXCITATION; COLLISIONS; BLOCKADE; STATES; COLD AB We study the nonequilibrium many-body dynamics of a cold gas of ground-state alkali-metal atoms weakly admixed by Rydberg states with laser light. On a time scale shorter than the lifetime of the dressed states, effective dipole-dipole or van der Waals interactions between atoms can lead to the formation of strongly correlated phases, such as atomic crystals. Using a semiclassical approach, we study the long-time dynamics where decoherence and dissipative processes due to spontaneous emission and blackbody radiation dominate, leading to heating and melting of atomic crystals as well as particle losses. These effects can be substantially mitigated by performing active laser cooling in the presence of atomic dressing. C1 [Glaetzle, A. W.; Nath, R.; Zhao, B.; Pupillo, G.; Zoller, P.] Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Glaetzle, A. W.; Nath, R.; Zhao, B.; Pupillo, G.; Zoller, P.] Austrian Acad Sci, Inst Quantum Opt & Quantum Informat, A-6020 Innsbruck, Austria. [Glaetzle, A. W.; Zoller, P.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Glaetzle, A. W.; Zoller, P.] NIST, Joint Quantum Inst, Gaithersburg, MD 20899 USA. [Glaetzle, A. W.; Zoller, P.] Univ Maryland, Gaithersburg, MD 20899 USA. [Pupillo, G.] Univ Strasbourg, ISIS, UMR 7006, Strasbourg, France. [Pupillo, G.] Univ Strasbourg, IPCMS, UMR 7504, Strasbourg, France. [Pupillo, G.] CNRS, Strasbourg, France. RP Glaetzle, AW (reprint author), Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. RI Zoller, Peter/O-1639-2014 OI Zoller, Peter/0000-0003-4014-1505 FU COHERENCE; EOARD; EPSRC through CHIST-ERA R-ION; Austrian Science Fund; ERC Starting Grant [307688] FX The authors thank E. Arimondo, M. Baranov, I. Lesanovsky, M. D. Lukin, and H. R. Sadeghpour for stimulating discussions. P.Z. and A.G. thank ITAMP, the Harvard Physics Department and the Joint Quantum Institute, University of Maryland, where part of this work was done, for their hospitality. Work was supported in parts by COHERENCE, EOARD, and EPSRC through CHIST-ERA R-ION and the Austrian Science Fund. G.P. was funded by the ERC Starting Grant No. (307688). NR 86 TC 26 Z9 26 U1 0 U2 17 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD OCT 2 PY 2012 VL 86 IS 4 AR 043403 DI 10.1103/PhysRevA.86.043403 PG 18 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 014OD UT WOS:000309384500003 ER PT J AU Hara, H Smith, DR AF Hara, Hideho Smith, David R. TI Nesodiprion orientalis sp nov., N. japonicus, and N. biremis, with a key to species of Nesodiprion (Hymenoptera, Diprionidae) SO ZOOTAXA LA English DT Article DE Symphyta; lectotype designation; host plant; Pinus ID SYMPHYTA; THAILAND AB Nesodiprion japonicus (Marlatt, 1898), the type species of Nesodiprion, from Japan, Korea, and Taiwan, and N. biremis (Konow, 1899) from China are redescribed based on their type specimens. Lectotypes are designated for both. Nesodiprion orientalis Hara & Smith, sp. nov. is described from Thailand and Yunnan Province, China. Larvae of all three species feed on Pinus. Generic characters of Nesodiprion are discussed, and a provisional key to species of the genus is given. C1 [Hara, Hideho] Hokkaido Res Org, Forestry Res Inst Doto Stn, Shintoku, Hokkaido 0810038, Japan. [Smith, David R.] Smithsonian Inst, Systemat Entomol Lab, PSI, Agr Res Serv,USDA,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Hara, H (reprint author), Hokkaido Res Org, Forestry Res Inst Doto Stn, Shintoku, Hokkaido 0810038, Japan. EM hara-hideho@hro.or.jp; sawfly2@aol.com FU Japan Society for the Promotion of Science [20580165] FX We thank A. Shinohara (NSMT) for his kind help in various ways. Our thanks are also due to S. M. Blank (SDEI) for the valuable information on the type material of N. biremis, and A. D. Liston and A. Taeger (SDEI), T. Hirowatari (OPU), H. Kojima (Nagano), K. Maeto (KU), G. M. Nishida (BPBM), K. Ozaki (FFPRIH) and I. Togashi (Hakusan) for gifts or loans of the material for this study. This study is partly supported by the Grant-in-aid for Scientific Research No. 20580165 from the Japan Society for the Promotion of Science NR 44 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 OCT 2 PY 2012 IS 3503 BP 1 EP 24 PG 24 WC Zoology SC Zoology GA 018PG UT WOS:000309673100001 ER PT J AU Mei, Z Shen, C Wu, N Lin, J Murphy, NA Roussev, II AF Mei, Z. Shen, C. Wu, N. Lin, J. Murphy, N. A. Roussev, I. I. TI Numerical experiments on magnetic reconnection in solar flare and coronal mass ejection current sheets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instabilities; magnetic reconnection; shock waves; turbulence; Sun: coronal mass ejections (CMEs); Sun: flares ID PLASMOID-INDUCED-RECONNECTION; SUPRA-ARCADE DOWNFLOWS; X-RAY; CATASTROPHE MODEL; TRANSPORT SCHEME; ERUPTIVE FLARES; FLUX-ROPE; CME-FLARE; SIMULATION; FIELD AB Magnetic reconnection plays a critical role in energy conversion during solar eruptions. This paper presents a set of magnetohydrodynamic experiments for the magnetic reconnection process in a current sheet (CS) formed in the wake of the rising flux rope. The eruption results from the loss of equilibrium in a magnetic configuration that includes a current-carrying flux rope, representing a pre-existing filament. In order to study the fine structure and micro processes inside the CS, mesh refinement is used to reduce the numerical diffusion. We start with a uniform, explicitly defined resistivity which results in a Lundquist number S = 10(4) in the vicinity of CS. The use of mesh refinement allows the simulation to capture high-resolution features such as plasmoids from the tearing mode and plasmoid instability regions of turbulence and slow-mode shocks. Inside the CS, magnetic reconnection goes through the Sweet-Parker and the fractal stages, and eventually displays a time-dependent Petschek pattern. Our results support the concept of fractal reconnection suggested by Shibata et al. and Shibata & Tanuma, and also suggest that the CS evolves through Sweet-Parker reconnection prior to the fast reconnection stage. For the first time, the detailed features and/or fine structures inside the coronal mass ejection/flare CS in the eruption were investigated in this work. C1 [Mei, Z.; Shen, C.; Lin, J.; Roussev, I. I.] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China. [Mei, Z.; Shen, C.] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. [Shen, C.; Lin, J.; Murphy, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wu, N.] Yunnan Normal Univ, Sch Tourism & Geog, Kunming 650031, Yunnan, Peoples R China. [Roussev, I. I.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP Mei, Z (reprint author), Chinese Acad Sci, Yunnan Astron Observ, POB 110, Kunming 650011, Yunnan, Peoples R China. EM meizhixing@ynao.ac.cn; jlin@ynao.ac.cn RI LIN, JUN/B-9890-2017; OI Murphy, Nicholas/0000-0001-6628-8033 FU Program 973 grant [2011CB811403]; NSFC [10873030]; CAS [2011T2J01, 2010Y2JB16, KJCX2-EW-T07]; NASA [NNX11AB61G]; NSF SHINE grant [AGS-1156076] FX We are grateful to T. G. Forbes and L. Ni for valuable discussions. We would like to thank the editor and an unknown referee as well for the useful comments made on the manuscript. This work was supported by the Program 973 grant 2011CB811403, the NSFC grant 10873030, and the CAS grants 2011T2J01, 2010Y2JB16 and KJCX2-EW-T07 to YNAO. JL and NAM acknowledge support from NASA grant NNX11AB61G and NSF SHINE grant AGS-1156076 to SAO. The NIRVANA v3.5 code was developed by Udo Ziegler at the Leibniz-Institut fur Astrophysik Potsdam. Calculations in this work were completed with the help of the HPC Center, Kunming Institute of Botany, CAS. NR 80 TC 24 Z9 28 U1 1 U2 6 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 OCT PY 2012 VL 425 IS 4 BP 2824 EP 2839 DI 10.1111/j.1365-2966.2012.21625.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135EN UT WOS:000318270500018 ER PT J AU Deason, AJ Belokurov, V Evans, NW Koposov, SE Cooke, RJ Penarrubia, J Laporte, CFP Fellhauer, M Walker, MG Olszewski, EW AF Deason, A. J. Belokurov, V. Evans, N. W. Koposov, S. E. Cooke, R. J. Penarrubia, J. Laporte, C. F. P. Fellhauer, M. Walker, M. G. Olszewski, E. W. TI The cold veil of the Milky Way stellar halo SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE blue stragglers; stars: carbon; stars: horizontal branch; Galaxy: halo; Galaxy: fundamental parameters; Galaxy: kinematics and dynamics ID COOL CARBON STARS; HORIZONTAL-BRANCH STARS; VELOCITY DISPERSION PROFILE; DARK-MATTER HALOS; GALACTIC HALO; CIRCULAR VELOCITY; GALAXY FORMATION; PROPER MOTION; MASS PROFILE; APM SURVEY AB We build a sample of distant (D > 80 kpc) stellar halo stars with measured radial velocities. Faint (20 < g < 22) candidate blue horizontal branch (BHB) stars were selected using the deep, but wide, multi-epoch Sloan Digital Sky Survey photometry. Follow-up spectroscopy for these A-type stars was performed using the Very Large Telescope (VLT) FOcal Reducer and low dispersion Spectrograph 2 (FORS2) instrument. We classify stars according to their Balmer line profiles, and find that seven are bona fide BHB stars and 31 are blue stragglers (BS). Owing to the magnitude range of our sample, even the intrinsically fainter BS stars can reach out to D similar to 90 kpc. We complement this sample of A-type stars with intrinsically brighter, intermediate-age, asymptotic giant branch stars. A set of four distant cool carbon stars is compiled from the literature and we perform spectroscopic follow-up on a further four N-type carbon stars using the William Herschel Telescope (WHT) Intermediate dispersion Spectrograph and Imaging System (ISIS) instrument. Altogether, this provides us with the largest sample to date of individual star tracers out to r similar to 150 kpc. We find that the radial velocity dispersion of these tracers falls rapidly at large distances and is surprisingly cold (sigma(r) approximate to 50-60 km s(-1)) between 100 and 150 kpc. Relating the measured radial velocities to the mass of the Milky Way requires knowledge of the (unknown) tracer density profile and anisotropy at these distances. Nonetheless, by assuming the stellar halo stars between 50 and 150 kpc have a moderate density fall-off (with power-law slope alpha < 5) and are on radial orbits (sigma(2)(t)/sigma(2)(r) < 1), we infer that the mass within 150 kpc is less than 10(12) M-circle dot and suggest it probably lies in the range (5-10) x 10(11) M-circle times. We discuss the implications of such a low mass for the Milky Way. C1 [Deason, A. J.; Belokurov, V.; Evans, N. W.; Koposov, S. E.; Cooke, R. J.; Laporte, C. F. P.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Koposov, S. E.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119991, Russia. [Penarrubia, J.] Inst Astrofis Andalucia CSIC, Granada 18008, Spain. [Laporte, C. F. P.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Fellhauer, M.] Univ Concepcion, Inst Astron, Concepcion, Chile. [Walker, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Olszewski, E. W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Deason, AJ (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM ajd75@ast.cam.ac.uk RI Koposov, Sergey/F-2754-2012; Walker, Matthew/P-1777-2014 OI Koposov, Sergey/0000-0003-2644-135X; Walker, Matthew/0000-0003-2496-1925 FU Science and Technology Facilities Council (STFC); Royal Society; STFC; Peterhouse College, Cambridge; Ramon y Cajal Program; Spanish grant [AYA2010-17631]; Ministerio of Economia y Competitividad; Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; FONDECYT [1095092]; BASAL; NASA [HST-HF-51283.01-A, NAS5-26555]; Space Telescope Science Institute; NSF [AST0807498] FX AJD thanks the Science and Technology Facilities Council (STFC) for the award of a studentship. VB acknowledges financial support from the Royal Society. SK acknowledges financial support from the STFC. RC is supported by a Research Fellowship at Peterhouse College, Cambridge. JP acknowledges support from the Ramon y Cajal Program as well as by the Spanish grant AYA2010-17631 awarded by the Ministerio of Economia y Competitividad. CFPL is currently supported by the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356. MF acknowledges funding through FONDECYT project No. 1095092 and BASAL. MGW is currently supported by NASA through Hubble Fellowship grant HST-HF-51283.01-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. EO was partially supported by NSF grant AST0807498. It is a pleasure to thank Mike Irwin and Paul Hewett for useful comments and advice. We also thank an anonymous referee for useful comments. NR 53 TC 53 Z9 53 U1 0 U2 5 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 OCT PY 2012 VL 425 IS 4 BP 2840 EP 2853 DI 10.1111/j.1365-2966.2012.21639.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135EN UT WOS:000318270500019 ER PT J AU Zaroubi, S de Bruyn, AG Harker, G Thomas, RM Labropolous, P Jelic, V Koopmans, LVE Brentjens, MA Bernardi, G Ciardi, B Daiboo, S Kazemi, S Martinez-Rubi, O Mellema, G Offringa, AR Pandey, VN Schaye, J Veligatla, V Vedantham, H Yatawatta, S AF Zaroubi, S. de Bruyn, A. G. Harker, G. Thomas, R. M. Labropolous, P. Jelic, V. Koopmans, L. V. E. Brentjens, M. A. Bernardi, G. Ciardi, B. Daiboo, S. Kazemi, S. Martinez-Rubi, O. Mellema, G. Offringa, A. R. Pandey, V. N. Schaye, J. Veligatla, V. Vedantham, H. Yatawatta, S. TI Imaging neutral hydrogen on large scales during the Epoch of Reionization with LOFAR SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; cosmology: observations; cosmology: theory; diffuse radiation; large-scale structure of Universe; radio lines: general ID 21 CENTIMETER FLUCTUATIONS; PROBE WMAP OBSERVATIONS; DIGITAL SKY SURVEY; ULTRA-DEEP-FIELD; INTERGALACTIC MEDIUM; HIGH-REDSHIFT; FOREGROUND REMOVAL; Z-GREATER-THAN-5.7 QUASARS; COSMIC REIONIZATION; ADDITIONAL QUASARS AB The first generation of redshifted 21 cm detection experiments, carried out with arrays like Low Frequency Array (LOFAR), Murchison Widefield Array (MWA) and Giant Metrewave Telescope (GMRT), will have a very low signal-to-noise ratio (S/N) per resolution element (less than or similar to 0.2). In addition, whereas the variance of the cosmological signal decreases on scales larger than the typical size of ionization bubbles, the variance of the formidable galactic foregrounds increases, making it hard to disentangle the two on such large scales. The poor sensitivity on small scales, on the one hand, and the foregrounds effect on large scales, on the other hand, make direct imaging of the Epoch of Reionization of the Universe very difficult, and detection of the signal therefore is expected to be statistical. Despite these hurdles, in this paper we argue that for many reionization scenarios low-resolution images could be obtained from the expected data. This is because at the later stages of the process one still finds very large pockets of neutral regions in the intergalactic medium, reflecting the clustering of the large-scale structure, which stays strong up to scales of approximate to 120 h(-1) comoving Mpc (approximate to 1 degrees). The coherence of the emission on those scales allows us to reach sufficient S/N (greater than or similar to 3) so as to obtain reionization 21 cm images. Such images will be extremely valuable for answering many cosmological questions but above all they will be a very powerful tool to test our control of the systematics in the data. The existence of this typical scale (approximate to 120 h(-1) comoving Mpc) also argues for designing future EoR experiments, e. g. with Square Kilometre Array, with a field of view of at least 4 degrees. C1 [Zaroubi, S.; de Bruyn, A. G.; Labropolous, P.; Koopmans, L. V. E.; Daiboo, S.; Kazemi, S.; Martinez-Rubi, O.; Offringa, A. R.; Pandey, V. N.; Veligatla, V.; Vedantham, H.; Yatawatta, S.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Zaroubi, S.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [de Bruyn, A. G.; Labropolous, P.; Jelic, V.; Brentjens, M. A.; Pandey, V. N.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Harker, G.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Thomas, R. M.] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mellema, G.] Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden. [Mellema, G.] Stockholm Univ, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Schaye, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Zaroubi, S (reprint author), Univ Groningen, Kapteyn Astron Inst, POB 800, NL-9700 AV Groningen, Netherlands. EM saleem@astro.rug.nl RI Jelic, Vibor/B-2938-2014; Thomas, Rajat/B-7105-2014; Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; OI Jelic, Vibor/0000-0002-6034-8610; Thomas, Rajat/0000-0002-5362-4816; Harker, Geraint/0000-0002-7894-4082; Schaye, Joop/0000-0002-0668-5560 FU Lady Davis Foundation; Netherlands Organization for Scientific Research (NWO) VICI; European Research Council; NASA Lunar Science Institute [NNA09DB30A] FX SZ would like to thank the Lady Davis Foundation and The Netherlands Organization for Scientific Research (NWO) VICI grant for financial support. LVEK thanks the European Research Council Starting Grant for support. GH is a member of the LUNAR consortium, which is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. NR 61 TC 29 Z9 29 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 OCT PY 2012 VL 425 IS 4 BP 2964 EP 2973 DI 10.1111/j.1365-2966.2012.21500.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135EN UT WOS:000318270500027 ER PT J AU Vogelsberger, M Sijacki, D Keres, D Springel, V Hernquist, L AF Vogelsberger, Mark Sijacki, Debora Keres, Dusan Springel, Volker Hernquist, Lars TI Moving mesh cosmology: numerical techniques and global statistics SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: formation; dark matter ID SMOOTHED PARTICLE HYDRODYNAMICS; COLD DARK-MATTER; LYMAN-ALPHA FOREST; SIMULATED GALAXY CLUSTERS; PHASE-SPACE STRUCTURE; LAMBDA-CDM UNIVERSE; STAR-FORMATION; BLACK-HOLES; EXTRA LIGHT; MERGER REMNANTS AB We present the first hydrodynamical simulations of structure formation using the new moving mesh code AREPO and compare the results with GADGET simulations based on a traditional smoothed particle hydrodynamics (SPH) technique. The two codes share the same Tree-PM gravity solver and include identical subresolution physics for the treatment of star formation, but employ different methods to solve the equations of hydrodynamics. This allows us to assess the impact of hydro-solver uncertainties on the results of cosmological studies of galaxy formation. In this paper, we focus on predictions for global baryon statistics, such as the cosmic star formation rate density, after we introduce our simulation suite and numerical methods. Properties of individual galaxies and haloes are examined by Keres et al., while a third paper by Sijacki et al. uses idealized simulations to analyse in more detail the differences between the hydrodynamical schemes. We find that the global baryon statistics differ significantly between the two simulation approaches. AREPO shows systematically higher star formation rates at late times, lower mean temperatures averaged over the simulation volume and different gas mass fractions in characteristic phases of the intergalactic medium, in particular a reduced amount of hot gas. Although both hydrodynamical codes use the same implementation of cooling and yield an identical dark matter halo mass function, more gas cools out of haloes in AREPO compared with GADGET towards low redshifts, which results in corresponding differences in the late-time star formation rates of galaxies. We show that this difference is caused by a higher heating rate with SPH in the outer parts of haloes, owing to viscous dissipation of SPH's inherent sonic velocity noise and SPH's efficient damping of subsonic turbulence injected in the halo infall region, and because of a higher efficiency of gas stripping in AREPO. As a result of such differences, AREPO leads also to more disc-like morphologies in the moving mesh calculation compared to GADGET. Our results hence indicate that inaccuracies in hydrodynamic solvers can lead to comparatively large systematic differences even at the level of predictions for the global state of baryons in the universe. C1 [Vogelsberger, Mark; Sijacki, Debora; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, La Jolla, CA 92093 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. RP Vogelsberger, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mvogelsberger@cfa.harvard.edu FU NASA [HSTHF-51282.01-A, HSTHF-51276.01-A] FX The simulations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. Scaling tests were done on the Ranger cluster at the Texas Advanced Computing Center (TACC). We thank Paul Torrey for allowing us to show Fig. 21 and Elena D'Onghia, Patrik Jonsson, Andrew MacFadyen, Diego J. Munoz for useful discussions. We also thank the anonymous referee for helpful comments. DS acknowledges NASA Hubble Fellowship through grant HSTHF-51282.01-A. DK acknowledges support from NASA through Hubble Fellowship grant HSTHF-51276.01-A. NR 152 TC 99 Z9 99 U1 0 U2 3 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 425 IS 4 BP 3024 EP 3057 DI 10.1111/j.1365-2966.2012.21590.x PG 34 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135EN UT WOS:000318270500031 ER PT J AU Ubach, C Maddison, ST Wright, CM Wilner, DJ Lommen, DJP Koribalski, B AF Ubach, C. Maddison, S. T. Wright, C. M. Wilner, D. J. Lommen, D. J. P. Koribalski, B. TI Grain growth signatures in the protoplanetary discs of Chamaeleon and Lupus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: thermal; protoplanetary discs; stars: variables: T Tauri, Herbig Ae/Be; radio continuum: planetary systems ID T-TAURI STARS; MAIN-SEQUENCE STARS; YOUNG STELLAR OBJECTS; SPITZER C2D SURVEY; INFRARED SPECTROGRAPH SURVEY; CIRCUMSTELLAR DUST DISKS; 2008 EXTREME OUTBURST; HERBIG AE/BE STARS; EX-LUPI; FORMING REGION AB We present Australia Telescope Compact Array results of a 3 and 7 mm continuum survey of 20 T Tauri stars in the Chamaeleon and Lupus star-forming regions. This survey aims to identify protoplanetary discs with signs of grain growth. We detected 90 per cent of the sources at 3 and 7 mm, and determined the spectral slopes, dust opacity indices and dust disc masses. We also present temporal monitoring results of a small subset of sources at 7, 15 mm and 3+6 cm to investigate grain growth to centimetre (cm) sizes and constrain emission mechanisms in these sources. Additionally, we investigated the potential correlation between grain growth signatures in the infrared (10 mu m silicate feature) and millimetre (1-3 mm spectral slope, alpha). Eleven sources at 3 and 7 mm have dominant thermal dust emission up to 7 mm, with seven of these having a 1-3 mm dust opacity index less than unity, suggesting grain growth up to at least mm sizes. The Chamaeleon sources observed at 15 mm and beyond show the presence of excess emission from an ionized wind and/or chromospheric emission. Long-time-scale monitoring at 7 mm indicated that cm-sized pebbles are present in at least four sources. Short-time-scale monitoring at 15 mm suggests that the excess emission is from thermal free-free emission. Finally, a weak correlation was found between the strength of the 10 mu m feature and alpha, suggesting simultaneous dust evolution of the inner and outer parts of the disc. This survey shows that grain growth up to cm-sized pebbles and the presence of excess emission at 15 mm and beyond are common in these systems, and that temporal monitoring is required to disentangle these emission mechanisms. C1 [Ubach, C.; Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Wright, C. M.] UNSW ADFA, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. [Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lommen, D. J. P.] Raffles Inst, Singapore 575954, Singapore. [Ubach, C.; Koribalski, B.] ATNF, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. RP Ubach, C (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, H30,POB 218, Hawthorn, Vic 3122, Australia. EM cubach@astro.swin.edu.au FU CSIRO OCE Postgraduate Top Up Scholarship; Australian Research Council [DP0345227, FT100100495]; National Aeronautics and Space Administration; National Science Foundation FX Special thanks to the ATCA staff, the Spitzer Science Center Helpdesk and Leonardo Testi, Lucca Ricci and Francois Menard for useful discussions. Thanks also to Philip Edwards for awarding some discretionary time to help complete this project. We would also like to thank the referee for the useful comments and suggestions. This research was supported in part by a CSIRO OCE Postgraduate Top Up Scholarship. CMW acknowledges support from the Australian Research Council through Discovery Grant DP0345227 and Future Fellowship FT100100495. 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, and 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 105 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 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 425 IS 4 BP 3137 EP 3161 DI 10.1111/j.1365-2966.2012.21603.x PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 135EN UT WOS:000318270500039 ER PT J AU Clough, GW AF Clough, G. Wayne TI From the Castle 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 OCT PY 2012 VL 43 IS 6 BP 9 EP 9 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 126ST UT WOS:000317642200005 ER PT J AU Nicole, S Negrisolo, E Eccher, G Mantovani, R Patarnello, T Erickson, DL Kress, WJ Barcaccia, G AF Nicole, Silvia Negrisolo, Enrico Eccher, Giulia Mantovani, Roberto Patarnello, Tomaso Erickson, David L. Kress, W. John Barcaccia, Gianni TI DNA Barcoding as a Reliable Method for the Authentication of Commercial Seafood Products SO FOOD TECHNOLOGY AND BIOTECHNOLOGY LA English DT Article DE DNA barcoding; genetic traceability; BOLD; seafood; mislabeling ID FISH SPECIES IDENTIFICATION; CYTOCHROME-B GENE; MITOCHONDRIAL-DNA; MEAT-PRODUCTS; PCR METHOD; SEQUENCE; FOOD; TUNA; AMPLIFICATION; SUBSTITUTION AB Animal DNA barcoding allows researchers to identify different species by analyzing a short nucleotide sequence, typically the mitochondrial gene cox1. In this paper, we use DNA barcoding to genetically identify seafood samples that were purchased from various locations throughout Italy. We adopted a multi-locus approach to analyze the cob, 16S-rDNA and cox1 genes, and compared our sequences to reference sequences in the BOLD and GenBank online databases. Our method is a rapid and robust technique that can be used to genetically identify crustaceans, mollusks and fishes. This approach could be applied in the future for conservation, particularly for monitoring illegal trade of protected and endangered species. Additionally, this method could be used for authentication in order to detect mislabeling of commercially processed seafood. C1 [Nicole, Silvia; Eccher, Giulia; Mantovani, Roberto; Barcaccia, Gianni] Univ Padua, Dept Agron Food Nat Resources Anim & Environm, Lab Genet & Genom, IT-35020 Legnaro, Italy. [Negrisolo, Enrico; Patarnello, Tomaso] Univ Padua, Dept Comparat Biomed & Food Sci, IT-35020 Legnaro, Italy. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20013 USA. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Amer Hist, Labs Analyt Biol, Washington, DC 20013 USA. RP Barcaccia, G (reprint author), Univ Padua, Dept Agron Food Nat Resources Anim & Environm, Lab Genet & Genom, Campus Agripolis,Via Univ 16, IT-35020 Legnaro, Italy. EM gianni.barcaccia@unipd.it RI Negrisolo, Enrico/K-8124-2015; OI Negrisolo, Enrico/0000-0002-6244-805X; PATARNELLO, Tomaso/0000-0003-1794-5791 FU Italian Ministry of Education, University and Research FX The authors gratefully acknowledge funding for this research from the Italian Ministry of Education, University and Research (Project: 'Development of molecular diagnostic assays for the genetic traceability of agrifood products). The authors wish to thank Silvio Collani for his help with editing of the nucleotide sequences. Silvia Nicole learned the DNA barcoding technique that is the foundation of this study during her internship at the Laboratories of Analytical Biology of the Smithsonian Institution, Washington DC, USA. NR 69 TC 14 Z9 15 U1 3 U2 59 PU FACULTY FOOD TECHNOLOGY BIOTECHNOLOGY PI ZAGREB PA UNIV ZAGREB, KACIECEVA 23, 41000 ZAGREB, CROATIA SN 1330-9862 J9 FOOD TECHNOL BIOTECH JI Food Technol. Biotechnol. PD OCT-DEC PY 2012 VL 50 IS 4 BP 387 EP 398 PG 12 WC Biotechnology & Applied Microbiology; Food Science & Technology SC Biotechnology & Applied Microbiology; Food Science & Technology GA 070WJ UT WOS:000313544400001 ER PT J AU Darling, JA Herborg, LM Davidson, IC AF Darling, John A. Herborg, Leif-Matthias Davidson, Ian C. TI Intracoastal shipping drives patterns of regional population expansion by an invasive marine invertebrate SO ECOLOGY AND EVOLUTION LA English DT Article DE Invasive species; microsatellite; population genetics; Styela clava; vector analysis ID STYELA-CLAVA TUNICATA; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; NORTH-AMERICA; POTENTIAL DISTRIBUTION; MICROSATELLITE DATA; SPECIES INVASIONS; UNITED-STATES; ZEBRA MUSSELS; DISPERSAL AB Understanding the factors contributing to expansion of nonnative populations is a critical step toward accurate risk assessment and effective management of biological invasions. Nevertheless, few studies have attempted explicitly to test hypotheses regarding factors driving invasive spread by seeking correlations between patterns of vector movement and patterns of genetic connectivity. Herein, we describe such an attempt for the invasive tunicate Styela clava in the northeastern Pacific. We utilized microsatellite data to estimate gene flow between samples collected throughout the known range of S. clava in the region, and assessed correlation of these estimates with patterns of intracoastal commercial vessel traffic. Our results suggest that recent shipping patterns have contributed to the contemporary distribution of genetic variation. However, the analysis also indicates that other factors-including a complex invasion history and the influence of other vectors-have partially obscured genetic patterns associated with intracoastal population expansion. C1 [Darling, John A.] US EPA, Natl Exposure Res Lab, Durham, NC 27711 USA. [Herborg, Leif-Matthias] British Columbia Minist Environm, Victoria, BC V8W9M1, Canada. [Davidson, Ian C.] Portland State Univ, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. [Davidson, Ian C.] Smithsonian Environm Res Ctr, Portland, OR 97207 USA. RP Darling, JA (reprint author), US EPA, Natl Exposure Res Lab, 109 TW Alexander Dr, Durham, NC 27711 USA. EM darling.john@epa.gov OI Davidson, Ian/0000-0002-8729-6048 FU EPA Regional Applied Research Effort; Office of Research and Development; United States Environmental Protection Agency, through its Office of Research and Development FX Funded in part through an EPA Regional Applied Research Effort with Region 9, Region 10, and the Office of Research and Development.; The authors thank R Fairey, JT Carlton, J Bishop, L Dupont, T Therriault, LC Hannah, and HN Gartner for providing S. clava samples for genetic analysis. Fisheries and Oceans Canada, the California State Lands Commission, the Oregon ballast water reporting pilot program (at Portland State University), and the Washington Department of Fish & Wildlife provided shipping data. The United States Environmental Protection Agency, through its Office of Research and Development, funded and managed the research described here. It has been subjected to Agency administrative review and approved for publication. NR 61 TC 14 Z9 14 U1 3 U2 55 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD OCT PY 2012 VL 2 IS 10 BP 2552 EP 2561 DI 10.1002/ece3.362 PG 10 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 055XM UT WOS:000312451300017 PM 23145340 ER PT J AU Seely, J Feldman, U Brown, C Pereira, N Hudson, L Glover, J Silver, E AF Seely, John Feldman, Uri Brown, Charles Pereira, Nino Hudson, Lawrence Glover, Jack Silver, Eric TI Transmission crystal x-ray spectrometer covering the 6 keV-18 keV energy range with E/Delta E=1800 instrumental resolving power SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article; Proceedings Paper CT 19th Topical Conference on High-Temperature Plasma Diagnostics CY MAY 06-10, 2012 CL Monterey, CA AB A high-resolution x-ray spectrometer utilizing a thin quartz transmission crystal and covering the 6 keV-18 keV energy range has been developed and tested. The spectrometer consists of a cylindrically bent crystal in a vacuum housing. The crystal position and the range of Bragg angles that are incident on the crystal can be adjusted to record an approximate to 4 keV wide spectrum in the 6 keV-18 keV range. The spectrometer is of the Cauchois type and has a compact linear geometry that is convenient for deployment at laser-produced plasma, EBIT, and other x-ray sources. Test spectra of the W L and Mo K lines from laboratory sources have linewidths as small as 11 eV, approaching the natural widths, and instrumental resolving power as high as 1800. Techniques for enhancing the energy resolution are experimentally demonstrated. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4732184] C1 [Seely, John; Feldman, Uri] Artep Inc, Ellicott City, MD 21042 USA. [Brown, Charles] USN, Res Lab, Washington, DC 20375 USA. [Pereira, Nino] Ecopulse Inc, Springfield, VA 22150 USA. [Hudson, Lawrence; Glover, Jack] NIST, Gaithersburg, MD 20899 USA. [Silver, Eric] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Seely, J (reprint author), Artep Inc, 2922 Excelsior Springs Court, Ellicott City, MD 21042 USA. EM seelyjf@gmail.com NR 3 TC 3 Z9 3 U1 0 U2 5 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD OCT PY 2012 VL 83 IS 10 AR 10E112 DI 10.1063/1.4732184 PN 2 PG 3 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 043RB UT WOS:000311562900120 PM 23126934 ER PT J AU Ando, A AF Ando, Atsushi TI TAXONOMIC REEXAMINATION AND TYPE-LOCALITY ASSEMBLAGE CHARACTERIZATION OF THE LATE ALBIAN PLANKTONIC FORAMINIFERA HEDBERGELLA YEZOANA TAKAYANAGI AND IWAMOTO, 1962, FROM JAPAN SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID OCEAN; SEA; BIOSTRATIGRAPHY; CLASSIFICATION; TURNOVER; ZONATION; PACIFIC AB The late Albian planktonic foraminifera Hedbergella trocoidea yezoana Takayanagi and Iwamoto, 1962, from Japan, whose primary distinguishing feature is 7-8 chambers in the final whorl, has been internationally cited with a species rank as Hedbergella yezoana. Still, its taxonomic position is not well understood, as manifested by the fact that published hypotypes have six or fewer chambered forms, and such ambiguity is due partly to a lack of updated knowledge about the primary types (a holotype and single paratype), topotypes, and hypotypes from the northwestern Pacific region. This study reexamines the species concept of Hd. yezoana through uncoated SEM observations of the primary types and newly obtained type-locality material. The holotype is synonymous with Ticinella primula Luterbacher, 1963, as judged by its uneven wall surface, pseudoplanispiral (slightly streptospiral) mode of coiling, somewhat tangentially elongate last chambers, and a possible porticus-like structure. The topotypes exhibit important characters such as supplementary apertures and well-developed portici, thus confirming the synonymy of Hd. yezoana and T. primula. This outcome, however, is troublesome because T. primula is the widely used name for this morphology, and accepting the priority of "Ticinella yezoana" affects the nomenclatural stability in Cretaceous planktonic foraminifera. Conservation of the junior name T. primula is supported not only by the insufficient preservation of the Hokkaido material but also by the concept of Article 23.9 (reversal of precedence) in the International Code of Zoological Nomenclature (4th edition, 1999), although a ruling from the Zoological Commission would be eventually necessary. The paratype, in contrast, exhibits a smooth, microperforate wall, and is identified in open nomenclature as Microhedbergella sp. A (multi-chambered form). In addition to this wall-surface feature, this potential new Microhedbergella taxon differs from the "Hd. yezoana" holotype (and hence from T. primula) by lacking a streptospiral mode of coiling, exhibiting isomorphic globular chambers between the umbilical and spiral sides, and possessing a very poorly developed or nearly absent lip. The type-locality assemblage of "Hd. yezoana" is marked by the common occurrence of several other "ticinellid" taxa (Biticinella breggiensis and at least three species of Ticinella) and Microhedbergella with very rare Favusella. The Microhedbergella specimens have a remarkably wide range of morphologies, some comparable to those recorded in a local Texas assemblage, but the rest undescribed. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Ando, A (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012,MRC 121, Washington, DC 20013 USA. EM AndoA@si.edu FU Japan Society for the Promotion of Science (JSPS) FX The author would like to express his sincere gratitude to Yokichi Takayanagi (Emeritus Professor, Tohoku University) for comments on the draft of this paper, with warm words of agreement on this taxonomic treatment and encouragement. Thanks are extended to Shulamit Lipson-Benitah and Michel Moullade for their reviews, Brian T. Huber for permission to use his research collection for supplementary work on this study and for improvement of the revised manuscript, Scott D. Whittaker for his help with the use of SEM facilities at the Smithsonian Institution, and Paul Brenckle for his thorough editorial work. This research was financially supported by a grant-in-aid for the Japan Society for the Promotion of Science (JSPS) Research Fellow to A. A. (Chiba University; FY 2003-2005). Some material used in this study was provided by the Integrated Ocean Drilling Program. NR 58 TC 2 Z9 3 U1 0 U2 4 PU CUSHMAN FOUNDATION FORAMINIFERAL RES PI CAMBRIDGE PA MUSEUM COMPARATIVE ZOOLOGY, DEPT INVERTEBRATE PALEONTOLOGY 26 OXFORD ST, HARVARD UNIV, CAMBRIDGE, MA 02138 USA SN 0096-1191 J9 J FORAMIN RES JI J. Foraminifer. Res. PD OCT PY 2012 VL 42 IS 4 BP 271 EP 285 PG 15 WC Paleontology SC Paleontology GA 036GC UT WOS:000311013400001 ER PT J AU Krakker, JJ AF Krakker, James J. TI MUD WASP NESTS AS MARKERS OF MIDDLE HOLOCENE HOUSE STRUCTURES IN THE CENTRAL MISSISSIPPI VALLEY SO AMERICAN ANTIQUITY LA English DT Article AB Lumps of burned clay recovered from the Lepold site (23RI59) include four mud wasp nests deposited 5500 to 6200 B.P. or perhaps slightly earlier. These provide indirect evidence of structures at the site. Existence of structures would be consistent with intensive occupation and increased occupation episode length evident at this site and elsewhere in the central Mississippi valley during the Middle Holocene. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Krakker, JJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM krakkerj@si.edu NR 28 TC 0 Z9 0 U1 0 U2 0 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 0002-7316 J9 AM ANTIQUITY JI Am. Antiq. PD OCT PY 2012 VL 77 IS 4 BP 800 EP 807 PG 8 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 031PD UT WOS:000310653500011 ER PT J AU Dick, SJ AF Dick, Steven J. TI Critical Issues in the History, Philosophy, and Sociology of Astrobiology SO ASTROBIOLOGY LA English DT Review DE Bioastronomy; Astrobiology; Intelligence; Life; SETI ID EXTRATERRESTRIAL LIFE DEBATE; DEFINING LIFE; EXOBIOLOGY; COMPANION; SCIENCE; EARTH; BIOSIGNATURES; ORGANIZATION; SOCIETY; BIOLOGY AB Fifty years after serious scientific research began in the field of exobiology, and forty years after serious historical research began on the subject of extraterrestrial life, this paper identifies and examines some of the most important issues in the history, philosophy, and sociology of what is today known as astrobiology. As in the philosophy of science in general, and in the philosophies of particular sciences, critical issues in the philosophy and sociology of astrobiology are both stimulated and illuminated by history. Among those issues are (1) epistemological issues such as the status of astrobiology as a science, the problematic nature of evidence and inference, and the limits of science; (2) metaphysical/scientific issues, including the question of defining the fundamental concepts of life, mind, intelligence, and culture in a universal context; the role of contingency and necessity in the origin of these fundamental phenomena; and whether or not the universe is in some sense fine-tuned for life and perhaps biocentric; (3) societal issues such as the theological, ethical, and worldview impacts of the discovery of microbial or intelligent life; and the question of whether the search for extraterrestrial life should be pursued at all, and with what precautions; and (4) issues related to the sociology of scientific knowledge, including the diverse attitudes and assumptions of different scientific communities and different cultures to the problem of life beyond Earth, the public "will to believe," and the formation of the discipline of astrobiology. All these overlapping issues are framed by the concept of cosmic evolution-the 13.7 billion year Master Narrative of the Universe-which may result in a physical, biological, or postbiological universe and determine the long-term destiny of humanity. C1 [Dick, Steven J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Dick, SJ (reprint author), 21406 Clearfork Ct, Ashburn, VA 20147 USA. EM stevedick1@comcast.net NR 271 TC 4 Z9 4 U1 2 U2 42 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD OCT PY 2012 VL 12 IS 10 BP 906 EP 927 DI 10.1089/ast.2011.0786 PG 22 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 025TQ UT WOS:000310217900002 PM 23078642 ER PT J AU Rivers, JW Young, S Gonzalez, EG Horton, B Lock, J Fleischer, RC AF Rivers, James W. Young, Sarah Gonzalez, Elena G. Horton, Brent Lock, Justin Fleischer, Robert C. TI HIGH LEVELS OF RELATEDNESS BETWEEN BROWN-HEADED COWBIRD (MOLOTHRUS ATER) NESTMATES IN A HEAVILY PARASITIZED HOST COMMUNITY SO AUK LA English DT Article DE Brown-headed Cowbird; generalist brood parasite; kinship; laying pattern; Molothrus ater; nestmate relatedness ID GENERALIST BROOD PARASITE; MULTIPLE PARASITISM; TEMPORAL PATTERNS; BEGGING BEHAVIOR; DICKCISSELS; NESTLINGS; SUCCESS; NESTS; PARENTS; PRAIRIE AB Multiple parasitism of host nests by generalist brood parasites reflects the decisions of laying females and may influence the development and behavior of parasitic young. We used microsatellite and mtDNA control-region haplotype data to examine the relatedness of Brown-headed Cowbird (Molothrus ater) offspring in multiply parasitized nests sampled from a heavily parasitized host community in northeastern Kansas. We also examined how host nest availability influenced the degree of multiple parasitism, and used community-wide parasitism data to explore whether female cowbirds were constrained in their laying decisions. Relatedness estimates for all suitable pairwise comparisons (n = 94 from 41 multiply parasitized nests) found that the mean likelihood than an individual cowbird in a multiply parasitized nest shared its nest with a full sibling was 40.4% (95% confidence interval: 28.4-52.4%), indicating that many cowbird offspring were reared with full siblings. Extensive community-wide parasitism data revealed that most cowbird offspring shared the nest with >= 1 other conspecific. Additionally, we found that the proportion of available host nests increased steeply at the start of the breeding season and remained high for most of the breeding season, but that the degree of multiple parasitism was unrelated to the number of new nests. We found evidence that laying decisions of female cowbirds were constrained, which suggests that heavy parasitism levels were due to a high degree of competition for host nests. This intense competition for host nests, in turn, results in cowbird offspring often competing with conspecifics in our population, including full siblings, for host parental care. Received 14 October 2011, accepted 13 July 2012. C1 [Rivers, James W.] Univ Calif Santa Barbara, Dept Ecol Evolut & Marine Biol, Santa Barbara, CA 93106 USA. [Young, Sarah; Gonzalez, Elena G.; Horton, Brent; Lock, Justin; Fleischer, Robert C.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Rivers, JW (reprint author), Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. EM jim.rivers@oregonstate.edu RI Gonzalez, Elena/E-4465-2013; Young, Sarah/E-2883-2014 OI Gonzalez, Elena/0000-0002-4614-3889; Young, Sarah/0000-0002-8301-5106 FU American Ornithologists' Union; Animal Behavior Society; Chapman Fund of the American Museum of Natural History; Cooper Ornithological Society; Helmetcamera.com; Sigma Xi Honor Society; Los Angeles Audubon Society; Graduate Division; Academic Senate at the University of California, Santa Barbara; National Science Foundation (NSF) Doctoral Dissertation Improvement Grant program [IOB-0608263]; NSF Long-Term Ecological Research Program at Konza Prairie Biological Station; Smithsonian Institution's Center for Conservation and Evolutionary Genetics FX Financial support was provided by the American Ornithologists' Union, Animal Behavior Society, Chapman Fund of the American Museum of Natural History, Cooper Ornithological Society, Helmetcamera.com, Sigma Xi Honor Society, Los Angeles Audubon Society, the Graduate Division and the Academic Senate at the University of California, Santa Barbara, the National Science Foundation (NSF) Doctoral Dissertation Improvement Grant program (IOB-0608263), the NSF Long-Term Ecological Research Program at Konza Prairie Biological Station, and the Smithsonian Institution's Center for Conservation and Evolutionary Genetics. We thank M. Blundell, J. Hite, W. Janousek, A. Lyon, E. McCarthy, R. Rehmeier, B. Sandercock, and B. Van Korff for assistance in locating nests, B. K. Sandercock for extensive logistical support, C. McIntosh and N. Rotzel for facilitation of laboratory work at the Smithsonian, W. E. Jensen, P. Klug, K. L. Kosciuch and E. Hewett for sharing parasitism data, T. M. Loughin for statistical advice, and J. V. Briskie, B. D. Peer, J. C. Reboreda, S. I. Rothstein, and several anonymous reviewers for helpful comments on the manuscript. NR 54 TC 12 Z9 13 U1 1 U2 32 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2012 VL 129 IS 4 BP 623 EP 631 DI 10.1525/auk.2012.11236 PG 9 WC Ornithology SC Zoology GA 031RJ UT WOS:000310659700004 ER PT J AU Zhang, ZH Huang, YP James, HF Hou, LH AF Zhang, Zihui Huang, Yunping James, Helen F. Hou, Lianhai TI A MARABOU (CICONIIDAE: LEPTOPTILOS) FROM THE MIDDLE PLEISTOCENE OF NORTHEASTERN CHINA SO AUK LA English DT Article DE biogeography; Jinniushan site; Leptoptilos lui sp nov.; Middle Pleistocene; northeastern China ID STORK; AVES; MIOCENE AB A new species of marabou, Leptoptilos lui sp. nov., is described on the basis of a cranium, distal humerus, and proximal phalanx of the major digit, from the Middle Pleistocene Jinniushan locality, Liaoning Province of northeastern China. Fossil crania of the genus Leptoptilos are rare, and that of the new bird is distinct from the crania of its extant relatives. The forelimb elements are the largest and most robust among living and fossil species of Leptoptilos and are characterized by autapomorphic characters. Leptoptilos lui, like the African Marabou Stork (L. crumeniferus), probably possessed a considerable flight capability and fed mainly on pieces of carrion torn from carcasses by other, sympatric large scavengers. The new stork aids in our understanding of the paleoecology and paleoenvironment of northeastern China in the Middle Pleistocene, helps us characterize the scavenger guild that fed on the Middle Pleistocene megafauna, and shows that the genus Leptoptilos, now restricted to the Old World tropics, extended into higher latitudes in the Middle Pleistocene. Received 7 October 2011, accepted 11 June 2012. C1 [Zhang, Zihui; Hou, Lianhai] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Huang, Yunping] Peking Univ, Sch Archaeol & Museol, Beijing 100871, Peoples R China. [James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Hou, Lianhai] Chinese Acad Sci, Inst Vertebrate Paleontol & Paleoanthropol, Beijing 100044, Peoples R China. RP Zhang, ZH (reprint author), Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. EM zihuizhang@mail.cnu.edu.cn FU National Natural Science Foundation of China [30870263, 31071877] FX We are grateful to personnel of the field group from the School of Archaeology and Museology at Peking University and the Cultural Relics and Archaeology Institute of Liaoning Province for discovering the specimens; H. Meijer for sharing calipers and research articles, and for her useful comments and discussion; J. DiLoreto, M. Spitzer, and T. Hsu for help with photography and illustration; and G. Mayr, A. Louchart, J. Noriega, and A. Feduccia for reviewing and helping to improve the manuscript. This work was supported partly by the National Natural Science Foundation of China (30870263, 31071877) and was performed during a residency in the Division of Birds, National Museum of Natural History, Smithsonian Institution, Washington, D.C. NR 27 TC 2 Z9 2 U1 0 U2 5 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2012 VL 129 IS 4 BP 699 EP 706 DI 10.1525/auk.2012.11227 PG 8 WC Ornithology SC Zoology GA 031RJ UT WOS:000310659700013 ER PT J AU Rockwell, SM Bocetti, CI Marra, PP AF Rockwell, Sarah M. Bocetti, Carol I. Marra, Peter P. TI CARRY-OVER EFFECTS OF WINTER CLIMATE ON SPRING ARRIVAL DATE AND REPRODUCTIVE SUCCESS IN AN ENDANGERED MIGRATORY BIRD, KIRTLAND'S WARBLER (SETOPHAGA KIRTLANDII) SO AUK LA English DT Article DE arrival dates; climate change; Kirtland's Warbler; migratory birds; reproductive success; Setophaga kirtlandii; winter rainfall ID NEOTROPICAL MIGRANT SONGBIRD; NORTH-ATLANTIC OSCILLATION; WEST-AFRICAN RAINFALL; HABITAT SEGREGATION; NONBREEDING-SEASON; AMERICAN REDSTARTS; FOOD AVAILABILITY; PIED FLYCATCHERS; SEXUAL SELECTION; BODY CONDITION AB Understanding how animals will adapt to climate change requires understanding how climate variables influence their biology year round, and how events in different seasons interact. Migratory birds may be especially vulnerable because of the wide range of geographic areas that they depend on throughout the annual cycle. We examined the potential effects of non-breeding season climate change on the breeding biology of Kirtland's Warbler (Setophaga kirtlandii, formerly Dendroica kirtlandii), an endangered songbird that breeds in the Northern Lower Peninsula of Michigan and winters in the Bahamas. Our objectives were to determine whether spring arrival dates on the breeding grounds correlate with late winter rainfall in non-breeding areas and whether this has consequences for reproductive success. We used data on spring arrival dates and number of fledglings per year, sampling many individuals across multiple years, to show that males arrive on breeding grounds later following drier winters. There was a strong male age * rainfall interaction, which indicates that first-time breeders were much more sensitive to changes in rainfall than experienced adults. Regardless of age, however, drier winters and delayed arrival and nest initiation were significantly associated with fewer offspring fledged. These results are important because the Caribbean region is currently experiencing a significant drying trend, and climate change models predict that the severity of this drought will continue to increase. Any resulting adjustments to the timing of migration could constrain spring arrival dates and limit reproductive success for the endangered Kirtland's Warbler, as well as other Neotropical migrants wintering in the Caribbean. Received 6 January 2012, accepted 30 March 2012. C1 [Rockwell, Sarah M.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. RP Rockwell, SM (reprint author), Univ Maryland, Dept Biol, 1210 Biol Psychol Bldg, College Pk, MD 20742 USA. EM rockwell@umd.edu FU American Ornithologists' Union; Cooper Ornithological Society; Manomet Center for Conservation Science; Smithsonian Institution; University of Maryland; U.S. Fish and Wildlife Service; U.S. Forest Service FX This research was supported by funding from the American Ornithologists' Union, Cooper Ornithological Society, Manomet Center for Conservation Science, Smithsonian Institution, University of Maryland, U.S. Fish and Wildlife Service, and U.S. Forest Service. We thank M. Thomas, E. Joseph, R. Badia, R. Slebodnik, A. Frazee, S. Brounce, A. Demko, P. Falatek, E. Banfield, L. Williams, M. Thomas, A. Rogers, B. Kaimal, V. Shevade, and D. Wloch for their hard work in the field. We are grateful to J. Wunderle for sharing his findings, D. Ewert for assistance in the field, C. Studds for help with field work and statistical analyses, and P. Blank for GIS assistance. This work was done in cooperation with the Kirtland's Warbler Recovery Team, who granted their support and access to field sites. D. Inouye, T. S. Sillett, and two anonymous reviewers provided comments that helped improve the manuscript. The National Climatic Data Center of the National Oceanic and Atmospheric Association is available online at www7.ncdc.noaa.gov/IPS/mcdw/mcdw.html. NR 79 TC 27 Z9 28 U1 11 U2 143 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2012 VL 129 IS 4 BP 744 EP 752 DI 10.1525/auk.2012.12003 PG 9 WC Ornithology SC Zoology GA 031RJ UT WOS:000310659700018 ER PT J AU Olson, SL AF Olson, Storrs L. TI IN MEMORIAM: EVGENY N. KUROCHKIN, 1940-2011 SO AUK LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 3 U2 3 PU AMER ORNITHOLOGISTS UNION PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0004-8038 J9 AUK JI AUK PD OCT PY 2012 VL 129 IS 4 BP 790 EP 791 PG 2 WC Ornithology SC Zoology GA 031RJ UT WOS:000310659700026 ER PT J AU Sillett, TS Chandler, RB Royle, JA Kery, M Morrison, SA AF Sillett, T. Scott Chandler, Richard B. Royle, J. Andrew Kery, Marc Morrison, Scott A. TI Hierarchical distance-sampling models to estimate population size and habitat-specific abundance of an island endemic SO ECOLOGICAL APPLICATIONS LA English DT Article DE Aphelocoma insularis; biodiversity conservation; California Channel Islands; distance sampling; hierarchical models ID SANTA-CRUZ ISLAND; WEST-NILE-VIRUS; SCRUB-JAY; APHELOCOMA-INSULARIS; CALIFORNIA; METAPOPULATION; CONSERVATION; INFERENCE; SURVIVAL; WARBLERS AB Population size and habitat-specific abundance estimates are essential for conservation management. A major impediment to obtaining such estimates is that few statistical models are able to simultaneously account for both spatial variation in abundance and heterogeneity in detection probability, and still be amenable to large-scale applications. The hierarchical distance-sampling model of J. A. Royle, D. K. Dawson, and S. Bates provides a practical solution. Here, we extend this model to estimate habitat-specific abundance and rangewide population size of a bird species of management concern, the Island Scrub-Jay (Aphelocoma insularis), which occurs solely on Santa Cruz Island, California, USA. We surveyed 307 randomly selected, 300 m diameter, point locations throughout the 250-km(2) island during October 2008 and April 2009. Population size was estimated to be 2267 (95% CI 1613-3007) and 1705 (1212-2369) during the fall and spring respectively, considerably lower than a previously published but statistically problematic estimate of 12 500. This large discrepancy emphasizes the importance of proper survey design and analysis for obtaining reliable information for management decisions. Jays were most abundant in low-elevation chaparral habitat; the detection function depended primarily on the percent cover of chaparral and forest within count circles. Vegetation change on the island has been dramatic in recent decades, due to release from herbivory following the eradication of feral sheep (Ovis aries) from the majority of the island in the mid-1980s. We applied best-fit fall and spring models of habitat-specific jay abundance to a vegetation map from 1985, and estimated the population size of A. insularis was 1400-1500 at that time. The 20-30% increase in the jay population suggests that the species has benefited from the recovery of native vegetation since sheep removal. Nevertheless, this jay's tiny range and small population size make it vulnerable to natural disasters and to habitat alteration related to climate change. Our results demonstrate that hierarchical distance-sampling models hold promise for estimating population size and spatial density variation at large scales. Our statistical methods have been incorporated into the R package unmarked to facilitate their use by animal ecologists, and we provide annotated code in the Supplement. C1 [Sillett, T. Scott] Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Chandler, Richard B.; Royle, J. Andrew] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Kery, Marc] Swiss Ornithol Inst, CH-6204 Sempach, Switzerland. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA 94105 USA. RP Sillett, TS (reprint author), Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Natl Zool Pk,MRC 5503, Washington, DC 20013 USA. EM silletts@si.edu RI Chandler, Richard/D-8831-2014; Chandler, Richard/F-9702-2016; OI Royle, Jeffrey/0000-0003-3135-2167 FU Nature Conservancy; Smithsonian Institution; Channel Islands National Park; U.S. Fish and Wildlife Service FX We thank The Nature Conservancy and Channel Islands National Park for ongoing support of the Island Scrub-Jay Conservation Initiative, John Knapp and Native Range, Inc., for coordinating safe and efficient helicopter support of the jay surveys, Kathryn McEachern for sharing her vegetation data set, Victoria Bakker for assistance with selection of survey points, Brian Cohen for GIS analyses and all project cartography, and our talented, adrenaline-fueled field technicians (Allison Byrd, Luke Caldwell, Michelle Desrosiers, Jenelle Dowling, Benjamin Griffith, Jonathan Gunther, Kathryn Langin, and Anna Potter) for making this study possible. Our sampling design and this paper were improved by comments from V. Bakker, Reed Bowman, L. Caldwell, Daniel Doak, John Fitzpatrick, David Graber, K. Langin, Lyndal Laughrin, Jim Lyons, Frank Rivera, J. Michael Scott, Jerre Stallcup, and two anonymous reviewers. Funding was provided by The Nature Conservancy, the Smithsonian Institution, Channel Islands National Park, and the U.S. Fish and Wildlife Service. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. Government. NR 46 TC 25 Z9 25 U1 4 U2 113 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1051-0761 EI 1939-5582 J9 ECOL APPL JI Ecol. Appl. PD OCT PY 2012 VL 22 IS 7 BP 1997 EP 2006 PG 10 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 031GA UT WOS:000310626100011 PM 23210315 ER PT J AU Ogburn, MB Forward, RB AF Ogburn, Matthew B. Forward, Richard B., Jr. TI Effect of sampling interval on estimates of larval supply SO FISHERY BULLETIN LA English DT Article ID CALLINECTES-SAPIDUS MEGALOPAE; NORTH-CAROLINA ESTUARY; BLUE-CRAB; SETTLEMENT; ABUNDANCE; VARIABILITY AB Estimates of larval supply can provide information on year-class strength that is useful for fisheries management. However, larval supply is difficult to monitor because long-term, high-frequency sampling is needed. The purpose of this study was to subsample an 11-year record of daily larval supply of blue crab (Callinectes sapidus) to determine the effect of sampling interval on variability in estimates of supply. The coefficient of variation in estimates of supply varied by 0.39 among years at a 2-day sampling interval and 0.84 at a 7-day sampling interval. For 8 of the 11 years, there was a significant correlation between mean daily larval supply and lagged fishery catch per trip (coefficient of correlation [r] = 0.88). When these 8 years were subsampled, a 2-day sampling interval yielded a significant correlation with fishery data only 64.5% of the time and a 3-day sampling interval never yielded a significant correlation. Therefore, high-frequency sampling (daily or every other day) may be needed to characterize interannual variability in larval supply. C1 [Ogburn, Matthew B.; Forward, Richard B., Jr.] Duke Univ, Marine Lab, Beaufort, NC 28516 USA. [Ogburn, Matthew B.] Savannah State Univ, Savannah, GA 31404 USA. RP Ogburn, MB (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM ogburnm@si.edu OI Ogburn, Matthew/0000-0001-5417-555X FU North Carolina Sea Grants [2004-1772-01, 2004-1772-33, 2004-1772-43]; National Science Foundation [OCE-9819355, OCE-0095092]; U. S. Department of Commerce, NOAA, National Marine Fisheries Service under NOAA Living Marine Resources Cooperative Science Center [PL 88-309, 2-296-R, NA05OAR4811017] FX We thank H. Diaz, R. Irvine, J. Lax, R. Mitchell, A. Schick, M. Smith, J. Thompson, and J. Venezia for assistance with larval sampling. Technical assistance was provided by J. Priddy. This study was supported under North Carolina Sea Grants 2004-1772-01, -33, and -43, National Science Foundation Grants no. OCE-9819355 and OCE-0095092, and U. S. Department of Commerce, NOAA, National Marine Fisheries Service, under PL 88-309, Project 2-296-R, NOAA Living Marine Resources Cooperative Science Center NA05OAR4811017. NR 17 TC 0 Z9 0 U1 0 U2 6 PU NATL MARINE FISHERIES SERVICE SCIENTIFIC PUBL OFFICE PI SEATTLE PA 7600 SAND POINT WAY NE BIN C15700, SEATTLE, WA 98115 USA SN 0090-0656 J9 FISH B-NOAA JI Fish. Bull. PD OCT PY 2012 VL 110 IS 4 BP 451 EP 457 PG 7 WC Fisheries SC Fisheries GA 030HM UT WOS:000310561700005 ER PT J AU Adamczak, J Werner, K Rauch, T Schuh, S Drake, JJ Kruk, JW AF Adamczak, J. Werner, K. Rauch, T. Schuh, S. Drake, J. J. Kruk, J. W. TI Chandra grating spectroscopy of three hot white dwarfs SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE white dwarfs; stars: abundances; stars: atmospheres; stars: individual: LB1919; stars: individual: GD246; stars: individual: PG1520+525 ID PG 1159 STARS; MASS-DISTRIBUTION; EQUILIBRIUM ABUNDANCES; RADIATIVE LEVITATION; FUSE OBSERVATIONS; INTERSTELLAR; STELLAR; DIFFUSION; HELIUM; LINES AB Context. High-resolution soft X-ray spectroscopic observations of single hot white dwarfs are scarce. With the Chandra Low-Energy Transmission Grating, we have observed two white dwarfs, one is of spectral type DA (LB 1919) and the other is a non-DA of spectral type PG1159 (PG1520+525). The spectra of both stars are analyzed, together with an archival Chandra spectrum of another DA white dwarf (GD246). Aims. The soft X-ray spectra of the two DA white dwarfs are investigated in order to study the effect of gravitational settling and radiative levitation of metals in their photospheres. LB1919 is of interest because it has a significantly lower metallicity than DAs with otherwise similar atmospheric parameters. GD246 is the only white dwarf known that shows identifiable individual iron lines in the soft X-ray range. For the PG1159 star, a precise effective temperature determination is performed in order to confine the position of the blue edge of the GW Vir instability region in the HRD. Methods. The Chandra spectra are analyzed with chemically homogeneous as well as stratified NLTE model atmospheres that assume equilibrium between gravitational settling and radiative acceleration of chemical elements. Archival EUV and UV spectra obtained with EUVE, FUSE, and HST are utilized to support the analysis. Results. No metals could be identified in LB1919. All observations are compatible with a pure hydrogen atmosphere. This is in stark contrast to the vast majority of hot DA white dwarfs that exhibit light and heavy metals and to the stratified models that predict significant metal abundances in the atmosphere. For GD246 we find that neither stratified nor homogeneous models can fit the Chandra spectrum. The Chandra spectrum of PG1520+525 constrains the effective temperature to T-eff = 150 000 +/- 10 000 K. Therefore, this nonpulsating star together with the pulsating prototype of the GWVir class (PG 1159-035) defines the location of the blue edge of the GWVir instability region. The result is in accordance with predictions from nonadiabatic stellar pulsation models. Such models are therefore reliable tools to investigate the interior structure of GW Vir variables. Conclusions. Our soft X-ray study reveals that the understanding of metal abundances in hot DA white dwarf atmospheres is still incomplete. On the other hand, model atmospheres of hydrogen-deficient PG 1159-type stars are reliable and reproduce well the observed spectra from soft X-ray to optical wavelengths. C1 [Adamczak, J.; Werner, K.; Rauch, T.] Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Adamczak, J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Schuh, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kruk, J. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Adamczak, J (reprint author), Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany. EM adamczak@astro.as.utexas.edu FU German Research Foundation (DFG) [WE 1312/39-1]; German Aerospace Center (DLR) [05 OR 0806]; NASA [NAS8-39073, NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We thank the referee for a thorough and constructive report. J.A. and T. R. were supported by the German Research Foundation (DFG) under grant WE 1312/39-1 and the German Aerospace Center (DLR) under grant 05 OR 0806, respectively. J.J.D. was supported by NASA contract NAS8-39073 to the Chandra X-ray Center during the course of this work. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (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 59 TC 1 Z9 1 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A1 DI 10.1051/0004-6361/201219718 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100001 ER PT J AU Bjerkeli, P Liseau, R Larsson, B Rydbeck, G Nisini, B Tafalla, M Antoniucci, S Benedettini, M Bergman, P Cabrit, S Giannini, T Melnick, G Neufeld, D Santangelo, G van Dishoeck, EF AF Bjerkeli, P. Liseau, R. Larsson, B. Rydbeck, G. Nisini, B. Tafalla, M. Antoniucci, S. Benedettini, M. Bergman, P. Cabrit, S. Giannini, T. Melnick, G. Neufeld, D. Santangelo, G. van Dishoeck, E. F. TI H2O line mapping at high spatial and spectral resolution Herschel observations of the VLA 1623 outflow SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: individual objects: VLA1623; ISM: molecules; ISM: abundances; ISM: jets and outflows; stars: formation; stars: winds, outflows ID RHO-OPHIUCHI CLOUD; WAVE-ASTRONOMY-SATELLITE; STAR-FORMING REGIONS; MOLECULAR OUTFLOWS; WATER EMISSION; SHOCK-WAVES; H-2; EXCITATION; HIFI; CO AB Context. Apart from being an important coolant, water is known to be a tracer of high-velocity molecular gas. Recent models predict relatively high abundances behind interstellar shockwaves. The dynamical and physical conditions of the water emitting gas, however, are not fully understood yet. Using the Herschel Space Observatory, it is now possible to observe water emission from supersonic molecular outflows at high spectral and spatial resolution. Several molecular outflows from young stars are currently being observed as part of the WISH (Water In Star-forming regions with Herschel) key program. Aims. We aim to determine the abundance and distribution of water, its kinematics, and the physical conditions of the gas responsible for the water emission. The observed line profile shapes help us understand the dynamics in molecular outflows. Methods. We mapped the VLA1623 outflow, in the ground-state transitions of o-H2O, with the HIFI and PACS instruments. We also present observations of higher energy transitions of o-H2O and p-H2O obtained with HIFI and PACS towards selected outflow positions. From comparison with non-LTE radiative transfer calculations, we estimate the physical parameters of the water emitting regions. Results. The observed water emission line profiles vary over the mapped area. Spectral features and components, tracing gas in different excitation conditions, allow us to constrain the density and temperature of the gas. The water emission originates in a region where temperatures are comparable to that of the warm H-2 gas (T greater than or similar to 200 K). Thus, the water emission traces a gas component significantly warmer than the gas responsible for the low-J CO emission. The water column densities at the CO peak positions are low, i.e. N(H2O) similar or equal to (0.03-10) x 10(14) cm(-2). Conclusions. The water abundance with respect to H-2 in the extended outflow is estimated at X(H2O) < 1 x 10(-6), significantly lower than what would be expected from most recent shock models. The H2O emission traces a gas component moving at relatively high velocity compared to the low-J CO emitting gas. However, other dynamical quantities such as the momentum rate, energy, and mechanical luminosity are estimated to be the same, independent of the molecular tracer used, CO or H2O. C1 [Bjerkeli, P.; Liseau, R.; Rydbeck, G.] Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. [Larsson, B.] Stockholm Univ, Dept Astron, S-10691 Stockholm, Sweden. [Nisini, B.; Antoniucci, S.; Giannini, T.; Santangelo, G.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Benedettini, M.] INAF Inst Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Cabrit, S.] CNRS, UMR 8112, Observ Paris, LERMA, F-75014 Paris, France. [Neufeld, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Bjerkeli, P (reprint author), Chalmers, Onsala Space Observ, Dept Earth & Space Sci, S-43992 Onsala, Sweden. EM per.bjerkeli@chalmers.se OI Giannini, Teresa/0000-0002-0224-096X; Bjerkeli, Per/0000-0002-7993-4118 FU Swedish National Space Board (SNSB); ASI [I/005/011/0]; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX The Swedish authors appreciate the support from the Swedish National Space Board (SNSB). Italian authors acknowledge the support from ASI through the contract I/005/011/0. We appreciate the valuable comments made by the anonymous referee. We also thank the HIFI and PACS ICC's for excellent support and the WISH internal referee Lars Kristensen for insightful comments and careful reading of the manuscipt. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri - INAF; The Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAF-IFSI/OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). NR 55 TC 20 Z9 20 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A29 DI 10.1051/0004-6361/201219776 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100029 ER PT J AU Israel, H Erben, T Reiprich, TH Vikhlinin, A Sarazin, CL Schneider, P AF Israel, H. Erben, T. Reiprich, T. H. Vikhlinin, A. Sarazin, C. L. Schneider, P. TI The 400d Galaxy Cluster Survey weak lensing programme II. Weak lensing study of seven clusters with MMT/MegaCam SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; cosmology: observations; gravitational lensing: weak; X-rays: galaxies: clusters ID DIGITAL SKY SURVEY; BONN DEEP SURVEY; X-RAY-CLUSTERS; DARK-MATTER; PHOTOMETRIC REDSHIFTS; COSMOLOGICAL CONSTRAINTS; SCALING RELATIONS; MASS MEASUREMENTS; NON-GAUSSIANITY; DATA RELEASE AB Context. Evolution in the mass function of galaxy clusters sensitively traces both the expansion history of the Universe and cosmological structure formation. Robust cluster mass determinations are a key ingredient for a reliable measurement of this evolution, especially at high redshift. Weak gravitational lensing is a promising tool for, on average, unbiased mass estimates. Aims. This weak lensing project aims at measuring reliable weak lensing masses for a complete X-ray selected sample of 36 high redshift (0.35 < z < 0.9) clusters. The goal of this paper is to demonstrate the robustness of the methodology against commonly encountered problems, including pure instrumental effects, the presence of bright (8-9 mag) stars close to the cluster centre, ground based measurements of high-z (z similar to 0.8) clusters, and the presence of massive unrelated structures along the line-sight. Methods. We select a subsample of seven clusters observed with MMT/MegaCam. Instrumental effects are checked in detail by cross-comparison with an archival CFHT/MegaCam observation. We derive mass estimates for seven clusters by modelling the tangential shear with an NFW profile, in two cases with multiple components to account for projected structures in the line-of-sight. Results. We firmly detect lensing signals from all seven clusters at more than 3.5 sigma and determine their masses, ranging from 10(14) M-circle dot to 10(15) M-circle dot, despite the presence of nearby bright stars. We retrieve the lensing signal of more than one cluster in the CL 1701+6414 field, while apparently observing CL 1701+6414 through a massive foreground filament. We also find a multi-peaked shear signal in CL 1641+4001. Shear structures measured in the MMT and CFHT images of CL 1701+6414 are highly correlated. Conclusions. We confirm the capability of MMT/MegaCam to infer weak lensing masses from high-z clusters, demonstrated by the high level of consistency between MMT and CFHT results for CL 1701+6414. This shows that, when a sophisticated analysis is applied, instrumental effects are well under control. C1 [Israel, H.; Erben, T.; Reiprich, T. H.; Schneider, P.] Argelander Inst Astron, D-53121 Bonn, Germany. [Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Israel, H (reprint author), Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM hisrael@astro.uni-bonn.de FU Deutsche Forschungsgemeinschaft (DFG) through Transregional Collaborative Research Centre [TRR 33]; Schwerpunkt Program [1177]; DFG through Heisenberg grant [RE 1462/5, RE 1462/6]; Chandra grants [GO9-0135X, GO9-0148X, GO1-12169X]; Silicon Valley Community Foundation; MMT through NOAO public access [2007B-0046] FX H.I. likes to thank Frank Bertoldi for support of this work and Matthias Klein, Reiko Nakajima, Mischa Schirmer, Ismael Tereno, Bharadwaj Vijaysarathy, Daniela Wuttke, and Yu-Ying Zhang for helpful discussions. Partial support for this work has come from the Deutsche Forschungsgemeinschaft (DFG) through Transregional Collaborative Research Centre TRR 33 as well as through the Schwerpunkt Program 1177. T.H.R. acknowledges support from the DFG through Heisenberg grant RE 1462/5 and grant RE 1462/6. C.L.S. was supported in part by Chandra grants GO9-0135X, GO9-0148X, and GO1-12169X, and by the F. H. Levinson Fund of the Silicon Valley Community Foundation, which helped support the MMT observations. We acknowledge the grant of MMT observation time (program 2007B-0046) through NOAO public access. NR 86 TC 15 Z9 15 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A79 DI 10.1051/0004-6361/201118676 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100079 ER PT J AU Larsen, SS Brodie, JP Strader, J AF Larsen, S. S. Brodie, J. P. Strader, J. TI Detailed abundance analysis from integrated high-dispersion spectroscopy: globular clusters in the Fornax dwarf spheroidal SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: abundances; galaxies: individual: Fornax dSph; galaxies: star clusters: individual: Fornax 3; galaxies: star clusters: individual: Fornax 4; galaxies: star clusters: individual: Fornax 5; methods: data analysis ID GALACTIC CHEMICAL EVOLUTION; INITIAL MASS FUNCTION; EARLY-TYPE GALAXIES; METAL-POOR STARS; HORIZONTAL-BRANCH STARS; RED GIANT BRANCH; TO-LIGHT RATIOS; STELLAR POPULATIONS; MILKY-WAY; HALO STARS AB Aims. We describe our newly developed approach to detailed abundance analysis from integrated-light high-dispersion spectra of star clusters. As a pilot project, we measure abundances of several Fe-peak, alpha- and neutron capture elements from spectra of three globular clusters (GCs) in the Fornax dwarf spheroidal galaxy, obtained with UVES on the ESO Very Large Telescope. Methods. We divided the cluster colour-magnitude diagrams into about 100 bins and used the Kurucz ATLAS9 and SYNTHE codes to compute synthetic spectra for each bin. Stellar parameters were derived empirically from Hubble Space Telescope data for the brighter stars, while theoretical isochrones were used for extrapolation below the detection limit. The individual model spectra were co-added and the abundances were iteratively adjusted until the best match to the observed spectra was achieved. Results. We find [Fe/H] = -2.3, -1.4 and -2.1 for Fornax 3, 4 and 5, with estimated +/- 0.1 dex uncertainties. Fornax 3 and 5 are thus similar in metallicity to the most metal-poor Milky Way GCs and fall near the extreme metal-poor end of the field star metallicity distribution in Fornax. The [alpha/Fe] ratios, as traced by Ca and Ti, are enhanced with respect to the solar composition at the level of similar to+0.25 dex for Fornax 3 and 5, and possibly slightly less (similar to+0.13 dex) for Fornax 4. For all three clusters the [Mg/Fe] ratio is significantly less elevated than [Ca/Fe] and [Ti/Fe], possibly an effect of the abundance anomalies that are well-known in Galactic GCs. We thus confirm that Mg may be a poor proxy for the overall a- element abundances for GCs. The abundance patterns of heavy elements (Y, Ba and Eu) indicate a dominant contribution to nucleosynthesis from the r-process in all three clusters, with a mean [Ba/Eu] similar to -0.7, suggesting rapid formation of the GCs. Conclusions. Combining our results with literature data for Fornax 1 and 2, it is now clear that four of the five Fornax GCs fall in the range -2.5 < [Fe/H] < -2, while Fornax 4 is unambiguously and substantially more metal- rich than the others. The indications that abundance anomalies are detectable in integrated light are encouraging, particularly for the prospects of detecting such anomalies in young, massive star clusters of which few are close enough for individual stars to be observed in detail. C1 [Larsen, S. S.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Brodie, J. P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Strader, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Larsen, SS (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM s.larsen@astro.ru.nl FU NWO/VIDI grant; NSF grant [AST-1109878] FX When we discussed the M33 globular cluster spectra published in Larsen et al. (2002), John Huchra posed the question: What are the plans to say anything about the line strengths and abundances from the HIRES spectra? The analysis presented here would not have been computationally feasible in its current form with the hardware available to us then, but it is appropriate to acknowledge John's role in stimulating our thoughts on this issue. We further thank Ruth Peterson for discussions and advice, C.E. Corsi for kindly providing the photometry of Fornax 3 and 5, and the referee for a very careful reading of the manuscript andmany helpful suggestions. This research has made use of NASA's Astrophysics Data System Bibliographic Services. S.S.L. acknowledges support by an NWO/VIDI grant and J.P.B. acknowledges NSF grant AST-1109878. NR 145 TC 19 Z9 19 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A53 DI 10.1051/0004-6361/201219895 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100053 ER PT J AU Moullet, A Lellouch, E Moreno, R Gurwell, M Sagawa, H AF Moullet, A. Lellouch, E. Moreno, R. Gurwell, M. Sagawa, H. TI Wind mapping in Venus' upper mesosphere with the IRAM-Plateau de Bure interferometer SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual: Venus; instrumentation: interferometers ID HETERODYNE SPECTROSCOPY; GLOBAL CIRCULATION; CO; ATMOSPHERE; LINE; THERMOSPHERE; TEMPERATURE AB Context. The dynamics of the upper mesosphere of Venus (similar to 85-115 km) have been characterized as a combination of a retrograde superrotating zonal wind (RSZ) with a sub-solar-to-antisolar flow (SSAS). Numerous mm-wave single-dish observations have been obtained and been able to directly measure the mesospheric line-of-sight winds by mapping the Doppler shifts of CO rotational lines, but their limited spatial resolution makes their interpretation difficult. Aims. By using interferometric facilities, one can achieve a higher resolution in Doppler-shift maps, allowing us in particular to place firmer constraints on the respective contributions of the SSAS and RSZ circulations to the global mesospheric wind field. Methods. We report on interferometric observations of the CO(1-0) line obtained with the IRAM-Plateau de Bure interferometer in November 2007 and June 2009, which was able to map the upper mesosphere dynamics on the morning hemisphere with a high spatial resolution (3.5-5.5 ''). Results. All the obtained measurements show, with a remarkably high temporal stability, that the wind globally flows in the (sky) east-west direction, corresponding in the observed geometry to either an unexpected prograde zonal wind or a SSAS flow. A very localized inversion of the wind direction, which could correspond to a RSZ wind, is also repeatedly detected in the night hemisphere. The presence of significant meridional winds is not evidenced. Using models with different combinations of zonal and SSAS winds, we find that the data is most accurately reproduced by a dominant SSAS flow with a maximal velocity at the terminator of similar to 200 m/s, displaying large diurnal and latitudinal asymmetries, combined with an equatorial RSZ wind of 70-100 m/s. Overall, this is indicative of a wind-field structure consistent with but much more complex than the usual representation of the mesospheric dynamics. C1 [Moullet, A.] Natl Radio Astron Observ, Charlottesville, VA 22902 USA. [Moullet, A.; Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lellouch, E.; Moreno, R.] LESIA Observ Paris, F-92195 Meudon, France. [Sagawa, H.] Natl Inst Informat & Commun Technol, Koganei, Tokyo 1848795, Japan. RP Moullet, A (reprint author), Natl Radio Astron Observ, Charlottesville, VA 22902 USA. EM amoullet@nrao.edu FU INSU/CNRS (France); MPG (Germany); IGN (Spain) FX Arielle Moullet is a Jansky Fellow of 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. We thank T. Clancy for providing us with the reference atmospheric profiles. We acknowledge the commitment of the staff at IRAM-PdBI in performing these challenging observations. IRAM is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). NR 30 TC 3 Z9 3 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A102 DI 10.1051/0004-6361/201118451 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100102 ER PT J AU Rovilos, E Comastri, A Gilli, R Georgantopoulos, I Ranalli, P Vignali, C Lusso, E Cappelluti, N Zamorani, G Elbaz, D Dickinson, M Hwang, HS Charmandaris, V Ivison, RJ Merloni, A Daddi, E Carrera, FJ Brandt, WN Mullaney, JR Scott, D Alexander, DM Del Moro, A Morrison, G Murphy, EJ Altieri, B Aussel, H Dannerbauer, H Kartaltepe, J Leiton, R Magdis, G Magnelli, B Popesso, P Valtchanov, I AF Rovilos, E. Comastri, A. Gilli, R. Georgantopoulos, I. Ranalli, P. Vignali, C. Lusso, E. Cappelluti, N. Zamorani, G. Elbaz, D. Dickinson, M. Hwang, H. S. Charmandaris, V. Ivison, R. J. Merloni, A. Daddi, E. Carrera, F. J. Brandt, W. N. Mullaney, J. R. Scott, D. Alexander, D. M. Del Moro, A. Morrison, G. Murphy, E. J. Altieri, B. Aussel, H. Dannerbauer, H. Kartaltepe, J. Leiton, R. Magdis, G. Magnelli, B. Popesso, P. Valtchanov, I. TI GOODS-Herschel: ultra-deep XMM-Newton observations reveal AGN/star-formation connection SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; galaxies: Seyfert; galaxies: statistics; galaxies: star formation; X-rays: galaxies; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; STAR-FORMATION RATE; SUPERMASSIVE BLACK-HOLES; FIELD-SOUTH SURVEY; SIMILAR-TO 2; LYMAN BREAK GALAXIES; YALE-CHILE MUSYC; FAR-INFRARED PROPERTIES; MERGER-AGN CONNECTION; HEAVILY OBSCURED AGN AB Models of galaxy evolution assume some connection between the AGN and star formation activity in galaxies. We use the multi-wavelength information of the CDFS to assess this issue. We select the AGNs from the 3 Ms XMM-Newton survey and measure the star-formation rates of their hosts using data that probe rest-frame wavelengths longward of 20 mu m, predominantly from deep 100 mu m and 160 mu m Herschel observations, but also from Spitzer-MIPS-70 mu m. Star-formation rates are obtained from spectral energy distribution fits, identifying and subtracting an AGN component. Our sample consists of sources in the z approximate to 0.5-4 redshift range, with star-formation rates SFR approximate to 10(1)-10(3) M(circle dot)yr(-1) and stellar masses M-star approximate to 10(10)-10(11.5) M-circle dot. We divide the star-formation rates by the stellar masses of the hosts to derive specific star-formation rates (sSFR) and find evidence for a positive correlation between the AGN activity (proxied by the X-ray luminosity) and the sSFR for the most active systems with X-ray luminosities exceeding L-x similar or equal to 10(43) erg s(-1) and redshifts z greater than or similar to 1. We do not find evidence for such a correlation for lower luminosity systems or those at lower redshifts, consistent with previous studies. We do not find any correlation between the SFR (or the sSFR) and the X-ray absorption derived from high-quality XMM-Newton spectra either, showing that the absorption is likely to be linked to the nuclear region rather than the host, while the star-formation is not nuclear. Comparing the sSFR of the hosts to the characteristic sSFR of star-forming galaxies at the same redshift (the so-called "main sequence") we find that the AGNs reside mostly in main-sequence and starburst hosts, reflecting the AGN-sSFR connection; however the infrared selection might bias this result. Limiting our analysis to the highest X-ray luminosity AGNs (X-ray QSOs with L-x > 10(44) erg s(-1)), we find that the highest-redshift QSOs (with z greater than or similar to 2) reside predominantly in starburst hosts, with an average sSFR more than double that of the "main sequence", and we find a few cases of QSOs at z approximate to 1.5 with specific star-formation rates compatible with the main-sequence, or even in the "quiescent" region. Finally, we test the reliability of the colour-magnitude diagram (plotting the rest-frame optical colours against the stellar mass) in assessing host properties, and find a significant correlation between rest-frame colour (without any correction for AGN contribution or dust extinction) and sSFR excess relative to the "main sequence" at a given redshift. This means that the most "starbursty" objects have the bluest rest-frame colours. C1 [Rovilos, E.; Comastri, A.; Gilli, R.; Georgantopoulos, I.; Ranalli, P.; Vignali, C.; Cappelluti, N.; Zamorani, G.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Rovilos, E.; Mullaney, J. R.; Alexander, D. M.; Del Moro, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Georgantopoulos, I.; Ranalli, P.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Lusso, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Elbaz, D.; Daddi, E.; Mullaney, J. R.; Aussel, H.; Dannerbauer, H.; Leiton, R.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Dickinson, M.; Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Charmandaris, V.] Univ Crete, Dept Phys & 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. [Ivison, R. J.] Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Merloni, A.; Magnelli, B.; Popesso, P.] Max Planck Inst Eextraterrestr Phys, D-85471 Garching Bai Munchen, Germany. [Carrera, F. J.] CSIC Univ Cantabria, Inst Fis Cantabria, Santander 39005, Spain. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Morrison, G.] Univ Hawaii, Inst Astron, Manoa, HI 96822 USA. [Morrison, G.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Altieri, B.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Dannerbauer, H.] Univ Wien, Inst Astron, A-1180 Vienna, Austria. [Leiton, R.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. RP Rovilos, E (reprint author), INAF Osservatorio Astron Bologna, Via Ranzani 1, I-40127 Bologna, Italy. EM emmanouil.rovilos@durham.ac.uk RI Charmandaris, Vassilis/A-7196-2008; Vignali, Cristian/J-4974-2012; Ranalli, Piero/K-6363-2013; Georgantopoulos, Ioannis/L-3687-2013; Magdis, Georgios/C-7295-2014; Daddi, Emanuele/D-1649-2012; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; Ivison, R./G-4450-2011 OI Altieri, Bruno/0000-0003-3936-0284; Cappelluti, Nico/0000-0002-1697-186X; Zamorani, Giovanni/0000-0002-2318-301X; Alexander, David/0000-0002-5896-6313; Charmandaris, Vassilis/0000-0002-2688-1956; Vignali, Cristian/0000-0002-8853-9611; Ranalli, Piero/0000-0003-3956-755X; Leiton, Roger/0000-0002-0744-489X; Scott, Douglas/0000-0002-6878-9840; Magdis, Georgios/0000-0002-4872-2294; Daddi, Emanuele/0000-0002-3331-9590; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Ivison, R./0000-0001-5118-1313 FU ESA Member States; USA (NASA); ASI-INAF [I/009/10/00]; Marie-Curie Fellowship [RF040294]; Spanish Ministry of Science and Innovation [AYA2010-21490-C02-01]; STFC FX This work is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA).; We acknowledge financial contribution from the agreement ASI-INAF I/009/10/00. E.R. acknowledges financial support from the Marie-Curie Fellowship grant RF040294. F.J.C. acknowledges financial support for this work by the Spanish Ministry of Science and Innovation through the grant AYA2010-21490-C02-01. D.M.A. and A.D.M. acknowledge support from the STFC. NR 162 TC 40 Z9 40 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A58 DI 10.1051/0004-6361/201218952 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100058 ER PT J AU van Weeren, RJ Rottgering, HJA Intema, HT Rudnick, L Bruggen, M Hoeft, M Oonk, JBR AF van Weeren, R. J. Rottgering, H. J. A. Intema, H. T. Rudnick, L. Brueggen, M. Hoeft, M. Oonk, J. B. R. TI The "toothbrush-relic": evidence for a coherent linear 2-Mpc scale shock wave in a massive merging galaxy cluster? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radio continuum: galaxies; galaxies: active; galaxies: clusters: individual: 1RXS J0603.3+4214; large-scale structure of Universe ID EXTENDED RADIO-SOURCES; X-RAY-EMISSION; COSMIC-RAYS; SKY SURVEY; COSMOLOGICAL SIMULATIONS; PARTICLE-ACCELERATION; MAGNETIC-FIELDS; ASTROPHYSICAL SHOCKS; NONTHERMAL EMISSION; ROTATION MEASURES AB Some merging galaxy clusters host diffuse extended radio emission, so-called radio halos and relics, unrelated to individual galaxies. The origin of these halos and relics is still debated, although there is compelling evidence now that they are related to cluster merger events. Here we present detailed Westerbork Synthesis Radio Telescope (WSRT) and Giant Metrewave Radio Telescope (GMRT) radio observations between 147 MHz and 4.9 GHz of a new radio-selected galaxy cluster 1RXS J0603.3+4214, for which we find a redshift of 0.225. The cluster is detected as an extended X-ray source in the ROSAT All Sky Survey with an X-ray luminosity of L-X, (0.1-2.4 keV) similar to 1 x 10(45) erg s(-1). The cluster hosts a large bright 1.9 Mpc radio relic, an elongated similar to 2 Mpc radio halo, and two fainter smaller radio relics. The large radio relic has a peculiar linear morphology. For this relic we observe a clear spectral index gradient from the front of the relic towards the back, in the direction towards the cluster center. Parts of this relic are highly polarized with a polarization fraction of up to 60%. We performed rotation measure (RM) synthesis between 1.2 and 1.7 GHz. The results suggest that for the west part of the large relic some of the Faraday rotation is caused by the intracluster medium and not only due to galactic foregrounds. We also carried out a detailed spectral analysis of this radio relic and created radio color-color diagrams. We find (i) an injection spectral index of -0.6 to -0.7; (ii) steepening spectral index and increasing spectral curvature in the post-shock region; and (iii) an overall power-law spectrum between 74 MHz and 4.9 GHz with alpha = -1.10 +/- 0.02. Mixing of emission in the beam from regions with different spectral ages is probably the dominant factor that determines the shape of the radio spectra. Changes in the magnetic field, total electron content, or adiabatic gains/losses do not play a major role. A model in which particles are (re) accelerated in a first order Fermi process at the front of the relic provides the best match to the observed spectra. We speculate that in the post-shock region particles are re-accelerated by merger induced turbulence to form the radio halo as the relic and halo are connected. The orientation of the bright relic and halo indicate a north-south merger event, but the peculiar linear shape and the presence of another relic, perpendicular to the bright relic, suggest a more complex merger event. Deep X-ray observations will be needed to determine the merger scenario. C1 [van Weeren, R. J.; Rottgering, H. J. A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Weeren, R. J.; Oonk, J. B. R.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Intema, H. T.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Rudnick, L.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. [Brueggen, M.] Univ Bremen, D-28725 Bremen, Germany. [Brueggen, M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Hoeft, M.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. RP van Weeren, RJ (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM rvanweeren@cfa.harvard.edu RI Intema, Huib/D-1438-2012; OI Intema, Huib/0000-0002-5880-2730; van Weeren, Reinout/0000-0002-0587-1660 FU Netherlands Foundation for Scientific Research (NWO); National Aeronautics and Space Administration; National Science Foundation; NASA [PF2-130104]; Chandra X-ray Center; Smithsonian Astrophysical Observatory for NASA [NAS8-03060]; Royal Netherlands Academy of Arts and Sciences; Deutsche Forschungsgemeinschaft; US National Science Foundation [AST0908668]; [FOR 1254] FX We would like to thank the anonymous referee for useful comments. We thank the staff of the GMRT who have made these observations possible. The GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. The Westerbork Synthesis Radio Telescope is operated by ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands Foundation for Scientific Research (NWO). The William Herschel Telescope are 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. 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. Support for this work was provided by NASA through Einstein Postdoctoral grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. R.J.v.W. acknowledges funding from the Royal Netherlands Academy of Arts and Sciences. M. B. and M. H. acknowledges support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft. LR acknowledges support from the US National Science Foundation, under grant AST0908668 to the University of Minnesota. H. T. I. is Jansky Fellow of the National Radio Astronomy Observatory. R.J.v.W. would like to thank C. Pfrommer for discussions and G. Heald for his explanation of the RM-CLEAN algorithm. NR 108 TC 35 Z9 35 U1 0 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A124 DI 10.1051/0004-6361/201219000 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100124 ER PT J AU Vinko, J Sarneczky, K Takats, K Marion, GH Hegedus, T Biro, IB Borkovits, T Szegedi-Elek, E Farkas, A Klagyivik, P Kiss, LL Kovacs, T Pal, A Szakats, R Szalai, N Szalai, T Szatmary, K Szing, A Vida, K Wheeler, JC AF Vinko, J. Sarneczky, K. Takats, K. Marion, G. H. Hegedus, T. Biro, I. B. Borkovits, T. Szegedi-Elek, E. Farkas, A. Klagyivik, P. Kiss, L. L. Kovacs, T. Pal, A. Szakats, R. Szalai, N. Szalai, T. Szatmary, K. Szing, A. Vida, K. Wheeler, J. C. TI Testing supernovae Ia distance measurement methods with SN 2011fe SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE supernovae: individual: SN 2011fe; galaxies: individual: M101 ID WIDTH-LUMINOSITY RELATION; LIGHT-CURVE SHAPES; RISE-TIME; M101; ULTRAVIOLET; SPECTROGRAPH; CONSTANT; SPECTRA; SPEX; STAR AB Aims. The nearby, bright, almost completely unreddened Type Ia supernova 2011fe in M101 provides a unique opportunity to test both the precision and the accuracy of the extragalactic distances derived from SNe Ia light curve fitters. Methods. We applied the current, public versions of the independent light curve fitting codes MLCS2k2 and SALT2 to compute the distance modulus of SN 2011fe from high-precision, multi-color (BVRI) light curves. Results. The results from the two fitting codes confirm that 2011fe is a "normal" (not peculiar) and only slightly reddened SN Ia. New unreddened distance moduli are derived as 29.21 +/- 0.07 mag (D similar to 6.95 +/- 0.23 Mpc, MLCS2k2), and 29.05 +/- 0.07 mag (6.46 +/- 0.21 Mpc). Conclusions. Despite the very good fitting quality achieved with both light curve fitters, the resulting distance moduli are inconsistent by 2 sigma. Both are marginally consistent (at similar to 1 sigma) with the Hubble Space Telescope key project distance modulus for M101. The SALT2 distance is in good agreement with the recently revised Cepheid- and TRGB-distance to M101. Averaging all SN- and Cepheid-based estimates, the absolute distance to M101 is similar to 6.6 +/- 0.5 Mpc. C1 [Vinko, J.; Takats, K.; Szalai, T.] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Vinko, J.; Wheeler, J. C.] Univ Texas Austin, Dept Astron, Univ Stn C1400 1, Austin, TX 78712 USA. [Sarneczky, K.; Borkovits, T.; Szegedi-Elek, E.; Farkas, A.; Klagyivik, P.; Kiss, L. L.; Kovacs, T.; Pal, A.; Szakats, R.; Szalai, N.; Szing, A.; Vida, K.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Sarneczky, K.; Borkovits, T.] ELTE Gothard Lendulet Res Grp, H-9700 Szombathely, Hungary. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hegedus, T.; Biro, I. B.; Borkovits, T.] Baja Astron Observ, H-6500 Baja, Hungary. [Farkas, A.; Pal, A.] Eotvos Lorand Univ, Dept Astron, H-1518 Budapest, Hungary. [Kiss, L. L.] Univ Sydney, Sch Phys A28, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Szatmary, K.] Univ Szeged, Dept Expt Phys, H-6720 Szeged, Hungary. RP Vinko, J (reprint author), Univ Szeged, Dept Opt & Quantum Elect, Dom Ter 9, H-6720 Szeged, Hungary. EM vinko@physx.u-szeged.hu FU Hungarian OTKA [K76816, MB08C 81013, K83790, K81421]; NSF [AST 11-09881, AST 09-07903, PHY-1066293]; European Union; European Social Fund through the TAMOP [4.2.2/B-10/1-2010-0012]; National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program [NNX-08AE38A]; ESA [PECS 98073]; Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences; OTKA [K81373]; Hungarian Academy of Sciences FX We are indebted to the referee, Peter Nugent, for his valuable comments and suggestions that helped us improving the paper. This project has been supported by Hungarian OTKA grant K76816, by NSF Grant AST 11-09881 (to J.C.W.), and by the European Union together with the European Social Fund through the TAMOP 4.2.2/B-10/1-2010-0012 grant. G. H. M. and the CfA Supernova Program is supported by NSF Grant AST 09-07903. G. H. M. is a visiting Astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. A. P. has been supported by the ESA grant PECS 98073 and by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. T. K. has been supported by OTKA Grant K81373. K. S., L. L. K. and K. V. acknowledge support from the "Lendulet" Young Researchers' Program of the Hungarian Academy of Sciences and the Hungarian OTKA Grants MB08C 81013, K83790 and K81421. J.C.W. is grateful for the hospitality of the Aspen Center for Physics supported by NSF PHY-1066293. Thanks are also due to the staff of McDonald and Konkoly Observatories for the prompt scheduling and helpful assistance during the time-critical ToO observations. The Hobby-Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitt Mnchen, and Georg-August-Universitt Gttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The SIMBAD database at CDS, the NASA ADS and NED databases have been used to access data and references. The availability of these services is gratefully acknowledged. NR 40 TC 19 Z9 19 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A12 DI 10.1051/0004-6361/201220043 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100012 ER PT J AU Zhang, Z Gilfanov, M Bogdan, A AF Zhang, Z. Gilfanov, M. Bogdan, A. TI Dependence of the low-mass X-ray binary population on stellar age SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; globular clusters: general; Galaxy: stellar content ID EARLY-TYPE GALAXIES; GLOBULAR-CLUSTER SYSTEMS; STAR-FORMATION HISTORY; ELLIPTIC GALAXIES; LUMINOSITY FUNCTIONS; POINT SOURCES; IONIZED-GAS; HOST GALAXY; CHANDRA; FIELD AB Aims. We investigate the dependence of the low-mass X-ray binary (LMXB) population in early-type galaxies on stellar age. Methods. We selected 20 massive nearby early-type galaxies from the Chandra archive occupying a relatively narrow range of masses and spanning a broad range of ages, from 1.6 Gyr to more than 10 Gyr, with the median value of 6 Gyr. With the similar to 2000 X-ray point sources detected in total, we correlated the specific number of LMXBs in each galaxy with its stellar age and globular cluster (GC) content. Results. We found a correlation between the LMXB population and stellar age: older galaxies tend to possess about approximate to 50% more LMXBs (per unit stellar mass) than the younger ones. The interpretation of this dependence is complicated by large scatter and a rather strong correlation between stellar age and GC content of galaxies in our sample. We present evidence suggesting that the more important factor may be the evolution of the LMXB population with time. Its effect is further amplified by the larger GC content of older galaxies and correspondingly, the larger numbers of dynamically formed binaries in them. We also found clear evolution of the X-ray luminosity function (XLF) with age, i.e., that younger galaxies have more bright sources and fewer faint sources per unit stellar mass. The XLF of LMXBs in younger galaxies appears to extend significantly beyond 10(39) erg/s. Such bright sources seem to be less frequent in older galaxies. We found that 6 out of approximate to 12 (ultra-) luminous sources are located in GCs. C1 [Zhang, Z.; Gilfanov, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Bogdan, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Zhang, Z (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM zzhang@mpa-garching.mpg.de; gilfanov@mpa-garching.mpg.de FU NASA through Einstein Postdoctoral Fellowship [PF1-120081]; Chandra X-ray Center; NASA [NAS8-03060] FX This research made use of Chandra archival data provided by Chandra X-ray Center and the 2MASS Large Galaxy Atlas data provided by NASA/IPAC infrared science archive. Akos Bogdan acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant number PF1-120081 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We also wish to thank Rasmus Voss, Andrew Cooper, Diederik Kruijssen, Junhua Gu, and Jingying Wang for the discussions which have greatly improved the quality of this paper. NR 68 TC 18 Z9 18 U1 0 U2 1 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD OCT PY 2012 VL 546 AR A36 DI 10.1051/0004-6361/201219015 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 027JT UT WOS:000310349100036 ER PT J AU Fishman, J Iraci, LT Al-Saadi, J Chance, K Chavez, F Chin, M Coble, P Davis, C DiGiacomo, PM Edwards, D Eldering, A Goes, J Herman, J Hu, C Jacob, DJ Jordan, C Kawa, SR Key, R Liu, X Lohrenz, S Mannino, A Natraj, V Neil, D Neu, J Newchurch, M Pickering, K Salisbury, J Sosik, H Subramaniam, A Tzortziou, M Wang, J Wang, M AF Fishman, J. Iraci, L. T. Al-Saadi, J. Chance, K. Chavez, F. Chin, M. Coble, P. Davis, C. DiGiacomo, P. M. Edwards, D. Eldering, A. Goes, J. Herman, J. Hu, C. Jacob, D. J. Jordan, C. Kawa, S. R. Key, R. Liu, X. Lohrenz, S. Mannino, A. Natraj, V. Neil, D. Neu, J. Newchurch, M. Pickering, K. Salisbury, J. Sosik, H. Subramaniam, A. Tzortziou, M. Wang, J. Wang, M. TI THE UNITED STATES' NEXT GENERATION OF ATMOSPHERIC COMPOSITION AND COASTAL ECOSYSTEM MEASUREMENTS NASA's Geostationary Coastal and Air Pollution Events (GEO-CAPE) Mission SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID GULF-OF-MEXICO; OZONE MONITORING INSTRUMENT; SATELLITE MEASUREMENTS; MARINE-PHYTOPLANKTON; TROPOSPHERIC OZONE; CLIMATE-CHANGE; URBAN OZONE; OCEAN; AEROSOL; SPACE AB THE UNITED STATES' NEXT GENERATION OF ATMOSPHERIC COMPOSITION AND COASTAL ECOSYSTEM MEASUREMENTS: NASA'S GEOSTATIONARY COASTAL AND AIR POLLUTION EVENTS (GEO-CAPE) MISSION The Geostationary Coastal and Air Pollution Events (GEO-CAPE) mission was recommended by the National Research Council's (NRC's) Earth Science Decadal Survey to measure tropospheric trace gases and aerosols' and coastal ocean phytoplankton, water quality, and biogeochemistry from geostationary orbit, providing continuous observations within the field of view. To fulfill the mandate and address the challenge put forth by the NRC, two GEO-CAPE Science Working Groups (SWGs), representing the atmospheric composition and ocean color disciplines, have developed realistic science objectives using input drawn from several community workshops. The GEO-CAPE mission will take advantage of this revolutionary advance in temporal frequency for both of these disciplines. Multiple observations per day are required to explore the physical, chemical, and dynamical processes that determine tropospheric composition and air quality over spatial scales ranging from urban to continental, and over temporal scales ranging from diurnal to seasonal. Likewise, high-frequency satellite Observations are critical to studying and quantifying biological, chemical, and physical processes within the coastal ocean. These observations are to be achieved from a vantage point near 95 degrees-100 degrees W, providing a complete view of North America as well as the adjacent oceans. The SWGs have also endorsed the concept of phased implementation using commercial satellites to reduce mission risk and cost. GEO-CAPE will join the global constellation. of geostationary atmospheric chemistry and coastal ocean color sensors planned to be in orbit in the 2020 time frame. C1 [Fishman, J.] St Louis Univ, Dept Earth & Atmospher Sci, St Louis, MO 63108 USA. [Iraci, L. T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Al-Saadi, J.] NASA, Washington, DC 20546 USA. [Al-Saadi, J.; Neil, D.] NASA, Langley Res Ctr, Hampton, VA 23665 USA. [Chance, K.; Liu, X.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chavez, F.] Monterey Bay Aquarium Res Inst, Moss Landing, CA USA. [Chin, M.; Herman, J.; Kawa, S. R.; Mannino, A.; Pickering, K.; Tzortziou, M.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Tzortziou, M.] Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. [Coble, P.; Hu, C.] Univ S Florida, Tampa, FL USA. [Davis, C.] Oregon State Univ, Corvallis, OR 97331 USA. [DiGiacomo, P. M.; Wang, M.] NOAA, NESDIS Ctr Satellite Applicat & Res, Camp Springs, MD USA. [DiGiacomo, P. M.; Wang, M.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Eldering, A.; Key, R.; Natraj, V.; Neu, J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Goes, J.; Subramaniam, A.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Jacob, D. J.] Harvard Univ, Cambridge, MA 02138 USA. [Jordan, C.; Salisbury, J.] Univ New Hampshire, Durham, NH 03824 USA. [Lohrenz, S.] Univ So Mississippi, Dept Marine Sci, Stennis Space Ctr, MS USA. [Newchurch, M.] Univ Alabama, Huntsville, AL 35899 USA. [Sosik, H.] Woods Hole Oceanog Inst, Woods Hole, MA USA. [Wang, J.] Univ Nebraska, Lincoln, NE USA. RP Fishman, J (reprint author), St Louis Univ, Dept Earth & Atmospher Sci, 300-F ONeil Hall,3642 Lindell Blvd, St Louis, MO 63108 USA. EM jfishma2@slu.edu RI Wang, Menghua/F-5631-2010; Chin, Mian/J-8354-2012; DiGiacomo, Paul/F-5584-2010; Pickering, Kenneth/E-6274-2012; Kawa, Stephan/E-9040-2012; Mannino, Antonio/I-3633-2014; Liu, Xiong/P-7186-2014; Wang, Jun/A-2977-2008; OI Sosik, Heidi/0000-0002-4591-2842; Lohrenz, Steven/0000-0003-3811-2975; Wang, Menghua/0000-0001-7019-3125; DiGiacomo, Paul/0000-0003-4550-1899; Liu, Xiong/0000-0003-2939-574X; Wang, Jun/0000-0002-7334-0490; Herman, Jay/0000-0002-9146-1632; Chance, Kelly/0000-0002-7339-7577; Subramaniam, Ajit/0000-0003-1316-5827 FU Earth Science Division of the National Aeronautics and Space Administration FX Funding for GEO-CAPE definition activities is provided by the Earth Science Division of the National Aeronautics and Space Administration. Portions of this work were carried out at the jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Contributions to this work were made by the GEO-CAPE Atmospheric Science Working Group: J. Al-Saadi, K. Bowman, K. Chance, R. Chatfield, M. Chin, R. Cohen, J. Crawford D. Edwards, A. Eldering, J. Fishman, D. Henze, L. Iraci, D.J. Jacob, K. Jucks, S. R. Kawa, S. Kondragunta, N. Krotkov, X. Liu, C. McLinden, V. Natraj, D. Neil, J. Neu, M. Newchurch, K. Pickering, R. Pierce, R. Pinder, J. Rodriguez, S. Sander, R. Scheffe, R. Spurr, J. Szykman, O. Torres, J. Wang, J. Worden and the GEO-CAPE Ocean Science Working Group: J. Al-Saadi, B. Arnone, W. Balch, P. Bontempi, J. Campbell, J. Chaves, F. Chavez, P. Coble, C. Davis, C. del Castillo, P.M. DiGiacomo, J. Goes, J. Herman, S. Hooker, C. Hu, L. Iraci, C. Jordan, Z. P. Lee, S. Lohrenz, A. Mannino, P. Matrai, C. McClain, R. Morrison, C. Mouw, F. Muller-Karger, A. Neeley, J. Salisbury, B. Schaeffer, H. Sosik, R. Stumpf, A. Subramaniam, G. Toro-Farmer, O. Torres, M. Tzortziou, M. Wang, J. Werdell, C. Wilson. NR 80 TC 65 Z9 65 U1 2 U2 48 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0003-0007 EI 1520-0477 J9 B AM METEOROL SOC JI Bull. Amer. Meteorol. Soc. PD OCT PY 2012 VL 93 IS 10 BP 1547 EP 1566 DI 10.1175/BAMS-D-11-00201.1 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 024HU UT WOS:000310101100013 ER PT J AU Pilat, MA McFarland, A Snelgrove, A Collins, K Waliczek, TM Zajicek, J AF Pilat, Monica Ann McFarland, Amy Snelgrove, Amy Collins, Kevin Waliczek, Tina Marie Zajicek, Jayne TI The Effect of Tree Cover and Vegetation on Incidence of Childhood Asthma in Metropolitan Statistical Areas of Texas SO HORTTECHNOLOGY LA English DT Article DE urban forest; canopy cover; ArcView (TM); normalized difference vegetation index ID AIR-POLLUTION; CHILDREN; PLANTS AB The number of asthma cases in children has increased significantly in the last couple of decades. Studies on links between outdoor air pollutants and asthma have had mixed results, suggesting the need for more focused studies. An increase in tree plantings for urban areas is now being called upon as a solution to the higher heat indexes and pollution rates for more densely populated areas. Green spaces and trees could further benefit some urban areas by providing an effective means to improve air conditions. The purpose of this study was to assess whether there is a relationship between levels of vegetation and reported rates of childhood asthma in Texas. Childhood asthma data were collected from the Center for Health Statistics and the Texas Department of State Health Services for the years 2005 and 2006. The asthma rates for each metropolitan statistical area (MSA) were mapped and inserted into a corresponding vegetation map using geographical mapping software. A comparison of vegetation rates and asthma rates in metropolitan areas was used to investigate whether vegetation and tree cover led to higher or lower incidences of childhood asthma rates. Asthma data, normalized difference vegetation index (NDVI), and canopy cover data were analyzed using statistical software. Regression analysis and correlations were calculated to analyze the data for the tree coverage/vegetation rates and asthma rates variable. No statistically significant relationships between NDVI, canopy cover, and asthma were found in this study. C1 [Pilat, Monica Ann; Waliczek, Tina Marie] Texas State Univ, Dept Agr, San Marcos, TX 78666 USA. [McFarland, Amy] Smithsonian Inst, Washington, DC 20013 USA. [Snelgrove, Amy] Texas A&M Inst Renewable Nat Resources, College Stn, TX 77843 USA. [Collins, Kevin] Texas State Univ, Dept Resp Care, San Marcos, TX 78666 USA. [Zajicek, Jayne] Texas A&M Univ, Dept Hort Sci, College Stn, TX 77845 USA. RP Waliczek, TM (reprint author), Texas State Univ, Dept Agr, San Marcos, TX 78666 USA. EM tc10@txstate.edu NR 33 TC 7 Z9 7 U1 2 U2 20 PU AMER SOC HORTICULTURAL SCIENCE PI ALEXANDRIA PA 113 S WEST ST, STE 200, ALEXANDRIA, VA 22314-2851 USA SN 1063-0198 J9 HORTTECHNOLOGY JI HortTechnology PD OCT PY 2012 VL 22 IS 5 BP 631 EP 637 PG 7 WC Horticulture SC Agriculture GA 024GL UT WOS:000310097600011 ER PT J AU Sapir, N Dudley, R AF Sapir, Nir Dudley, Robert TI Backward flight in hummingbirds employs unique kinematic adjustments and entails low metabolic cost SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE avian locomotor mode; Calypte anna; flight agility; mask respirometry; mass-specific metabolic rate; nectarivory ID EVAPORATIVE WATER-LOSS; WIND-TUNNEL; OXYGEN-CONSUMPTION; POWER REQUIREMENTS; MOTOR PATTERNS; ENERGY-COST; BIRD FLIGHT; WALKING; ENERGETICS; RESPONSES AB Backward flight is a frequently used transient flight behavior among members of the species-rich hummingbird family (Trochilidae) when retreating from flowers, and is known from a variety of other avian and hexapod taxa, but the biomechanics of this intriguing locomotor mode have not been described. We measured rates of oxygen uptake ((V) over dot(O2)) and flight kinematics of Anna's hummingbirds, Calypte anna (Lesson), within a wind tunnel using mask respirometry and high-speed videography, respectively, during backward, forward and hovering flight. We unexpectedly found that (V) over dot(O2) in sustained backward flight is similar to that in forward flight at equivalent airspeed, and is about 20% lower than hovering (V) over dot(O2). For a bird that was measured throughout a range of backward airspeeds up to a speed of 4.5 m s(-1), the power curve resembled that of forward flight at equivalent airspeeds. Backward flight was facilitated by steep body angles coupled with substantial head flexion, and was also characterized by a higher wingbeat frequency, a flat stroke plane angle relative to horizontal, a high stroke plane angle relative to the longitudinal body axis, a high ratio of maximum:minimum wing positional angle, and a high upstroke:downstroke duration ratio. Because of the convergent evolution of hummingbird and some hexapod flight styles, flying insects may employ similar kinematics while engaged in backward flight, for example during station keeping or load lifting. We propose that backward flight behavior in retreat from flowers, together with other anatomical, physiological, morphological and behavioral adaptations, enables hummingbirds to maintain strictly aerial nectarivory. C1 [Sapir, Nir; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Sapir, N (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM nir.sapir@berkeley.edu OI Sapir, Nir/0000-0002-2477-0515 FU National Science Foundation, Division of Integrative Organismal Systems [0837866] FX This study was supported by the National Science Foundation, Division of Integrative Organismal Systems [grant number 0837866]. NR 58 TC 7 Z9 7 U1 3 U2 57 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 OCT PY 2012 VL 215 IS 20 BP 3603 EP 3611 DI 10.1242/jeb.073114 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 016TY UT WOS:000309543600016 PM 23014570 ER PT J AU Moncrief, ND Lack, JB Maldonado, JE Bryant, KL Edwards, CW Van Den Bussche, RA AF Moncrief, Nancy D. Lack, Justin B. Maldonado, Jesus E. Bryant, Katherine L. Edwards, Cody W. Van Den Bussche, Ronald A. TI General lack of phylogeographic structure in two sympatric, forest obligate squirrels (Sciurus niger and S. carolinensis) SO JOURNAL OF MAMMALOGY LA English DT Article DE coalescent; eastern North America; fox squirrel; glacial refugia; gray squirrel; incomplete lineage sorting; mismatch distribution; mitochondrial DNA; phylogeography; Pleistocene ID EASTERN NORTH-AMERICA; LAST GLACIAL MAXIMUM; QUERCUS-RUBRA L.; MITOCHONDRIAL-DNA; TREE SQUIRRELS; FOX SQUIRRELS; HABITAT USE; PLEISTOCENE BIOGEOGRAPHY; CONSERVATION GENETICS; POPULATION-GROWTH AB We examined intraspecific relationships in the eastern fox squirrel (Sciurus niger) and the eastern gray squirrel (S. carolinensis) using sequence variation in a portion of the mitochondrial DNA cytochrome-h gene and part of the D-loop in the control region. These closely related species are codistributed temperate forest obligates that have similar generation time and population ecologies. For both species, we documented high haplotype diversity, low nucleotide variation, and several groups of divergent haplotypes. However, there is a general lack of spatial structure in maternal lineages within each species. For S. carolinensis, we observed a pattern of population genetic structure that suggests the presence of at least 2 distinct refugial populations that evolved in isolation during the Pleistocene (approximately 98.3-266.3 thousand years ago [kya]) and subsequently expanded to the species' current range following the last glacial maximum. For S. niger, the genetic structure was much less pronounced, with fewer strongly diverged haplotypes. This finding suggests that eastern fox squirrels persisted in either a single population in a glacial refugium or as several refugial populations that maintained gene flow throughout the Pleistocene. For both species, there is evidence that scattered populations were present in multiple, small refugia close to the Laurentide Ice Sheet, allowing rapid range expansion following glacial recession. Taken together, our results indicate that S. niger and S. carolinensis underwent multiple episodes of genetic divergence during isolation in glacial refugia, followed by range expansion and contact that resulted in admixture of divergent maternal lineages within each species during interglacials. Examination of our data further indicates that the most recent ranee expansion in both species occurred within the past 12-20 kya. C1 [Moncrief, Nancy D.] Virginia Museum Nat Hist, Martinsville, VA 24112 USA. [Lack, Justin B.] Univ Wisconsin, Genet Lab, Madison, WI 53706 USA. [Lack, Justin B.; Van Den Bussche, Ronald A.] Oklahoma State Univ, Dept Zool, Stillwater, OK 74078 USA. [Maldonado, Jesus E.] Ctr Conservat & Evolutionary Genet, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Bryant, Katherine L.] Emory Univ, Program Neurosci, Atlanta, GA 30033 USA. [Bryant, Katherine L.; Edwards, Cody W.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Moncrief, ND (reprint author), Virginia Museum Nat Hist, Martinsville, VA 24112 USA. EM nancy.moncrief@vmnh.virginia.gov NR 71 TC 6 Z9 6 U1 4 U2 36 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 EI 1545-1542 J9 J MAMMAL JI J. Mammal. PD OCT PY 2012 VL 93 IS 5 BP 1247 EP 1264 DI 10.1644/11-MAMM-A-383.1 PG 18 WC Zoology SC Zoology GA 025HQ UT WOS:000310179700003 ER PT J AU Delaney, M AF Delaney, Michelle TI Photographers of the Western Isles SO SCOTTISH HISTORICAL REVIEW LA English DT Book Review C1 [Delaney, Michelle] Smithsonian Inst, Washington, DC 20560 USA. RP Delaney, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0036-9241 J9 SCOT HIST REV JI Scott. Hist. Rev. PD OCT PY 2012 VL 91 IS 232 BP 383 EP 385 DI 10.3366/shr.2012.0132 PG 4 WC History SC History GA 022OE UT WOS:000309967900033 ER PT J AU Moser, WE Richardson, DJ Hammond, CI Govedich, FR Lazo-Wasem, EA AF Moser, William E. Richardson, Dennis J. Hammond, Charlotte I. Govedich, Fredric R. Lazo-Wasem, Eric A. TI Resurrection and Redescription of Placobdella rugosa (Verrill, 1874) (Hirudinida: Glossiphoniidae) SO BULLETIN OF THE PEABODY MUSEUM OF NATURAL HISTORY LA English DT Article DE Placobdella rugosa; P. ali; P. ornata; Glossiphoniidae; Hirudinida; Hirudinea; leeches; Verrill AB The identification and taxonomy of papillated leeches of the genus Placobdella have been extremely problematic, confounded by vague descriptions, redescriptions of species without reference to type material or type locality, and more than a century of numerous dubious taxonomic acts. Leeches collected on August 5 and 6, 2011, from North Dakota, USA, the type locality of Clepsine ornata rugosa Verrill, 1874, were determined to be conspecific with Placobdella rugosa (Verrill, 1874) Moore, 1901 on the basis of comparison to the syntype series. The acquisition of these specimens from the type locality facilitated resurrection and redescription of P. rugosa. Placobdella rugosa is similar to P. ali but differs in salivary gland morphology and ventral pigmentation. Molecular comparison of CO-I revealed differences of 16.1% between P. rugosa and P. ali. C1 [Moser, William E.] Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Museum Support Ctr MRC 534, Suitland, MD 20746 USA. [Richardson, Dennis J.; Hammond, Charlotte I.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Govedich, Fredric R.] So Utah Univ, Dept Biol, Cedar City, UT 84720 USA. [Lazo-Wasem, Eric A.] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Moser, WE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Museum Support Ctr MRC 534, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM moserw@si.edu; Dennis.Richardson@quinnipiac.edu; Charlotte.Hammond@quinnipiac.edu; govedich@suu.edu; eric.lazo-wasem@yale.edu NR 20 TC 4 Z9 4 U1 2 U2 5 PU PEABODY MUSEUM NATURAL HISTORY-YALE UNIV PI NEW HAVEN PA 170 WHITNEY AVE, PO BOX 208118, NEW HAVEN, CT 06520-8118 USA SN 0079-032X J9 B PEABODY MUS NAT HI JI Bull. Peabody Mus. Natl. Hist. PD OCT PY 2012 VL 53 IS 2 BP 375 EP 381 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 022IE UT WOS:000309950700003 ER PT J AU Gulbransen, DJ McGlathery, KJ Marklund, M Norris, JN Gurgel, CFD AF Gulbransen, Dana J. McGlathery, Karen J. Marklund, Maria Norris, James N. Gurgel, Carlos Frederico D. TI GRACILARIA VERMICULOPHYLLA (RHODOPHYTA, GRACILARIALES) IN THE VIRGINIA COASTAL BAYS, USA: COX1 ANALYSIS REVEALS HIGH GENETIC RICHNESS OF AN INTRODUCED MACROALGA SO JOURNAL OF PHYCOLOGY LA English DT Article DE cox1; cox2-cox3 spacer; DNA barcode; Gracilaria vermiculophylla; marine algae; rbcL; species introductions; Virginia ID NORTH-CAROLINA; SUBUNIT RDNA; IMPACTS; SYSTEMATICS; SEQUENCES; PACIFIC; MARINE; ESTUARINE; INVASIONS; ATLANTIC AB Gracilaria vermiculophylla (Ohmi) Papenfuss is an invasive alga that is native to Southeast Asia and has invaded many estuaries in North America and Europe. It is difficult to differentiate G. vermiculophylla from native forms using morphology and therefore molecular techniques are needed. In this study, we used three molecular markers (rbcL, cox2-cox3 spacer, cox1) to identify G. vermiculophylla at several locations in the western Atlantic. RbcL and cox2-cox3 spacer markers confirmed the presence of G. vermiculophylla on the east coast of the USA from Massachusetts to South Carolina. We used a 507 base pair region of cox1 mtDNA to (i) verify the widespread distribution of G. vermiculophylla in the Virginia (VA) coastal bays and (ii) determine the intraspecific diversity of these algae. Cox1 haplotype richness in the VA coastal bays was much higher than that previously found in other invaded locations, as well as some native locations. This difference is likely attributed to the more intensive sampling design used in this study, which was able to detect richness created by multiple, diverse introductions. On the basis of our results, we recommend that future studies take differences in sampling design into account when comparing haplotype richness and diversity between native and non-native studies in the literature. C1 [Gulbransen, Dana J.; McGlathery, Karen J.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. [Marklund, Maria; Gurgel, Carlos Frederico D.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Norris, James N.] Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Gurgel, Carlos Frederico D.] State Herbarium, Plant Biodivers Ctr, Adelaide, SA 5001, Australia. [Gurgel, Carlos Frederico D.] S Australia Res & Dev Inst, Henley Beach, SA 5022, Australia. RP Gulbransen, DJ (reprint author), Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. EM djg4j@virginia.edu RI Gurgel, Carlos/E-6897-2014; OI Gurgel, Carlos/0000-0003-3989-1704; Gurgel, Carlos Frederico Deluqui/0000-0002-7321-6115 FU Virginia Coastal Reserve Long Term Ecological Research [DEB-0621014] FX We thank Dr. Wilson Freshwater (UNW) for kindly providing information and nine unpublished rbcL sequences to this study; Dr. Jan Rueness for providing extracted DNA from his 2005 paper so that gaps in some European rbcL DNA sequences could be filled; Prof. Suzanne Fredericq (Univ. Louisiana, Lafayette) and the staff of the Anheuser Busch Coastal Research Center in VA and the Smithsonian Marine Station at Fort Pierce, Florida for field and lab support; Dr. Loren Coen (Marine Resources Research Institute, South Carolina Department of Natural Resources, Charleston), for providing time aboard the R/V Silver Cresent to dredge on the Charleston shrimp bars and Shaun Norris for collection assistance; The Nature Conservancy in the VA coastal reserve for research permits. This is Smithsonian Marine Station at Fort Pierce contribution. Funding for part of this work was provided by the Virginia Coastal Reserve Long Term Ecological Research grant DEB-0621014. NR 33 TC 8 Z9 9 U1 2 U2 15 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD OCT PY 2012 VL 48 IS 5 BP 1278 EP 1283 DI 10.1111/j.1529-8817.2012.01218.x PG 6 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 015RA UT WOS:000309462500020 PM 27011285 ER PT J AU McKenna, MF Cranford, TW Berta, A Pyenson, ND AF McKenna, Megan F. Cranford, Ted W. Berta, Annalisa Pyenson, Nicholas D. TI Morphology of the odontocete melon and its implications for acoustic function SO MARINE MAMMAL SCIENCE LA English DT Article DE odontocetes; sound production; echolocation; melon; functional morphology; computed tomography ID PORPOISE PHOCOENA-PHOCOENA; BOTTLE-NOSED-DOLPHIN; TRANSMISSION BEAM PATTERN; WHALE ZIPHIUS-CAVIROSTRIS; TURSIOPS-TRUNCATUS; SPERM-WHALE; HARBOR PORPOISE; ECHOLOCATION SIGNALS; SOUND-TRANSMISSION; KOGIA-BREVICEPS AB Toothed whales (crown Odontoceti) are unique among mammals in their ability to echolocate underwater, using specialized tissue structures. The melon, a structure composed of fat and connective tissue, is an important component in the production of an echolocation beam; it is known to focus high frequency, short duration echolocation clicks. Here, we report on the morphology of the odontocete melon to provide a comprehensive understanding of melon structure across odontocete taxa. This study examined nine odontocete species (12 individual specimens), from five of the ten extant odontocete families. We established standardized definitions using computed tomography scans of the melon to investigate structure without losing geometric integrity. The morphological features that relate to the focusing capacity of the melon include internal density topography, melon size and shape, and relationship to other forehead structures. The potential for melon structure to act as a filter is discussed: establishing a lower limit to the frequency of sounds that can be propagated through the head. Collectively, the results of this study provide a robust, quantitative and comparative framework for evaluating tissue structures that form a key component of the echolocation apparatus. C1 [McKenna, Megan F.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Cranford, Ted W.; Berta, Annalisa] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Pyenson, Nicholas D.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Mammal, Seattle, WA 98195 USA. [Pyenson, Nicholas D.] Burke Museum Nat Hist & Culture, Dept Paleontol, Seattle, WA 98195 USA. RP McKenna, MF (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, 9500 Gilman Dr,Mail Code 0205, La Jolla, CA 92093 USA. EM megan.mckenna@gmail.com FU San Diego State University Fund; ARCS Fellowship; Mabel Myer Scholarship; Smithsonian Institution's Remington Kellogg Fund; San Diego State University; Department of Biology; Evolutionary Biology Program Area FX Some funding for this project came to M. F. McKenna from the San Diego State University Fund, ARCS Fellowship, Mabel Myer Scholarship, Smithsonian Institution's Remington Kellogg Fund, San Diego State University, Department of Biology, Evolutionary Biology Program Area. The most significant support for this research was provided to Dr. Ted W. Cranford by Dr. Robert Gisiner at the Office of Naval Research, and by Frank Stone and Ernie Young at the Chief of Naval Operations (CNO45). NR 71 TC 18 Z9 18 U1 13 U2 94 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD OCT PY 2012 VL 28 IS 4 BP 690 EP 713 DI 10.1111/j.1748-7692.2011.00526.x PG 24 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 017TB UT WOS:000309612800015 ER PT J AU Davis, DR Davis, MM Mannion, C AF Davis, Donald R. Davis, Mignon M. Mannion, Catharine TI NEOTROPICAL TINEIDAE IX: A REVIEW OF THE WEST INDIAN XYSTROLOGA AND BIOLOGY OF XYSTROLOGA GRENADELLA (WLSM.), AN INVASIVE PEST OF CULTIVATED GREENHOUSE PLANTS IN SOUTHERN FLORIDA, USA AND GERMANY (LEPIDOPTERA: TINEOIDEA) SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Distribution; genital morphology; invasive species; larval morphology; orchid pest; parasitoids; root-feeding AB Only two species, Xystrologa grenadella (Walsingham) and X. nigrovitta (Walsingham), of the predominantly Neotropical genus Xystrologa are known to occur in the West Indies. Xystrologa antipathetica (Forbes), originally described from Puerto Rico but also reported from the United States (Florida), is considered a junior synonym of X. grenadella. The adults of both species and the larva and pupa of X. grenadella are described and illustrated. The larval habits of the genus are reported for the first time as a general detritovore, feeding on woody refuse, the bark of Ficus trees (in Florida, USA), fungi, and the roots of orchids, and pineapple (in Puerto Rico). The injury that larvae of X. grenadella can inflict upon cultivated orchids in Florida is summarized. The introduction of X. grenadella is reported for the first time in the Old World, as a pest of greenhouse plants in Germany. C1 [Davis, Donald R.; Davis, Mignon M.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Mannion, Catharine] Univ Florida, Ctr Trop Res & Educ, Homestead, FL 33031 USA. RP Davis, DR (reprint author), Smithsonian Inst, Dept Entomol, NHB 105,POB 37012, Washington, DC 20013 USA. EM davisd@si.edu; cmannion@ufl.edu NR 17 TC 0 Z9 0 U1 0 U2 9 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2012 VL 114 IS 4 BP 439 EP 455 DI 10.4289/0013-8797.114.4.439 PG 17 WC Entomology SC Entomology GA 024OA UT WOS:000310117300002 ER PT J AU Linnen, CR Smith, DR AF Linnen, Catherine R. Smith, David R. TI RECOGNITION OF TWO ADDITIONAL PINE-FEEDING NEODIPRION SPECIES (HYMENOPTERA: DIPRIONIDAE) IN THE EASTERN UNITED STATES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE sawflies; Nearctic; Pinus AB DNA sequence studies revealed two additional species of Neodiprion in eastern United States, and morphological studies support their recognition. One, which is sympatric with and morphologically similar to Neodiprion abbotii (Leach) in southeastern United States, is recognized as Neodiprion fabricii (Leach), revised status. The larvae feed on Pin us taeda L. and P. echinata Miller. The other, described as Neodiprion knereri Linnen and Smith, n. sp., on Pinus clausa (Chapm. ex Englem.) in Florida, is close to Neodiprion virginiana Rohwer. C1 [Linnen, Catherine R.] Univ Kentucky, Dept Biol, Lexington, KY 40506 USA. [Smith, David R.] Smithsonian Inst, Natl Museum Nat Hist, PSI, Systemat Entomol Lab,Agr Res Serv, Washington, DC 20013 USA. RP Linnen, CR (reprint author), Univ Kentucky, Dept Biol, Lexington, KY 40506 USA. EM catherine.linnen@uky.edu; sawfly2@aol.com NR 16 TC 2 Z9 2 U1 0 U2 1 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD OCT PY 2012 VL 114 IS 4 BP 492 EP 500 DI 10.4289/0013-8797.114.4.492 PG 9 WC Entomology SC Entomology GA 024OA UT WOS:000310117300006 ER PT J AU Dick, SJ AF Dick, Steven J. TI Cosmic evolution: the context for astrobiology and its cultural implications SO INTERNATIONAL JOURNAL OF ASTROBIOLOGY LA English DT Article DE biological universe; cosmic evolution; cosmotheology; cultural evolution; human destiny; postbiological universe; societal impact of astrobiology ID INTELLIGENT LIFE AB Astrobiology must be seen in the context of cosmic evolution, the 13.7 billion-year master narrative of the universe. The idea of an evolving universe dates back only to the 19th century, and became a guiding principle for astronomical research only in the second half of the 20th century. The modern synthesis in evolutionary biology hastened the acceptance of the idea in its cosmic setting, as did the confirmation of the Big Bang theory for the origin of the universe. NASA programmes such as Origins incorporated it as a guiding principle. Cosmic evolution encompasses physical, biological and cultural evolution, and may result in a physical, biological or postbiological universe, each with its own implications for long-term human destiny, and each imbuing the meaning of life with different values. It has the status of an increasingly accepted worldview that is beginning to have a profound effect not only in science but also in religion and philosophy. Received 16 February 2012, accepted 28 February 2012, first published online 27 March 2012 C1 Smithsonian Inst, Div Space Hist, Natl Air & Space Museum, Washington, DC 20013 USA. RP Dick, SJ (reprint author), Smithsonian Inst, Div Space Hist, Natl Air & Space Museum, NASM 3559,MRC 311, Washington, DC 20013 USA. EM stevedick1@comcast.net NR 106 TC 3 Z9 3 U1 1 U2 15 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1473-5504 EI 1475-3006 J9 INT J ASTROBIOL JI Int. J. Astrobiol. PD OCT PY 2012 VL 11 IS 4 SI SI BP 203 EP 216 DI 10.1017/S1473550412000110 PG 14 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 019GF UT WOS:000309724800003 ER PT J AU Guarcello, MG Wright, NJ Drake, JJ Garcia-Alvarez, D Drew, JE Aldcroft, T Kashyap, VL AF Guarcello, M. G. Wright, N. J. Drake, J. J. Garcia-Alvarez, D. Drew, J. E. Aldcroft, T. Kashyap, V. L. TI OPTICAL PHOTOMETRIC GTC/OSIRIS OBSERVATIONS OF THE YOUNG MASSIVE ASSOCIATION CYGNUS OB2 SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; stars: formation; stars: pre-main sequence ID MAIN-SEQUENCE STARS; STELLAR PHOTOMETRY; GLOBULAR-CLUSTER; X REGION; IPHAS; CHANDRA; SDSS; EXTINCTION; OBJECTS; CYG-OB2 AB In order to fully understand the gravitational collapse of molecular clouds, the star formation process, and the evolution of circumstellar disks, these phenomena must be studied in different Galactic environments with a range of stellar contents and positions in the Galaxy. The young massive association Cygnus OB2, in the Cygnus-X region, is a unique target to study how star formation and the evolution of circumstellar disks proceed in the presence of a large number of massive stars. We present a catalog obtained with recent optical observations in the r, i, z filters with OSIRIS, mounted on the 10.4 m Gran Telescopio CANARIAS telescope, which is the deepest optical catalog of Cyg OB2 to date. The catalog consists of 64,157 sources down to M = 0.15 M-circle dot at the adopted distance and age of Cyg OB2. A total of 38,300 sources have good photometry in all three bands. We combined the optical catalog with existing X-ray data of this region, in order to define the cluster locus in the optical diagrams. The cluster locus in the r - i versus i - z diagram is compatible with an extinction of the optically selected cluster members in the 2.64(m) < A(V) < 5.57(m) range. We derive an extinction map of the region, finding a median value of A(V) = 4.33(m) in the center of the association, decreasing toward the northwest. In the color-magnitude diagrams, the shape of the distribution of main-sequence stars is compatible with the presence of an obscuring cloud in the foreground similar to 850 +/- 25 pc from the Sun. C1 [Guarcello, M. G.; Wright, N. J.; Drake, J. J.; Aldcroft, T.; Kashyap, V. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Garcia-Alvarez, D.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Garcia-Alvarez, D.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Garcia-Alvarez, D.] Grantecan CALP, E-38712 Brena Baja, La Palma, Spain. [Drew, J. E.] Univ Hertfordshire, CAR STRI, Hatfield AL10 9AB, Herts, England. RP Guarcello, MG (reprint author), Smithsonian Astrophys Observ, MS-67,60 Garden St, Cambridge, MA 02138 USA. OI Drew, Janet/0000-0003-1192-7082 FU NASA [NAS8-39073]; Harvey Tananbaum; Spanish MICINN [AYA2008-02038]; [GO0-11040X] FX This article is based on observations made with the Gran Telescopio CANARIAS (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de CANARIAS, in the island of La Palma, and it also makes use of data obtained as part of the INT Photometric Ha Survey of the Northern Galactic Plane (IPHAS) carried out at the Isaac Newton Telescope (INT; all IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge) and from archival Chandra/ACIS-I observations. M. G. G. and N.J.W. were supported by the Chandra grant GO0-11040X. J.J.D., V. L. K., and T. A. were supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC) and thank the Director, Harvey Tananbaum, and the CXC science staff for advice and support. D. G. A. acknowledges support from the Spanish MICINN through grant AYA2008-02038. We thank the anonymous referee for the useful comments. NR 41 TC 9 Z9 9 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD OCT PY 2012 VL 202 IS 2 AR 19 DI 10.1088/0067-0049/202/2/19 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016ZM UT WOS:000309558400009 ER PT J AU Forbes, DA Cortesi, A Pota, V Foster, C Romanowsky, AJ Merrifield, MR Brodie, JP Strader, J Coccato, L Napolitano, N AF Forbes, Duncan A. Cortesi, Arianna Pota, Vincenzo Foster, Caroline Romanowsky, Aaron J. Merrifield, Michael R. Brodie, Jean P. Strader, Jay Coccato, Lodovico Napolitano, Nicola TI Radially extended kinematics in the S0 galaxy NGC 2768 from planetary nebulae, globular clusters and starlight SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: elliptical and lenticular; cD; galaxies: individual: NGC 2768; galaxies: kinematics and dynamics ID TULLY-FISHER RELATION; ELLIPTIC GALAXIES; STELLAR POPULATION; EFFECTIVE RADII; DARK-MATTER; SPECTROSCOPY; PHOTOMETRY; GRADIENTS; EVOLUTION; PROFILES AB There are only a few tracers available to probe the kinematics of individual early-type galaxies beyond one effective radius. Here we directly compare a sample of planetary nebulae (PNe), globular clusters (GCs) and galaxy starlight velocities out to approximately four effective radii, in the S0 galaxy NGC 2768. Using a bulge-to-disc decomposition of a K-band image we assign PNe and starlight to either the disc or the bulge. We show that the bulge PNe and bulge starlight follow the same radial density distribution as the red subpopulation of GCs, whereas the disc PNe and disc starlight are distinct components. We find good kinematic agreement between the three tracers to several effective radii (and with stellar data in the inner regions). Further support for the distinct nature of the two galaxy components comes from our kinematic analysis. After separating the tracers into bulge and disc components we find the bulge to be a slowly rotating pressure-supported system, whereas the disc reveals a rapidly rising rotation curve with a declining velocity dispersion profile. The resulting Vrot/s ratio for the disc resembles that of a spiral galaxy and hints at an origin for NGC 2768 as a transformed late-type galaxy. A two-component kinematic analysis for a sample of S0s will help to elucidate the nature of this class of galaxy. C1 [Forbes, Duncan A.; Cortesi, Arianna; Pota, Vincenzo] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Cortesi, Arianna; Merrifield, Michael R.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Foster, Caroline] European So Observ, Santiago 19, Chile. [Romanowsky, Aaron J.; Brodie, Jean P.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Coccato, Lodovico] European So Observ, D-85748 Garching, Germany. [Napolitano, Nicola] Osserv Astron Capodimonte, Ist Nazl Astrofis, I-80131 Naples, Italy. RP Forbes, DA (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM dforbes@swin.edu.au OI Merrifield, Michael/0000-0002-4202-4727; Napolitano, Nicola Rosario/0000-0003-0911-8884; Foster, Caroline/0000-0003-0247-1204 FU European Commission; European Community [229517]; NSF [AST-0808099, AST-0909237, AST-1109878] FX We thank C. Blom, J. Arnold, L. Spitler for their help with the Keck observations. We also thank the referee for several useful comments. CF acknowledges co-funding under the Marie Curie Actions of the European Commission (FP7-COFUND). LC has received funding from the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement no 229517. JB and AR acknowledge support from the NSF through grants AST-0808099, AST-0909237 and AST-1109878. NR 43 TC 13 Z9 13 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 426 IS 2 BP 975 EP 982 DI 10.1111/j.1365-2966.2012.21877.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 015OQ UT WOS:000309456200014 ER PT J AU Usher, C Forbes, DA Brodie, JP Foster, C Spitler, LR Arnold, JA Romanowsky, AJ Strader, J Pota, V AF Usher, Christopher Forbes, Duncan A. Brodie, Jean P. Foster, Caroline Spitler, Lee R. Arnold, Jacob A. Romanowsky, Aaron J. Strader, Jay Pota, Vincenzo TI The SLUGGS survey: calcium triplet-based spectroscopic metallicities for over 900 globular clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE globular clusters: general; galaxies: abundances; galaxies: star clusters: general; galaxies: stellar content ID EARLY-TYPE GALAXIES; STELLAR POPULATION-MODELS; INFRARED CAII TRIPLET; INITIAL MASS FUNCTION; ACS VIRGO CLUSTER; ELLIPTIC GALAXIES; EMPIRICAL CALIBRATION; COLOR DISTRIBUTIONS; WIDE-FIELD; NGC 5128 AB Although the colour distribution of globular clusters in massive galaxies is well known to be bimodal, the spectroscopic metallicity distribution has been measured in only a few galaxies. After redefining the calcium triplet indexmetallicity relation, we use our relation to derive the metallicity of 903 globular clusters in 11 early-type galaxies. This is the largest sample of spectroscopic globular cluster metallicities yet assembled. We compare these metallicities with those derived from Lick indices finding good agreement. In six of the eight galaxies with sufficient numbers of high-quality spectra we find bimodality in the spectroscopic metallicity distribution. Our results imply that most massive early-type galaxies have bimodal metallicity as well as colour distributions. This bimodality suggests that most massive early-type galaxies experienced two periods of star formation. C1 [Usher, Christopher; Forbes, Duncan A.; Spitler, Lee R.; Pota, Vincenzo] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Brodie, Jean P.; Arnold, Jacob A.; Romanowsky, Aaron J.] Univ Calif Observ, Santa Cruz, CA 95064 USA. [Foster, Caroline] European So Observ, Santiago 19, Chile. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Usher, C (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM cusher@astro.swin.edu.au RI Spitler, Lee/A-9867-2013; OI Spitler, Lee/0000-0001-5185-9876; Usher, Christopher/0000-0002-7383-7106; Foster, Caroline/0000-0003-0247-1204 FU National Aeronautics and Space Administration; National Science Foundation; NSF [AST-0071048]; W. M. Keck Foundation; NASA [NAS 5-26555]; European Commission; National Science Foundation [AST-0808099, AST-0909237] FX We thank Karl Glazebrook, Lee Spitler and Albin Gaignette for providing data in advance of publication. We thank Michael Murphy, Vincenzo Pota and Christina Blom for valuable discussions and comments. We thank Mark Norris for assistance with the NGC 3115 Lick metallicities. We thank the anonymous referee for proving useful comments. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Adminackistration. The analysis pipeline used to reduce the DEIMOS data was developed at UC Berkeley with support from NSF grant AST-0071048. This publication made use of PYRAF and PYFITS which are products of the Space Telescope Science Institute, which is operated by AURA for NASA. This research made use of TOPCAT (Taylor 2005). This research is partially based on data from the MILES project. Some of the data presented herein were obtained at the W. M. Keck Observatory, 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 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. This research is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. This research is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. CF acknowledges co-funding under the Marie Curie Actions of the European Commission (FP7-COFUND). This material is based upon work supported by the National Science Foundation under grants AST-0808099 and AST-0909237. NR 116 TC 47 Z9 48 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 426 IS 2 BP 1475 EP 1495 DI 10.1111/j.1365-2966.2012.21801.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 015OQ UT WOS:000309456200054 ER PT J AU Cervantes-Sodi, B Hernandez, X Hwang, HS Park, C Le Borgne, D AF Cervantes-Sodi, Bernardo Hernandez, X. Hwang, Ho Seong Park, Changbom Le Borgne, Damien TI The spin of late-type galaxies at redshifts z <= 1.2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: general; galaxies: high-redshift; galaxies: statistics; galaxies: structure ID GOODS-SOUTH FIELD; TULLY-FISHER RELATION; ORIGINS DEEP SURVEY; DARK-MATTER HALOES; DIGITAL SKY SURVEY; DISK GALAXIES; ANGULAR-MOMENTUM; STELLAR MASS; VLT/FORS2 SPECTROSCOPY; SURFACE-BRIGHTNESS AB We study the evolution of the galactic spin using data of high-redshift galaxies in the fields of the Great Observatories Origins Deep Survey. Through simple dynamical considerations we estimate the spin for the disc galaxies in our sample and find that its distribution is consistent with that found for nearby galaxies. Defining a dimensionless angular momentum parameter for the disc component of the galaxies (?d), we do not find signs of evolution in the redshift range 0.4 = z = 1.2. We find that the mass and environmental dependences of the spin of our high-redshift galaxies are similar to those of low-z galaxies, showing a strong dependence on mass, in the sense that low-mass systems present higher ?d values than high-mass galaxies, with no significant dependence on the environmental density. These results lead us to conclude that although individual disc galaxies might occasionally suffer strong evolution, they evolve in such a way that the overall spin distribution of the galactic population remains constant from z similar to 1 to the present epoch. C1 [Cervantes-Sodi, Bernardo] Chinese Acad Sci, Shanghai Astron Observ, Max Planck Inst Astrophys, Partner Grp, Shanghai 200030, Peoples R China. [Cervantes-Sodi, Bernardo] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Hernandez, X.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Park, Changbom] Korea Inst Adv Study, Seoul 130722, South Korea. [Le Borgne, Damien] Univ Paris 06, Inst Astrophys Paris, UMR 7095, CNRS, F-75014 Paris, France. RP Cervantes-Sodi, B (reprint author), Chinese Acad Sci, Shanghai Astron Observ, Max Planck Inst Astrophys, Partner Grp, Nandan Rd 80, Shanghai 200030, Peoples R China. EM bernardo@shao.ac.cn FU NSFC [11173045]; Shanghai Pujiang Programme [11PJ1411600]; CAS/SAFEA International Partnership Programme for Creative Research Teams [KJCX2-YW-T23]; UNAM DGAPA [IN103011] FX This work is supported by NSFC (no. 11173045), Shanghai Pujiang Programme (no. 11PJ1411600) and the CAS/SAFEA International Partnership Programme for Creative Research Teams (KJCX2-YW-T23). XH acknowledges financial assistance from UNAM DGAPA grant IN103011. CBP thanks Korea Institute for Advanced Study for providing computing resources (KIAS Center for Advanced Computation Linux Cluster System, QUEST). NR 92 TC 2 Z9 2 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 426 IS 2 BP 1606 EP 1612 DI 10.1111/j.1365-2966.2012.21812.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 015OQ UT WOS:000309456200062 ER PT J AU Sing, DK Huitson, CM Lopez-Morales, M Pont, F Desert, JM Ehrenreich, D Wilson, PA Ballester, GE Fortney, JJ des Etangs, AL Vidal-Madjar, A AF Sing, D. K. Huitson, C. M. Lopez-Morales, M. Pont, F. Desert, J. -M. Ehrenreich, D. Wilson, P. A. Ballester, G. E. Fortney, J. J. des Etangs, A. Lecavelier Vidal-Madjar, A. TI GTC OSIRIS transiting exoplanet atmospheric survey: detection of sodium in XO-2b from differential long-slit spectroscopy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: spectroscopic; stars: individual: XO-2; planetary systems ID EXTRASOLAR GIANT PLANETS; HUBBLE-SPACE-TELESCOPE; HD 189733B; HOT JUPITER; TRANSMISSION SPECTRUM; TUNABLE IMAGER; LIGHT CURVES; HIGH ALBEDO; GJ 1214B; MU-M AB We present two transits of the hot-Jupiter exoplanet XO-2b using the Gran Telescopio Canarias (GTC). The time series observations were performed using long-slit spectroscopy of XO-2 and a nearby reference star with the Optical System for Imaging and low Resolution Integrated Spectroscopy (OSIRIS) instrument, enabling differential spectrophotometric transit light curves capable of measuring the exoplanet's transmission spectrum. Two optical low-resolution grisms were used to cover the optical wavelength range from 3800 to 9300?angstrom. We find that sub-mmag-level slit losses between the target and reference star prevent full optical transmission spectra from being constructed, limiting our analysis to differential absorption depths over similar to 1000 angstrom regions. Wider long slits or multi-object grism spectroscopy with wide masks will likely prove effective in minimizing the observed slit-loss trends. During both transits, we detect significant absorption in the planetary atmosphere of XO-2b using a 50-angstrom bandpass centred on the Na?i doublet, with absorption depths of ?(Rpl/R?)2 = 0.049 +/- 0.017 per cent using the R500R grism and 0.047 +/- 0.011 per cent using the R500B grism (combined 5.2s significance from both transits). The sodium feature is unresolved in our low-resolution spectra, with detailed modelling also likely ruling out significant line-wing absorption over an similar to 800 angstrom region surrounding the doublet. Combined with narrow-band photometric measurements, XO-2b is the first hot Jupiter with evidence for both sodium and potassium present in the planet's atmosphere. C1 [Sing, D. K.; Huitson, C. M.; Pont, F.; Wilson, P. A.] Univ Exeter, Sch Phys, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Lopez-Morales, M.] CSIC, Fac Ciencias, ICE, E-08193 Barcelona, Spain. [Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ehrenreich, D.] UJF Grenoble 1, CNRS, INSU, IPAG,UMR 5274, F-38041 Grenoble, France. [Ballester, G. E.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [des Etangs, A. Lecavelier; Vidal-Madjar, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, F-75014 Paris, France. RP Sing, DK (reprint author), Univ Exeter, Sch Phys, Astrophys Grp, Stocker Rd, Exeter EX4 4QL, Devon, England. EM sing@astro.ex.ac.uk OI HUITSON, CATHERINE/0000-0002-4734-691X; Fortney, Jonathan/0000-0002-9843-4354; Ehrenreich, David/0000-0001-9704-5405; Sing, David /0000-0001-6050-7645 FU STFC; Spanish Plan Nacional de Astronomia y Astrofisica [AYA2008-06311-C02-01] FX We thank the entire GTC staff and especially Antonio Cabrera-Lavers for his continued excellent work in executing this programme. DKS and CMH both acknowledge support from STFC. This work was partially supported by the Spanish Plan Nacional de Astronomia y Astrofisica under grant AYA2008-06311-C02-01. NR 42 TC 46 Z9 46 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 426 IS 2 BP 1663 EP 1670 DI 10.1111/j.1365-2966.2012.21938.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 015OQ UT WOS:000309456200066 ER PT J AU Turner, BL Wells, A Andersen, KM Condron, LM AF Turner, Benjamin L. Wells, Andrew Andersen, Kelly M. Condron, Leo M. TI Patterns of tree community composition along a coastal dune chronosequence in lowland temperate rain forest in New Zealand SO PLANT ECOLOGY LA English DT Article DE Chronosequence; Holocene; Mantel tests; New Zealand; Nitrogen; Nothofagus; Phosphorus; Podocarpaceae; Podzol; Retrogression ID LONG-TERM CHRONOSEQUENCES; WESTERN NEW-ZEALAND; TROPICAL FOREST; ECOSYSTEM RETROGRESSION; PALEOSEISMIC ACTIVITY; SOIL CHRONOSEQUENCE; ECOLOGICAL DISTRICT; PRIMARY SUCCESSION; SOUTH WESTLAND; LEAF LITTER AB Soil chronosequences provide an opportunity to examine the influence of long-term pedogenesis on the biomass and composition of associated tree communities. We assessed variation in the species composition of trees, saplings, and seedlings, and the basal area of adult trees, in lowland temperate rain forest along the Haast chronosequence on the west coast of the South Island of New Zealand. The sequence consists of Holocene dune ridges formed following periodic earthquake disturbance and is characterized by rapid podzol development, including a marked decline in phosphorus concentrations, accumulation of a thick organic horizon, and formation of a cemented iron pan. Tree basal area increased for the first few hundred years and then declined in parallel with the decline in total soil phosphorus, consistent with the concept of forest retrogression. There were also marked changes in the composition of the tree community, from dominance by conifers on young soils to a mixed conifer-angiosperm forest on old soils. Although a variety of factors could account for these changes, partial Mantel tests revealed strong correlations between tree community composition and soil nutrients. The relationships differed among life history stages, however, because the adult tree community composition was correlated strongly with nutrients in the mineral soil, whereas the seedling community composition was correlated with nutrients in the organic horizon, presumably reflecting differences in rooting depth. The changes in the tree community at Haast are consistent with disturbance-related succession in conifer-angiosperm forests in the region, but the opposite of patterns along the nearby Franz Josef post-glacial chronosequence, where conifers are most abundant on old soils. The Haast chronosequence is therefore an important additional example of forest retrogression linked to long-term soil phosphorus depletion, and provides evidence for the role of soil nutrients in determining the distribution of tree species during long-term succession in lowland temperate rain forests in New Zealand. C1 [Turner, Benjamin L.; Andersen, Kelly M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Wells, Andrew; Condron, Leo M.] Lincoln Univ, Canterbury 7647, New Zealand. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Condron, Leo/E-9458-2013; Turner, Benjamin/E-5940-2011 OI Turner, Benjamin/0000-0002-6585-0722 FU Smithsonian Institution Postdoctoral Fellowship; Lincoln University FX We thank Peter Bellingham and David Coomes for helpful discussion. Kelly Andersen was supported by a Smithsonian Institution Postdoctoral Fellowship. Funding for travel and consumables was provided by Lincoln University. NR 52 TC 10 Z9 12 U1 1 U2 52 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD OCT PY 2012 VL 213 IS 10 BP 1525 EP 1541 DI 10.1007/s11258-012-0108-3 PG 17 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 017AP UT WOS:000309561400001 ER PT J AU Bartelmann, M Springel, V AF Bartelmann, Matthias Springel, Volker TI Editorial: Special Issue: Dark Matter SO ANNALEN DER PHYSIK LA English DT Editorial Material C1 [Bartelmann, Matthias] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bartelmann, Matthias; Springel, Volker] Univ Heidelberg, D-6900 Heidelberg, Germany. RP Bartelmann, M (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM bartelmann@uni-heidelberg.de; volker.springel@h-its.org NR 0 TC 0 Z9 0 U1 0 U2 2 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0003-3804 J9 ANN PHYS-BERLIN JI Ann. Phys.-Berlin PD OCT PY 2012 VL 524 IS 9-10 SI SI BP A133 EP A134 DI 10.1002/andp.201200744 PG 2 WC Physics, Multidisciplinary SC Physics GA 014UX UT WOS:000309402300008 ER PT J AU Graham, AM Bullock, AL Maizel, AC Elias, DA Gilmour, CC AF Graham, Andrew M. Bullock, Allyson L. Maizel, Andrew C. Elias, Dwayne A. Gilmour, Cynthia C. TI Detailed Assessment of the Kinetics of Hg-Cell Association, Hg Methylation, and Methylmercury Degradation in Several Desulfovibrio Species SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID SULFATE-REDUCING BACTERIA; DESULFOBULBUS-PROPIONICUS 1PR3; FRESH-WATER SEDIMENTS; MERCURY-METHYLATION; ANAEROBIC-BACTERIA; MARINE-SEDIMENTS; PURE CULTURES; CONTAMINATED SEDIMENTS; PRINCIPAL METHYLATORS; ESTUARINE SEDIMENT AB The kinetics of inorganic Hg [Hg(II)(i)] association, methylation, and methylmercury (MeHg) demethylation were examined for a group of Desulfovibrio species with and without MeHg production capability. We employed a detailed method for assessing MeHg production in cultures, including careful control of medium chemistry, cell density, and growth phase, plus mass balance of Hg(II)(i) and MeHg during the assays. We tested the hypothesis that differences in Hg(II)(i) sorption and/or uptake rates drive observed differences in methylation rates among Desulfovibrio species. Hg(II)(i) associated rapidly and with high affinity to both methylating and nonmethylating species. MeHg production by Hg-methylating strains was rapid, plateauing after similar to 3 h. All MeHg produced was rapidly exported. We also tested the idea that all Desulfovibrio species are capable of Hg(II)(i) methylation but that rapid demethylation masks its production, but we found this was not the case. Therefore, the underlying reason why MeHg production capability is not universal in the Desulfovibrio is not differences in Hg affinity for cells nor differences in the ability of strains to degrade MeHg. However, Hg methylation rates varied substantially between Hg-methylating Desulfovibrio species even in these controlled experiments and after normalization to cell density. Thus, biological differences may drive cross-species differences in Hg methylation rates. As part of this study, we identified four new Hg methylators (Desulfovibrio aespoeensis, D. alkalitolerans, D. psychrotolerans, and D. sulfodismutans) and four nonmethylating species (Desulfovibrio alcohol-ivorans, D. tunisiensis, D. carbinoliphilus, and D. piger) in our ongoing effort to generate a library of strains for Hg methylation genomics. C1 [Graham, Andrew M.; Bullock, Allyson L.; Maizel, Andrew C.; Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Elias, Dwayne A.] Oak Ridge Natl Lab, Biosci Div, Oak Ridge, TN USA. RP Gilmour, CC (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM gilmourc@si.edu RI Elias, Dwayne/B-5190-2011; Gilmour, Cynthia/G-1784-2010 OI Elias, Dwayne/0000-0002-4469-6391; Gilmour, Cynthia/0000-0002-1720-9498 FU U.S. Department of Energy under the Subsurface Biogeochemical Research Program (SBR); Office of Biological and Environmental Research, Office of Science through the Mercury Science Focus Area Program at Oak Ridge National Laboratory (ORNL); National Science Foundation grant [DEB0351050]; University of Tennessee UT-Battelle, LLC [DEAC05-00OR22725]; Smithsonian Institution Fellowship Program 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, through the Mercury Science Focus Area Program at Oak Ridge National Laboratory (ORNL), and by National Science Foundation grant DEB0351050 (C.C.G.). ORNL is managed by University of Tennessee UT-Battelle, LLC, for the Department of Energy under contract no. DEAC05-00OR22725. A.M.G. acknowledges support from the Smithsonian Institution Fellowship Program. NR 60 TC 15 Z9 17 U1 3 U2 55 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 OCT PY 2012 VL 78 IS 20 BP 7337 EP 7346 DI 10.1128/AEM.01792-12 PG 10 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 013TL UT WOS:000309328700019 PM 22885751 ER PT J AU Van Loo, S Hartquist, TW Falle, SAEG AF Van Loo, S. Hartquist, T. W. Falle, S. A. E. G. TI Magnetic fields and star formation SO ASTRONOMY & GEOPHYSICS LA English DT Article ID MAGNETOHYDRODYNAMIC SHOCK-WAVES; WEAKLY IONIZED CLOUDS; C-TYPE SHOCKS; AMBIPOLAR DIFFUSION; MOLECULAR CLOUDS; INTERSTELLAR CLOUDS; DENSE CORES; TRIGGERED FORMATION; PROTOSTELLAR DISKS; DOMINATED CLOUDS C1 [Van Loo, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hartquist, T. W.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Falle, S. A. E. G.] Univ Leeds, Dept Appl Math, Leeds LS2 9JT, W Yorkshire, England. RP Van Loo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Van Loo, Sven/0000-0003-4746-8500 FU UK Science and Technology Funding Council; Smithsonian SMA Fellowship FX The authors are grateful to the UK Science and Technology Funding Council for support. SVL greatly appreciates funding provided by the Smithsonian SMA Fellowship he holds. NR 68 TC 1 Z9 1 U1 8 U2 68 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1366-8781 J9 ASTRON GEOPHYS JI Astron. Geophys. PD OCT PY 2012 VL 53 IS 5 BP 31 EP 36 DI 10.1111/j.1468-4004.2012.53531.x PG 6 WC Astronomy & Astrophysics; Geochemistry & Geophysics SC Astronomy & Astrophysics; Geochemistry & Geophysics GA 007GR UT WOS:000308877300025 ER PT J AU Palow, DT Nolting, K Kitajima, K AF Palow, Danielle T. Nolting, Kristen Kitajima, Kaoru TI Functional trait divergence of juveniles and adults of nine Inga species with contrasting soil preference in a tropical rain forest SO FUNCTIONAL ECOLOGY LA English DT Article DE fabaceae; ingeae; leaf traits; ontogeny; seed traits; soil fertility; tropical forests; wood density ID HABITAT ASSOCIATIONS; SEEDLING GROWTH; LEAF TRAITS; ECONOMICS SPECTRUM; NEOTROPICAL FOREST; DEMOGRAPHIC RATES; AMAZONIAN FOREST; NUTRIENT CONTENT; SHADE TOLERANCE; GOOD PREDICTORS AB 1. Community-wide studies have shown that functional traits of tropical trees vary with soil-type preference, but few have examined trait diversification among closely related taxa. In this study, we asked how functional traits of adults and saplings within a speciose genus, Inga, differ in relation to their soil-type preferences. 2. We quantified soil-type preference and functional traits of nine Inga species (Fabaceae) in the wet tropical forest at La Selva Biological Station, Costa Rica, where rich alluvial soil and less fertile residual soil of volcanic origin occur in close proximity. 3. From the extensive trail network, we randomly selected 104 trail segments, each 50m long, along which all Inga individuals >50cm tall were counted and identified to species. Five and three common species showed significant bias to residual or alluvial soil, respectively, while the remaining one showed no significant bias. For these nine species, we quantified five leaf traits for saplings and adults, as well as wood-specific gravity (WSG) and three seed traits. 4. For both adults and saplings, leaf mass per area (LMA) and lamina density were higher for residual-soil specialists than fertile alluvial-soil specialists. The opposite trend was found for nitrogen (N) and phosphorus (P) concentrations in leaves. Lamina thickness did not differ between soil-type preference groups. All leaf trait values except N concentration increased from saplings to adults, with adults showing larger interspecific variations in trait values than saplings. 5. Saplings and adults of the single species found on both soils had trait values intermediate between residual and alluvial-soil specialists. 6. Seed mass and seed N, as well as WSG of adults, were higher in residual-soil specialists than alluvial-soil specialists. Higher seed N indicates higher maternal investment of species growing on less fertile soil. 7. These differences in traits among closely related species across continuous soils suggest that habitat filtering has contributed to the evolution of seed, juvenile and adult traits within a speciose tropical tree genus. C1 [Palow, Danielle T.; Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Nolting, Kristen] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Kitajima, Kaoru] Smithsonian Trop Res Inst, Balboa, Panama. RP Palow, DT (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM dpalow@ufl.edu FU South East Alliance for Graduate Education and the Professoriate; Organization for Tropical Studies; Research Experience for Undergraduates Program of the National Science Foundation of the United States FX We thank Orlando Vargas and Nelson Zamora for their assistance with species identification, Deborah Clark and David Clark for advice on experimental design, Julia Reiskind and Grace Crummer for the chemical analyses, the staff at La Selva Biological Station for logistic support and Steven Oberbauer, John Ewel, Martijn Slot and Jared Westbrook for constructive comments. DP was funded by fellowships from the South East Alliance for Graduate Education and the Professoriate and the Organization for Tropical Studies, and KN was funded by Research Experience for Undergraduates Program of the National Science Foundation of the United States. NR 59 TC 10 Z9 10 U1 1 U2 49 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 J9 FUNCT ECOL JI Funct. Ecol. PD OCT PY 2012 VL 26 IS 5 BP 1144 EP 1152 DI 10.1111/j.1365-2435.2012.02019.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 014QT UT WOS:000309391500017 ER PT J AU Larjavaara, M Muller-Landau, HC AF Larjavaara, Markku Muller-Landau, Helene C. TI Temperature explains global variation in biomass among humid old-growth forests SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Carbon stocks; climate change; ecosystem respiration; gross primary productivity (GPP); humid forests; maintenance cost; net primary productivity (NPP); temperature sensitivity ID TROPICAL FORESTS; CARBON-DIOXIDE; VEGETATION DYNAMICS; PLANT RESPIRATION; MODEL; CLIMATE; STAND; GPP; BALANCE; NPP AB Aim To develop and test a simple climate-based ecophysiological model of above-ground biomass an approach that can be applied directly to predicting the effects of climate change on forest carbon stores. Location Humid lowland forests world-wide. Methods We developed a new approach to modelling the aboveground biomass of old-growth forest (AGBmax) based on the influences of temperature on gross primary productivity (GPP) and what we call total maintenance cost (TMC), which includes autotrophic respiration as well as leaf, stem and other plant construction required to maintain biomass. We parameterized the models with measured carbon fluxes and tested them by comparing predicted AGBmax with measured AGB for another 109 old-growth sites. Results Our models explained 57% of the variation in GPP across 95 sites and 79% of the variation in TMC across 17 sites. According to the best-fit models, the ratio of GPP to maintenance cost per unit biomass (MCB) peaks at 16.5 degrees C, indicating that this is the air temperature leading to the highest possible AGBmax when temperatures are constant. Seasonal temperature variation generally reduces predicted AGBmax, and thus maritime temperate climates are predicted to have the highest AGBmax. The shift in temperatures from temperate maritime to tropical climates increases MCB more than GPP, and thus decreases AGBmax. Overall, our model explains exactly 50% of the variation in AGB among humid lowland old-growth forests. Main conclusions Temperature plays an important role in explaining global variation in biomass among humid lowland old-growth forests, a role that can be understood in terms of the dual effects of temperature on GPP and TMC. Our simple model captures these influences, and could be an important tool for predicting the effects of climate change on forest carbon stores. C1 [Larjavaara, Markku; Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Panama City, Panama. [Larjavaara, Markku] Univ Helsinki, Dept Forest Sci, FI-00014 Helsinki, Finland. RP Larjavaara, M (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Panama City, Panama. EM markku.larjavaara@gmail.com OI Larjavaara, Markku/0000-0002-3484-889X FU HSBC Climate Partnership FX We thank Ryan A. Chisholm, Matteo Detto, David A. King, Pasi Kolari, Edbert G. Leigh and Jeremy W. Lichstein for helpful comments. We acknowledge the financial support of the HSBC Climate Partnership. We relied on data published in compiled articles and thank investigators and funding agencies of the original studies and various regional flux networks (Afriflux, AmeriFlux, AsiaFlux, CarboAfrica, CarboEurope-IP, ChinaFlux, Fluxnet-Canada, KoFlux, LBA, NECC, OzFlux, TCOS-Siberia, USCCC) and the Fluxnet project, whose support is essential for obtaining the measurements without which the type of integrated analyses conducted in this study would not be possible. NR 48 TC 24 Z9 27 U1 5 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD OCT PY 2012 VL 21 IS 10 BP 998 EP 1006 DI 10.1111/j.1466-8238.2011.00740.x PG 9 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 003WG UT WOS:000308641500005 ER PT J AU Young, CM He, RY Emlet, RB Li, YZ Qian, H Arellano, SM Van Gaest, A Bennett, KC Wolf, M Smart, TI Rice, ME AF Young, Craig M. He, Ruoying Emlet, Richard B. Li, Yizhen Qian, Hui Arellano, Shawn M. Van Gaest, Ahna Bennett, Kathleen C. Wolf, Maya Smart, Tracey I. Rice, Mary E. TI Dispersal of Deep-Sea Larvae from the Intra-American Seas: Simulations of Trajectories using Ocean Models SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article ID MUSSEL BATHYMODIOLUS-CHILDRESSI; GULF-OF-MEXICO; GENETIC DIVERSITY; BENTHIC INVERTEBRATES; STYLOCIDARIS-LINEATA; POPULATION-STRUCTURE; HYDROTHERMAL VENTS; RIFTIA-PACHYPTILA; SEEP COMMUNITIES; EASTERN PACIFIC AB Using data on ocean circulation with a Lagrangian larval transport model, we modeled the potential dispersal distances for seven species of bathyal invertebrates whose durations of larval life have been estimated from laboratory rearing, MOCNESS plankton sampling, spawning times, and recruitment. Species associated with methane seeps in the Gulf of Mexico and/or Barbados included the bivalve "Bathymodiolus" childressi, the gastropod Bathynerita naticoidea, the siboglinid polychaete tube worm Lamellibrachia luymesi, and the asteroid Sclerasterias tanneri. Non-seep species included the echinoids Cidaris blakei and Stylocidaris lineata from sedimented slopes in the Bahamas and the wood-dwelling sipunculan Phascolosoma turnerae, found in Barbados, the Bahamas, and the Gulf of Mexico. Durations of the planktonic larval stages ranged from 3 weeks in lecithotrophic tubeworms to more than 2 years in planktotrophic starfish. Planktotrophic sipunculan larvae from the northern Gulf of Mexico were capable of reaching the mid-Atlantic off Newfoundland, a distance of more than 3000 km, during a 7- to 14-month drifting period, but the proportion retained in the Gulf of Mexico varied significantly among years. Larvae drifting in the upper water column often had longer median dispersal distances than larvae drifting for the same amount of time below the permanent thermocline, although the shapes of the distance-frequency curves varied with depth only in the species with the longest larval trajectories. Even species drifting for >2 years did not cross the ocean in the North Atlantic Drift. C1 [Young, Craig M.; Emlet, Richard B.; Arellano, Shawn M.; Van Gaest, Ahna; Bennett, Kathleen C.; Wolf, Maya; Smart, Tracey I.] Univ Oregon, Oregon Inst Marine Biol, Charleston, OR 97420 USA. [He, Ruoying; Li, Yizhen; Qian, Hui] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Rice, Mary E.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Young, CM (reprint author), Univ Oregon, Oregon Inst Marine Biol, Charleston, OR 97420 USA. EM cmyoung@uoregon.edu RI Arellano, Shawn/A-3960-2013; Li, Yizhen/O-3869-2015 OI Li, Yizhen/0000-0001-6565-1339 FU National Science Foundation [OCE-0527139, OCE-0119733, OCE-9633784, OCE-1029841, OCE-1030453] FX This work was supported by National Science Foundation grants OCE-0527139, OCE-0119733, OCE-9633784, OCE-1029841, and OCE-1030453. NR 63 TC 29 Z9 31 U1 4 U2 67 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD OCT PY 2012 VL 52 IS 4 BP 483 EP 496 DI 10.1093/icb/ics090 PG 14 WC Zoology SC Zoology GA 014KK UT WOS:000309374400005 PM 22669174 ER PT J AU Schulze, A Maiorova, A Timm, LE Rice, ME AF Schulze, Anja Maiorova, Anastassya Timm, Laura E. Rice, Mary E. TI Sipunculan Larvae and "Cosmopolitan" Species SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article ID DISPERSAL; CONNECTIVITY; WORMS; SEA; PHYLOGENY; EVOLUTION; DURATION; DISTANCE; GENES; JAPAN AB Sipuncula is a relatively small taxon with roughly 150 recognized species. Many species are geographically widespread or "cosmopolitan." The pelagosphera larvae of some species are estimated to spend several months in the plankton. However, recent molecular evidence suggests that many of the "cosmopolitan" species actually represent species-complexes, some not even monophyletic. Herein, we present data on three sipunculan species with different developmental modes that occur both in the Sea of Japan and in the Northeast Pacific. The development of the three species-Phascolosoma agnssizii, Thysanocardin nigra, and Themiste pyroides-is exceptionally well studied in both regions of the Pacific. Significant differences have been observed between the two regions with respect to egg size, developmental mode, and developmental timing. In general, eggs are larger and development slower in the Northeast Pacific when compared with the Sea of Japan. These differences have been explained as a result of phenotypic plasticity exhibited under different environmental conditions, in particular temperature, but we show that the populations of all three species are also remarkably distinct genetically and that gene flow between the two regions is extremely unlikely. In Thysanocardia nigra, we even found two very distinct genetic lineages within the same location in the Northeast Pacific. The amount of genetic divergence between populations from the Sea of Japan and those from the Northeast Pacific is not correlated with developmental mode. Themiste pyroides, the species with the most abbreviated development, actually has the least degree of genetic divergence between the regions. Analyses of molecular variance show that the majority of the observed variation in all three species is between the regions. We conclude that all three "cosmopolitan" species actually represent complexes of cryptic or pseudo-cryptic species. These examples demonstrate that a solid taxonomic framework based on molecular and morphological evidence is a prerequisite for evaluating relationships between dispersal capabilities, species' ranges, and the connectivity of populations. C1 [Schulze, Anja; Timm, Laura E.] Texas A&M Univ, Dept Marine Biol, Galveston, TX 77553 USA. [Maiorova, Anastassya] Russian Acad Sci, Far E Branch, AV Zhirmunsky Inst Marine Biol, Lab Prod Biol, Vladivostok 690059, Russia. [Maiorova, Anastassya] Far Eastern Fed Univ, Interdept Lab Biol Marine Invertebrates, Vladivostok 690091, Russia. [Rice, Mary E.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Schulze, A (reprint author), Texas A&M Univ, Dept Marine Biol, POB 1675, Galveston, TX 77553 USA. EM schulzea@tamug.edu RI Schulze, Anja/I-4215-2012 FU American Microscopical Society; Society for Integrative and Comparative Biology Divisions of Evolutionary Developmental Biology, Ecology & Evolution, and Invertebrate Zoology; National Science Foundation [IOS-1148884]; Far East Branch of the Russian Academy of Science; Civilian Research and Development Foundation (CRDF Global) [RUB1-2996VL-11]; National Science Foundation Assembling the Tree of Life grant [DEB-1036186]; Far East Branch of the Russian Academy of Sciences [12-HHC-007, 12-I-0-06-003]; RFBR [11-04-98546 r_vostok, 12-04-10132-K]; Ministry of Education and Science of Russian Federation [11.G34.31.0010] FX Our participation in the symposium was supported by the American Microscopical Society, Society for Integrative and Comparative Biology Divisions of Evolutionary Developmental Biology, Ecology & Evolution, and Invertebrate Zoology, and by National Science Foundation Grant IOS-1148884 to Sara M. Lindsay. The research was funded by a collaborative grant from the Far East Branch of the Russian Academy of Science and Civilian Research and Development Foundation (CRDF Global) to A.S. and A.M. (RUB1-2996VL-11), by National Science Foundation Assembling the Tree of Life grant DEB-1036186 to A.S. Further funding was provided by the Far East Branch of the Russian Academy of Sciences (grants 12-HHC-007, 12-I-0-06-003), RFBR 11-04-98546 r_vostok, 12-04-10132-K and Ministry of Education and Science of Russian Federation (grant 11.G34.31.0010). NR 36 TC 9 Z9 9 U1 0 U2 24 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD OCT PY 2012 VL 52 IS 4 BP 497 EP 510 DI 10.1093/icb/ics082 PG 14 WC Zoology SC Zoology GA 014KK UT WOS:000309374400006 PM 22634356 ER PT J AU Dainotti, MG Ostrowski, M Harris, D Siemiginowska, A Siejkowski, H AF Dainotti, M. G. Ostrowski, M. Harris, D. Siemiginowska, A. Siejkowski, H. TI A cosmic ray cocoon along the X-ray jet of M87? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; galaxies: active; galaxies: jets ID SUPERMASSIVE BLACK-HOLE; XMM-NEWTON; TEMPERATURE STRUCTURE; RELATIVISTIC JETS; IONIZED-GAS; M-87; ACCELERATION; PARTICLES; FILAMENTS; HST-1 AB Relativistic jets propagating through an ambient medium must produce some observational effects along their side boundaries because of interactions across the large velocity gradient. One possible effect of such an interaction would be a sheared magnetic field structure at the jet boundaries, leading to a characteristic radio polarization pattern. As proposed by Ostrowski, another effect can come from the generation of a high-energy cosmic ray component at the boundary, producing dynamic effects on the medium surrounding the jet and forming a cocoon dominated by cosmic rays with a decreased thermal gas emissivity. We selected this process for our first attempt to look for the effects of this type of interaction. We analysed the Chandra X-ray data for the radio galaxy M87 in order to verify if the expected regions of diminished emissivity may be present near the spectacular X-ray jet in this source. The detailed analysis of the data, merged from 42 separate observations, shows signatures of lower emissivity surrounding the jet. In particular we detect an intensity dip along the part of the jet, which would be approximately 1.5 X 0.15?kpc2 in size, if situated along the jet which is inclined towards us. Due to a highly non-uniform X-ray background in the central region, we are not able to claim the discovery of a cosmic ray cocoon around the M87 jet: we only have demonstrated that the data show morphological structures which could be accounted for if a cosmic ray cocoon exists. C1 [Dainotti, M. G.; Ostrowski, M.; Siejkowski, H.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland. [Harris, D.; Siemiginowska, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Dainotti, MG (reprint author), Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, Ul Orla 171, PL-30244 Krakow, Poland. EM dainotti@oa.uj.edu.pl FU Polish MNiSW [N N203 380336]; Angelo Della Riccia Foundation; NASA [NAS8-39073, GOO-11120X] FX We thank Edoardo Trussoni for valuable comments, W. Forman and W. Sparks for discussions on the vagaries of the hot ISM, M. Paolillo, A. Gibiec and A. Szostek for comments and discussions on data analysis techniques and L. Stawarz for valuable criticism and advice. MGD and MO are grateful for the support from Polish MNiSW through the grant N N203 380336. MGD is also grateful for the support from Angelo Della Riccia Foundation. This research is funded in part by NASA contract NAS8-39073 and NASA grant GOO-11120X. NR 37 TC 0 Z9 0 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 426 IS 1 BP 218 EP 225 DI 10.1111/j.1365-2966.2012.21086.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009ZQ UT WOS:000309064600017 ER PT J AU Scudder, JM Ellison, SL Torrey, P Patton, DR Mendel, JT AF Scudder, Jillian M. Ellison, Sara L. Torrey, Paul Patton, David R. Mendel, J. Trevor TI Galaxy pairs in the Sloan Digital Sky Survey - V. Tracing changes in star formation rate and metallicity out to separations of 80 kpc SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: interactions; galaxies: star formation ID ACTIVE GALACTIC NUCLEI; FORMING GALAXIES; CLOSE PAIRS; INTERACTING GALAXIES; MERGING GALAXIES; MAJOR MERGERS; MINOR MERGERS; 2DF SURVEY; GAS-FLOWS; MASS AB We present a sample of 1899 galaxies with a close companion taken from the Sloan Digital Sky Survey Data Release 7. The galaxy pairs are selected to have velocity differences ?v < 300 km?s-1, projected separations (rp) < 80 h70-1?kpc, mass ratios between 0.1 and 10, and robust measurements of star formation rates and gas-phase metallicities. We match the galaxies in total stellar mass, redshift and local density to a set of 10 control galaxies per pair galaxy. For each pair galaxy, we can therefore calculate the statistical change in star formation rate (SFR) and metallicity associated with the interaction process. Relative to the control sample, we find that galaxies in pairs show typical SFR enhancements that are, on average, 60 per cent higher than the control sample at rp < 30 h70-1?kpc. It is at these small separations that the strongest enhancements in SFR (by up to a factor of 10) are measured, although such starbursts are rare, even amongst the closest pairs. In addition, the pairs demonstrate more modest SFR enhancements of 30 per cent out to at least 80 h70-1?kpc (the widest separations in our sample). This is the first time that enhanced SFRs have been robustly detected out to such large projected separations. Galaxies in both major and minor mergers show significant SFR enhancements at all rp, although the strongest starbursts (with SFR enhancements of a factor of 10) appear to be found only in the major mergers. We also find evidence that SFR enhancements are synchronized in an interacting pair, such that a higher SFR in one galaxy is accompanied by an increased SFR in its companion. For the first time, we are also able to trace the metallicity changes in galaxy pairs as a function of projected separation. The metallicity is generally diluted in galaxy pairs by 0.02 dex, with an average metallicity decrement of -0.03 dex at the smallest separations, a trend that mirrors the SFR enhancements as a function of rp. The SFR and metallicity trends with projected separation are interpreted through a comparison with theoretical models. These simulations indicate that the peak in SFR enhancements at small separations is due to systems near the end of the merger process. The extended plateau in SFR enhancements out to at least 80 h70-1?kpc is dominated by galaxies that have made a pericentric passage and are now experiencing triggered star formation on their trajectory towards apogalacticon, or on a subsequent close approach. C1 [Scudder, Jillian M.; Ellison, Sara L.; Mendel, J. Trevor] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Torrey, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Patton, David R.] Trent Univ, Dept Phys & Astron, Peterborough, ON K9J 7B8, Canada. RP Scudder, JM (reprint author), Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. EM jscudder@uvic.ca OI Scudder, Jillian/0000-0002-8798-3972; Torrey, Paul/0000-0002-5653-0786 FU NSERC; 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 We thank the anonymous referee for a constructive report. We are grateful to the MPA/JHU group for access to their data products and catalogues (maintained by Jarle Brinchmann at http://www.mpagarching.mpg.de/SDSS/). SLE and DRP acknowledge the receipt of an NSERC Discovery grant which funded this research.; 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 64 TC 70 Z9 70 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD OCT PY 2012 VL 426 IS 1 BP 549 EP 565 DI 10.1111/j.1365-2966.2012.21749.x PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009ZQ UT WOS:000309064600041 ER PT J AU Guerra, A Portela, JM Roura, A del Rio, JL Vecchione, M AF Guerra, Angel Portela, Julio M. Roura, Alvaro Luis del Rio, Jose Vecchione, Michael TI Morphological variability of the rare bush-club squid Batoteuthis (Cephalopoda, Batoteuthidae)? SO NEUES JAHRBUCH FUR GEOLOGIE UND PALAONTOLOGIE-ABHANDLUNGEN LA English DT Article DE Systematics; Batoteuthis skolops; cephalopods; Patagonian slope AB A specimen of Batoteuthidae was caught during the research cruise ATLANTIS 2009 on 21 March 2009 at 45 degrees 09.51' S - 45 degrees 08.07' S - 59 degrees 29.04' W - 59 degrees 27.98' W (Patagonian slope), depth 1195-1221 m. This specimen is a juvenile male, 105 mm mantle length. It is the largest Batoteuthis with complete tentacles captured to date. It shares the main diagnostic characters of the family. We compared that specimen with the types of Batoteuthis skolops, the only known species in the family. Our specimen has several differences from the types (lower tail length index, different fin shape, arm length indices 3-4 times longer, tentacles and clubs 4 or 5 times longer than the types, distinct arrangement of suckers in ventral arms, and different number, size and disposition of suckers in tentacular clubs) suggesting that it might be a different species. However, we cannot refute the alternative hypothesis that the differences are ontogenic. Until additional good specimens become available or molecular analyses are undertaken, we recommend a conservative approach of considering our specimen tentatively to be a growth form of Batoteuthis skolops. C1 [Guerra, Angel; Roura, Alvaro] CSIC, Inst Invest Marinas, Vigo 36208, Spain. [Portela, Julio M.; Luis del Rio, Jose] CO Vigo, IEO, Vigo 36200, Spain. [Vecchione, Michael] Smithsonian Inst, NMFS Natl Systemat Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Guerra, A (reprint author), CSIC, Inst Invest Marinas, Eduardo Cabello 6, Vigo 36208, Spain. EM angelguerra@iim.csic.es; julio.portela@vi.ieo.es; aroura@iim.csic.es; joseluis.delrio@vi.ieo.es; VecchioneM@si.edu RI Roura, Alvaro/L-6754-2014 OI Roura, Alvaro/0000-0003-3532-6759 NR 13 TC 2 Z9 2 U1 0 U2 3 PU E SCHWEIZERBARTSCHE VERLAGS PI STUTTGART PA NAEGELE U OBERMILLER, SCIENCE PUBLISHERS, JOHANNESSTRASSE 3A, D 70176 STUTTGART, GERMANY SN 0077-7749 J9 NEUES JAHRB GEOL P-A JI Neues. Jahrb. Geol. Palaontol.-Abh. PD OCT PY 2012 VL 266 IS 1 BP 77 EP 83 DI 10.1127/0077-7749/2012/0267 PG 7 WC Paleontology SC Paleontology GA 016HQ UT WOS:000309508800010 ER PT J AU Ubelaker, DH AF Ubelaker, Douglas H. TI Obituary: Donald J. Ortner (1938-2012) SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Biographical-Item C1 Smithsonian Inst, Dept Anthropol, Washington, DC 20013 USA. RP Ubelaker, DH (reprint author), Smithsonian Inst, Dept Anthropol, NMNH MRC 112,POB 37012,10th & Constitut Ave NW, Washington, DC 20013 USA. EM ubelaked@si.edu NR 1 TC 1 Z9 1 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD OCT PY 2012 VL 149 IS 2 BP 155 EP 156 DI 10.1002/ajpa.22129 PG 2 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 007HJ UT WOS:000308879100001 ER PT J AU Ak, NF Brandt, WN Hall, PB Schneider, DP Anderson, SF Gibson, RR Lundgren, BF Myers, AD Petitjean, P Ross, NP Shen, Y York, DG Bizyaev, D Brinkmann, J Malanushenko, E Oravetz, DJ Pan, K Simmons, AE Weaver, BA AF Ak, N. Filiz Brandt, W. N. Hall, P. B. Schneider, D. P. Anderson, S. F. Gibson, R. R. Lundgren, B. F. Myers, A. D. Petitjean, P. Ross, Nicholas P. Shen, Yue York, D. G. Bizyaev, D. Brinkmann, J. Malanushenko, E. Oravetz, D. J. Pan, K. Simmons, A. E. Weaver, B. A. TI BROAD ABSORPTION LINE DISAPPEARANCE ON MULTI-YEAR TIMESCALES IN A LARGE QUASAR SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: absorption lines ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; DATA RELEASE; SDSS-III; STELLAR OBJECTS; MILKY-WAY; SI IV; C IV; OUTFLOWS; VARIABILITY AB We present 21 examples of CIV broad absorption line (BAL) trough disappearance in 19 quasars selected from systematic multi-epoch observations of 582 bright BAL quasars (1.9 < z < 4.5) by the Sloan Digital Sky Survey-I/II (SDSS-I/II) and SDSS-III. The observations span 1.1-3.9 yr rest-frame timescales, longer than have been sampled in many previous BAL variability studies. On these timescales, approximate to 2.3% of C iv BAL troughs disappear and approximate to 3.3% of BAL quasars show a disappearing trough. These observed frequencies suggest that many CIV BAL absorbers spend on average at most a century along our line of sight to their quasar. Ten of the 19 BAL quasars showing C iv BAL disappearance have apparently transformed from BAL to non-BAL quasars; these are the first reported examples of such transformations. The BAL troughs that disappear tend to be those with small-to-moderate equivalent widths, relatively shallow depths, and high outflow velocities. Other non-disappearing CIV BALs in those nine objects having multiple troughs tend to weaken when one of them disappears, indicating a connection between the disappearing and non-disappearing troughs, even for velocity separations as large as 10,000-15,000 km s(-1). We discuss possible origins of this connection including disk-wind rotation and changes in shielding gas. C1 [Ak, N. Filiz; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Ak, N. Filiz; Brandt, W. N.; Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Ak, N. Filiz] Erciyes Univ, Dept Astron & Space Sci, Fac Sci, TR-38039 Kayseri, Turkey. [Hall, P. B.] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Anderson, S. F.; Gibson, R. R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Lundgren, B. F.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Myers, A. D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Petitjean, P.] Univ Paris 06, Inst Astrophys Paris, F-75014 Paris, France. [Ross, Nicholas P.] Lawrence Berkeley Natl Lab, Berkeley, CA 92420 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [York, D. G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, D. G.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bizyaev, D.; Brinkmann, J.; Malanushenko, E.; Oravetz, D. J.; Pan, K.; Simmons, A. E.] Apache Point Observ, Sunspot, NM 88349 USA. [Weaver, B. A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Ak, NF (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM nfilizak@astro.psu.edu RI Filiz Ak, Nurten/C-9686-2015; Brandt, William/N-2844-2015 OI Filiz Ak, Nurten/0000-0003-3016-5490; Brandt, William/0000-0002-0167-2453 FU National Science Foundation [AST-1108604]; NSERC; Alfred P. Sloan Foundation; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; U.S. Department of Energy Office of Science FX We gratefully acknowledge financial support from National Science Foundation Grant AST-1108604 (NFA, WNB, DPS) and from NSERC (PBH). We thank D. M. Capellupo and F. Hamann for sharing their EW measurements for the Capellupo et al. (2011) sample in Figure 1. We thank K. Dawson, M. Eracleous, D. Proga, and J. Wu for helpful discussions. We also thank the anonymous referee for useful feedback.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 59 TC 22 Z9 22 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 114 DI 10.1088/0004-637X/757/2/114 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500007 ER PT J AU Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Dumm, J Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Holder, J Huan, H Hughes, G Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lee, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Skole, C Smith, AW Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Varlotta, A Vivier, M Wakely, SP Ward, JE Weinstein, A Welsing, R Williams, DA Zitzer, B Pfrommer, C Pinzke, A AF Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Dumm, J. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Holder, J. Huan, H. Hughes, G. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lee, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pohl, M. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Skole, C. Smith, A. W. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Varlotta, A. Vivier, M. Wakely, S. P. Ward, J. E. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. Pfrommer, C. Pinzke, A. TI CONSTRAINTS ON COSMIC RAYS, MAGNETIC FIELDS, AND DARK MATTER FROM GAMMA-RAY OBSERVATIONS OF THE COMA CLUSTER OF GALAXIES WITH VERITAS AND FERMI SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic rays; dark matter; galaxies: clusters: general; galaxies: clusters: individual (Coma (ACO 1656)); gamma rays: galaxies: clusters; magnetic fields ID LARGE-SCALE STRUCTURE; ATMOSPHERIC CHERENKOV TELESCOPES; DIFFUSE RADIO-EMISSION; ALL-SKY SURVEY; X-RAY; UPPER LIMITS; SHOCK-WAVES; NONTHERMAL EMISSION; GALACTIC-CENTER; SOURCE CATALOG AB Observations of radio halos and relics in galaxy clusters indicate efficient electron acceleration. Protons should likewise be accelerated and, on account of weak energy losses, can accumulate, suggesting that clusters may also be sources of very high energy (VHE; E > 100 GeV) gamma-ray emission. We report here on VHE gamma-ray observations of the Coma galaxy cluster with the VERITAS array of imaging Cerenkov telescopes, with complementing Fermi Large Area Telescope observations at GeV energies. No significant gamma-ray emission from the Coma Cluster was detected. Integral flux upper limits at the 99% confidence level were measured to be on the order of (2-5) x 10(-8) photonsm(-2) s(-1) (VERITAS, >220 GeV) and similar to 2 x 10(-6) photonsm(-2) s(-1) (Fermi, 1-3GeV), respectively. We use the gamma-ray upper limits to constrain cosmic rays (CRs) and magnetic fields in Coma. Using an analytical approach, the CR-to-thermal pressure ratio is constrained to be < 16% from VERITAS data and <1.7% from Fermi data (averaged within the virial radius). These upper limits are starting to constrain the CR physics in self-consistent cosmological cluster simulations and cap the maximum CR acceleration efficiency at structure formation shocks to be <50%. Alternatively, this may argue for non-negligible CR transport processes such as CR streaming and diffusion into the outer cluster regions. Assuming that the radio-emitting electrons of the Coma halo result from hadronic CR interactions, the observations imply a lower limit on the central magnetic field in Coma of similar to(2-5.5) mu G, depending on the radial magnetic field profile and on the gamma-ray spectral index. Since these values are below those inferred by Faraday rotation measurements in Coma (for most of the parameter space), this renders the hadronic model a very plausible explanation of the Coma radio halo. Finally, since galaxy clusters are dark matter (DM) dominated, the VERITAS upper limits have been used to place constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the DM particles, . C1 [Arlen, T.; Majumdar, P.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; 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.; Lee, K.; McArthur, S.; Thibadeau, S.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Godambe, S.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Griffin, S.; 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. [Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Pfrommer, C.] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Pinzke, A.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Arlen, T (reprint author), Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. EM pohlmadq@gmail.com; christoph.pfrommer@h-its.org RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K; National Aeronautics and Space Administration; Department of Energy in the United States; Commissariat a l'Energie Atomique; Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France; Agenzia Spaziale Italiana; Istituto Nazionale di Fisica Nucleare in Italy; Ministry of Education, Culture, Sports, Science and Technology (MEXT); High Energy Accelerator Research Organization (KEK); Japan Aerospace Exploration Agency (JAXA) in Japan; K. A. Wallenberg Foundation; Swedish Research Council; Swedish National Space Board in Sweden; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Klaus Tschira Foundation; NSF [AST-0908480] FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument.; The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT, as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden.; Additional support for science analysis during the operation phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; C. P. gratefully acknowledges financial support of the Klaus Tschira Foundation. A. P. acknowledges NSF grant AST-0908480 for support. NR 97 TC 43 Z9 43 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 OCT 1 PY 2012 VL 757 IS 2 AR 123 DI 10.1088/0004-637X/757/2/123 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500016 ER PT J AU Berry, M Ivezic, Z Sesar, B Juric, M Schlafly, EF Bellovary, J Finkbeiner, D Vrbanec, D Beers, TC Brooks, KJ Schneider, DP Gibson, RR Kimball, A Jones, L Yoachim, P Krughoff, S Connolly, AJ Loebman, S Bond, NA Schlegel, D Dalcanton, J Yanny, B Majewski, SR Knapp, GR Gunn, JE Smith, JA Fukugita, M Kent, S Barentine, J Krzesinski, J Long, D AF Berry, Michael Ivezic, Zeljko Sesar, Branimir Juric, Mario Schlafly, Edward F. Bellovary, Jillian Finkbeiner, Douglas Vrbanec, Dijana Beers, Timothy C. Brooks, Keira J. Schneider, Donald P. Gibson, Robert R. Kimball, Amy Jones, Lynne Yoachim, Peter Krughoff, Simon Connolly, Andrew J. Loebman, Sarah Bond, Nicholas A. Schlegel, David Dalcanton, Julianne Yanny, Brian Majewski, Steven R. Knapp, Gillian R. Gunn, James E. Smith, J. Allyn Fukugita, Masataka Kent, Steve Barentine, John Krzesinski, Jurek Long, Dan TI THE MILKY WAY TOMOGRAPHY WITH SLOAN DIGITAL SKY SURVEY. IV. DISSECTING DUST SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; dust; extinction; stars: statistics; surveys ID SURVEY PHOTOMETRIC SYSTEM; INTERSTELLAR EXTINCTION; STELLAR LOCUS; ULTRAVIOLET EXTINCTION; GALACTIC EXTINCTION; WHITE-DWARFS; DATA RELEASE; PAN-STARRS; SDSS; GALAXY AB We use Sloan Digital Sky Survey (SDSS) photometry of 73 million stars to simultaneously constrain best-fit main-sequence stellar spectral energy distribution (SED) and amount of dust extinction along the line of sight toward each star. Using a subsample of 23 million stars with Two Micron All Sky Survey (2MASS) photometry, whose addition enables more robust results, we show that SDSS photometry alone is sufficient to break degeneracies between intrinsic stellar color and dust amount when the shape of extinction curve is fixed. When using both SDSS and 2MASS photometry, the ratio of the total to selective absorption, R-V, can be determined with an uncertainty of about 0.1 for most stars in high-extinction regions. These fits enable detailed studies of the dust properties and its spatial distribution, and of the stellar spatial distribution at low Galactic latitudes (vertical bar b vertical bar < 30 degrees). Our results are in good agreement with the extinction normalization given by the Schlegel et al. (SFD) dust maps at high northern Galactic latitudes, but indicate that the SFD extinction map appears to be consistently overestimated by about 20% in the southern sky, in agreement with recent study by Schlafly et al. The constraints on the shape of the dust extinction curve across the SDSS and 2MASS bandpasses disfavor the reddening law of O'Donnell, but support the models by Fitzpatrick and Cardelli et al. For the latter, we find a ratio of the total to selective absorption to be R-V = 3.0 +/- 0.1(random)+/- 0.1 (systematic) over most of the high-latitude sky. At low Galactic latitudes (vertical bar b vertical bar < 5 degrees), we demonstrate that the SFD map cannot be reliably used to correct for extinction because most stars are embedded in dust, rather than behind it, as is the case at high Galactic latitudes. We analyze three-dimensional maps of the best-fit R-V and find that R-V = 3.1 cannot be ruled out in any of the 10 SEGUE stripes at a precision level of similar to 0.1-0.2. Our best estimate for the intrinsic scatter of R-V in the regions probed by SEGUE stripes is similar to 0.2. We introduce a method for efficient selection of candidate red giant stars in the disk, dubbed "dusty parallax relation," which utilizes a correlation between distance and the extinction along the line of sight. We make these best-fit parameters, as well as all the input SDSS and 2MASS data, publicly available in a user-friendly format. These data can be used for studies of stellar number density distribution, the distribution of dust properties, for selecting sources whose SED differs from SEDs for high-latitude main-sequence stars, and for estimating distances to dust clouds and, in turn, to molecular gas clouds. C1 [Berry, Michael; Ivezic, Zeljko; Brooks, Keira J.; Gibson, Robert R.; Jones, Lynne; Yoachim, Peter; Krughoff, Simon; Connolly, Andrew J.; Loebman, Sarah; Dalcanton, Julianne] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Berry, Michael; Bond, Nicholas A.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Sesar, Branimir] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Juric, Mario] Harvard Coll Observ, Cambridge, MA 02138 USA. [Schlafly, Edward F.; Finkbeiner, Douglas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bellovary, Jillian] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Vrbanec, Dijana] Univ Zagreb, Fac Sci, Dept Phys, Zagreb 10000, Croatia. [Beers, Timothy C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Beers, Timothy C.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Beers, Timothy C.] Michigan State Univ, JINA, E Lansing, MI 48824 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kimball, Amy] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Schlegel, David] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Yanny, Brian; Kent, Steve] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Knapp, Gillian R.; Gunn, James E.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Smith, J. Allyn] Austin Peay State Univ, Dept Phys & Astron, Clarksville, TN 37044 USA. [Fukugita, Masataka] Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba, Japan. [Barentine, John; Krzesinski, Jurek; Long, Dan] Apache Point Observ, Sunspot, NM 88349 USA. RP Berry, M (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. OI Bellovary, Jillian/0000-0001-7596-8372; Yoachim, Peter/0000-0003-2874-6464; Schlafly, Edward Ford/0000-0002-3569-7421 FU NSF [AST-615991, AST-0707901, AST-0551161, PHY05-51164]; Croatian National Science Foundation [O-1548-2009]; NASA [NNX10AD69G]; Office of Science, Office of High Energy Physics, of the U.S. Department of Energy [DE-AC02-05CH11231]; Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA) [PHY 08-22648]; United States Department of Energy [DE-AC02-07CH11359]; Alfred P. Sloan 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-PlanckInstitute 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 Z. Ivezic and B. Sesar acknowledge support by NSF grants AST-615991 and AST-0707901, and by NSF grant AST-0551161 to LSST for design and development activity.. Z. Ivezic thanks the University of Zagreb, where a portion of this work was completed, for its hospitality, and acknowledges support by the Croatian National Science Foundation grant O-1548-2009. M. Berry,. Z. Ivezic, and B. Sesar acknowledge hospi-tality by the Institute for Astronomy, University of Hawaii. D. Finkbeiner and E. Schlafly acknowledge the support of NASA grant NNX10AD69G. This work was supported by the Director, Office of Science, Office of High Energy Physics, of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. T.C. Beers acknowledges partial support from PHY 08-22648: Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the U.S. National Science Foundation. We acknowledge the hospitality of the KITP at the University of California, Santa Barbara, where part of this work was completed (supported by NSF grant PHY05-51164). Fermilab is operated by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the United States Department of Energy.; 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-PlanckInstitute 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 57 TC 32 Z9 32 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 166 DI 10.1088/0004-637X/757/2/166 PG 35 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500059 ER PT J AU Corsaro, E Stello, D Huber, D Bedding, TR Bonanno, A Brogaard, K Kallinger, T Benomar, O White, TR Mosser, B Basu, S Chaplin, WJ Christensen-Dalsgaard, J Elsworth, YP Garcia, RA Hekker, S Kjeldsen, H Mathur, S Meibom, S Hall, JR Ibrahim, KA Klaus, TC AF Corsaro, Enrico Stello, Dennis Huber, Daniel Bedding, Timothy R. Bonanno, Alfio Brogaard, Karsten Kallinger, Thomas Benomar, Othman White, Timothy R. Mosser, Benoit Basu, Sarbani Chaplin, William J. Christensen-Dalsgaard, Jorgen Elsworth, Yvonne P. Garcia, Rafael A. Hekker, Saskia Kjeldsen, Hans Mathur, Savita Meibom, Soren Hall, Jennifer R. Ibrahim, Khadeejah A. Klaus, Todd C. TI ASTEROSEISMOLOGY OF THE OPEN CLUSTERS NGC 6791, NGC 6811, AND NGC 6819 FROM 19 MONTHS OF KEPLER PHOTOMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual; stars: evolution; stars: oscillations; techniques: photometric ID SOLAR-LIKE OSCILLATIONS; MAIN-SEQUENCE STARS; INFRARED FLUX METHOD; RED-GIANT STARS; 1ST 4 MONTHS; STELLAR OSCILLATIONS; HELIUM CONTENT; PARAMETERS; COROT; DIAGRAMS AB We studied solar-like oscillations in 115 red giants in the three open clusters, NGC 6791, NGC 6811, and NGC 6819, based on photometric data covering more than 19 months with NASA's Kepler space telescope. We present the asteroseismic diagrams of the asymptotic parameters delta nu(02), delta nu(01), and epsilon, which show clear correlation with fundamental stellar parameters such as mass and radius. When the stellar populations from the clusters are compared, we see evidence for a difference in mass of the red giant branch stars and possibly a difference in structure of the red clump stars, from our measurements of the small separations delta nu(02) and delta nu(01). Ensemble echelle diagrams and upper limits to the linewidths of l = 0 modes as a function of Delta nu of the clusters NGC 6791 and NGC 6819 are also shown, together with the correlation between the l = 0 ridge width and the T-eff of the stars. Lastly, we distinguish between red giant branch and red clump stars through the measurement of the period spacing of mixed dipole modes in 53 stars among all the three clusters to verify the stellar classification from the color-magnitude diagram. These seismic results also allow us to identify a number of special cases, including evolved blue stragglers and binaries, as well as stars in late He-core burning phases, which can be potentially interesting targets for detailed theoretical modeling. C1 [Corsaro, Enrico] Univ Catania, Dept Phys & Astron, Astrophys Sect, I-95123 Catania, Italy. [Corsaro, Enrico; Bonanno, Alfio] Astrophys Observ Catania, INAF, I-95123 Catania, Italy. [Stello, Dennis; Huber, Daniel; Bedding, Timothy R.; Benomar, Othman; White, Timothy R.] Univ Sydney, SIfA, Sch Phys, Sydney, NSW 2006, Australia. [Brogaard, Karsten] Univ Victoria, Dept Phys & Astron, Victoria, BC V8W 3P6, Canada. [Kallinger, Thomas] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Mosser, Benoit] Univ Paris 07, Univ Paris 06, LESIA Observ Paris, CNRS, F-92195 Meudon, France. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Chaplin, William J.; Elsworth, Yvonne P.; Mathur, Savita] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Chaplin, William J.; Christensen-Dalsgaard, Jorgen; Garcia, Rafael A.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, DASC, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Garcia, Rafael A.] Univ Paris Diderot IRFU SAp, Lab AIM, CEA DSM CNRS, F-91191 Gif Sur Yvette, France. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Mathur, Savita] NCAR, High Altitude Observ, Boulder, CO 80307 USA. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hall, Jennifer R.; Ibrahim, Khadeejah A.; Klaus, Todd C.] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Corsaro, E (reprint author), Univ Catania, Dept Phys & Astron, Astrophys Sect, Via S Sofia 78, I-95123 Catania, Italy. RI Bonanno, Alfio/J-1845-2012; OI Kallinger, Thomas/0000-0003-3627-2561; Bonanno, Alfio/0000-0003-3175-9776; Brogaard, Karsten/0000-0003-2001-0276; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Basu, Sarbani/0000-0002-6163-3472; Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate; European Community [269194]; Australian Research Council; Carlsberg Foundation; Netherlands Organisation for Scientific Research (NWO); FWO-Flanders [O6260-G.0728.11]; National Science Foundation [NSF PHY05-51164] FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors thank the entire Kepler team, without whom this investigation would not have been possible. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 269194. D. S. acknowledges support from the Australian Research Council. K. B. acknowledges funding from the Carlsberg Foundation. S. H. acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO). T. K. is supported by the FWO-Flanders under project O6260-G.0728.11. NCAR is partially supported by the National Science Foundation. This research was supported in part by the National Science Foundation under grant No. NSF PHY05-51164. Data presented in this paper are available upon request to the first author. NR 60 TC 72 Z9 72 U1 2 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 OCT 1 PY 2012 VL 757 IS 2 AR 190 DI 10.1088/0004-637X/757/2/190 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500083 ER PT J AU Hirsch, L Adams, JD Herter, TL Hora, JL De Buizer, JM Megeath, ST Gull, GE Henderson, CP Keller, LD Schoenwald, J Vacca, W AF Hirsch, Lea Adams, Joseph D. Herter, Terry L. Hora, Joseph L. De Buizer, James M. Megeath, S. Thomas Gull, George E. Henderson, Charles P. Keller, Luke D. Schoenwald, Justin Vacca, William TI SOFIA/FORCAST AND SPITZER/IRAC IMAGING OF THE ULTRACOMPACT HII REGION W3(OH) AND ASSOCIATED PROTOSTARS IN W3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; HII regions; infrared: stars; radiative transfer; stars: formation ID GIANT MOLECULAR CLOUD; SPECTRAL ENERGY-DISTRIBUTIONS; YOUNG STELLAR OBJECTS; ARRAY CAMERA IRAC; SPACE-TELESCOPE; STAR-FORMATION; EMISSION; MASERS; AMMONIA; GRAINS AB We present infrared observations of the ultracompact HII region W3(OH) made by the FORCAST instrument aboard the Stratospheric Observatory for Infrared Astronomy (SOFIA) and by the Spitzer/Infrared Array Camera. We contribute new wavelength data to the spectral energy distribution (SED), which constrains the optical depth, grain size distribution, and temperature gradient of the dusty shell surrounding the HII region. We model the dust component as a spherical shell containing an inner cavity with radius similar to 600 AU, irradiated by a central star of type O9 and temperature similar to 31,000 K. The total luminosity of this system is 7.1x10(4) L-circle dot. An observed excess of 2.2-x4.5 mu m emission in the SED can be explained by our viewing a cavity opening or clumpiness in the shell structure whereby radiation from the warm interior of the shell can escape. We claim to detect the nearby water maser source W3 (H2O) at 31.4 and 37.1 mu m using beam deconvolution of the FORCAST images. We constrain the flux densities of this object at 19.7-x37.1 mu m. Additionally, we present in situ observations of four young stellar and protostellar objects in the SOFIA field, presumably associated with the W3 molecular cloud. Results from the model SED fitting tool of Robitaille et al. suggest that two objects (2MASS J02270352+6152357 and 2MASS J02270824+6152281) are intermediate-luminosity (similar to 236-x432 L-circle dot) protostars; one object (2MASS J02270887+6152344) is either a high-mass protostar with luminosity 3 x 10(3) L-circle dot or a less massive young star with a substantial circumstellar disk but depleted envelope; and the other (2MASS J02270743+6152281) is an intermediate-luminosity (similar to 768 L-circle dot) protostar nearing the end of its envelope accretion phase or a young star surrounded by a circumstellar disk with no appreciable circumstellar envelope. C1 [Hirsch, Lea; Adams, Joseph D.; Herter, Terry L.; Gull, George E.; Henderson, Charles P.; Schoenwald, Justin] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [De Buizer, James M.; Vacca, William] NASA, Ames Res Ctr, SOFIA Univ Space Res Assoc, Moffett Field, CA 94035 USA. [Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Keller, Luke D.] Ithaca Coll, Dept Phys, Ctr Nat Sci 264, Ithaca, NY 14850 USA. RP Hirsch, L (reprint author), Cornell Univ, Dept Astron, 105 Space Sci Bldg, Ithaca, NY 14853 USA. OI Hora, Joseph/0000-0002-5599-4650 FU NASA [NAS2-97001, 8500-98-014]; Deutsches SOFIA Institut (DSI) under DLR [50 OK 0901]; USRA; National Science Foundation FX We thank R. Grashius, S. Adams, H. Jakob, A. Reinacher, and U. Lampeter for their SOFIA telescope engineering and operations support. We also thank the SOFIA flight crews and mission operations team (A. Meyer, N. McKown, C. Kaminski) for their SOFIA flight planning and flight support. We are grateful to an anonymous referee for his or her comments which have improved this manuscript. This work is based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA science mission operations are conducted jointly by the Universities Space Research Association, Inc. (USRA), under NASA contract NAS2-97001, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901. Financial support for FORCAST was provided to Cornell by NASA through award 8500-98-014 issued by USRA. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. This 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. This research has made use of the NASA/IPAC Infrared Science ArChive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of NASA's Astrophysics Data System Abstract Service. NR 40 TC 8 Z9 8 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 113 DI 10.1088/0004-637X/757/2/113 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500006 ER PT J AU Komugi, S Tateuchi, K Motohara, K Takagi, T Iono, D Kaneko, H Ueda, J Saitoh, TR Kato, N Konishi, M Koshida, S Morokuma, T Takahashi, H Tanabe, T Yoshii, Y AF Komugi, S. Tateuchi, K. Motohara, K. Takagi, T. Iono, D. Kaneko, H. Ueda, J. Saitoh, T. R. Kato, N. Konishi, M. Koshida, S. Morokuma, T. Takahashi, H. Tanabe, T. Yoshii, Y. TI THE SCHMIDT-KENNICUTT LAW OF MATCHED-AGE STAR-FORMING REGIONS; Pa alpha OBSERVATIONS OF THE EARLY-PHASE INTERACTING GALAXY TAFFY I SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: interactions; galaxies: ISM; galaxies: starburst; HII regions; ISM: molecules ID CO-TO-H-2 CONVERSION FACTOR; LUMINOUS INFRARED GALAXIES; MOLECULAR GAS; NEARBY GALAXIES; SPIRAL GALAXIES; PATTERN SPEED; STELLAR MASS; H-ALPHA; MU-M; CO AB In order to test a recent hypothesis that the dispersion in the Schmidt-Kennicutt law arises from variations in the evolutionary stage of star-forming molecular clouds, we compared molecular gas and recent star formation in an early-phase merger galaxy pair, Taffy I (UGC 12915/UGC 12914, VV 254) which went through a direct collision 20 Myr ago and whose star-forming regions are expected to have similar ages. Narrowband Pa alpha image is obtained using the ANIR near-infrared camera on the mini-TAO 1 m telescope. The image enables us to derive accurate star formation rates within the galaxy directly. The total star formation rate, 22.2 M-circle dot yr(-1), was found to be much higher than previous estimates. Ages of individual star-forming blobs estimated from equivalent widths indicate that most star-forming regions are similar to 7 Myr old, except for a giant HII region at the bridge which is much younger. Comparison between star formation rates and molecular gas masses for the regions with the same age exhibits a surprisingly tight correlation, a slope of unity, and star formation efficiencies comparable to those of starburst galaxies. These results suggest that Taffy I has just evolved into a starburst system after the collision, and the star-forming sites are at a similar stage in their evolution from natal molecular clouds except for the bridge region. The tight Schmidt-Kennicutt law supports the scenario that dispersion in the star formation law is in large part due to differences in evolutionary stage of star-forming regions. C1 [Komugi, S.] Joint ALMA Observ, Santiago 7630355, Chile. [Tateuchi, K.; Motohara, K.; Kato, N.; Konishi, M.; Koshida, S.; Morokuma, T.; Takahashi, H.; Tanabe, T.; Yoshii, Y.] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Takagi, T.] JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. [Iono, D.; Kaneko, H.; Ueda, J.] Natl Astron Observ, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan. [Saitoh, T. R.] Tokyo Inst Technol, Interact Res Ctr Sci, Meguro Ku, Tokyo 1520033, Japan. [Komugi, S.] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Tateuchi, K.; Motohara, K.; Ueda, J.] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Kaneko, H.] Grad Univ Adv Studies SOKENDAI, Sch Phys Sci, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. [Kaneko, H.] Univ Tsukuba, Inst Phys, Tsukuba, Ibaraki 3058577, Japan. [Ueda, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Komugi, S (reprint author), Joint ALMA Observ, Alonso de Cordova 3107, Santiago 7630355, Chile. EM skomugi@alma.cl RI Saitoh, Takayuki/A-2740-2014; MOTOHARA, KENTARO/G-4905-2014; OI MOTOHARA, KENTARO/0000-0002-0724-9146; Kaneko, Hiroyuki/0000-0002-2699-4862 FU Japan Science Society; Ministry of Education, Culture, Sports, Science and Technology of Japan; National Astronomical Observatory of Japan (NAOJ) Research Grant for Universities; HPCI Strategic Program Field 5 "The Origin of Matter and the Universe"; JSPS [20040003, 20041003, 21018003, 21018005, 21684006, 22253002]; Optical & Near-Infrared Astronomy Inter-University Cooperation Program FX The authors acknowledge H. Bushouse for kindly providing the H alpha image, and S. Onodera for kindly providing the M33 data set for deriving the dispersion in the SK law. J.U. was supported by the Sasakawa Scientific Research Grant from The Japan Science Society. Operation of ANIR on the miniTAO 1 m telescope is supported by the Ministry of Education, Culture, Sports, Science and Technology of Japan, Grant-in-Aid for Scientific Research (20040003, 20041003, 21018003, 21018005, 21684006, and 22253002) from the JSPS, Research Grant for Universities, and Optical & Near-Infrared Astronomy Inter-University Cooperation Program. Part of this work has been supported by National Astronomical Observatory of Japan (NAOJ) Research Grant for Universities. This work is supported by HPCI Strategic Program Field 5 "The Origin of Matter and the Universe." NR 51 TC 5 Z9 5 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 138 DI 10.1088/0004-637X/757/2/138 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500031 ER PT J AU Park, HS Lee, MG Hwang, HS AF Park, Hong Soo Lee, Myung Gyoon Hwang, Ho Seong TI SUBARU SPECTROSCOPY OF THE GLOBULAR CLUSTERS IN THE VIRGO GIANT ELLIPTICAL GALAXY M86 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: abundances; galaxies: elliptical and lenticular, cD; galaxies: individual (M86, NGC 4406); galaxies: kinematics and dynamics; galaxies: star clusters: general ID STELLAR POPULATION-MODELS; CCD SURFACE PHOTOMETRY; WIDE-FIELD SURVEY; M60 NGC 4649; DARK-MATTER; OBJECT CAMERA; LINE INDEXES; M49 NGC-4472; LARGE-SAMPLE; SYSTEM AB We present the first spectroscopic study of the globular clusters (GCs) in the giant elliptical galaxy (gE) M86 in the Virgo Cluster. Using spectra obtained in the Multi-Object Spectroscopy mode of the Faint Object Camera and Spectrograph on the Subaru telescope, we measure the radial velocities for 25 GCs in M86. The mean velocity of the GCs is derived to be (nu(p)) over bar = -354(-79)(+81) km s(-1), which is different from the velocity of the M86 nucleus (nu(gal) = -234 +/- 41 km s(-1)). We estimate the velocity dispersion of the GCs, sigma(p) = 292(-32)(+32) km s(-1), and find a hint of rotation in the M86 GC system. A comparison of the observed velocity dispersion profiles of the GCs and stars with a prediction based on the stellar mass profile strongly suggests the existence of an extended dark matter halo in M86. We also estimate the metallicities and ages for 16 and 8 GCs, respectively. The metallicities of M86 GCs are in the range of -2.0 < [Fe/H] < -0.2 with a mean value of -1.13 +/- 0.47. These GCs show a wide age distribution from 4 to 15 Gyr. C1 [Park, Hong Soo; Lee, Myung Gyoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Park, HS (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. EM hspark@astro.snu.ac.kr; mglee@astro.snu.ac.kr; hhwang@cfa.harvard.edu FU NRF; MEST [2010-0013875]; Smithsonian Institution FX The authors thank the anonymous referee for his/her useful comments that improved the original manuscript. The authors are grateful to the staff of the Subaru telescope for their kind help during the observation and to our collaborator Nobuo Arimoto. This work is supported in part by Mid-career Researcher Program through an NRF grant funded by MEST (No. 2010-0013875). H. S. H. acknowledges the support of the Smithsonian Institution. NR 79 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 184 DI 10.1088/0004-637X/757/2/184 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500077 ER PT J AU Rosenfeld, KA Qi, CH Andrews, SM Wilner, DJ Corder, SA Dullemond, CP Lin, SY Hughes, AM D'Alessio, P Ho, PTP AF Rosenfeld, Katherine A. Qi, Chunhua Andrews, Sean M. Wilner, David J. Corder, Stuartt A. Dullemond, C. P. Lin, Shin-Yi Hughes, A. M. D'Alessio, Paola Ho, P. T. P. TI KINEMATICS OF THE CO GAS IN THE INNER REGIONS OF THE TW Hya DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (TW Hya) ID CIRCUMSTELLAR DISK; PROTOPLANETARY DISK; BETA-PICTORIS; GM AURIGAE; ACCRETION DISKS; TAURI STARS; AB-AURIGAE; SUBMILLIMETER ARRAY; TRANSITIONAL DISKS; INCLINED PLANETS AB We present a detailed analysis of the spatially and spectrally resolved (CO)-C-12 J=2-1 and J=3-2 emission lines from the TW Hya circumstellar disk, based on science verification data from the Atacama Large Millimeter/submillimeter Array (ALMA). These lines exhibit substantial emission in their high-velocity wings (with projected velocities out to 2.1 km s(-1), corresponding to intrinsic orbital velocities >20 km s(-1)) that trace molecular gas as close as 2 AU from the central star. However, we are not able to reproduce the intensity of these wings and the general spatio-kinematic pattern of the lines with simple models for the disk structure and kinematics. Using three-dimensional non-local thermodynamic equilibrium molecular excitation and radiative transfer calculations, we construct some alternative models that successfully account for these features by modifying either (1) the temperature structure of the inner disk (inside the dust-depleted disk cavity; r < 4 AU), (2) the intrinsic (Keplerian) disk velocity field, or (3) the distribution of disk inclination angles (a warp). The latter approach is particularly compelling because a representative warped disk model qualitatively reproduces the observed azimuthal modulation of optical light scattered off the disk surface. In any model scenario, the ALMA data clearly require a substantial molecular gas reservoir located inside the region where dust optical depths are known to be substantially diminished in the TW Hya disk, in agreement with previous studies based on infrared spectroscopy. The results from these updated model prescriptions are discussed in terms of their potential physical origins, which might include dynamical perturbations from a low-mass companion with an orbital separation of a few AU. C1 [Rosenfeld, Katherine A.; Qi, Chunhua; Andrews, Sean M.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Corder, Stuartt A.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Dullemond, C. P.] Heidelberg Univ, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Lin, Shin-Yi] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Hughes, A. M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [D'Alessio, Paola] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Rosenfeld, KA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Dullemond, Cornelis/0000-0002-7078-5910 FU Miller Institute for Basic Research in Science FX We are grateful to Rebekah Dawson, Diego Munoz, Christian Brinch, and Joanna Brown for their helpful suggestions, as well as the ALMA commissioning and science verification team for kindly providing detailed instructions that guided the calibration of these data. A. M. H. is supported by a fellowship from the Miller Institute for Basic Research in Science. The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America, and East Asia in cooperation with the Republic of Chile. This article makes use of the following ALMA Science Verification data: ADS/JAO.ALMA#2011.0.00001.SV. NR 76 TC 34 Z9 34 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 129 DI 10.1088/0004-637X/757/2/129 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500022 ER PT J AU Sazonov, S Willner, SP Goulding, AD Hickox, RC Gorjian, V Werner, MW Churazov, E Krivonos, R Revnivtsev, M Sunyaev, R Jones, C Murray, SS Vikhlinin, A Fabian, AC Forman, WR AF Sazonov, S. Willner, S. P. Goulding, A. D. Hickox, R. C. Gorjian, V. Werner, M. W. Churazov, E. Krivonos, R. Revnivtsev, M. Sunyaev, R. Jones, C. Murray, S. S. Vikhlinin, A. Fabian, A. C. Forman, W. R. TI CONTRIBUTION OF THE ACCRETION DISK, HOT CORONA, AND OBSCURING TORUS TO THE LUMINOSITY OF SEYFERT GALAXIES: INTEGRAL AND SPITZER OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; galaxies: Seyfert; infrared: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; X-RAY-EMISSION; ALL-SKY SURVEY; POLYCYCLIC AROMATIC-HYDROCARBONS; SWIFT-BAT SURVEY; SIMILAR-TO 0.1; SPACE-TELESCOPE; NEARBY GALAXIES AB We estimate the relative contributions of the supermassive black hole (SMBH) accretion disk, corona, and obscuring torus to the bolometric luminosity of Seyfert galaxies, using Spitzer mid-infrared (MIR) observations of a complete sample of 68 nearby active galactic nuclei (AGNs) from the INTEGRAL all-sky hard X-ray (HX) survey. This is the first HX-selected (above 15 keV) sample of AGNs with complementary high angular resolution, high signal-to-noise, MIR data. Correcting for the host galaxy contribution, we find a correlation between HX and MIR luminosities: L-15 mu m alpha L-HX(0.74 +/- 0.06). Assuming that the observed MIR emission is radiation from an accretion disk reprocessed in a surrounding dusty torus that subtends a solid angle decreasing with increasing luminosity (as inferred from the declining fraction of obscured AGNs), the intrinsic disk luminosity, L-Disk, is approximately proportional to the luminosity of the corona in the 2-300 keV energy band, L-Corona, with the L-Disk/L-Corona ratio varying by a factor of 2.1 around a mean value of 1.6. This ratio is a factor of similar to 2 smaller than for typical quasars producing the cosmic X-ray background. Therefore, over three orders of magnitude in luminosity, HX radiation carries a large, and roughly comparable, fraction of the bolometric output of AGNs. We estimate the cumulative bolometric luminosity density of local AGNs at similar to(1-3) x 10(40) erg s(-1) Mpc(-3). Finally, the Compton temperature ranges between kT(c) approximate to 2 and approximate to 6 keV for nearby AGNs, compared to kT(c) approximate to 2 keV for typical quasars, confirming that radiative heating of interstellar gas can play an important role in regulating SMBH growth. C1 [Sazonov, S.; Churazov, E.; Krivonos, R.; Revnivtsev, M.; Sunyaev, R.; Vikhlinin, A.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Sazonov, S.; Churazov, E.; Krivonos, R.; Sunyaev, R.; Forman, W. R.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Willner, S. P.; Goulding, A. D.; Jones, C.; Murray, S. S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Gorjian, V.; Werner, M. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Sazonov, S (reprint author), Russian Acad Sci, Space Res Inst, Profsoyuznaya 84-32, Moscow 117997, Russia. RI Churazov, Eugene/A-7783-2013 FU Russian Academy of Sciences [P-21, OFN-16]; Scientific and educational personnel of the innovative Russia [2012-1.2.2-12-000-1012-023]; Dynasty Foundation; NASA; [RFBR 09-02-00867]; [RFBR 11-02-12271-ofi-m]; [NSh-5603.2012.2] FX We thank the referee for helpful comments. This work is based on observations made with the Spitzer Space Telescope, operated by the Jet Propulsion Laboratory at Caltech under a contract with NASA, and with INTEGRAL, an ESA project funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Spain, and Switzerland), Czech Republic and Poland, and with the participation of Russia and the USA. The research made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. The research made use of grants RFBR 09-02-00867, RFBR 11-02-12271-ofi-m, and NSh-5603.2012.2, programs of the Russian Academy of Sciences P-21 and OFN-16, and the program "Scientific and educational personnel of the innovative Russia 2009-2013" (2012-1.2.2-12-000-1012-023). S.S. acknowledges the support of the Dynasty Foundation. NR 129 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 181 DI 10.1088/0004-637X/757/2/181 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500074 ER PT J AU Shen, Y AF Shen, Yue TI ASTROMETRIC REVERBERATION MAPPING SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; quasars: general ID ACTIVE GALACTIC NUCLEI; BROAD-LINE REGION; IONIZING CONTINUUM VARIATIONS; HIGH-PRECISION ASTROMETRY; BLACK-HOLE; ACCRETION DISK; EMISSION-LINES; ARP 151; QUASARS; MASS AB Spatially extended emission regions of active galactic nuclei respond to continuum variations, if such emission regions are powered by energy reprocessing of the continuum. The response from different parts of the reverberating region arrives at different times lagging behind the continuum variation. The lags can be used to map the geometry and kinematics of the emission region (i.e., reverberation mapping, RM). If the extended emission region is not spherically symmetric in configuration and velocity space, reverberation may produce astrometric offsets in the emission region photocenter as a function of time delay and velocity, detectable with future mu as to tens of mu as astrometry. Such astrometric responses provide independent constraints on the geometric and kinematic structure of the extended emission region, complementary to traditional RM. In addition, astrometric RM is more sensitive to infer the inclination of a flattened geometry and the rotation angle of the extended emission region. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shen, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM yshen@cfa.harvard.edu FU Smithsonian Astrophysical Observatory through a Clay Postdoctoral Fellowship FX It is a pleasure to thank the anonymous referee for suggestions that led to improvement of the paper, and Brad Peterson, Chris Kochanek, and Luis Ho for useful comments on the draft. Special thanks to Shu Jia for a stimulating discussion that inspired this study. I gratefully acknowledge support from the Smithsonian Astrophysical Observatory through a Clay Postdoctoral Fellowship. NR 44 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 OCT 1 PY 2012 VL 757 IS 2 AR 152 DI 10.1088/0004-637X/757/2/152 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500045 ER PT J AU Simionescu, A Werner, N Urban, O Allen, SW Fabian, AC Sanders, JS Mantz, A Nulsen, PEJ Takei, Y AF Simionescu, A. Werner, N. Urban, O. Allen, S. W. Fabian, A. C. Sanders, J. S. Mantz, A. Nulsen, P. E. J. Takei, Y. TI LARGE-SCALE MOTIONS IN THE PERSEUS GALAXY CLUSTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE X-rays: galaxies: clusters; X-rays: individual (Perseus Cluster) ID XMM-NEWTON OBSERVATIONS; INTRACLUSTER MEDIUM; COLD FRONTS; COOL-CORE; GAS; ENTROPY; TEMPERATURE; EDGE AB By combining large-scale mosaics of ROSAT PSPC, XMM-Newton, and Suzaku X-ray observations, we present evidence for large-scale motions in the intracluster medium of the nearby, X-ray bright Perseus Cluster. These motions are suggested by several alternating and interleaved X-ray bright, low-temperature, low-entropy arcs located along the east-west axis, at radii ranging from similar to 10 kpc to over a Mpc. Thermodynamic features qualitatively similar to these have previously been observed in the centers of cool-core clusters, and were successfully modeled as a consequence of the gas sloshing/swirling motions induced by minor mergers. Our observations indicate that such sloshing/swirling can extend out to larger radii than previously thought, on scales approaching the virial radius. C1 [Simionescu, A.; Werner, N.; Urban, O.; Allen, S. W.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Simionescu, A.; Werner, N.; Urban, O.; Allen, S. W.] Stanford Univ, Dept Phys, Stanford, CA 94305 USA. [Allen, S. W.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Mantz, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Mantz, A.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Takei, Y.] JAXA, ISAS, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. RP Simionescu, A (reprint author), Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA. RI XRAY, SUZAKU/A-1808-2009; OI Sanders, Jeremy/0000-0003-2189-4501; Nulsen, Paul/0000-0003-0297-4493 FU NASA [PF9-00070, NAS8-03060]; Chandra X-ray Center; NSF [AST-0838187]; U.S. Department of Energy [DE-AC02-76SF00515]; ESA member states; USA (NASA); [NNX12AB64G]; [NNX10AR48G]; [NNX09AV64G] FX The authors thank M. Bruggen and S. Heinz for helpful discussion. Support for this work was 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 further acknowledge support from awards NNX12AB64G, NNX10AR48G, NNX09AV64G, and NSF AST-0838187. The work was supported in part by the U.S. Department of Energy under contract number DE-AC02-76SF00515. This research 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). The authors thank the Suzaku operation team and Guest Observer Facility, supported by JAXA and NASA. NR 35 TC 28 Z9 28 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 182 DI 10.1088/0004-637X/757/2/182 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500075 ER PT J AU Su, YN van Ballegooijen, A AF Su, Yingna van Ballegooijen, Adriaan TI OBSERVATIONS AND MAGNETIC FIELD MODELING OF A SOLAR POLAR CROWN PROMINENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: evolution; Sun: filaments, prominences; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID ACTIVE-REGION 10953; RAY TELESCOPE XRT; TWISTED FLUX-TUBE; QUIESCENT PROMINENCE; FILAMENT CHANNELS; VERTICAL THREADS; FINE-STRUCTURE; HINODE; DYNAMICS; SUN AB We present observations and magnetic field modeling of the large polar crown prominence that erupted on 2010 December 6. Combination of Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) and STEREO_Behind/EUVI allows us to see the fine structures of this prominence both at the limb and on the disk. We focus on the structures and dynamics of this prominence before the eruption. This prominence contains two parts: an active region part containing mainly horizontal threads and a quiet-Sun part containing mainly vertical threads. On the northern side of the prominence channel, both AIA and EUVI observe bright features which appear to be the lower legs of loops that go above then join in the filament. Filament materials are observed to frequently eject horizontally from the active region part to the quiet-Sun part. This ejection results in the formation of a dense-column structure (concentration of dark vertical threads) near the border between the active region and the quiet Sun. Using the flux rope insertion method, we create nonlinear force-free field models based on SDO/Helioseismic and Magnetic Imager line-of-sight magnetograms. A key feature of these models is that the flux rope has connections with the surroundings photosphere, so its axial flux varies along the filament path. The height and location of the dips of field lines in our models roughly replicate those of the observed prominence. Comparison between model and observations suggests that the bright features on the northern side of the channel are the lower legs of the field lines that turn into the flux rope. We suggest that plasma may be injected into the prominence along these field lines. Although the models fit the observations quiet well, there are also some interesting differences. For example, the models do not reproduce the observed vertical threads and cannot explain the formation of the dense-column structure. C1 [Su, Yingna; van Ballegooijen, Adriaan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 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; OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU NASA [NNM07AB07C]; LMSAL [SP02H1701R]; NASA grant [NNX12AI30G] FX We thank the anonymous referee for valuable comments to improve this paper. 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 team of SDO/AIA, SDO/HMI, STEREO/EUVI, Hinode/XRT, KSO, and SOLIS for providing the valuable data. The EUVI and HMI data are downloaded via the Virtual Solar Observatory and the Joint Science Operations Center. Y. Su acknowledges Dr. Mark Weber for helpful discussions and thanks Dr. Suli Ma for helping on the radial filter technique. This project is partially supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO, as well as NASA grant NNX12AI30G. NR 74 TC 27 Z9 27 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 168 DI 10.1088/0004-637X/757/2/168 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500061 ER PT J AU Torres, G Fischer, DA Sozzetti, A Buchhave, LA Winn, JN Holman, MJ Carter, JA AF Torres, Guillermo Fischer, Debra A. Sozzetti, Alessandro Buchhave, Lars A. Winn, Joshua N. Holman, Matthew J. Carter, Joshua A. TI IMPROVED SPECTROSCOPIC PARAMETERS FOR TRANSITING PLANET HOSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: abundances; stars: fundamental parameters; techniques: spectroscopic ID LOW-DENSITY PLANET; BRIGHT F-STAR; HOT-JUPITER; LIGHT-CURVE; EXTRASOLAR PLANET; ECCENTRIC ORBIT; K STAR; THERMAL EMISSION; KEPLER FIELD; METAL-POOR AB We report homogeneous spectroscopic determinations of the effective temperature, metallicity, and projected rotational velocity for the host stars of 56 transiting planets. Our analysis is based primarily on the stellar parameter classification (SPC) technique. We investigate systematic errors by examining subsets of the data with two other methods that have often been used in previous studies (Spectroscopy Made Easy (SME) and MOOG). The SPC and SME results, both based on comparisons between synthetic spectra and actual spectra, show strong correlations between T-eff, [Fe/H], and log g when solving for all three quantities simultaneously. In contrast the MOOG results, based on a more traditional curve-of-growth approach, show no such correlations. To combat the correlations and improve the accuracy of the temperatures and metallicities, we repeat the SPC analysis with a constraint on log g based on the mean stellar density that can be derived from the analysis of the transit light curves. Previous studies that have not taken advantage of this constraint have been subject to systematic errors in the stellar masses and radii of up to 20% and 10%, respectively, which can be larger than other observational uncertainties, and which also cause systematic errors in the planetary mass and radius. C1 [Torres, Guillermo; Holman, Matthew J.; Carter, Joshua A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Sozzetti, Alessandro] INAF Osservatorio Astron Torino, I-10025 Pino Torinese, Italy. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu RI Carter, Joshua/A-8280-2013; OI Fischer, Debra/0000-0003-2221-0861; Sozzetti, Alessandro/0000-0002-7504-365X; Carter, Joshua/0000-0001-8152-2561; Buchhave, Lars A./0000-0003-1605-5666 FU NASA [NNX09AF59G]; NSF [AST-10-07992] FX We are grateful to Jeff Valenti for helpful discussions, and to P. Berlind, M. Calkins, G. Esquerdo, D. W. Latham, and R. P. Stefanik for their help in obtaining the TRES spectra used here. We also thank the anonymous referee for helpful comments. G.T. acknowledges partial support for this work from NASA's Origins of Solar Systems program, through grant NNX09AF59G, and from NSF grant AST-10-07992. The research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Abstract Service. NR 88 TC 134 Z9 134 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD OCT 1 PY 2012 VL 757 IS 2 AR 161 DI 10.1088/0004-637X/757/2/161 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 010QF UT WOS:000309108500054 ER PT J AU Wickramasinghe, NC Wallis, J Wallis, DH Schild, RE Gibson, CH AF Wickramasinghe, N. Chandra Wallis, Jamie Wallis, Daryl H. Schild, Rudolph E. Gibson, Carl H. TI Life-bearing primordial planets in the solar vicinity SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Primordial planets; Panspermia; HGD cosmology; Solid hydrogen; Comets; Star formation ID SOLID HYDROGEN; BACTERIA; CLUSTERS AB The space density of life-bearing primordial planets in the solar vicinity may amount to similar to 8.1x10(4) pc(-3) giving total of similar to 10(14) throughout the entire galactic disk. Initially dominated by H-2 these planets are stripped of their hydrogen mantles when the ambient radiation temperature exceeds 3 K as they fall from the galactic halo to the mid-plane of the galaxy. The zodiacal cloud in our solar system encounters a primordial planet once every 26 My (on our estimate) thus intercepting an average mass of 10(3) tonnes of interplanetary dust on each occasion. If the dust included microbial material that originated on Earth and was scattered via impacts or cometary sublimation into the zodiacal cloud, this process offers a way by which evolved genes from Earth life could become dispersed through the galaxy. C1 [Wickramasinghe, N. Chandra; Wallis, Daryl H.; Gibson, Carl H.] Univ Buckingham, Buckingham Ctr Astrobiol, Buckingham MK18 1EG, England. [Wallis, Jamie] Cardiff Univ, Sch Math, Cardiff, S Glam, Wales. [Schild, Rudolph E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gibson, Carl H.] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Wickramasinghe, NC (reprint author), Univ Buckingham, Buckingham Ctr Astrobiol, Buckingham MK18 1EG, England. EM ncwick@gmail.com NR 27 TC 1 Z9 1 U1 0 U2 13 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X EI 1572-946X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD OCT PY 2012 VL 341 IS 2 BP 295 EP 299 DI 10.1007/s10509-012-1092-8 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 008MI UT WOS:000308960700010 ER PT J AU Yasuhara, M Hunt, G Dowsett, HJ Robinson, MM Stoll, DK AF Yasuhara, Moriaki Hunt, Gene Dowsett, Harry J. Robinson, Marci M. Stoll, Danielle K. TI Latitudinal species diversity gradient of marine zooplankton for the last three million years SO ECOLOGY LETTERS LA English DT Article DE Biodiversity; climate changes; fossil records; latitudinal species diversity gradients; macroecology; North Atlantic; pelagic ecosystem; planktic foraminifera; temperature ID FORAMINIFER TRANSFER-FUNCTION; NORTH-ATLANTIC; TAXONOMIC DIVERSITY; MOUNTAIN PASSES; TEMPERATURE; BIODIVERSITY; PATTERNS; TROPICS; SCALE; OCEAN AB High tropical and low polar biodiversity is one of the most fundamental patterns characterising marine ecosystems, and the influence of temperature on such marine latitudinal diversity gradients is increasingly well documented. However, the temporal stability of quantitative relationships among diversity, latitude and temperature is largely unknown. Herein we document marine zooplankton species diversity patterns at four time slices [modern, Last Glacial Maximum (18 000 years ago), last interglacial (120 000 years ago), and Pliocene ( 3.33.0 million years ago)] and show that, although the diversity-latitude relationship has been dynamic, diversity-temperature relationships are remarkably constant over the past three million years. These results suggest that species diversity is rapidly reorganised as species' ranges respond to temperature change on ecological time scales, and that the ecological impact of future human-induced temperature change may be partly predictable from fossil and paleoclimatological records. C1 [Yasuhara, Moriaki] Univ Hong Kong, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki] Univ Hong Kong, Swire Inst Marine Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki] Kochi Univ, Ctr Adv Marine Core Res, Nankoku, Kochi 7838502, Japan. [Yasuhara, Moriaki; Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Dowsett, Harry J.; Robinson, Marci M.; Stoll, Danielle K.] US Geol Survey, Eastern Geol & Paleoclimate Sci Ctr, Reston, VA 20192 USA. RP Yasuhara, M (reprint author), Univ Hong Kong, Sch Biol Sci, Pok Fu Lam Rd, Hong Kong, Hong Kong, Peoples R China. EM moriakiyasuhara@gmail.com RI Yasuhara, Moriaki/A-4986-2008; Hunt, Gene/B-3783-2010; OI Yasuhara, Moriaki/0000-0001-8501-4863; Hunt, Gene/0000-0001-6430-5020; Dowsett, Harry/0000-0003-1983-7524 NR 50 TC 30 Z9 31 U1 1 U2 57 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD OCT PY 2012 VL 15 IS 10 BP 1174 EP 1179 DI 10.1111/j.1461-0248.2012.01828.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 000QN UT WOS:000308402300012 PM 22738438 ER PT J AU Feroci, M Stella, L van der Klis, M Courvoisier, TJL Hernanz, M Hudec, R Santangelo, A Walton, D Zdziarski, A Barret, D Belloni, T Braga, J Brandt, S Budtz-Jorgensen, C Campana, S den Herder, JW Huovelin, J Israel, GL Pohl, M Ray, P Vacchi, A Zane, S Argan, A Attina, P Bertuccio, G Bozzo, E Campana, R Chakrabarty, D Costa, E De Rosa, A Del Monte, E Di Cosimo, S Donnarumma, I Evangelista, Y Haas, D Jonker, P Korpela, S Labanti, C Malcovati, P Mignani, R Muleri, F Rapisarda, M Rashevsky, A Rea, N Rubini, A Tenzer, C Wilson-Hodge, C Winter, B Wood, K Zampa, G Zampa, N Abramowicz, MA Alpar, MA Altamirano, D Alvarez, JM Amati, L Amoros, C Antonelli, LA Artigue, R Azzarello, P Bachetti, M Baldazzi, G Barbera, M Barbieri, C Basa, S Baykal, A Belmont, R Boirin, L Bonvicini, V Burderi, L Bursa, M Cabanac, C Cackett, E Caliandro, GA Casella, P Chaty, S Chenevez, J Coe, MJ Collura, A Corongiu, A Covino, S Cusumano, G D'Amico, F Dall'Osso, S De Martino, D De Paris, G Di Persio, G Di Salvo, T Done, C Dovciak, M Drago, A Ertan, U Fabiani, S Falanga, M Fender, R Ferrando, P Ferreira, DD Fraser, G Frontera, F Fuschino, F Galvez, JL Gandhi, P Giommi, P Godet, O Gogus, E Goldwurm, A Gotz, D Grassi, M Guttridge, P Hakala, P Henri, G Hermsen, W Horak, J Hornstrup, A in't Zand, JJM Isern, J Kalemci, E Kanbach, G Karas, V Kataria, D Kennedy, T Klochkov, D Kluzniak, W Kokkotas, K Kreykenbohm, I Krolik, J Kuiper, L Kuvvetli, I Kylafis, N Lattimer, JM Lazzarotto, F Leahy, D Lebrun, F Lin, D Lund, N Maccarone, T Malzac, J Marisaldi, M Martindale, A Mastropietro, M McClintock, J McHardy, I Mendez, M Mereghetti, S Miller, MC Mineo, T Morelli, E Morsink, S Motch, C Motta, S Munoz-Darias, T Naletto, G Neustroev, V Nevalainen, J Olive, JF Orio, M Orlandini, M Orleanski, P Ozel, F Pacciani, L Paltani, S Papadakis, I Papitto, A Patruno, A Pellizzoni, A Petracek, V Petri, J Petrucci, PO Phlips, B Picolli, L Possenti, A Psaltis, D Rambaud, D Reig, P Remillard, R Rodriguez, J Romano, P Romanova, M Schanz, T Schmid, C Segreto, A Shearer, A Smith, A Smith, PJ Soffitta, P Stergioulas, N Stolarski, M Stuchlik, Z Tiengo, A Torres, D Torok, G Turolla, R Uttley, P Vaughan, S Vercellone, S Waters, R Watts, A Wawrzaszek, R Webb, N Wilms, J Zampieri, L Zezas, A Ziolkowski, J AF Feroci, M. Stella, L. van der Klis, M. Courvoisier, T. J. -L. Hernanz, M. Hudec, R. Santangelo, A. Walton, D. Zdziarski, A. Barret, D. Belloni, T. Braga, J. Brandt, S. Budtz-Jorgensen, C. Campana, S. den Herder, J. -W. Huovelin, J. Israel, G. L. Pohl, M. Ray, P. Vacchi, A. Zane, S. Argan, A. Attina, P. Bertuccio, G. Bozzo, E. Campana, R. Chakrabarty, D. Costa, E. De Rosa, A. Del Monte, E. Di Cosimo, S. Donnarumma, I. Evangelista, Y. Haas, D. Jonker, P. Korpela, S. Labanti, C. Malcovati, P. Mignani, R. Muleri, F. Rapisarda, M. Rashevsky, A. Rea, N. Rubini, A. Tenzer, C. Wilson-Hodge, C. Winter, B. Wood, K. Zampa, G. Zampa, N. Abramowicz, M. A. Alpar, M. A. Altamirano, D. Alvarez, J. M. Amati, L. Amoros, C. Antonelli, L. A. Artigue, R. Azzarello, P. Bachetti, M. Baldazzi, G. Barbera, M. Barbieri, C. Basa, S. Baykal, A. Belmont, R. Boirin, L. Bonvicini, V. Burderi, L. Bursa, M. Cabanac, C. Cackett, E. Caliandro, G. A. Casella, P. Chaty, S. Chenevez, J. Coe, M. J. Collura, A. Corongiu, A. Covino, S. Cusumano, G. D'Amico, F. Dall'Osso, S. De Martino, D. De Paris, G. Di Persio, G. Di Salvo, T. Done, C. Dovciak, M. Drago, A. Ertan, U. Fabiani, S. Falanga, M. Fender, R. Ferrando, P. Ferreira, D. Della Monica Fraser, G. Frontera, F. Fuschino, F. Galvez, J. L. Gandhi, P. Giommi, P. Godet, O. Gogus, E. Goldwurm, A. Goetz, D. Grassi, M. Guttridge, P. Hakala, P. Henri, G. Hermsen, W. Horak, J. Hornstrup, A. in't Zand, J. J. M. Isern, J. Kalemci, E. Kanbach, G. Karas, V. Kataria, D. Kennedy, T. Klochkov, D. Kluzniak, W. Kokkotas, K. Kreykenbohm, I. Krolik, J. Kuiper, L. Kuvvetli, I. Kylafis, N. Lattimer, J. M. Lazzarotto, F. Leahy, D. Lebrun, F. Lin, D. Lund, N. Maccarone, T. Malzac, J. Marisaldi, M. Martindale, A. Mastropietro, M. McClintock, J. McHardy, I. Mendez, M. Mereghetti, S. Miller, M. C. Mineo, T. Morelli, E. Morsink, S. Motch, C. Motta, S. Munoz-Darias, T. Naletto, G. Neustroev, V. Nevalainen, J. Olive, J. F. Orio, M. Orlandini, M. Orleanski, P. Ozel, F. Pacciani, L. Paltani, S. Papadakis, I. Papitto, A. Patruno, A. Pellizzoni, A. Petracek, V. Petri, J. Petrucci, P. O. Phlips, B. Picolli, L. Possenti, A. Psaltis, D. Rambaud, D. Reig, P. Remillard, R. Rodriguez, J. Romano, P. Romanova, M. Schanz, T. Schmid, C. Segreto, A. Shearer, A. Smith, A. Smith, P. J. Soffitta, P. Stergioulas, N. Stolarski, M. Stuchlik, Z. Tiengo, A. Torres, D. Toeroek, G. Turolla, R. Uttley, P. Vaughan, S. Vercellone, S. Waters, R. Watts, A. Wawrzaszek, R. Webb, N. Wilms, J. Zampieri, L. Zezas, A. Ziolkowski, J. TI The Large Observatory for X-ray Timing (LOFT) SO EXPERIMENTAL ASTRONOMY LA English DT Article DE Missions; X-ray timing; compact objects; black holes; neutron stars ID SILICON DRIFT DETECTOR; BLACK-HOLE; PROPORTIONAL COUNTER; OSCILLATIONS; ALICE; CONSTRAINTS; SUPERAGILE; DISCOVERY; BINARIES; EQUATION AB High-time-resolution X-ray observations of compact objects provide direct access to strong-field gravity, to the equation of state of ultradense matter and to black hole masses and spins. A 10 m(2)-class instrument in combination with good spectral resolution is required to exploit the relevant diagnostics and answer two of the fundamental questions of the European Space Agency (ESA) Cosmic Vision Theme "Matter under extreme conditions", namely: does matter orbiting close to the event horizon follow the predictions of general relativity? What is the equation of state of matter in neutron stars? The Large Observatory For X-ray Timing (LOFT), selected by ESA as one of the four Cosmic Vision M3 candidate missions to undergo an assessment phase, will revolutionise the study of collapsed objects in our galaxy and of the brightest supermassive black holes in active galactic nuclei. Thanks to an innovative design and the development of large-area monolithic silicon drift detectors, the Large Area Detector (LAD) on board LOFT will achieve an effective area of similar to 12 m(2) (more than an order of magnitude larger than any spaceborne predecessor) in the 2-30 keV range (up to 50 keV in expanded mode), yet still fits a conventional platform and small/medium-class launcher. With this large area and a spectral resolution of < 260 eV, LOFT will yield unprecedented information on strongly curved spacetimes and matter under extreme conditions of pressure and magnetic field strength. C1 [Feroci, M.; Campana, R.; Costa, E.; De Rosa, A.; Del Monte, E.; Di Cosimo, S.; Donnarumma, I.; Evangelista, Y.; Muleri, F.; Rapisarda, M.; Rubini, A.; Di Persio, G.; Fabiani, S.; Lazzarotto, F.; Mastropietro, M.; Morelli, E.; Pacciani, L.; Soffitta, P.] INAF IASF Roma, I-00133 Rome, Italy. [Feroci, M.; Campana, R.; Del Monte, E.; Rapisarda, M.; Rubini, A.; Pacciani, L.] INFN Roma Tor Vergata, Rome, Italy. [Stella, L.; Israel, G. L.; Antonelli, L. A.] INAF OAR, I-00040 Monte Porzio Catone, Italy. [van der Klis, M.; Altamirano, D.; Patruno, A.; Watts, A.] Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. [Courvoisier, T. J. -L.; Bozzo, E.; Azzarello, P.; Paltani, S.] Univ Geneva, ISDC, Geneva, Switzerland. [Hernanz, M.; Rea, N.; Altamirano, D.; Alvarez, J. M.; Caliandro, G. A.; Galvez, J. L.; Isern, J.; Torres, D.] IEEC CSIC, Barcelona, Spain. [Hudec, R.; Petracek, V.] Czech Tech Univ, CR-16635 Prague, Czech Republic. [Santangelo, A.; Tenzer, C.; Klochkov, D.; Kokkotas, K.; Schanz, T.] Univ Tubingen, Tubingen, Germany. [Walton, D.; Zane, S.; Mignani, R.; Winter, B.; Guttridge, P.; Kataria, D.; Kennedy, T.; Smith, A.; Smith, P. J.] MSSL UCL, Surrey, England. [Zdziarski, A.; Kluzniak, W.; Ziolkowski, J.] Nicholas Copernicus Astron Ctr, Warsaw, Poland. [Barret, D.; Amoros, C.; Artigue, R.; Bachetti, M.; Belmont, R.; Cabanac, C.; Godet, O.; Lin, D.; Malzac, J.; Olive, J. F.; Rambaud, D.; Webb, N.] IRAP, Toulouse, France. [Belloni, T.; Campana, S.; Covino, S.; Motta, S.; Munoz-Darias, T.] INAF OA Brera, Milan, Italy. [Braga, J.; D'Amico, F.] INPE, Sao Jose Dos Campos, Brazil. [Brandt, S.; Budtz-Jorgensen, C.; Chenevez, J.; Ferreira, D. Della Monica; Hornstrup, A.; Kuvvetli, I.; Lund, N.] DTU Space, Copenhagen, Denmark. [den Herder, J. -W.; Haas, D.; Jonker, P.; Hermsen, W.; in't Zand, J. J. M.; Kuiper, L.; Waters, R.] SRON, Utrecht, Netherlands. [Huovelin, J.; Korpela, S.; Nevalainen, J.] Univ Helsinki, Helsinki, Finland. [Pohl, M.] Univ Geneva, DPNC, CH-1211 Geneva, Switzerland. [Ray, P.; Wood, K.; Phlips, B.] NRL, Washington, DC USA. [Vacchi, A.; Rashevsky, A.; Zampa, G.; Zampa, N.; Bonvicini, V.] Ist Nazl Fis Nucl, Trieste, Italy. [Argan, A.; De Paris, G.] INAF Headquarters, Rome, Italy. [Attina, P.] Thales Alenia, Turin, Italy. [Bertuccio, G.] Politecn Milan, I-20133 Milan, Italy. [Chakrabarty, D.; Remillard, R.] MIT, Cambridge, MA 02139 USA. [Labanti, C.; Amati, L.; Fuschino, F.; Marisaldi, M.; Orlandini, M.] INAF IASF Bologna, Bologna, Italy. [Malcovati, P.; Grassi, M.; Picolli, L.] Univ Pavia, I-27100 Pavia, Italy. [Mignani, R.] Univ Zielona Gora, Inst Astron, Geneva, Poland. [Rapisarda, M.] ENEA Frascati, Rome, Italy. [Wilson-Hodge, C.] NASA MSFC, Huntsville, AL USA. [Abramowicz, M. A.] Gothenburg Univ, Gothenburg, Sweden. [Alpar, M. A.; Ertan, U.; Gogus, E.; Kalemci, E.] Sabanci Univ, Istanbul, Turkey. [Baldazzi, G.] Ist Nazl Fis Nucl, I-40126 Bologna, Italy. [Barbera, M.; Collura, A.; Di Salvo, T.] Univ Palermo, Palermo, Italy. [Barbieri, C.; Naletto, G.; Turolla, R.] Univ Padua, Padua, Italy. [Basa, S.] LAM, Marseille, France. [Baykal, A.] Middle E Tech Univ, TR-06531 Ankara, Turkey. [Boirin, L.; Motch, C.; Petri, J.] Observ Astron, Strasbourg, France. [Burderi, L.] Univ Cagliari, Cagliari, Italy. [Bursa, M.; Dovciak, M.; Horak, J.; Karas, V.] Prague Astron Inst, Prague, Czech Republic. [Cackett, E.] Univ Cambridge, Cambridge, England. [Casella, P.; Coe, M. J.; Fender, R.; Maccarone, T.; McHardy, I.; Uttley, P.] Univ Southampton, Southampton SO9 5NH, Hants, England. [Chaty, S.; Ferrando, P.; Goldwurm, A.; Goetz, D.; Lebrun, F.; Rodriguez, J.] CEA Saclay, Gi Sur Yvette, France. [Corongiu, A.; Papitto, A.; Pellizzoni, A.; Possenti, A.] INAF OA Cagliari, Cagliari, Italy. [Cusumano, G.; Mineo, T.; Romano, P.; Segreto, A.; Vercellone, S.] INAF IASF Palermo, Palermo, Italy. [Dall'Osso, S.] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. [De Martino, D.] INAF OA Capodimonte, Naples, Italy. [Done, C.] Univ Durham, Durham, England. [Drago, A.; Frontera, F.] Univ Ferrara, I-44100 Ferrara, Italy. [Falanga, M.] ISSI Bern, Bern, Switzerland. [Fraser, G.; Martindale, A.; Vaughan, S.] Univ Leicester, Leicester, Leics, England. [Gandhi, P.] SAS JAXA, Kanagawa, Japan. [Giommi, P.] ASI, Rome, Italy. [Hakala, P.; Nevalainen, J.] Finnish Ctr Astron ESO, FINCA, Piikkio, Finland. [Henri, G.; Petrucci, P. O.] Lab Astrophys Grenoble, Grenoble, France. [Kanbach, G.] MPE, Garching, Germany. [Kreykenbohm, I.; Schmid, C.; Wilms, J.] Univ Erlangen Nurnberg, Erlangen, Germany. [Krolik, J.] Johns Hopkins Univ, Baltimore, MD USA. [Kylafis, N.; Paltani, S.; Papadakis, I.; Reig, P.; Zezas, A.] Univ Crete, Iraklion, Greece. [Lattimer, J. M.] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Leahy, D.] Univ Calgary, Calgary, AB, Canada. [McClintock, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mendez, M.] Univ Groningen, Groningen, Netherlands. [Mereghetti, S.; Tiengo, A.] INAF IASF Milano, Milan, Italy. [Miller, M. C.] Univ Maryland, College Pk, MD 20742 USA. [Morsink, S.] Univ Alberta, Edmonton, AB, Canada. [Neustroev, V.] Oulu Univ, Oulu, Finland. [Orio, M.] INAF OA Torino, Turin, Italy. [Orleanski, P.; Stolarski, M.; Wawrzaszek, R.] Polish Acad Sci, Space Res Ctr, PL-01237 Warsaw, Poland. [Ozel, F.; Psaltis, D.] Univ Arizona, Tucson, AZ USA. [Reig, P.] FORTH, Iraklion, Greece. [Romanova, M.] Cornell Univ, Ithaca, NY USA. [Shearer, A.] Galway Univ, Galway, Ireland. [Stergioulas, N.] Aristotle Univ Thessaloniki, GR-54006 Thessaloniki, Greece. [Stuchlik, Z.; Toeroek, G.] Silesian Univ Opava, Opava, Czech Republic. [Torres, D.] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Zampieri, L.] INAF OA Padova, Padua, Italy. RP Feroci, M (reprint author), INAF IASF Roma, Via Fosso del Cavaliere 100, I-00133 Rome, Italy. EM marco.feroci@iasf-roma.inaf.it; luigi.stella@oa-roma.inaf.it RI Drago, Alessandro/F-6347-2012; Lazzarotto, Francesco/J-4670-2012; Baldazzi, Giuseppe/B-4112-2011; Wilms, Joern/C-8116-2013; Kylafis, Nikolaos/C-4555-2011; Schmid, Christian/H-9633-2013; Kreykenbohm, Ingo/H-9659-2013; Tecnologias espaciai, Inct/I-2415-2013; Reig, Pablo/A-1198-2014; Papadakis, Iossif/C-3235-2011; Mendez, Mariano/C-8011-2012; Karas, Vladimir/C-1559-2013; Bursa, Michal/G-9004-2014; Orlandini, Mauro/H-3114-2014; Horak, Jiri/G-9015-2014; Hernanz, Margarita/K-1770-2014; Vacchi, Andrea/C-1291-2010; Dovciak, Michal/F-4258-2014; Shearer, Andy/N-7609-2014; Kokkotas, Kostas/B-7878-2010; Isern, Jordi/B-1844-2015; Campana, Riccardo/F-5272-2015; Neustroev, Vitaly/B-6351-2008; Rea, Nanda/I-2853-2015; Amati, Lorenzo/N-5586-2015; done, chris/D-4605-2016; Ferreira, Desiree/M-1666-2016; Malcovati, Piero/S-2458-2016; Naletto, Giampiero/S-6329-2016; Zezas, Andreas/C-7543-2011; OI Baldazzi, Giuseppe/0000-0002-6657-1645; Wilms, Joern/0000-0003-2065-5410; Kylafis, Nikolaos/0000-0003-0928-0996; Kreykenbohm, Ingo/0000-0001-7335-1803; Reig, Pablo/0000-0002-6446-3050; Mendez, Mariano/0000-0003-2187-2708; Karas, Vladimir/0000-0002-5760-0459; Orlandini, Mauro/0000-0003-0946-3151; Hernanz, Margarita/0000-0002-8651-7910; Vacchi, Andrea/0000-0003-3855-5856; Dovciak, Michal/0000-0003-0079-1239; Shearer, Andy/0000-0001-7903-0074; Kokkotas, Kostas/0000-0001-6048-2919; Isern, Jordi/0000-0002-0819-9574; Campana, Riccardo/0000-0002-4794-5453; Rea, Nanda/0000-0003-2177-6388; Amati, Lorenzo/0000-0001-5355-7388; done, chris/0000-0002-1065-7239; Ferreira, Desiree/0000-0003-4003-3256; Malcovati, Piero/0000-0001-6514-9672; Naletto, Giampiero/0000-0003-2007-3138; Zezas, Andreas/0000-0001-8952-676X; Di Salvo, Tiziana/0000-0002-3220-6375; collura, alfonso/0000-0001-9534-1235; Corongiu, Alessandro/0000-0002-5924-3141; Israel, GianLuca/0000-0001-5480-6438; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Campana, Sergio/0000-0001-6278-1576; Pacciani, Luigi/0000-0001-6897-5996; Segreto, Alberto/0000-0001-7341-6603; giommi, paolo/0000-0002-2265-5003; Mineo, Teresa/0000-0002-4931-8445; Labanti, Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104; Cusumano, Giancarlo/0000-0002-8151-1990; de Martino, Domitilla/0000-0002-5069-4202; De Rosa, Alessandra/0000-0001-5668-6863; Covino, Stefano/0000-0001-9078-5507; Ray, Paul/0000-0002-5297-5278; Casella, Piergiorgio/0000-0002-0752-3301; Huovelin, Juhani/0000-0002-6276-5776; Bachetti, Matteo/0000-0002-4576-9337; Rodriguez, Jerome/0000-0002-4151-4468; Chaty, Sylvain/0000-0002-5769-8601; Tiengo, Andrea/0000-0002-6038-1090; MEREGHETTI, SANDRO/0000-0003-3259-7801; Zampieri, Luca/0000-0002-6516-1329; Vercellone, Stefano/0000-0003-1163-1396; Fuschino, Fabio/0000-0003-2139-3299; Lazzarotto, Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523; Barbera, Marco/0000-0002-3188-7420; Donnarumma, Immacolata/0000-0002-4700-4549; Marisaldi, Martino/0000-0002-4000-3789 NR 32 TC 128 Z9 128 U1 5 U2 69 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD OCT PY 2012 VL 34 IS 2 SI SI BP 415 EP 444 DI 10.1007/s10686-011-9237-2 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012IU UT WOS:000309230600010 ER PT J AU Walters, CL Freeman, R Collen, A Dietz, C Fenton, MB Jones, G Obrist, MK Puechmaille, SJ Sattler, T Siemers, BM Parsons, S Jones, KE AF Walters, Charlotte L. Freeman, Robin Collen, Alanna Dietz, Christian Fenton, M. Brock Jones, Gareth Obrist, Martin K. Puechmaille, Sebastien J. Sattler, Thomas Siemers, Bjoern M. Parsons, Stuart Jones, Kate E. TI A continental-scale tool for acoustic identification of European bats SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE acoustic monitoring; Chiroptera; classification; echolocation; ensembles of artificial neural networks; indicator species; species identification ID TIME-EXPANDED RECORDINGS; ECHOLOCATION CALLS; FIELD IDENTIFICATION; NEURAL-NETWORKS; CLASSIFICATION; RECOGNITION; CHIROPTERA; EVOLUTION; VOCALIZATIONS; DETECTORS AB Acoustic methods are used increasingly to survey and monitor bat populations. However, the use of acoustic methods at continental scales can be hampered by the lack of standardized and objective methods to identify all species recorded. This makes comparable continent-wide monitoring difficult, impeding progress towards developing biodiversity indicators, trans-boundary conservation programmes and monitoring species distribution changes. Here we developed a continental-scale classifier for acoustic identification of bats, which can be used throughout Europe to ensure objective, consistent and comparable species identifications. We selected 1350 full-spectrum reference calls from a set of 15 858 calls of 34 European species, from EchoBank, a global echolocation call library. We assessed 24 call parameters to evaluate how well they distinguish between species and used the 12 most useful to train a hierarchy of ensembles of artificial neural networks to distinguish the echolocation calls of these bat species. Calls are first classified to one of five call-type groups, with a median accuracy of 97.6%. The median species-level classification accuracy is 83.7%, providing robust classification for most European species, and an estimate of classification error for each species. These classifiers were packaged into an online tool, iBatsID, which is freely available, enabling anyone to classify European calls in an objective and consistent way, allowing standardized acoustic identification across the continent. Synthesis and applications. iBatsID is the first freely available and easily accessible continental-scale bat call classifier, providing the basis for standardized, continental acoustic bat monitoring in Europe. This method can provide key information to managers and conservation planners on distribution changes and changes in bat species activity through time. C1 [Walters, Charlotte L.; Collen, Alanna; Jones, Kate E.] Zool Soc London, Inst Zool, London NW1 4RY, England. [Walters, Charlotte L.] Bat Conservat Trust, London SE11 5RD, England. [Walters, Charlotte L.] Univ Kent, DICE, Canterbury CT2 7NR, Kent, England. [Freeman, Robin] UCL, CoMPLEX, London WC1E 6BT, England. [Freeman, Robin] Microsoft Res, Computat Ecol & Environm Sci, Cambridge CB3 0FB, England. [Dietz, Christian] Univ Tubingen, Dept Anim Physiol, D-72076 Tubingen, Germany. [Fenton, M. Brock] Western Univ, Dept Biol, London, ON N6A 5B7, Canada. [Jones, Gareth] Univ Bristol, Sch Biol Sci, Bristol BS8 1UG, Avon, England. [Obrist, Martin K.] Swiss Fed Inst Forest Snow & Landscape Res WSL, CH-8903 Birmensdorf, ZH, Switzerland. [Puechmaille, Sebastien J.] Univ Coll Dublin, Sch Biol & Environm Sci, Dublin 4, Ireland. [Puechmaille, Sebastien J.; Siemers, Bjoern M.] Max Planck Inst Ornithol, Sensory Ecol Grp, D-82319 Seewiesen, Germany. [Puechmaille, Sebastien J.] CREN, GCMP, Toulouse, France. [Sattler, Thomas] Swiss Fed Inst Forest Snow & Landscape Res WSL, CH-6500 Bellinzona, Switzerland. [Sattler, Thomas] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Sattler, Thomas] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Parsons, Stuart] Univ Auckland, Sch Biol Sci, Auckland 1, New Zealand. [Jones, Kate E.] UCL, Dept Genet Evolut & Environm, London WC1E 6BT, England. RP Walters, CL (reprint author), Zool Soc London, Inst Zool, Regents Pk, London NW1 4RY, England. EM charlotte.walters@ioz.ac.uk RI Jones, Kate/G-4768-2010; Puechmaille, Sebastien/D-1612-2010; OI Jones, Kate/0000-0001-5231-3293; Puechmaille, Sebastien/0000-0001-9517-5775; Parsons, Stuart/0000-0003-1025-5616 FU NERC [NE/H525003/1]; University of Auckland; Leverhulme Trust; Darwin Initiative [15033, EI-DPO036, EIDPR075] FX This work was financially supported by a NERC studentship to C. L. W (NE/H525003/1), a sabbatical to S. P. from The University of Auckland, a Leverhulme Trust award to K.E.J and The Darwin Initiative (15033, EI-DPO036, EIDPR075). We also thank Nancy Jennings (dotmoth.co.uk) and Michel Barataud for providing echolocation calls, Jon Russ, Andriy-Taras Bashta and the Ukraine iBats volunteers for data collection, Catherine Sayer, Joe Szewczak and Victor Obolonkin for assistance and Danilo Russo and two anonymous referees for helpful comments on the manuscript. This study is dedicated to the memory of Bjorn Siemers, who passed away before publication. We miss him, his enthusiasm for life and his massive contribution to our understanding of bat acoustics and evolution. NR 52 TC 47 Z9 51 U1 7 U2 103 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD OCT PY 2012 VL 49 IS 5 BP 1064 EP 1074 DI 10.1111/j.1365-2664.2012.02182.x PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 008BQ UT WOS:000308932600011 ER PT J AU Hong, T AF Hong, Terry TI Lenin's Kisses 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 1 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 OCT 1 PY 2012 VL 137 IS 16 BP 75 EP 75 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 013TH UT WOS:000309328300074 ER PT J AU Yang, ZF Landry, JF Handfield, L Zhang, YL Solis, MA Handfield, D Scholtens, BG Mutanen, M Nuss, M Hebert, PDN AF Yang, Zhaofu Landry, Jean-Francois Handfield, Louis Zhang, Yalin Solis, M. Alma Handfield, Daniel Scholtens, Brian G. Mutanen, Marko Nuss, Matthias Hebert, Paul D. N. TI DNA barcoding and morphology reveal three cryptic species of Anania (Lepidoptera: Crambidae: Pyraustinae) in North America, all distinct from their European counterpart SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID INTEGRATIVE TAXONOMY; MAXIMUM-LIKELIHOOD; MITOCHONDRIAL-DNA; EVOLUTIONARY; BIODIVERSITY; MOTH; BUTTERFLIES; SYMBIONTS; ACCURATE; COMPLEX AB Anania coronata (Hufnagel), a Holarctic species of pyraustine crambid moth, has long been treated as having two geographically separated subspecies the nominotypical Anania coronata in the Palaearctic Region and Anania coronata tertialis (Guenee) in the Nearctic Region. Maximum likelihood and Bayesian inference analysis of mitochondrial DNA barcodes both recover four well-supported, reciprocally monophyletic groups within Anania coronata. Qualitative and quantitative analyses of genital structures reveal diagnostic differences that correspond to the four barcode lineages. On the basis of both molecular and morphological evidence, we conclude that Anania coronata is actually a complex of four species. Anania coronata (Hufnagel) is restricted to Europe, whereas three species occur in North America: Anania tertialis (Guenee), Anania plectilis (Grote & Robinson) and Anania tennesseensissp.n. Yang. C1 [Yang, Zhaofu; Zhang, Yalin] NW A&F Univ, Key Lab Plant Protect Resources & Pest Management, Minist Educ, Entomol Museum, Yangling 712100, Peoples R China. [Landry, Jean-Francois] Agr & Agri Food Canada, Eastern Cereal & Oilseed Res Ctr, CEF, Ottawa, ON K1A 0C6, Canada. [Solis, M. Alma] USDA, Systemat Entomol Lab, Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Scholtens, Brian G.] Coll Charleston, Dept Biol, Charleston, SC USA. [Mutanen, Marko] Univ Oulu, Zool Museum, Dept Biol, Oulu, Finland. [Nuss, Matthias] Senckenberg Nat Hist Collect Dresden, Museum Zool, D-01109 Dresden, Germany. [Hebert, Paul D. N.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. RP Zhang, YL (reprint author), NW A&F Univ, Key Lab Plant Protect Resources & Pest Management, Minist Educ, Entomol Museum, Yangling 712100, Peoples R China. EM yalinzh@yahoo.com RI Yakovlev, Roman/J-7243-2013; Hebert, Paul/C-4161-2013 OI Hebert, Paul/0000-0002-3081-6700 FU Ministry of Science and Technology of the People's Republic of China [2011FY120200]; NSERC; government of Canada through Genome Canada; government of Canada through Ontario Genomics Institute; China Scholarship Council FX We thank colleagues at the Biodiversity Institute of Ontario for assistance with DNA sequencing. We thank Vazrick Nazari for assistance with photography of the genitalia at the CNC, and Mark Metz for measurement and photography of the type specimen at the USNM. We thank Andreas Segerer, Brandon Laforest, Evgeny Zakharov and Jeremy deWaard for permission to access their data. We are also grateful to Suzanne Rab Green and David Grimaldi (AMNH) for permission to analyse the type specimen, J. Donald Lafontaine who aided work on the type specimen in the British Museum of Natural History, and Tim McCabe, NY State Museum (Albany), for searching the collection under his care for possible types. This study was supported by The Ministry of Science and Technology of the People's Republic of China (2011FY120200) and by grants from NSERC, and from the government of Canada through Genome Canada and the Ontario Genomics Institute in support of the International Barcode of Life project to PDNH. Z. Yang thanks the China Scholarship Council for its support. NR 73 TC 17 Z9 18 U1 1 U2 34 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD OCT PY 2012 VL 37 IS 4 BP 686 EP 705 DI 10.1111/j.1365-3113.2012.00637.x PG 20 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 003VH UT WOS:000308639000006 ER PT J AU Prado, A McKenna, DD Windsor, D AF Prado, Alberto McKenna, Duane D. Windsor, Donald TI Molecular evidence of cycad seed predation by immature Aulacoscelidinae (Coleoptera: Orsodacnidae) SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID LEAF BEETLES CHRYSOMELIDAE; ZAMIACEAE; WEEVILS; DIVERSIFICATION; SYSTEMATICS; PLACEMENT; EVOLUTION; HABITAT; MEXICO; LARVA AB Adult beetles in the small subfamily Aulacoscelidinae (superfamily Chrysomeloidea) are known to feed on the foliage and juices of New World cycads (Order Cycadales; family Zamiaceae), but the habits of larvae have long remained a mystery. We provide the first direct evidence that Aulacoscelidinae larvae feed on and develop within the megagametophyte of the Mesoamerican cycad, Dioon merolae (Zamiaceae). Phylogenetic analyses based on partial DNA sequences from 3 genes recover a cycad seed-feeding larva proposed to belong to Aulacoscelidinae. These observations reveal a more intimate feeding relationship between Aulacoscelidinae and their New World cycad host plants than was previously recognized. Further, adult Aulacoscelidinae have long been noted to resemble Jurassic fossil chrysomeloids in the extinct subfamily Protoscelidinae. The molecular, morphological, ecological and fossil data reported herein are broadly compatible with an early association between Aulacoscelidinae and their gymnosperm hosts. C1 [Prado, Alberto] McGill Univ, Dept Plant Sci, Ste Anne De Bellevue, PQ H9X 3V9, Canada. [McKenna, Duane D.] Univ Memphis, Dept Biol Sci, Memphis, TN 38152 USA. [Windsor, Donald] Smithsonian Trop Res Inst, Balboa, Panama. RP Prado, A (reprint author), McGill Univ, Dept Plant Sci, R2-019 Raymond Bldg,21,111 Lakeshore Rd, Ste Anne De Bellevue, PQ H9X 3V9, Canada. EM alberto.prado@mail.mcgill.ca NR 66 TC 4 Z9 6 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD OCT PY 2012 VL 37 IS 4 BP 747 EP 757 DI 10.1111/j.1365-3113.2012.00639.x PG 11 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 003VH UT WOS:000308639000008 ER PT J AU Gunther, HM Wolk, SJ Spitzbart, B Gutermuth, RA Forbrich, J Wright, NJ Allen, L Bourke, TL Megeath, ST Pipher, JL AF Guenther, H. M. Wolk, S. J. Spitzbart, B. Gutermuth, R. A. Forbrich, J. Wright, N. J. Allen, L. Bourke, T. L. Megeath, S. T. Pipher, J. L. TI IRAS 20050+2720: ANATOMY OF A YOUNG STELLAR CLUSTER SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: formation; stars: pre-main sequence; X-rays: stars ID STAR-FORMING REGION; T-TAURI-STARS; PROTOSTELLAR COLLAPSE CANDIDATES; POINT-SOURCE IDENTIFICATION; GALACTIC PLANE IPHAS; X-RAY SPECTROSCOPY; H-ALPHA SURVEY; MOLECULAR CLOUDS; MULTIPOLAR OUTFLOW; EMBEDDED CLUSTERS AB IRAS 20050+2720 is young star-forming region at a distance of 700 pc without apparent high-mass stars. We present results of our multi-wavelength study of IRAS 20050+2720 which includes observations by Chandra and Spitzer, and Two Micron All Sky Survey and UBVRI photometry. In total, about 300 young stellar objects (YSOs) in different evolutionary stages are found. We characterize the distribution of YSOs in this region using a minimum spanning tree analysis. We newly identify a second cluster core, which consists mostly of class II objects, about 10' from the center of the cloud. YSOs of earlier evolutionary stages are more clustered than more evolved objects. The X-ray luminosity function (XLF) of IRAS 20050+2720 is roughly lognormal, but steeper than the XLF of the more massive Orion Nebula complex. IRAS 20050+2720 shows a lower N-H/A(K) ratio compared with the diffuse interstellar medium. C1 [Guenther, H. M.; Wolk, S. J.; Spitzbart, B.; Forbrich, J.; Wright, N. J.; Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Megeath, S. T.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Pipher, J. L.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hguenther@cfa.harvard.edu RI Pillitteri, Ignazio/L-1549-2016; OI Pillitteri, Ignazio/0000-0003-4948-6550; Gunther, Hans Moritz/0000-0003-4243-2840; Wolk, Scott/0000-0002-0826-9261 FU NASA; National Aeronautics and Space Administration; National Science Foundation; Chandra Award [GO6-7017X] 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. This publication makes use of data products from IPHAS (carried out at the Isaac Newton Telescope, INT, operated on the island of La Palma by the Isaac Newton Group) and 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. PyRAF is a product of the Space Telescope Science Institute, which is operated by AURA for NASA. This work was funded by Chandra Award GO6-7017X. NR 79 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD OCT PY 2012 VL 144 IS 4 AR 101 DI 10.1088/0004-6256/144/4/101 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007WO UT WOS:000308919300011 ER PT J AU Axelsson, M Baldini, L Barbiellini, G Baring, MG Bellazzini, R Bregeon, J Brigida, M Bruel, P Buehler, R Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Chaves, RCG Chekhtman, A Chiang, J Claus, R Conrad, J Cutini, S D'Ammando, F de Palma, F Dermer, CD Silva, EDE Drell, PS Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Fukazawa, Y Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giglietto, N Giroletti, M Godfrey, G Guiriec, S Hadasch, D Hanabata, Y Hayashida, M Hou, X Iyyani, S Jackson, MS Kocevski, D Kuss, M Larsson, J Larsson, S Longo, F Loparco, F Lundman, C Mazziotta, MN McEnery, JE Mizuno, T Monzani, ME Moretti, E Morselli, A Murgia, S Nuss, E Nymark, T Ohno, M Omodei, N Pesce-Rollins, M Piron, F Pivato, G Racusin, JL Raino, S Razzano, M Razzaque, S Reimer, A Roth, M Ryde, F Sanchez, DA Sgro, C Siskind, EJ Spandre, G Spinelli, P Stamatikos, M Tibaldo, L Tinivella, M Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Waite, AP Winer, BL Wood, KS Burgess, JM Bhat, PN Bissaldi, E Briggs, MS Connaughton, V Fishman, G Fitzpatrick, G Foley, S Gruber, D Kippen, RM Kouveliotou, C Jenke, P McBreen, S McGlynn, S Meegan, C Paciesas, WS Pelassa, V Preece, R Tierney, D von Kienlin, A Wilson-Hodge, C Xiong, S Pe'er, A AF Axelsson, M. Baldini, L. Barbiellini, G. Baring, M. G. Bellazzini, R. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Chaves, R. C. G. Chekhtman, A. Chiang, J. Claus, R. Conrad, J. Cutini, S. D'Ammando, F. de Palma, F. Dermer, C. D. do Couto e Silva, E. Drell, P. S. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Fukazawa, Y. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giglietto, N. Giroletti, M. Godfrey, G. Guiriec, S. Hadasch, D. Hanabata, Y. Hayashida, M. Hou, X. Iyyani, S. Jackson, M. S. Kocevski, D. Kuss, M. Larsson, J. Larsson, S. Longo, F. Loparco, F. Lundman, C. Mazziotta, M. N. McEnery, J. E. Mizuno, T. Monzani, M. E. Moretti, E. Morselli, A. Murgia, S. Nuss, E. Nymark, T. Ohno, M. Omodei, N. Pesce-Rollins, M. Piron, F. Pivato, G. Racusin, J. L. Raino, S. Razzano, M. Razzaque, S. Reimer, A. Roth, M. Ryde, F. Sanchez, D. A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Stamatikos, M. Tibaldo, L. Tinivella, M. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Waite, A. P. Winer, B. L. Wood, K. S. Burgess, J. M. Bhat, P. N. Bissaldi, E. Briggs, M. S. Connaughton, V. Fishman, G. Fitzpatrick, G. Foley, S. Gruber, D. Kippen, R. M. Kouveliotou, C. Jenke, P. McBreen, S. McGlynn, S. Meegan, C. Paciesas, W. S. Pelassa, V. Preece, R. Tierney, D. von Kienlin, A. Wilson-Hodge, C. Xiong, S. Pe'er, A. TI GRB110721A: AN EXTREME PEAK ENERGY AND SIGNATURES OF THE PHOTOSPHERE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (GRB110721A); radiation mechanisms: thermal ID GAMMA-RAY-BURSTS; NONTHERMAL EMISSION; SPECTRAL COMPONENT; PROMPT EMISSION; GRB090902B; MONITOR; PULSES AB GRB110721A was observed by the Fermi Gamma-ray Space Telescope using its two instruments, the Large Area Telescope (LAT) and the Gamma-ray Burst Monitor (GBM). The burst consisted of one major emission episode which lasted for similar to 24.5 s (in the GBM) and had a peak flux of (5.7 +/- 0.2) x 10(-5) erg s(-1) cm(-2). The time-resolved emission spectrum is best modeled with a combination of a Band function and a blackbody spectrum. The peak energy of the Band component was initially 15 +/- 2 MeV, which is the highest value ever detected in a GRB. This measurement was made possible by combining GBM/BGO data with LAT Low Energy events to achieve continuous 10-100 MeV coverage. The peak energy later decreased as a power law in time with an index of -1.89 +/- 0.10. The temperature of the blackbody component also decreased, starting from similar to 80 keV, and the decay showed a significant break after similar to 2 s. The spectrum provides strong constraints on the standard synchrotron model, indicating that alternative mechanisms may give rise to the emission at these energies. C1 [Axelsson, M.; Iyyani, S.; Jackson, M. S.; Lundman, C.; Moretti, E.; Nymark, T.; Ryde, F.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Axelsson, M.; Larsson, J.; Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.; Conrad, J.; Iyyani, S.; Jackson, M. S.; Larsson, J.; Larsson, S.; Lundman, C.; Moretti, E.; Nymark, T.; Ryde, F.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Baring, M. G.] Rice Univ, Dept Phys & Astron, Houston, TX 77251 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Loparco, F.; Raino, S.; Spinelli, P.] Univ & Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Loparco, F.; Mazziotta, M. N.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.] IN2P3, CNRS, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France. [Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Godfrey, G.; Hayashida, M.; Kocevski, D.; Monzani, M. E.; Murgia, S.; Omodei, N.; Reimer, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Buehler, R.; Cameron, R. A.; Chiang, J.; Claus, R.; do Couto e Silva, E.; Drell, P. S.; Focke, W. B.; Godfrey, G.; Hayashida, M.; Kocevski, D.; Monzani, M. E.; Murgia, S.; Omodei, N.; Reimer, A.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Waite, A. P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Caliandro, G. A.; Hadasch, D.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cecchi, C.; D'Ammando, F.; Germani, S.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Cecchi, C.; Germani, S.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Chaves, R. C. G.] Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA,IRFU,CNRS, F-91191 Gif Sur Yvette, France. [Chekhtman, A.; Razzaque, S.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Conrad, J.; Iyyani, S.; Larsson, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Rome, Italy. [D'Ammando, F.] IASF Palermo, I-90146 Palermo, Italy. [D'Ammando, F.] INAF Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. [Dermer, C. D.; Racusin, J. L.; Stamatikos, M.; Wood, K. S.] USN, Div Space Sci, Res Lab, Washington, DC 20375 USA. [Ferrara, E. C.; Gehrels, N.; Guiriec, S.; McEnery, J. E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fukazawa, Y.; Hanabata, Y.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Giroletti, M.; Jenke, P.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hou, X.] Univ Bordeaux 1, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3, Montpellier, France. [Ohno, M.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Pivato, G.; Tibaldo, L.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Razzano, M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Bissaldi, E.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Sanchez, D. A.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Stamatikos, M.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Tibaldo, L.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Burgess, J. M.; Bhat, P. N.; Briggs, M. S.; Connaughton, V.; Pelassa, V.; Preece, R.; Xiong, S.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Fishman, G.; Kouveliotou, C.; Jenke, P.; Wilson-Hodge, C.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Fitzpatrick, G.; Foley, S.; McBreen, S.; Tierney, D.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Foley, S.; Gruber, D.; McBreen, S.; von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kippen, R. M.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [McGlynn, S.] Tech Univ Munich, D-85748 Garching, Germany. [Meegan, C.; Paciesas, W. S.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Pe'er, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Axelsson, M (reprint author), Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. EM magnusa@astro.su.se; josefin.larsson@astro.su.se; moretti@particle.kth.se; felix@particle.kth.se; james.m.burgess@nasa.gov RI Bissaldi, Elisabetta/K-7911-2016; Iyyani, Shabnam/D-8736-2017; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Morselli, Aldo/G-6769-2011; Racusin, Judith/D-2935-2012; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; OI Sgro', Carmelo/0000-0001-5676-6214; Burgess, James/0000-0003-3345-9515; Omodei, Nicola/0000-0002-5448-7577; /0000-0003-0065-2933; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Giroletti, Marcello/0000-0002-8657-8852; Moretti, Elena/0000-0001-5477-9097; Cutini, Sara/0000-0002-1271-2924; Gasparrini, Dario/0000-0002-5064-9495; Bissaldi, Elisabetta/0000-0001-9935-8106; Iyyani, Shabnam/0000-0002-2525-3464; Preece, Robert/0000-0003-1626-7335; Caraveo, Patrizia/0000-0003-2478-8018; giglietto, nicola/0000-0002-9021-2888; Morselli, Aldo/0000-0002-7704-9553; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; Mazziotta, Mario /0000-0001-9325-4672; Baldini, Luca/0000-0002-9785-7726 FU K. A. Wallenberg Foundation; NASA, United States; DOE, United States; CEA/Irfu, France; IN2P3/CNRS, France; ASI, Italy; INFN, Italy; MEXT, Japan; KEK, Japan; JAXA, Japan; K. A. Wallenberg Foundation, Sweden; Swedish Research Council, Sweden [623-2009-691]; SNSB, Sweden; BMWi/DLR in Germany; Carl Tryggers Stiftelse for Vetenskaplig Forskning FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; The Fermi LAT Collaboration acknowledges support from a number of agencies and institutes for both development and the operation of the LAT as well as scientific data analysis. These include NASA and DOE in the United States, CEA/Irfu and IN2P3/CNRS in France, ASI and INFN in Italy, MEXT, KEK, and JAXA in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council (623-2009-691), and the SNSB in Sweden. Additional support from INAF in Italy and CNES in France for science analysis during the operations phase is also gratefully acknowledged. The Fermi GBM Collaboration acknowledges support for GBM development, operations, and data analysis from NASA in the US and BMWi/DLR in Germany. E. M. is supported by Carl Tryggers Stiftelse for Vetenskaplig Forskning. NR 26 TC 69 Z9 70 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 OCT 1 PY 2012 VL 757 IS 2 AR L31 DI 10.1088/2041-8205/757/2/L31 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007XM UT WOS:000308921700012 ER PT J AU Barthel, P Haas, M Leipski, C Wilkes, B AF Barthel, Peter Haas, Martin Leipski, Christian Wilkes, Belinda TI EXTREME HOST GALAXY GROWTH IN POWERFUL EARLY-EPOCH RADIO GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: starburst; infrared: galaxies ID HIGH-REDSHIFT; STAR-FORMATION; UNIFIED SCHEMES; 3CR SOURCES; X-RAY; QUASARS; DUST; AGN AB During the first half of the universe's life, a heyday of star formation must have occurred because many massive galaxies are in place after that epoch in cosmic history. Our observations with the revolutionary Herschel Space Observatory reveal vigorous optically obscured star formation in the ultra-massive hosts of many powerful high-redshift 3C quasars and radio galaxies. This symbiotic occurrence of star formation and black hole driven activity is in marked contrast to recent results dealing with Herschel observations of X-ray-selected active galaxies. Three archetypal radio galaxies at redshifts 1.132, 1.575, and 2.474 are presented here, with inferred star formation rates of hundreds of solar masses per year. A series of spectacular coeval active galactic nucleus/starburst events may have formed these ultra-massive galaxies and their massive central black holes during their relatively short lifetimes. C1 [Barthel, Peter] Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. [Haas, Martin] Ruhr Univ Bochum, Inst Astron, Bochum, Germany. [Leipski, Christian] Max Planck Inst Astron, D-6900 Heidelberg, Germany. [Wilkes, Belinda] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Barthel, P (reprint author), Univ Groningen, Kapteyn Astron Inst, NL-9700 AB Groningen, Netherlands. EM pdb@astro.rug.nl OI Wilkes, Belinda/0000-0003-1809-2364 NR 32 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD OCT 1 PY 2012 VL 757 IS 2 AR L26 DI 10.1088/2041-8205/757/2/L26 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007XM UT WOS:000308921700007 ER PT J AU Hermes, JJ Kilic, M Brown, WR Winget, DE Prieto, CA Gianninas, A Mukadam, AS Cabrera-Lavers, A Kenyon, SJ AF Hermes, J. J. Kilic, Mukremin Brown, Warren R. Winget, D. E. Allende Prieto, Carlos Gianninas, A. Mukadam, Anjum S. Cabrera-Lavers, Antonio Kenyon, Scott J. TI RAPID ORBITAL DECAY IN THE 12.75-MINUTE BINARY WHITE DWARF J0651+2844 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; binaries: eclipsing; gravitational waves; stars: individual (SDSS J065133.338+284423.37); white dwarfs ID OSIRIS TUNABLE IMAGER; SPECTROSCOPIC ANALYSIS; ECLIPSING BINARY; MERGER SYSTEMS; CCD PHOTOMETRY; PERIOD; SPECTROGRAPH; J0806.3+1527; DISCOVERY; HELIUM AB We report the detection of orbital decay in the 12.75-minute, detached binary white dwarf (WD) SDSS J065133.338+284423.37 (hereafter J0651). Our photometric observations over a 13 month baseline constrain the orbital period to 765.206543(55) s and indicate that the orbit is decreasing at a rate of (-9.8 +/- 2.8) x 10(-12) s s(-1) (or -0.31 +/- 0.09 ms yr(-1)). We revise the system parameters based on our new photometric and spectroscopic observations: J0651 contains two WDs with M-1 = 0.26 +/- 0.04 M-circle dot and M-2 = 0.50 +/- 0.04 M-circle dot. General relativity predicts orbital decay due to gravitational wave radiation of (-8.2 +/- 1.7) x 10(-12) s s(-1) (or -0.26 +/- 0.05 ms yr(-1)). Our observed rate of orbital decay is consistent with this expectation. J0651 is currently the second-loudest gravitational wave source known in the milli-Hertz range and the loudest non-interacting binary, which makes it an excellent verification source for future missions aimed at directly detecting gravitational waves. Our work establishes the feasibility of monitoring this system's orbital period decay at optical wavelengths. C1 [Hermes, J. J.; Winget, D. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.; Winget, D. E.] McDonald Observ, Ft Davis, TX 79734 USA. [Kilic, Mukremin; Gianninas, A.; Kenyon, Scott J.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Allende Prieto, Carlos; Cabrera-Lavers, Antonio] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Allende Prieto, Carlos; Cabrera-Lavers, Antonio] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Mukadam, Anjum S.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Mukadam, Anjum S.] Apache Point Observ, Sunspot, NM 88349 USA. RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jjhermes@astro.as.utexas.edu RI Alexandros, Gianninas/B-8352-2016; OI Alexandros, Gianninas/0000-0002-8655-4308; Kenyon, Scott/0000-0003-0214-609X FU NSF [AST-0909107, AST-1008734]; Norman Hackerman Advanced Research Program [003658-0252-2009] FX We acknowledge the referee for valuable suggestions. The authors are grateful to those who contributed to these observations: John W. Kuehne, K. I. Winget, E. L. Robinson, Paul A. Mason, and Samuel T. Harrold. C. A. P. is thankful to Alessandro Ederoclite for suggesting to observe J0651 with GTC, and to Sebastian Hidalgo for help with photometric reductions. J.J.H., M. H. M., and D. E. W. acknowledge the support of the NSF under grant AST-0909107 and the Norman Hackerman Advanced Research Program under grant 003658-0252-2009. A. S. M. acknowledges observing support from NSF grant AST-1008734. NR 39 TC 32 Z9 32 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 OCT 1 PY 2012 VL 757 IS 2 AR L21 DI 10.1088/2041-8205/757/2/L21 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007XM UT WOS:000308921700002 ER PT J AU Narayan, R Ozel, F Sironi, L AF Narayan, Ramesh Oezel, Feryal Sironi, Lorenzo TI RADIO SYNCHROTRON EMISSION FROM A BOW SHOCK AROUND THE GAS CLOUD G2 HEADING TOWARD THE GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; Galaxy: center ID SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; X-RAY; PARTICLE-ACCELERATION; 1 MILLIMETER; VARIABILITY; ACCRETION; SPECTRUM; MODEL; CENTIMETER AB A dense ionized cloud of gas has been recently discovered to be moving directly toward the supermassive black hole, Sgr A*, at the Galactic center. In 2013 June, at the pericenter of its highly eccentric orbit, the cloud will be approximately 3100 Schwarzschild radii from the black hole and will move supersonically through the ambient hot gas with a velocity of v(p) approximate to 5400 km s(-1). A bow shock is likely to form in front of the cloud and could accelerate electrons to relativistic energies. We estimate via particle-in-cell simulations the energy distribution of the accelerated electrons and show that the non-thermal synchrotron emission from these electrons might exceed the quiescent radio emission from Sgr A* by a factor of several. The enhanced radio emission should be detectable at GHz and higher frequencies around the time of pericentric passage and in the following months. The bow shock emission is expected to be displaced from the quiescent radio emission of Sgr A* by similar to 33 mas. Interferometric observations could resolve potential changes in the radio image of Sgr A* at wavelengths less than or similar to 6 cm. C1 [Narayan, Ramesh; Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oezel, Feryal] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. RP Narayan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AE16G, NAS8-03060]; NSF [AST-1108753]; NASA through Einstein Postdoctoral Fellowship [PF1-120090]; Chandra X-ray Center; [TG-AST120010] FX R.N. thanks A. Loeb and N. Stone for useful discussions and L. S. thanks A. Spitkovsky for insightful comments. R. N. gratefully acknowledges support from NASA grant NNX11AE16G, and F.O. from NSF grant AST-1108753. L. S. is supported by NASA through Einstein Postdoctoral Fellowship grant No. PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. The simulations were performed on the Odyssey cluster at Harvard University, on the PICSciE-OIT High Performance Computing Center and Visualization Laboratory at Princeton University, and on TeraGrid resources under contract No. TG-AST120010. NR 25 TC 24 Z9 24 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 OCT 1 PY 2012 VL 757 IS 2 AR L20 DI 10.1088/2041-8205/757/2/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007XM UT WOS:000308921700001 ER PT J AU Ahlering, MA Maldonado, JE Fleischer, RC Western, D Eggert, LS AF Ahlering, M. A. Maldonado, J. E. Fleischer, R. C. Western, David Eggert, L. S. TI Fine-scale group structure and demography of African savanna elephants recolonizing lands outside protected areas SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Demography; dispersal; Loxodonta africana; relatedness ID LOXODONTA-AFRICANA; SOCIAL-ORGANIZATION; NATIONAL-PARK; GENETIC-STRUCTURE; MICROSATELLITE LOCI; FOREST ELEPHANTS; MATING SYSTEM; GAME-RESERVE; HABITAT USE; POPULATION AB Aim Dispersal is a critical component of animal ecology that is poorly understood for most species. In particular, savanna elephants (Loxodonta africana) have been studied for decades in national parks across Africa, but little is known about their dispersal into new or unused habitats or their population dynamics in human-dominated landscapes. We capitalized on a natural dispersal event of savanna elephants recolonizing communal land in southern Kenya to document their demographic characteristics and genetic relationships. Location Rift Valley province of Kenya. Methods We collected faecal samples and used genetic methods to identify individuals, estimate the sex ratio and evaluate the patterns of relatedness within the female groups and male aggregations. We also measured dung bolus circumference to assign age classes to individuals and estimate the age structure. Results We identified 112 individuals with a sex ratio not different from one (1.32:1.00). The age structure was skewed towards younger elephants (71%), suggesting the potential for rapid growth from reproduction. We detected significantly higher kinship levels within female groups (R = 0.124 +/- 0.023), suggesting that family groups colonized the site, but found little support for higher-order genetic relationships among female groups. Males detected together were unrelated (R = 0.003 +/- 0.030). Main conclusions Our results suggest that highly social mammals, such as savanna elephants, disperse into unoccupied habitat as family groups and that a young demographic structure and a large number of males might be expected in establishing populations. These findings highlight the potential value of indirect, non-invasive methods for assessing elephant herd and demographic characteristics when direct observations are difficult. C1 [Ahlering, M. A.; Eggert, L. S.] Univ Missouri, Div Biol Sci, Columbia, MO 65211 USA. [Ahlering, M. A.; Maldonado, J. E.; Fleischer, R. C.; Eggert, L. S.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Ahlering, M. A.; Western, David] African Conservat Ctr, Nairobi, Kenya. [Maldonado, J. E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Ahlering, MA (reprint author), Nature Conservancy, 10 Cornell Stop 9019, Grand Forks, ND 58202 USA. EM mahlering@tnc.org FU University of Missouri Research Board; Center for Conservation and Evolutionary Genetics at the Smithsonian Conservation Biology Institute, National Zoological Park; Smithsonian Postdoctoral Fellowship Program; Friends of the National Zoo; American Philosophical Society; Liz Claiborne and Art Ortenberg Foundation FX We thank the staff at the African Conservation Centre and the South Rift Association of Land Owners for their support in the field, especially Ken Mwathe, John Kamanga, Julius Muriuki, Jim Nyamu and Jeffery Worden. We extend a special thanks to Albert Kuseyo, Peter Meiponyi and Samantha Russell for their help in the field and to Alyce Johnson, Nancy Rotzel and the Eggert laboratory for assistance with laboratory work. This study was supported by the University of Missouri Research Board; the Center for Conservation and Evolutionary Genetics at the Smithsonian Conservation Biology Institute, National Zoological Park; the Smithsonian Postdoctoral Fellowship Program; Friends of the National Zoo; the American Philosophical Society; and the Liz Claiborne and Art Ortenberg Foundation. NR 57 TC 5 Z9 5 U1 3 U2 60 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD OCT PY 2012 VL 18 IS 10 BP 952 EP 961 DI 10.1111/j.1472-4642.2012.00896.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 001NH UT WOS:000308466900001 ER PT J AU Li, GJ Kocsis, B Loeb, A AF Li, Gongjie Kocsis, Bence Loeb, Abraham TI Gravitational wave heating of stars and accretion discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; gravitational waves; galaxies: nuclei ID ACTIVE GALACTIC NUCLEUS; SUPERMASSIVE BLACK-HOLES; LINE REGION KINEMATICS; CLOSE BINARY STARS; TIDAL CIRCULARIZATION; GALAXY MERGERS; GAS DISK; QUASAR; CONVECTION; DISCOVERY AB We investigate the electromagnetic counterpart of gravitational waves (GWs) emitted by a supermassive black hole binary (SMBHB) through the viscous dissipation of the GW energy in an accretion disc and stars surrounding the SMBHB. We account for the suppression of the heating rate if the forcing period is shorter than the turnover time of the largest turbulent eddies. We find that the viscous heating luminosity in 0.1?M? stars can be significantly higher than their intrinsic luminosity, but still too low to be detected for extragalactic sources. The relative brightening is small for accretion discs. C1 [Li, Gongjie; Kocsis, Bence; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Li, GJ (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM gli@cfa.harvard.edu RI Kocsis, Bence/C-3061-2013 OI Kocsis, Bence/0000-0002-4865-7517 FU NSF [AST-0907890]; NASA by the Chandra X-ray Observatory Center [NNX08AL43G, NNA09DB30A, PF9-00063]; National Aeronautics Space Administration [NAS8-03060] FX We thank Eliot Quataert, Sterl Phinney and Paul Groot for helpful discussions. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. BK acknowledges support from NASA through Einstein Post-doctoral Fellowship Award Number PF9-00063 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 73 TC 2 Z9 2 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 OCT PY 2012 VL 425 IS 4 BP 2407 EP 2412 DI 10.1111/j.1365-2966.2012.21206.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996ZC UT WOS:000308132500002 ER PT J AU Ross, CN Power, ML Tardif, SD AF Ross, Corinna N. Power, Michael L. Tardif, Suzette D. TI Establishing Meal Patterns by Lickometry in the Marmoset Monkey (Callithrix jacchus): Translational Applications From the Bench to the Field and the Clinic SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE meal pattern; diet-induced obesity; ingestion rate; microstructure ID REDUCES FOOD-INTAKE; COMMON MARMOSET; SOUTHEASTERN BRAZIL; LICK RATE; BEHAVIOR; TAMARIN; RATS; DIET; MICROSTRUCTURE; GEOFFROYI AB The ability to measure and interpret variables associated with feeding behavior and food intake is essential to a variety of nonhuman primate study modalities. The development of a technique to accurately and efficiently measure food intake and meal patterning in captivity will enhance both the interpretation of foraging behavior in the wild as well as our ability to model clinically relevant human feeding pathologies. In this study, we successfully developed the use of a rodent lickometer system to monitor meal patterning in captive common marmosets. We describe the modifications necessary for this type of instrumentation to be used successfully with marmosets. We define variables of interest that relate to both previous rodent literature and human clinical measures. Finally, we relate our findings to potential translational value for both primate field research and biomedical applications. Am. J. Primatol. 74:901-914, 2012. (c) 2012 Wiley Periodicals, Inc. C1 [Ross, Corinna N.; Tardif, Suzette D.] Univ Texas Hlth Sci Ctr San Antonio, Dept Cellular & Struct Biol, Barshop Inst Longev & Aging Studies, San Antonio, TX 78245 USA. [Power, Michael L.] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Nutr Lab,Conservat Ecol Ctr, Washington, DC 20008 USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. RP Ross, CN (reprint author), Univ Texas Hlth Sci Ctr San Antonio, Dept Cellular & Struct Biol, Barshop Inst Longev & Aging Studies, 15355 Lambda Dr,3-100-06 STCBM Bldg, San Antonio, TX 78245 USA. EM rossc4@uthscsa.edu OI Power, Michael/0000-0002-6120-3528 FU NIH [R01 DK077639] FX Contract grant sponsor: NIH; contract grant number: R01 DK077639. NR 40 TC 1 Z9 1 U1 1 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2012 VL 74 IS 10 BP 901 EP 914 DI 10.1002/ajp.22043 PG 14 WC Zoology SC Zoology GA 991UQ UT WOS:000307728200004 PM 22707067 ER PT J AU Turner, BL Zuckerman, MK Garofalo, EM Wilson, A Kamenov, GD Hunt, DR Amgalantugs, T Frohlich, B AF Turner, Bethany L. Zuckerman, Molly K. Garofalo, Evan M. Wilson, Andrew Kamenov, George D. Hunt, David R. Amgalantugs, Tsend Frohlich, Bruno TI Diet and death in times of war: isotopic and osteological analysis of mummified human remains from southern Mongolia SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Isotopes; Diet; Mobility; Trauma; Mongolia; Bioarchaeology ID HUMAN TOOTH ENAMEL; PREHISTORIC HUMAN DIET; STABLE CARBON; BONE-COLLAGEN; OXYGEN ISOTOPES; STRONTIUM ISOTOPES; SKELETAL REMAINS; FEMORAL MIDSHAFT; CLIMATIC-CHANGE; HUMAN MIGRATION AB This study presents the results of an isotopic analysis of nine naturally mummified individuals three adults, two adolescents, one juvenile, and three infants recovered from the Hets Mountain Cave site in southern Mongolia, where they had been secondarily deposited. All of the individuals show evidence of violent perimortem trauma, but no skeletal indicators of nutritional or disease-related stress. Multi-isotopic data (delta C-13, delta N-15, delta O-18, Sr-87/Sr-86, and Pb-20n/Pb-204) were characterized in multiple tissues from each individual when possible, in order to reconstruct diet composition and residential origin at different points in life. Specifically, delta C-13 and delta N-15 in bone carbonate and collagen (N = 8) and hair keratin (N = 4) were coupled with enamel carbonate delta O-18 and delta C-13 (N = 3) and enamel Sr-87/Sr-86, and Pb-20n/Pb-204 (N = 3) to assess diet and residential mobility in relation to skeletal indicators of health and trauma. Results are consistent with a persistence of mixed C-3/C-4 pastoral subsistence and general stability of diet composition over the life course, in contrast to contemporary accounts of widespread famine and a dependence on grains imported from China throughout the region. However, results also suggest that at least some individuals may have migrated to this region of southern Mongolia from elsewhere during life, meaning that their dietary isotopic profiles may not represent local subsistence patterns near the Hets Mountain Cave site. Overall, these results speak to the utility of life course oriented multi-isotopic analysis in complementing more top-down historical analyses in understanding variation in subsistence, nutrition, and migration in regions undergoing significant political and economic turmoil. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Turner, Bethany L.] Georgia State Univ, Dept Anthropol, Atlanta, GA 30302 USA. [Zuckerman, Molly K.] Mississippi State Univ, Dept Anthropol & Middle Eastern Studies, Starkville, MS 39762 USA. [Garofalo, Evan M.] Johns Hopkins Univ, Ctr Funct Anat & Evolut, Baltimore, MD 21205 USA. [Wilson, Andrew] Univ Bradford, Div Archaeol Geog & Environm Sci, Bradford BD7 1DP, W Yorkshire, England. [Kamenov, George D.] Univ Florida, Dept Geol Sci, Gainesville, FL 32611 USA. [Hunt, David R.; Frohlich, Bruno] Smithsonian Inst, Natl Museum Nat Hist, Dept Phys Anthropol, Washington, DC 20004 USA. [Amgalantugs, Tsend] Mongolian Acad Sci, Inst Archaeol, Ulaanbaatar 51, Mongol Peo Rep. RP Turner, BL (reprint author), Georgia State Univ, Dept Anthropol, POB 3998, Atlanta, GA 30302 USA. EM antblt@langate.gsu.edu; mkz12@msstate.edu; evan@jhmi.edu; A.S.Wilson2@Bradford.ac.uk; kamenov@ufl.edu; tugsuu_ts2001@yahoo.com; frohlich@si.edu RI Turner, Bethany/J-3213-2012; OI Kamenov, George/0000-0002-6041-6687; Zuckerman, Molly/0000-0001-8967-3321; wilson, andrew/0000-0003-1346-937X FU Department of Anthropology, Smithsonian Institution National Museum of Natural History (NMNH); Mongolian Academy of Sciences, Ulaanbaatar; Laney Graduate School of Arts and Sciences, Emory University; Director's office, Smithsonian Institution NMNH FX This study was supported by the Department of Anthropology, Smithsonian Institution National Museum of Natural History (NMNH); the Director's office, Smithsonian Institution NMNH, the Mongolian Academy of Sciences, Ulaanbaatar; The Laney Graduate School of Arts and Sciences, Emory University; and by Private funds. Many thanks also to Dr. Jason Curtis in the Department of Geological Sciences at the University of Florida Gainesville for light isotope mass spectrometry and Derek Anderson, Cobb Institute of Archaeology, Mississippi State University, for the classification of the rodent samples. NR 135 TC 6 Z9 6 U1 1 U2 44 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD OCT PY 2012 VL 39 IS 10 BP 3125 EP 3140 DI 10.1016/j.jas.2012.04.053 PG 16 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 001HZ UT WOS:000308452600008 ER PT J AU Pekarik, AJ Schreiber, JB AF Pekarik, Andrew J. Schreiber, James B. TI The Power of Expectation SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB In 1999, the first author and his colleagues at the Smithsonian Institution published an article in Curator: The Museum Journal introducing research on the experiences visitors find satisfying in museums. Subsequent data collection has expanded on these findings, as this Research Note will elucidate. In general, the team found that experiences that visitors were looking forward to on entrance tended to have a distribution similar to that of the experiences they found satisfying on exit. The aim of this note is to present data that demonstrates this consistency, and to observe that visitors' expectations that they would have certain types of experiences upon entering a museum or exhibition were a much larger factor in determining their responses than were minor differences in museum or exhibition content or presentation. In other words, on the whole they came in knowing what experiences they expected, and they left having found them, regardless of what museum personnel presented to them inside. C1 [Pekarik, Andrew J.] Smithsonian Inst, Off Policy & Anal, Washington, DC 20560 USA. [Schreiber, James B.] Duquesne Univ, Pittsburgh, PA 15282 USA. RP Pekarik, AJ (reprint author), Smithsonian Inst, Off Policy & Anal, Washington, DC 20560 USA. EM pekarika@si.edu; jbschreiber@gmail.com NR 11 TC 5 Z9 5 U1 1 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD OCT PY 2012 VL 55 IS 4 BP 487 EP 496 DI 10.1111/j.2151-6952.2012.00171.x PG 10 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V41AT UT WOS:000209519800010 ER PT J AU Castro, J Puerta-Pinero, C Leverkus, AB Moreno-Rueda, G Sanchez-Miranda, A AF Castro, J. Puerta-Pinero, C. Leverkus, A. B. Moreno-Rueda, G. Sanchez-Miranda, A. TI Post-fire salvage logging alters a key plant-animal interaction for forest regeneration SO ECOSPHERE LA English DT Article DE Garrulus glandarius; jay-oak interaction; oak colonization; Quercus ilex; resilience; salvage harvesting; seed dispersal; Sierra Nevada National Park; succession ID JAY GARRULUS-GLANDARIUS; QUERCUS-ILEX; SPATIAL-PATTERNS; SEED DISPERSERS; PINE FORESTS; MANAGEMENT; OAKS; RECRUITMENT; POPULATION; GRASSLAND AB Post-fire salvage logging is widely implemented worldwide, but there is an increasing concern about its potential impact on the ecosystem. Moreover, there is scant information about the effect of salvage logging on ecosystem processes mediated by species interactions. We manipulated a burnt pine forest to experimentally analyze the effect of burnt-wood management on the colonization of Holm oak (Quercus ilex) mediated by acorn dispersal by Eurasian jays (Garrulus glandarius). Three replicates of three treatments were established in an 18-ha plot: salvage logging (SL), non-intervention (NI), and partial cut plus lopping (PCL; felling and lopping most of the trees but leaving all the biomass in situ). We hypothesized that different burnt-wood management could alter jays' landscape perception and thus the pattern of seed dispersal and seedling recruitment. We monitored jay abundance in each treatment for three winters and three breeding periods, and jay flights of potential acorn dispersal between nearby oak trees and the treatments. We also searched for oak seedlings recruited in the experimental plot for five years following the fire. Jays were recorded significantly more times (87%) in NI, and movements to this treatment during the acorn dispersal period were also more frequent (81% of the flights). Oak seedlings were also more abundant in NI (ca. 55%) than in SL or PCL (ca. 25% each), despite a strong effect of small remnants of live pines. The results show that the burnt forest, if unsalvaged, still provides a suitable habitat for jays, while salvage logging reduces the strength of this key plant-animal interaction for oak natural regeneration. Nonintervention policies after a forest fire therefore provide the opportunity for adaptive management that helps reduce restoration costs and increase the resilience of the system. C1 [Castro, J.; Leverkus, A. B.; Sanchez-Miranda, A.] Univ Granada, Dept Ecol, E-18071 Granada, Spain. [Puerta-Pinero, C.] Smithsonian Trop Res Inst, Unit 0948, Washington, DC USA. [Moreno-Rueda, G.] Univ Granada, Dept Zool, E-18071 Granada, Spain. RP Castro, J (reprint author), Univ Granada, Dept Ecol, E-18071 Granada, Spain. EM jorge@ugr.es RI Puerta Pinero, Carolina/B-3186-2012; Castro, Jorge/M-1509-2014; Leverkus, Alexandro/C-4752-2016 OI Puerta Pinero, Carolina/0000-0002-0584-7548; Castro, Jorge/0000-0002-6362-2240; Leverkus, Alexandro/0000-0001-5452-3614 FU Organismo Autonomo de Parques Nacionales [10/2005]; Ministerio de Ciencia e Innovacion (Spanish Government) [CGL2008-01671]; University of Granada (Plan Propio de Investigacion); Consolider-Ingenio [CSD2008-00040]; Spanish Ministerio de Educacion, Cultura y Deporte [AP2010-0272] FX We thank the Direction of the Natural and National Park of Sierra Nevada for fieldwork permission, constant support, and facilities. Many thanks to a large list of colleagues and friends that helped in the field for data collection (particularly oak searching), among others: I. Garcia-Quiros, S. Maranon-Jimenez, E. Perez-Canete, R. Ruiz-Puche, and C. Serrano. This study was supported by Project 10/2005 from the Organismo Autonomo de Parques Nacionales, Project CGL2008-01671 from Ministerio de Ciencia e Innovacion (Spanish Government), Postdoctoral fellowships from the University of Granada (Plan Propio de Investigacion) and Consolider-Ingenio CSD2008-00040 to C. P-P, and PhD grant from the Spanish Ministerio de Educacion, Cultura y Deporte to A. L. (Ref: AP2010-0272). NR 53 TC 4 Z9 4 U1 3 U2 19 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 OCT PY 2012 VL 3 IS 10 AR UNSP 90 DI 10.1890/ES12-00089.1 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 256IP UT WOS:000327303500007 ER PT J AU Hamer, SA Goldberg, TL Kitron, UD Brawn, JD Anderson, TK Loss, SR Walker, ED Hamer, GL AF Hamer, Sarah A. Goldberg, Tony L. Kitron, Uriel D. Brawn, Jeffrey D. Anderson, Tavis K. Loss, Scott R. Walker, Edward D. Hamer, Gabriel L. TI Wild Birds and Urban Ecology of Ticks and Tick-borne Pathogens, Chicago, Illinois, USA, 2005-2010 SO EMERGING INFECTIOUS DISEASES LA English DT Article ID BURGDORFERI SENSU-LATO; LYME-DISEASE SPIROCHETE; BORRELIA-BURGDORFERI; UNITED-STATES; ANAPLASMA-PHAGOCYTOPHILUM; ACARI IXODIDAE; INFECTION; RICKETTSIA; IDENTIFICATION; DIVERSITY AB Bird-facilitated introduction of ticks and associated pathogens is postulated to promote invasion of tick-borne zoonotic diseases into urban areas. Results of a longitudinal study conducted in suburban Chicago, Illinois, USA, during 2005-2010 show that 1.6% of 6,180 wild birds captured in mist nets harbored ticks. Tick species in order of abundance were Haemaphysalis leporispalustris, Ixodes dentatus, and I. scapularis, but 2 neotropical tick species of the genus Amblyomma were sampled during the spring migration. I. scapularis ticks were absent at the beginning of the study but constituted the majority of ticks by study end and were found predominantly on birds captured in areas designated as urban green spaces. Of 120 ticks, 5 were infected with Borrelia burgdorferi, spanning 3 ribotypes, but none were infected with Anaplasma phagocytophilum. Results allow inferences about propagule pressure for introduction of tick-borne diseases and emphasize the large sample sizes required to estimate this pressure. C1 [Hamer, Sarah A.; Walker, Edward D.; Hamer, Gabriel L.] Michigan State Univ, E Lansing, MI 48824 USA. [Hamer, Sarah A.; Hamer, Gabriel L.] Texas A&M Univ, College Stn, TX 77843 USA. [Goldberg, Tony L.; Anderson, Tavis K.] Univ Wisconsin, Madison, WI USA. [Kitron, Uriel D.] Emory Univ, Atlanta, GA 30322 USA. [Brawn, Jeffrey D.; Loss, Scott R.] Univ Illinois, Urbana, IL 61801 USA. [Loss, Scott R.] Smithsonian Migratory Bird Ctr, Washington, DC USA. RP Hamer, SA (reprint author), Texas A&M Univ, Vet Integrat Biosci Dept, 107-A VMA Bldg, College Stn, TX 77843 USA. EM shamer@cvm.tamu.edu RI Loss, Scott/B-1504-2014; OI Anderson, Tavis/0000-0002-3138-5535 FU National Science Foundation Ecology of Infectious Disease [0429124, 0840403] FX This project was funded through National Science Foundation Ecology of Infectious Disease Grants 0429124 and 0840403. NR 38 TC 28 Z9 29 U1 4 U2 30 PU CENTERS DISEASE CONTROL PI ATLANTA PA 1600 CLIFTON RD, ATLANTA, GA 30333 USA SN 1080-6040 EI 1080-6059 J9 EMERG INFECT DIS JI Emerg. Infect. Dis PD OCT PY 2012 VL 18 IS 10 BP 1589 EP 1595 DI 10.3201/eid1810.120511 PG 7 WC Immunology; Infectious Diseases SC Immunology; Infectious Diseases GA 268LP UT WOS:000328172500005 PM 23017244 ER PT J AU Hagedorn, M van Oppen, MJH Carter, V Henley, M Abrego, D Puill-Stephan, E Negri, A Heyward, A MacFarlane, DR Spindler, R AF Hagedorn, Mary van Oppen, Madeleine J. H. Carter, Virginia Henley, Mike Abrego, David Puill-Stephan, Eneour Negri, Andrew Heyward, Andrew MacFarlane, Doug R. Spindler, Rebecca TI First frozen repository for the Great Barrier Reef coral created SO CRYOBIOLOGY LA English DT Article DE Coral; Genome repository; Frozen bank; Acropora tenuis; Acropora millepora; Great Barrier Reef ID CLIMATE-CHANGE; CONSERVATION; CRISIS AB To build new tools for the continued protection and propagation of coral from the Great Barrier Reef (GBR), an international group of coral and cryopreservation scientists known as the Reef Recovery Initiative joined forces during the November 2011 mass-spawning event. The outcome was the creation of the first frozen bank for Australian coral from two important GBR reef-building species, Acropora tenuis and Acropora millepora. Approximately 190 frozen samples each with billions of cells were placed into long-term storage. Sperm cells were successfully cryopreserved, and after thawing, samples were used to fertilize eggs, resulting in functioning larvae. Additionally, developing larvae were dissociated, and these pluripotent cells were cryopreserved and viable after thawing. Now, we are in a unique position to move our work from the laboratory to the reefs to develop collaborative, practical conservation management tools to help secure Australia's coral biodiversity. (C) 2012 Elsevier Inc. All rights reserved. C1 [Hagedorn, Mary; Carter, Virginia; Henley, Mike] Smithsonian Inst, Washington, DC 20560 USA. [Hagedorn, Mary; Carter, Virginia] Univ Hawaii, Kaneohe, HI USA. [van Oppen, Madeleine J. H.; Abrego, David; Puill-Stephan, Eneour; Negri, Andrew] Australian Inst Marine Sci, Townsville, Qld 4810, Australia. [Heyward, Andrew] Australian Inst Marine Sci, Perth, WA, Australia. [MacFarlane, Doug R.] Monash Univ, Clayton, Vic, Australia. [Spindler, Rebecca] Taronga Zoo, Mosman, Australia. RP Hagedorn, M (reprint author), Smithsonian Inst, POB 1346, Kaneohe Bay, HI USA. EM hagedornm@si.edu RI MacFarlane, Douglas/A-9642-2008; van Oppen, Madeleine/C-3261-2008; OI MacFarlane, Douglas/0000-0001-5963-9659; van Oppen, Madeleine/0000-0003-4607-0744 FU Australian Institute of Marine Science FX Statement of funding: This work was supported by a Visiting Scientist Award to M.H. from the Australian Institute of Marine Science. NR 10 TC 8 Z9 8 U1 0 U2 29 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0011-2240 J9 CRYOBIOLOGY JI Cryobiology PD OCT PY 2012 VL 65 IS 2 BP 157 EP 158 DI 10.1016/j.cryobiol.2012.05.008 PG 2 WC Biology; Physiology SC Life Sciences & Biomedicine - Other Topics; Physiology GA 991DZ UT WOS:000307683000013 PM 22659104 ER PT J AU Raboy, BE De Vleeschouwer, KM Zeigler, SL AF Raboy, B. E. De Vleeschouwer, K. M. Zeigler, S. L. TI USING FUNCTIONAL CONNECTIVITY AND FLOW MODELS TO PRIORITIZE AREAS FOR REFORESTATION IN SEVERELY FRAGMENTED REGIONS OF THE GOLDEN-HEADED LION TAMARIN (LEONTOPITHECUS CHRYSOMELAS) DISTRIBUTION SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Meeting Abstract CT 35th Meeting of the American-Society-of-Primatologists (ASP) CY JUN 20-23, 2012 CL Sacramento, CA SP Amer Soc Primatol (ASP), Calilf Natl Primate Res Ctr C1 [Raboy, B. E.] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. [Raboy, B. E.; De Vleeschouwer, K. M.] Royal Zool Soc Antwerp, Ctr Res & Conservat, Antwerp, Belgium. [Zeigler, S. L.] Virginia Tech, Dept Biol Sci, Blacksburg, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 17 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD OCT PY 2012 VL 74 SU 1 MA 28 BP 34 EP 34 PG 1 WC Zoology SC Zoology GA 991UT UT WOS:000307728700029 ER PT J AU Turner, BL Condron, LM Wells, A Andersen, KM AF Turner, Benjamin L. Condron, Leo M. Wells, Andrew Andersen, Kelly M. TI Soil nutrient dynamics during podzol development under lowland temperate rain forest in New Zealand SO CATENA LA English DT Article DE Chronosequence; Phosphorus; Nitrogen; Spodosol; Pedogenesis; Coastal dune ID WESTERN SOUTHERN ALPS; PHOSPHORUS TRANSFORMATIONS; PALEOSEISMIC ACTIVITY; ORGANIC PHOSPHORUS; COASTAL DUNES; CHRONOSEQUENCE; WESTLAND; PEDOGENESIS; RECORD; SUCCESSION AB The Haast chronosequence on the west coast of the South Island of New Zealand consists of a series of coastal dune ridges formed by periodic earthquake disturbance over the last 6500 years. It approximates an ideal chronosequence, because soils are under the same climate and vegetation, have similar topography, and are developed in the same parent material. We assessed soil development and the changes in nutrients at eleven sites along the sequence to determine rates of nutrient transformations and the potential for limitation of biological activity by nitrogen and phosphorus availability. Soils develop rapidly to podzols (Spodosols) under the superhumid climate, involving acidification and depletion of base cations in the first few hundred years, development of a bleached eluvial horizon under a thick organic horizon within 2000 years, and formation of a continuous cemented iron pan within 4000 years. Soil phosphorus concentrations decline markedly in the first few hundred years in both the organic and upper mineral soil horizons, with rapid depletion of primary mineral phosphate and the accumulation of organic phosphorus to -80% of the total phosphorus in the upper mineral soil. These changes lead to an increasing degree of phosphorus limitation along the sequence, as indicated by an increase in C:P and N:P ratios and a decline in available phosphate. The rates of soil development and phosphorus depletion are more rapid than at the nearby Franz Josef post-glacial chronosequence, where glacial moraine derived from graywacke contains a relatively high phosphorus concentration and weathers into fine-textured soils. The Haast chronosequence therefore provides an important additional example of soil development linked to long-term depletion of soil phosphorus under a perudic moisture regime. Published by Elsevier B.V. C1 [Turner, Benjamin L.; Andersen, Kelly M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Condron, Leo M.; Wells, Andrew] Lincoln Univ, Canterbury 7647, New Zealand. 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; Condron, Leo/E-9458-2013 OI Turner, Benjamin/0000-0002-6585-0722; FU Smithsonian Institution Postdoctoral Fellowship; Lincoln University FX We thank Peter Almond, Amanda Black, Victoria Nall, and Andre Eger (Lincoln University) for field assistance, Ellis Benham (USDANRCS, Lincoln, NE) for advice on soil classification, and Tania Romero, Luis Ramos, Dianne de la Cruz, and Dayana Agudo (STRI) for laboratory assistance. Kelly Andersen was supported by a Smithsonian Institution Postdoctoral Fellowship. Funding for travel and consumables was provided by Lincoln University. NR 50 TC 19 Z9 19 U1 7 U2 63 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0341-8162 J9 CATENA JI Catena PD OCT PY 2012 VL 97 BP 50 EP 62 DI 10.1016/j.catena.2012.05.007 PG 13 WC Geosciences, Multidisciplinary; Soil Science; Water Resources SC Geology; Agriculture; Water Resources GA 981RV UT WOS:000306988300006 ER PT J AU Safavi-Naini, A von Stecher, J Capogrosso-Sansone, B Rittenhouse, ST AF Safavi-Naini, A. von Stecher, J. Capogrosso-Sansone, B. Rittenhouse, Seth T. TI First-Order Phase Transitions in Optical Lattices with Tunable Three-Body Onsite Interaction SO PHYSICAL REVIEW LETTERS LA English DT Article ID LARGE SCATTERING LENGTH; EFIMOV STATES; BOSONS; INSULATOR; SYSTEM; GASES AB We study the two-dimensional Bose-Hubbard model in the presence of a three-body interaction term, both at a mean-field level and via quantum Monte Carlo simulations. The three-body term is tuned by coupling the triply occupied states to a trapped universal trimer. We find that, for a sufficiently attractive three-body interaction, the n = 2 Mott lobe disappears and the system displays first-order phase transitions separating the n = 1 from the n = 3 lobes and the n = 1 and n = 3 Mott insulator from the superfluid. We also analyze the effect of finite temperature and find that transitions are still of first order at temperatures T similar to J, where J is the hopping matrix element. C1 [Safavi-Naini, A.; Capogrosso-Sansone, B.; Rittenhouse, Seth T.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Safavi-Naini, A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [von Stecher, J.] Univ Colorado, Boulder, CO 80309 USA. [von Stecher, J.] Natl Inst Stand & Technol, JILA, Boulder, CO 80309 USA. [Capogrosso-Sansone, B.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. RP Safavi-Naini, A (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. FU NSF grant through ITAMP at Harvard University; Smithsonian Astrophysical Observatory; NSF; Tech-X Corporation FX We acknowledge fruitful discussions with H. R. Sadeghpour, M. Foss-Feig, and A. M. Rey. S. T. R. acknowledges the financial support of an NSF grant through ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. J. v.S. gratefully acknowledges the hospitality of the ITAMP visitor program, where this work was initiated, and partial support from NSF and Tech-X Corporation. NR 44 TC 13 Z9 13 U1 1 U2 14 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 SEP 28 PY 2012 VL 109 IS 13 AR 135302 DI 10.1103/PhysRevLett.109.135302 PG 5 WC Physics, Multidisciplinary SC Physics GA 014CD UT WOS:000309351800010 PM 23030100 ER PT J AU Baco, AR Cairns, SD AF Baco, Amy R. Cairns, Stephen D. TI Comparing Molecular Variation to Morphological Species Designations in the Deep-Sea Coral Narella Reveals New Insights into Seamount Coral Ranges SO PLOS ONE LA English DT Article ID POPULATION GENETIC-STRUCTURE; NORTHEAST PACIFIC SEAMOUNT; PHYLOGENETIC INFERENCE; OCTOCORALLIA CNIDARIA; COMMUNITY STRUCTURE; SEQUENCE EVOLUTION; WATER CORALS; ANTHOZOA; ENDEMISM; ATLANTIC AB Recent studies have countered the paradigm of seamount isolation, confounding conservation efforts at a critical time. Efforts to study deep-sea corals, one of the dominant taxa on seamounts, to understand seamount connectivity, are hampered by a lack of taxonomic keys. A prerequisite for connectivity is species overlap. Attempts to better understand species overlap using DNA barcoding methods suggest coral species are widely distributed on seamounts and nearby features. However, no baseline has been established for variation in these genetic markers relative to morphological species designations for deep-sea octocoral families. Here we assess levels of genetic variation in potential octocoral mitochondrial barcode markers relative to thoroughly examined morphological species in the genus Narella. The combination of six markers used here, approximately 3350 bp of the mitochondrial genome, resolved 83% of the morphological species. Our results show that two of the markers, ND2 and NCR1, are not sufficient to resolve genera within Primnoidae, let alone species. Re-evaluation of previous studies of seamount octocorals based on these results suggest that those studies were looking at distributions at a level higher than species, possibly even genus or subfamily. Results for Narella show that using more markers provides haplotypes with relatively narrow depth ranges on the seamounts studied. Given the lack of 100% resolution of species with such a large portion of the mitochondrial genome, we argue that previous genetic studies have not resolved the degree of species overlap on seamounts and that we may not have the power to even test the hypothesis of seamount isolation using mitochondrial markers, let alone refute it. Thus a precautionary approach is advocated in seamount conservation and management, and the potential for depth structuring should be considered. C1 [Baco, Amy R.] Woods Hole, Woods Hole, MA USA. [Cairns, Stephen D.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Baco, AR (reprint author), Florida State Univ, Dept Earth Ocean & Atmospher Sci, Tallahassee, FL 32306 USA. EM abacotaylor@fsu.edu FU Hawaii Undersea Research Laboratory; Hawaii Sea Grant; National Oceanographic and Atmospheric Administration's (NOAA) Office of Ocean Exploration Award [NA0OAR4600108, NA03OAR4600110, NA04OAR4600071]; NOAA West Coast and Polar Programs National Undersea Research Program Award [UAF-040118]; NOAA Office of Ocean Exploration grant [NA07OAR4600292]; [NA04OAR4600051] FX Remaining specimens were collected by ARB with grants in Hawaii funded by the Hawaii Undersea Research Laboratory, Hawaii Sea Grant, and the National Oceanographic and Atmospheric Administration's (NOAA) Office of Ocean Exploration Award Nos. NA0OAR4600108, NA03OAR4600110, and NA04OAR4600071; collections on the Gulf of Alaska seamounts funded by Award No. NA04OAR4600051; and collections on Derickson Seamount funded by NOAA West Coast and Polar Programs National Undersea Research Program Award No. UAF-040118. NOAA Office of Ocean Exploration grant No. NA07OAR4600292 to ARB funded the laboratory analyses. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 77 TC 13 Z9 13 U1 2 U2 28 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 27 PY 2012 VL 7 IS 9 AR e45555 DI 10.1371/journal.pone.0045555 PG 15 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 016KQ UT WOS:000309517500034 PM 23029093 ER PT J AU Garcia, JC Crawford, AJ Mendoza, AM Ospina, O Cardenas, H Castro, F AF Garcia, Juan C. Crawford, Andrew J. Maria Mendoza, Angela Ospina, Oscar Cardenas, Heiber Castro, Fernando TI Comparative Phylogeography of Direct-Developing Frogs (Anura: Craugastoridae: Pristimantis) in the Southern Andes of Colombia SO PLOS ONE LA English DT Article ID DNA-SEQUENCE VARIATION; GENETIC DIFFERENTIATION; POPULATION-GENETICS; SPECIES RICHNESS; MOUNTAIN PASSES; CENTRAL-AMERICA; COSTA-RICAN; DIVERSITY; ORIGIN; MITOCHONDRIAL AB The Andes of South America hosts perhaps the highest amphibian species diversity in the world, and a sizable component of that diversity is comprised of direct-developing frogs of the genus Pristimantis (Anura: Craugastoridae). In order to better understand the initial stages of species formation in these frogs, this study quantified local-scale spatial genetic structuring in three species of Pristimantis. DNA sequences of two mitochondrial gene fragments (16S and COI) were obtained from P. brevifrons, P. palmeri and P. jubatus at different locations in the Cordillera Occidental. We found high levels of genetic diversity in the three species, with highly structured populations (as measured by F-ST) in P. brevifrons and P. palmeri while P. jubatus showed panmixia. Large effective population sizes, inferred from the high levels of genetic diversity, were found in the three species and two highly divergent lineages were detected within P. jubatus and P. palmeri. Estimated divergence times among populations within P. brevifrons and P. palmeri coincide with the Pleistocene, perhaps due to similar responses to climatic cycling or recent geological history. Such insights have important implications for linking alpha and beta diversity, suggesting regional scale patterns may be associated with local scale processes in promoting differentiation among populations in the Andes. C1 [Garcia, Juan C.; Maria Mendoza, Angela; Ospina, Oscar; Cardenas, Heiber; Castro, Fernando] Univ Valle, Dept Biol, Cali, Colombia. [Crawford, Andrew J.] Smithsonian Trop Res Inst, Panama City, Panama. [Crawford, Andrew J.] Univ Los Andes, Dept Biol Sci, Bogota, Colombia. RP Garcia, JC (reprint author), Massey Univ, Inst Nat Resources, Palmerston North, New Zealand. EM j.c.garciaramirez@massey.ac.nz RI Mendoza, Angela Maria/D-6346-2013; OI Mendoza, Angela Maria/0000-0002-6752-9238; Crawford, Andrew J./0000-0003-3153-6898; Ospina, Oscar/0000-0001-5986-4207 FU Universidad del Valle [CI-746] FX This research was supported by Universidad del Valle (Convocatoria Interna CI-746). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 73 TC 6 Z9 6 U1 2 U2 34 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 25 PY 2012 VL 7 IS 9 AR e46077 DI 10.1371/journal.pone.0046077 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 016YP UT WOS:000309556100133 PM 23049941 ER PT J AU Machida, RJ Knowlton, N AF Machida, Ryuji J. Knowlton, Nancy TI PCR Primers for Metazoan Nuclear 18S and 28S Ribosomal DNA Sequences SO PLOS ONE LA English DT Article ID RNA GENES; BIODIVERSITY; DIVERSITY; BIOSPHERE C1 [Machida, Ryuji J.] Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan. [Knowlton, Nancy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Machida, RJ (reprint author), Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan. EM ryujimachida@gate.sinica.edu.tw FU Alfred P. Sloan Foundation; Sant Chair of Marine Science discretionary funds FX Financial support was provided by the Alfred P. Sloan Foundation and the Sant Chair of Marine Science discretionary funds. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 29 TC 19 Z9 20 U1 0 U2 54 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 25 PY 2012 VL 7 IS 9 AR e46180 DI 10.1371/journal.pone.0046180 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 016YP UT WOS:000309556100148 PM 23049971 ER PT J AU Vignolini, S Rudall, PJ Rowland, AV Reed, A Moyroud, E Faden, RB Baumberg, JJ Glover, BJ Steiner, U AF Vignolini, Silvia Rudall, Paula J. Rowland, Alice V. Reed, Alison Moyroud, Edwige Faden, Robert B. Baumberg, Jeremy J. Glover, Beverley J. Steiner, Ullrich TI Pointillist structural color in Pollia fruit SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE helicoidal self-assembly; mimicry; fruit dispersal ID CELL-WALLS; BLUE PLANTS; IRIDESCENCE; MICROTUBULE; SCALES; BIRDS AB Biological communication by means of structural color has existed for at least 500 million years. Structural color is commonly observed in the animal kingdom, but has been little studied in plants. We present a striking example of multilayer-based strong iridescent coloration in plants, in the fruit of Pollia condensata. The color is caused by Bragg reflection of helicoidally stacked cellulose microfibrils that form multilayers in the cell walls of the epicarp. We demonstrate that animals and plants have convergently evolved multilayer-based photonic structures to generate colors using entirely distinct materials. The bright blue coloration of this fruit is more intense than that of any previously described biological material. Uniquely in nature, the reflected color differs from cell to cell, as the layer thicknesses in the multilayer stack vary, giving the fruit a striking pixelated or pointillist appearance. Because the multilayers form with both helicoidicities, optical characterization reveals that the reflected light from every epidermal cell is polarized circularly either to the left or to the right, a feature that has never previously been observed in a single tissue. C1 [Reed, Alison; Moyroud, Edwige; Glover, Beverley J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Vignolini, Silvia; Baumberg, Jeremy J.; Steiner, Ullrich] Univ Cambridge, Cavendish Lab, Dept Phys, Cambridge CB3 0HE, England. [Rudall, Paula J.; Rowland, Alice V.] Royal Bot Gardens, Jodrell Lab, Richmond TW9 3AB, Surrey, England. [Faden, Robert B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Glover, BJ (reprint author), Univ Cambridge, Dept Plant Sci, Downing St, Cambridge CB2 3EA, England. EM bjg26@cam.ac.uk; u.steiner@phy.cam.ac.uk RI Vignolini, Silvia/A-5196-2009; Steiner, Ullrich/K-4777-2013; Vignolini, Silvia/O-5604-2016; OI Vignolini, Silvia/0000-0003-0664-1418; Steiner, Ullrich/0000-0001-5936-339X; Vignolini, Silvia/0000-0003-0664-1418; Moyroud, Edwige/0000-0001-7908-3205 FU Leverhulme Trust [F/09-741/G]; Engineering and Physical Sciences Research Council [EP/G060649/1] FX We thank R. M. Bateman and M. M. Thomas for helpful discussion. This work was supported by the Leverhulme Trust (F/09-741/G) and by the Engineering and Physical Sciences Research Council (EP/G060649/1). NR 30 TC 95 Z9 96 U1 9 U2 108 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 SEP 25 PY 2012 VL 109 IS 39 BP 15712 EP 15715 DI 10.1073/pnas.1210105109 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 017QD UT WOS:000309604500043 PM 23019355 ER PT J AU Reasenberg, RD Patla, BR Phillips, JD Thapa, R AF Reasenberg, Robert D. Patla, Biju R. Phillips, James D. Thapa, Rajesh TI Design and characteristics of a WEP test in a sounding-rocket payload SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID EQUIVALENCE PRINCIPLE; STEP; SATELLITE; ALIGNMENT; GAUGE AB We describe SR-POEM, a Galilean test of the weak equivalence principle that is to be conducted during the free fall portion of the flight of a sounding rocket payload. This test of a single pair of substances will have a measurement uncertainty of sigma(eta) < 2 x 10(-17) after averaging the results of eight separate drops, each of 120 s duration. The entire payload is inverted between successive drops to cancel potential sources of systematic error. The weak equivalence principle measurement is made with a set of four of the SAO laser gauges, which have achieved an Allan deviation of 0.04 pm for an averaging time of 30 s. We discuss aspects of the current design with an emphasis on those that bear on the accuracy of the determination of eta. 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.; Thapa, Rajesh] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Thapa, Rajesh] UA Sci & Technol Pk, NP Photon, Tucson, AZ 85747 USA. RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM reasenberg@cfa.harvard.edu FU NASA Science Mission Directorate [NNC04GB30G, NNX07AI11G, NNX08AO04G]; Smithsonian FX This work was supported in part by the NASA Science Mission Directorate through grants NNC04GB30G and NNX07AI11G (past) 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 34 TC 6 Z9 6 U1 1 U2 9 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 SEP 21 PY 2012 VL 29 IS 18 AR 184013 DI 10.1088/0264-9381/29/18/184013 PG 18 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 993RO UT WOS:000307877500014 ER PT J AU Orosz, JA Welsh, WF Carter, JA Fabrycky, DC Cochran, WD Endl, M Ford, EB Haghighipour, N MacQueen, PJ Mazeh, T Sanchis-Ojeda, R Short, DR Torres, G Agol, E Buchhave, LA Doyle, LR Isaacson, H Lissauer, JJ Marcy, GW Shporer, A Windmiller, G Barclay, T Boss, AP Clarke, BD Fortney, J Geary, JC Holman, MJ Huber, D Jenkins, JM Kinemuchi, K Kruse, E Ragozzine, D Sasselov, D Still, M Tenenbaum, P Uddin, K Winn, JN Koch, DG Borucki, WJ AF Orosz, Jerome A. Welsh, William F. Carter, Joshua A. Fabrycky, Daniel C. Cochran, William D. Endl, Michael Ford, Eric B. Haghighipour, Nader MacQueen, Phillip J. Mazeh, Tsevi Sanchis-Ojeda, Roberto Short, Donald R. Torres, Guillermo Agol, Eric Buchhave, Lars A. Doyle, Laurance R. Isaacson, Howard Lissauer, Jack J. Marcy, Geoffrey W. Shporer, Avi Windmiller, Gur Barclay, Thomas Boss, Alan P. Clarke, Bruce D. Fortney, Jonathan Geary, John C. Holman, Matthew J. Huber, Daniel Jenkins, Jon M. Kinemuchi, Karen Kruse, Ethan Ragozzine, Darin Sasselov, Dimitar Still, Martin Tenenbaum, Peter Uddin, Kamal Winn, Joshua N. Koch, David G. Borucki, William J. TI Kepler-47: A Transiting Circumbinary Multiplanet System SO SCIENCE LA English DT Article ID SPIN-ORBIT ALIGNMENT; HIERARCHICAL TRIPLE; PLANETS; STARSPOTS AB We report the detection of Kepler-47, a system consisting of two planets orbiting around an eclipsing pair of stars. The inner and outer planets have radii 3.0 and 4.6 times that of Earth, respectively. The binary star consists of a Sun-like star and a companion roughly one-third its size, orbiting each other every 7.45 days. With an orbital period of 49.5 days, 18 transits of the inner planet have been observed, allowing a detailed characterization of its orbit and those of the stars. The outer planet's orbital period is 303.2 days, and although the planet is not Earth-like, it resides within the classical "habitable zone," where liquid water could exist on an Earth-like planet. With its two known planets, Kepler-47 establishes that close binary stars can host complete planetary systems. C1 [Orosz, Jerome A.; Welsh, William F.; Short, Donald R.; Windmiller, Gur] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Carter, Joshua A.; Torres, Guillermo; Geary, John C.; Holman, Matthew J.; Kruse, Ethan; Ragozzine, Darin; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabrycky, Daniel C.; Fortney, Jonathan] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Haghighipour, Nader] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Mazeh, Tsevi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Doyle, Laurance R.; Clarke, Bruce D.; Jenkins, Jon M.; Tenenbaum, Peter] SETI Inst, Mountain View, CA 94043 USA. [Isaacson, Howard; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lissauer, Jack J.; Barclay, Thomas; Clarke, Bruce D.; Huber, Daniel; Jenkins, Jon M.; Kinemuchi, Karen; Still, Martin; Tenenbaum, Peter; Uddin, Kamal; Koch, David G.; Borucki, William J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Shporer, Avi] Las Cumbres Observ, Global Telescope Network, Goleta, CA 93117 USA. [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Shporer, Avi] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Barclay, Thomas; Kinemuchi, Karen] Bay Area Environm Res Inst Inc, Sonoma, CA 95476 USA. [Boss, Alan P.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Uddin, Kamal] Orbital Sci Corp, Dulles, VA 20166 USA. [Haghighipour, Nader] Univ Hawaii Manoa, NASA Astrobiol Inst, Honolulu, HI 96822 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 RI Carter, Joshua/A-8280-2013; Sanchis-Ojeda, Roberto/B-6574-2013; Agol, Eric/B-8775-2013; Ragozzine, Darin/C-4926-2013; OI Sanchis-Ojeda, Roberto/0000-0002-6193-972X; Agol, Eric/0000-0002-0802-9145; Fortney, Jonathan/0000-0002-9843-4354; Kruse, Ethan/0000-0002-0493-1342; Buchhave, Lars A./0000-0003-1605-5666; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA, Science Mission Directorate; NASA [NAS5-26555, NNX12AD23G, HF-51267.01-A, HF-51272.01-A]; NASA Office of Space Science [NXX09AF08G]; NSF [AST-1109928, AST-1007992]; STScI FX Kepler was selected as the 10th mission of the Discovery Program. Funding for this mission is provided by NASA, Science Mission Directorate. The Kepler data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). The Space Telescope Science Institute (STScI) is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HTS data is provided by the NASA Office of Space Science via grant NXX09AF08G and by other grants and contracts. This work is based in part on observations obtained with the Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. J.A.O. and W.F.W. acknowledge support from the Kepler Participating Scientist Program via NASA grant NNX12AD23G; J.A.O., W.F.W., and G.W. also gratefully acknowledge support from the NSF via grant AST-1109928. G.T. acknowledges partial support for this work from NSF grant AST-1007992. J.A.C. and D.C.F. acknowledge NASA support through Hubble Fellowship grants HF-51267.01-A and HF-51272.01-A, respectively, awarded by STScI. Our dear friend and colleague David G. Koch passed away after this work was completed. He was a critical part of Kepler's success, and he will be missed. NR 21 TC 137 Z9 139 U1 2 U2 12 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD SEP 21 PY 2012 VL 337 IS 6101 BP 1511 EP 1514 DI 10.1126/science.1228380 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 007UC UT WOS:000308912900044 PM 22933522 ER PT J AU Launius, RD AF Launius, Roger D. TI Neil Armstrong (1930-2012) SO NATURE LA English DT Biographical-Item C1 Smithsonian Inst, Div Space Hist, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Div Space Hist, Natl Air & Space Museum, Washington, DC 20560 USA. EM launiusr@si.edu NR 0 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 SEP 20 PY 2012 VL 489 IS 7416 BP 368 EP 368 PG 1 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 007AK UT WOS:000308860900028 PM 22996544 ER PT J AU Schnell, NK Johnson, GD AF Schnell, Nalani K. Johnson, G. David TI Ontogenetic Fusion of the Third and Fourth Pharyngobranchial in Barbeled Dragonfishes (Stomiidae, Teleostei) with a Revision of the Identity of the Single Posterior Upper Pharyngeal Toothplate SO COPEIA LA English DT Article AB Barbeled dragonfishes (Stomiidae) comprise about 281 species in 27 genera, most of them highly specialized mesopelagic predators. Fusion of pharyngobranchiais three and four has been reported in several genera, but without supporting ontogenetic evidence. We studied cleared and double stained ontogenetic series of species in 22 of the 27 recognized stomiid genera and found that the third and fourth pharyngobranchials fuse ontogenetically in 17 genera. In contrast, in four genera (Neonesthes, Borostomias, Rhadinesthes, and Stomias), the fourth pharyngobranchial cartilage remains separate from the third in adults, as it generally does in teleosts. One genus, Astronesthes, shows an intermediate state in which these two elements fuse only partially. Additionally, our data indicate that the posteriormost upper pharyngeal toothplate in stomiids is the fourth (UP4) rather than the fifth (UPS), as previously proposed. The fourth upper pharyngeal toothplate is closely associated with the ventral surface of the fourth pharyngobranchial cartilage during early larval ontogeny. Therewith, we address a long-standing homology problem regarding the identity of UP4 and UP5 among basal neoteleosts and our results are discussed comparatively. C1 [Johnson, G. David] Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, Washington, DC 20013 USA. [Schnell, Nalani K.] Coll William & Mary, Virginia Inst Marine Sci, Dept Fisheries Sci, Gloucester Point, VA 23062 USA. RP Johnson, GD (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Div Fishes, POB 37012,MRC 0159, Washington, DC 20013 USA. EM nschnell@vims.edu; johnsond@si.edu FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes; SYNTHESYS grant at the NHM [GB-TAF-3239] FX For loan of specimens C. Klepadlo (SIO), S. Charter (NMFS, SWFSC), J. Maclaine (BMNH), K. Hartel and A. Williston (MCZ), G. Shinohara (NSMT), T. Sutton and E. Hilton (VIMS), J. Williams, L. Palmer, S. Raredon, and K. Murphy (USNM). For the production of the serial sections we thank M. Meinert. We are grateful to V. Springer for helpful discussion and comments on the manuscript and during the project. For discussion, help, and assistance during the project we thank E. Hilton and the Hilton lab, T. Sutton, and A. Nonaka. This study was initiated during a Smithsonian Predoctoral Fellowship (2008) in the Division of Fishes at the National Museum of Natural History and further supported by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes (2008) and a SYNTHESYS grant at the NHM (2007, grant number GB-TAF-3239). NR 28 TC 2 Z9 2 U1 0 U2 4 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 J9 COPEIA JI Copeia PD SEP 20 PY 2012 IS 3 BP 394 EP 407 DI 10.1643/CG-11-051 PG 14 WC Zoology SC Zoology GA 014MD UT WOS:000309379000005 ER PT J AU Smith, DG Irmak, E Ozen, O AF Smith, David G. Irmak, Erhan Ozen, Ozcan TI A Redescription of the Eel Panturichthys fowleri (Anguilliformes: Heterenchelyidae), with a Synopsis of the Heterenchelyidae SO COPEIA LA English DT Article ID MEDITERRANEAN FISHES; HISTORY; ICHTHYOFAUNA; ISRAEL; SEA AB Panturichthys fowleri (Ben-Tuvia, 1953) is redescribed on the basis of 27 specimens from the coasts of Israel, Lebanon, and Turkey. The species is recorded from Turkey for the first time. Morphological variation, especially in dentition and relative head-trunk length was found to be greater than previously recognized. The osteology is described from two cleared-and-stained specimens. A synopsis of the family Heterenchelyidae is presented, and a key to the known species Is provided. C1 [Smith, David G.] Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. [Irmak, Erhan; Ozen, Ozcan] Canakkale Onsekiz Mart Univ, Fac Fisheries, Dept Fishing & Proc Technol, TR-17100 Canakkale, Turkey. RP Smith, DG (reprint author), Smithsonian Inst, Museum Support Ctr, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM smithd@si.edu; irmakerhan@yahoo.com; oozen@comu.edu.tr RI Ozen, Ozcan/A-2632-2008 OI Ozen, Ozcan/0000-0002-9961-0081 NR 36 TC 1 Z9 1 U1 0 U2 4 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD SEP 20 PY 2012 IS 3 BP 484 EP 493 DI 10.1643/CI-11-174 PG 10 WC Zoology SC Zoology GA 014MD UT WOS:000309379000016 ER PT J AU de Santana, CD Vari, RP AF de Santana, Carlos David Vari, Richard P. TI New Species of Adontosternarchus (Gymnotiformes, Apteronotidae) from the Rio Purus Basin, Brazil SO COPEIA LA English DT Article AB A new species of the genus Adontosternarchus (Gymnotiformes, Apteronotidae) is described from samples collected during high water periods in a relatively restricted area within the Rio Purus basin, Amazonas, Brazil. Adontostemarchus duartei differs from congeners in a series of details of pigmentation, meristics, and morphometrics and represents the sixth species in the genus. A key to the species of Adontostemarchus is provided. C1 [Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. [de Santana, Carlos David] Museu Paraense Emilio Goeldi, Setor Ictiol, BR-66040170 Belem, Para, Brazil. RP Vari, RP (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, MRC 159,POB 37012, Washington, DC 20013 USA. EM csantana@museu-goeldi.br; varir@si.edu FU CNPq; Fundacao de Amparo a Pesquisa do Estado do Para [FAPESPA: 154/2010]; National Museum of Natural History, Smithsonian Institution FX We thank the following individuals for access to specimens: J. Albert, G. Burgess, D. Catania, B. Chernoff, N. Chao, W. Eschmeyer, C. Cox-Fernandes, K. Hartel, L. Page, L. Py-Daniel, M. Retzer, M. Rogers, and W. Wosiacki. We thank B. Prudente and S. Raredon for the map and R. de Oliveira and L. Peixoto for the preparation of the illustration of the photograph of the fish. Support for this project was provided by a fellowship from CNPq and the Fundacao de Amparo a Pesquisa do Estado do Para (FAPESPA: 154/2010 to CDS) and the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology, National Museum of Natural History, Smithsonian Institution (RPV). NR 14 TC 0 Z9 2 U1 1 U2 6 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 J9 COPEIA JI Copeia PD SEP 20 PY 2012 IS 3 BP 535 EP 540 DI 10.1643/CI-11-135 PG 6 WC Zoology SC Zoology GA 014MD UT WOS:000309379000022 ER PT J AU Duplain, RR Chapleau, F Munroe, TA AF Duplain, Rene R. Chapleau, Francois Munroe, Thomas A. TI A New Species of Trinectes (Pleuronectiformes: Achiridae) from the Upper Rio San Juan and Rio Condoto, Colombia SO COPEIA LA English DT Article AB A new species of American sole, captured in freshwater tributaries of the Rio San Juan and Rio Condoto, near Andagoya, Colombia, is described from four specimens collected by H. G. F. Spurrell around 1913. These fish were deposited in the fish collection of the British Museum (Natural History) and originally identified as So lea panamensis Steindachner, 1876. In the 1960s, Carl L. Hubbs and John A. Bollinger re-examined the specimens and determined that they represented an undescribed species, as indicated by labels placed in jars containing these specimens and through correspondence with staff at the British Museum. However, no formal description of this nominal species was published and its taxonomic status remained unclear. Our re-examination of these specimens and comparisons with all other described species of Trinectes support the conclusions of Hubbs and Bollinger that they are not So lea panamensis, now considered a junior subjective synonym of Trinectes fonsecensis (Gunther, 1862), and that they represent an undescribed species. Formal description of the new species, Trinectes hubbsbollinger, named in recognition of the initial discoverers, is provided herein. Trinectes hubbsbollinger is distinguished from its congeners by the combination of 7-8 lightly pigmented, transverse chromatophore lines on the ocular side of the body, ocular-side lower lip with short fimbriae with few branches, few or no cirri on the scaleless area surrounding the ocular-side anterior naris, and absence of pectoral-fin rays. C1 [Duplain, Rene R.; Chapleau, Francois] Univ Ottawa, Dept Biol, Ottawa, ON K1N 6N5, Canada. [Munroe, Thomas A.] Natl Museum Nat Hist, Smithsonian Inst, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20560 USA. RP Chapleau, F (reprint author), Univ Ottawa, Dept Biol, 30 Marie Curie, Ottawa, ON K1N 6N5, Canada. EM rduplain@gmail.com; chapleau@uottawa.ca; munroet@si.edu FU NSERC FX We thank P. Campbell (BMNH) for providing loan of specimens and x-rays that allowed us to complete this study. We extend our gratitude to curators and staff at the USNM, AMNH, FMNH, ANSP, SIO, CAS, UMMZ, LACM, and MNRJ for providing access to collections and comparative material used in this study. Special thanks to the CMNFI for allowing use of their x-ray facilities and to R. Smith for providing copies of correspondence of Carl L. Hubbs dealing with specimens. S. Raredon provided photographs of the types. H. Vazquez kindly provided the Spanish translation of the abstract. Funding for this research was supported by a discovery grant from NSERC to FC. NR 10 TC 3 Z9 3 U1 0 U2 3 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 J9 COPEIA JI Copeia PD SEP 20 PY 2012 IS 3 BP 541 EP 546 DI 10.1643/CI-11-155 PG 6 WC Zoology SC Zoology GA 014MD UT WOS:000309379000023 ER PT J AU An, HJ Kaspi, VM Tomsick, JA Cumming, A Bodaghee, A Gotthelf, EV Rahoui, F AF An, Hongjun Kaspi, Victoria M. Tomsick, John A. Cumming, Andrew Bodaghee, Arash Gotthelf, E. V. Rahoui, Farid TI CHANDRA OBSERVATIONS OF SGR 1627-41 NEAR QUIESCENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: individual; stars: magnetars; stars: neutron; X-rays: bursts ID X-RAY PULSAR; SOFT GAMMA REPEATER; XMM-NEWTON OBSERVATIONS; MAGNETIZED NEUTRON-STARS; SPIN-DOWN; 1RXS J170849.0-400910; SWIFT J1822.3-1606; 2002 OUTBURST; GIANT FLARE; FIELD AB We report on an observation of SGR 1627-41 made with the Chandra X-Ray Observatory on 2011 June 16. Approximately three years after its outburst activity in 2008, the source's flux has been declining, as it approaches its quiescent state. For an assumed power-law spectrum, we find that the absorbed 2-10 keV flux for the source is 1.0(-0.2)(+0.3) x 10(-13) erg cm(-2) s(-1) with a photon index of 2.9 +/- 0.8 (N-H = 1.0 x 10(23) cm(-2)). This flux is approximately consistent with that measured at the same time after the source's outburst in 1998. With measurements spanning three years after the 2008 outburst, we analyze the long-term flux and spectral evolution of the source. The flux evolution is well described by a double exponential with decay times of 0.5 +/- 0.1 and 59 +/- 6 days, and a thermal cooling model fit suggests that SGR 1627-41 may have a hot core (T-c similar to 2 x 10(8) K). We find no clear correlation between flux and spectral hardness as found in other magnetars. We consider the quiescent X-ray luminosities of magnetars and the subset of rotation-powered pulsars with high magnetic fields (B greater than or similar to 10(13) G) in relation to their spin-inferred surface magnetic field strength and find a possible trend between the two quantities. C1 [An, Hongjun; Kaspi, Victoria M.; Cumming, Andrew] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Tomsick, John A.; Bodaghee, Arash] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Rahoui, Farid] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP An, HJ (reprint author), McGill Univ, Dept Phys, Rutherford Phys Bldg,3600 Univ St, Montreal, PQ H3A 2T8, Canada. RI Cumming, Andrew/A-6082-2013 OI Cumming, Andrew/0000-0002-6335-0169 FU Killam Fellowship; NSERC; FQRNT Centre de Recherche Astrophysique du Quebec; R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR); Canada Research Chairs Program; Lorne Trottier Chair in Astrophysics and Cosmology; NASA [GO1-12068A, NAS8-03060]; NSERC Discovery Grant and the Canadian Institute for Advanced Research (CIFAR; Canadian Institute for Advanced Research (CIFAR) FX V.M.K. acknowledges support from a Killam Fellowship, an NSERC Discovery Grant, the FQRNT Centre de Recherche Astrophysique du Quebec, an R. Howard Webster Foundation Fellowship from the Canadian Institute for Advanced Research (CIFAR), the Canada Research Chairs Program, and the Lorne Trottier Chair in Astrophysics and Cosmology. J.A.T., A.B., E. G., and F. R. acknowledge partial support from NASA through Chandra Award No. GO1-12068A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory under NASA Contract NAS8-03060. A. C. is supported by an NSERC Discovery Grant and the Canadian Institute for Advanced Research (CIFAR). NR 78 TC 13 Z9 13 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 SEP 20 PY 2012 VL 757 IS 1 AR 68 DI 10.1088/0004-637X/757/1/68 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800068 ER PT J AU Antonini, F Perets, HB AF Antonini, Fabio Perets, Hagai B. TI SECULAR EVOLUTION OF COMPACT BINARIES NEAR MASSIVE BLACK HOLES: GRAVITATIONAL WAVE SOURCES AND OTHER EXOTICA SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; Galaxy: center; gravitational waves; stars: kinematics and dynamics ID NUCLEAR STAR CLUSTER; SOLAR-TYPE STARS; GALACTIC-CENTER; TRIPLE STARS; DYNAMICAL EVOLUTION; ORBITAL EVOLUTION; STELLAR DYNAMICS; GLOBULAR-CLUSTER; KOZAI MECHANISM; TIDAL BREAKUP AB The environment near supermassive black holes (SMBHs) in galactic nuclei contains a large number of stars and compact objects. A fraction of these are likely to be members of binaries. Here we discuss the binary population of stellar black holes and neutron stars near SMBHs and focus on the secular evolution of such binaries, due to the perturbation by the SMBH. Binaries with highly inclined orbits with respect to their orbit around the SMBH are strongly affected by secular Kozai processes, which periodically change their eccentricities and inclinations (Kozai cycles). During periapsis approach, at the highest eccentricities during the Kozai cycles, gravitational wave (GW) emission becomes highly efficient. Some binaries in this environment can inspiral and coalesce at timescales much shorter than a Hubble time and much shorter than similar binaries that do not reside near an SMBH. The close environment of SMBHs could therefore serve as a catalyst for the inspiral and coalescence of binaries and strongly affect their orbital properties. Such compact binaries would be detectable as GW sources by the next generation of GW detectors (e. g., advanced-LIGO). Our analysis shows that similar to 0.5% of such nuclear merging binaries will enter the LIGO observational window while on orbits that are still very eccentric (e greater than or similar to 0.5). The efficient GW analysis for such systems would therefore require the use of eccentric templates. We also find that binaries very close to the SMBH could evolve through a complex dynamical (non-secular) evolution, leading to emission of several GW pulses during only a few years (though these are likely to be rare). Finally, we note that the formation of close stellar binaries, X-ray binaries, and their merger products could be induced by similar secular processes, combined with tidal friction rather than GW emission as in the case of compact object binaries. C1 [Antonini, Fabio] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Perets, Hagai B.] Technion Israel Inst Technol, Haifa, Israel. RP Antonini, F (reprint author), Univ Toronto, Canadian Inst Theoret Astrophys, 60 George St, Toronto, ON M5S 3H8, Canada. RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X FU Harvard/CFA Predoctoral Fellowship FX We are extremely grateful to S. Mikkola, who wrote the ARCHAIN integrator. We thank S. Prodan for a careful reading of an earlier version of this paper. We thank K. Cannon, C. Hopman, B. Kocsis, D. Merritt, A. Mroue, N. Murray, Harald Pfeiffer, and Y. Wu for useful comments. F. A. acknowledges partial support from Harvard/CFA Predoctoral Fellowship during the Summer 2011. NR 86 TC 58 Z9 58 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 SEP 20 PY 2012 VL 757 IS 1 AR 27 DI 10.1088/0004-637X/757/1/27 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800027 ER PT J AU Barnard, R Garcia, M Murray, SS AF Barnard, R. Garcia, M. Murray, S. S. TI 12 YEARS OF X-RAY VARIABILITY IN M31 GLOBULAR CLUSTERS, INCLUDING 8 BLACK HOLE CANDIDATES, AS SEEN BY CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; globular clusters: general; globular clusters: individual; X-rays: binaries; X-rays: general ID ROSAT PSPC SURVEY; XMM-NEWTON; SPECTRAL TRANSITIONS; UPDATED SURVEY; STAR-CLUSTERS; NEUTRON-STAR; ACCRETION; BINARIES; GALAXIES; BRIGHT AB We examined 134 Chandra observations of the population of X-ray sources associated with globular clusters (GCs) in the central region of M31. These are expected to be X-ray binary systems (XBs), consisting of a neutron star or black hole accreting material from a close companion. We created long-term light curves for these sources, correcting for background, interstellar absorption, and instrumental effects. We tested for variability by examining the goodness of fit for the best-fit constant intensity. We also created structure functions (SFs) for every object in our sample, the first time this technique has been applied to XBs. We found significant variability in 28 out of 34 GCs and GC candidates; the other 6 sources had 0.3-10 keV luminosities fainter than similar to 2 x 10(36) erg s(-1), limiting our ability to detect similar variability. The SFs of XBs with 0.3-10 keV luminosities similar to 2-50x10(36) erg s(-1) generally showed considerably more variability than the published ensemble SF of active galactic nuclei (AGNs). Our brightest XBs were mostly consistent with the AGN SF; however, their 2-10 keV fluxes could be matched by <1 AGN per square degree. These encouraging results suggest that examining the long-term light curves of other X-ray sources in the field may provide an important distinction between X-ray binaries and background galaxies, as the X-ray emission spectra from these two classes of X-ray sources are similar. Additionally, we identify 3 new black hole candidates (BHCs) using additional XMM-Newton data, bringing the total number of M31 GC BHCs to 9, with 8 covered in this survey. C1 [Barnard, R.; Garcia, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU ESA member states; US (NASA); Chandra [GO0-11106X, GO1-12109X]; HST [GO-11833, GO-12014]; NASA [NAS-03060] FX We thank Z. Li for merging the Chandra data. This research has made use of data obtained from the Chandra data archive, and software provided by the Chandra X-Ray Center (CXC). We also include analysis of data from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the US (NASA). R. B. is funded by Chandra grants GO0-11106X and GO1-12109X, along with HST grants GO-11833 and GO-12014. M. R. G. and S. S. M are partially supported by NASA grant NAS-03060. NR 50 TC 16 Z9 16 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 SEP 20 PY 2012 VL 757 IS 1 AR 40 DI 10.1088/0004-637X/757/1/40 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800040 ER PT J AU Bolton, AS Brownstein, JR Kochanek, CS Shu, YP Schlegel, DJ Eisenstein, DJ Wake, DA Connolly, N Maraston, C Arneson, RA Weaver, BA AF Bolton, Adam S. Brownstein, Joel R. Kochanek, Christopher S. Shu, Yiping Schlegel, David J. Eisenstein, Daniel J. Wake, David A. Connolly, Natalia Maraston, Claudia Arneson, Ryan A. Weaver, Benjamin A. TI THE BOSS EMISSION-LINE LENS SURVEY. II. INVESTIGATING MASS-DENSITY PROFILE EVOLUTION IN THE SLACS plus BELLS STRONG GRAVITATIONAL LENS SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: structure; gravitational lensing: strong ID EARLY-TYPE GALAXIES; DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; SPECTROSCOPICALLY SELECTED SAMPLE; DARK-MATTER HALOS; ACS SURVEY; ELLIPTIC GALAXIES; STELLAR SPECTRA; DISSIPATIONLESS MERGERS; DRY MERGERS AB We present an analysis of the evolution of the central mass-density profile of massive elliptical galaxies from the SLACS and BELLS strong gravitational lens samples over the redshift interval z approximate to 0.1-0.6, based on the combination of strong-lensing aperture mass and stellar velocity-dispersion constraints. We find a significant trend toward steeper mass profiles (parameterized by the power-law density model with rho proportional to r(-gamma)) at later cosmic times, with magnitude d /dz = -0.60 +/- 0.15. We show that the combined lens-galaxy sample is consistent with a non-evolving distribution of stellar velocity dispersions. Considering possible additional dependence of on lens-galaxy stellar mass, effective radius, and Sersic index, we find marginal evidence for shallower mass profiles at higher masses and larger sizes, but with a significance that is subdominant to the redshift dependence. Using the results of published Monte Carlo simulations of spectroscopic lens surveys, we verify that our mass-profile evolution result cannot be explained by lensing selection biases as a function of redshift. Interpreted as a true evolutionary signal, our result suggests that major dry mergers involving off-axis trajectories play a significant role in the evolution of the average mass-density structure of massive early-type galaxies over the past 6 Gyr. We also consider an alternative non-evolutionary hypothesis based on variations in the strong-lensing measurement aperture with redshift, which would imply the detection of an "inflection zone" marking the transition between the baryon-dominated and dark-matter halo-dominated regions of the lens galaxies. Further observations of the combined SLACS+BELLS sample can constrain this picture more precisely, and enable a more detailed investigation of the multivariate dependences of galaxy mass structure across cosmic time. C1 [Bolton, Adam S.; Brownstein, Joel R.; Shu, Yiping; Arneson, Ryan A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Kochanek, Christopher S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wake, David A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Connolly, Natalia] Hamilton Coll, Dept Phys, Clinton, NY 13323 USA. [Maraston, Claudia] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Arneson, Ryan A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP Bolton, AS (reprint author), Univ Utah, Dept Phys & Astron, 115 South,1400 East, Salt Lake City, UT 84112 USA. EM bolton@astro.utah.edu FU NSF [AST-1009756]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; NASA through a grant from the Space Telescope Science Institute [10174, 10494, 10587, 10798, 10886, 12209]; NASA [NAS 5-26555] FX A.S.B. and J.R.B. acknowledge the hospitality of the Max-Planck-Institut fur Astronomie, where a portion of this work was completed. C.S.K. is supported by NSF grant AST-1009756. The authors thank the anonymous referee for constructive comments and suggestions that led to substantial improvements in this work.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, University of Florida, the French Participation Group, the German Participation Group, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, The University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; Support for HST programs 10174, 10494, 10587, 10798, 10886, and 12209 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. NR 68 TC 39 Z9 39 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 SEP 20 PY 2012 VL 757 IS 1 AR 82 DI 10.1088/0004-637X/757/1/82 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800082 ER PT J AU Coe, D Umetsu, K Zitrin, A Donahue, M Medezinski, E Postman, M Carrasco, M Anguita, T Geller, MJ Rines, KJ Diaferio, A Kurtz, MJ Bradley, L Koekemoer, A Zheng, W Nonino, M Molino, A Mahdavi, A Lemze, D Infante, L Ogaz, S Melchior, P Host, O Ford, H Grillo, C Rosati, P Jimenez-Teja, Y Moustakas, J Broadhurst, T Ascaso, B Lahav, O Bartelmann, M Benitez, N Bouwens, R Graur, O Graves, G Jha, S Jouvel, S Kelson, D Moustakas, L Maoz, D Meneghetti, M Merten, J Riess, A Rodney, S Seitz, S AF Coe, Dan Umetsu, Keiichi Zitrin, Adi Donahue, Megan Medezinski, Elinor Postman, Marc Carrasco, Mauricio Anguita, Timo Geller, Margaret J. Rines, Kenneth J. Diaferio, Antonaldo Kurtz, Michael J. Bradley, Larry Koekemoer, Anton Zheng, Wei Nonino, Mario Molino, Alberto Mahdavi, Andisheh Lemze, Doron Infante, Leopoldo Ogaz, Sara Melchior, Peter Host, Ole Ford, Holland Grillo, Claudio Rosati, Piero Jimenez-Teja, Yolanda Moustakas, John Broadhurst, Tom Ascaso, Begona Lahav, Ofer Bartelmann, Matthias Benitez, Narciso Bouwens, Rychard Graur, Or Graves, Genevieve Jha, Saurabh Jouvel, Stephanie Kelson, Daniel Moustakas, Leonidas Maoz, Dan Meneghetti, Massimo Merten, Julian Riess, Adam Rodney, Steve Seitz, Stella TI CLASH: PRECISE NEW CONSTRAINTS ON THE MASS PROFILE OF THE GALAXY CLUSTER A2261 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark energy; dark matter; galaxies: clusters: individual (Abell 2261); galaxies: evolution; gravitational lensing: strong; gravitational lensing: weak ID DARK-MATTER HALOS; STRONG-LENSING ANALYSIS; HUBBLE-SPACE-TELESCOPE; EXTREME-VALUE STATISTICS; LARGE-SCALE STRUCTURE; DEEP ADVANCED CAMERA; DIGITAL SKY SURVEY; SIMILAR-TO 1; X-RAY; SUNYAEV-ZELDOVICH AB We precisely constrain the inner mass profile of A2261 (z = 0.225) for the first time and determine that this cluster is not "overconcentrated" as found previously, implying a formation time in agreement with Lambda CDM expectations. These results are based on multiple strong-lensing analyses of new 16-band Hubble Space Telescope imaging obtained as part of the Cluster Lensing and Supernova survey with Hubble. Combining this with revised weak-lensing analyses of Subaru wide-field imaging with five-band Subaru + KPNO photometry, we place tight new constraints on the halo virial mass M-vir = (2.2 +/- 0.2) x 10(15) M-circle dot h(70)(-1) (within r(vir) approximate to 3 Mpc h(70)(-1)) and concentration c(vir) = 6.2 +/- 0.3 when assuming a spherical halo. This agrees broadly with average c(M, z) predictions from recent Lambda CDM simulations, which span 5 less than or similar to < c > less than or similar to 8. Our most significant systematic uncertainty is halo elongation along the line of sight (LOS). To estimate this, we also derive a mass profile based on archival Chandra X-ray observations and find it to be similar to 35% lower than our lensing-derived profile at r(2500) similar to 600 kpc. Agreement can be achieved by a halo elongated with a similar to 2:1 axis ratio along our LOS. For this elongated halo model, we find M-vir = (1.7 +/- 0.2) x 10(15) M-circle dot h(70)(-1) and c(vir) = 4.6 +/- 0.2, placing rough lower limits on these values. The need for halo elongation can be partially obviated by non-thermal pressure support and, perhaps entirely, by systematic errors in the X-ray mass measurements. We estimate the effect of background structures based on MMT/Hectospec spectroscopic redshifts and find that these tend to lower M-vir further by similar to 7% and increase c(vir) by similar to 5%. C1 [Coe, Dan; Postman, Marc; Bradley, Larry; Koekemoer, Anton; Ogaz, Sara; Riess, Adam] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Umetsu, Keiichi] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Zitrin, Adi; Bartelmann, Matthias] Heidelberg Univ, Inst Theoret Astrophys, Zentrum Astron, D-6900 Heidelberg, Germany. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Medezinski, Elinor; Zheng, Wei; Lemze, Doron; Ford, Holland; Riess, Adam; Rodney, Steve] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Carrasco, Mauricio; Anguita, Timo; Infante, Leopoldo] Pontificia Univ Catolica Chile, AIUC, Dept Astron & Astrophys, Santiago, Chile. [Carrasco, Mauricio; Rosati, Piero] European So Observ, D-8046 Garching, Germany. [Anguita, Timo] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Geller, Margaret J.; Rines, Kenneth J.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Rines, Kenneth J.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [Nonino, Mario] Osserv Astron Trieste, Ist Nazl Astrofis, I-34131 Trieste, Italy. [Molino, Alberto; Jimenez-Teja, Yolanda; Ascaso, Begona; Benitez, Narciso] Inst Astrofis Andalucia, E-18080 Granada, Spain. [Mahdavi, Andisheh] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Melchior, Peter] Ohio State Univ, Dept Phys, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Host, Ole; Lahav, Ofer; Jouvel, Stephanie] UCL, Dept Phys & Astron, London, England. [Grillo, Claudio] Tech Univ Munich, Excellence Cluster Universe, D-8046 Garching, Germany. [Moustakas, John] Univ Calif San Diego, Ctr Astrophys & Space Sci, San Diego, CA 92103 USA. [Broadhurst, Tom] Univ Basque Country UPV EHU, Dept Theoret Phys, Bilbao, Spain. [Broadhurst, Tom] Basque Fdn Sci, Ikerbasque, Bilbao, Spain. [Bouwens, Rychard] Leiden Univ, Leiden Observ, Leiden, Netherlands. [Graur, Or; Maoz, Dan] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Graves, Genevieve] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jha, Saurabh] Rutgers State Univ, Dept Phys & Astron, New Brunswick, NJ 08903 USA. [Kelson, Daniel] Carnegie Observ, Carnegie Inst Sci, Pasadena, CA USA. [Moustakas, Leonidas; Merten, Julian] CALTECH, Jet Prop Lab, La Canada Flintridge, CA USA. [Meneghetti, Massimo] Astron Observ Bologna, Ist Nazl Astrofis, Bologna, Italy. [Seitz, Stella] Univ Sternwarte, Inst Astron, Munich, Germany. [Seitz, Stella] Univ Sternwarte, Inst Astrophys, Munich, Germany. RP Coe, D (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM DCoe@STScI.edu RI Bartelmann, Matthias/A-5336-2014; Molino Benito, Alberto/F-5298-2014; Jimenez-Teja, Yolanda/D-5933-2011; Grillo, Claudio/E-6223-2015; Meneghetti, Massimo/O-8139-2015; OI Benitez, Narciso/0000-0002-0403-7455; Koekemoer, Anton/0000-0002-6610-2048; Grillo, Claudio/0000-0002-5926-7143; Meneghetti, Massimo/0000-0003-1225-7084; Nonino, Mario/0000-0001-6342-9662; Kurtz, Michael/0000-0002-6949-0090; Graur, Or/0000-0002-4391-6137; Umetsu, Keiichi/0000-0002-7196-4822; Moustakas, Leonidas/0000-0003-3030-2360 FU NASA [NAS 5-26555, NAS 5-32864, HST-GO-12065.01-A]; National Science Council of Taiwan [NSC100-2112-M-001-008-MY3]; Israel Science Foundation; German Science Foundation [Transregio TR 33]; Spanish MICINN [YA2010-22111-C03-00]; Junta de Andalucia Proyecto de Excelencia [NBL2003]; INAF Contracts [ASI-INAF I/009/10/0, ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, PRIN INAF 2009, PRIN INAF 2010]; NSF [AST-0847157]; UK's STFC; Royal Society; Wolfson Foundation; Academia Sinica Career Development Award; Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung; Smithsonian Institution; Cottrell College Science Award from Research Corporation; INFN [PD51]; PRIN-MIUR [2008NR3EBK_003]; Conicyt FONDAP/BASAL grant; DFG FX The CLASH Multi-Cycle Treasury Program is based on observations made with the NASA/ESA Hubble Space Telescope. The Space Telescope Science Institute is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. ACS was developed under NASA Contract NAS 5-32864.; This research is supported in part by NASA Grant HST-GO-12065.01-A, National Science Council of Taiwan Grant NSC100-2112-M-001-008-MY3, the Israel Science Foundation, the German Science Foundation (Transregio TR 33), Spanish MICINN Grant YA2010-22111-C03-00, funding from the Junta de Andalucia Proyecto de Excelencia NBL2003, INAF Contracts ASI-INAF I/009/10/0, ASI-INAF I/023/05/0, ASI-INAF I/088/06/0, PRIN INAF 2009, and PRIN INAF 2010, NSF CAREER Grant AST-0847157, the UK's STFC, the Royal Society, and the Wolfson Foundation. K. U. acknowledges support from the Academia Sinica Career Development Award. A.Z. is supported by contract research Internationale Spitzenforschung II-1 of the Baden-Wurttemberg Stiftung. M.J.G., K.J.R., A. D., and M.J.K. acknowledge partial support from the Smithsonian Institution. K.J.R. was funded in part by a Cottrell College Science Award from the Research Corporation. A. D. gratefully acknowledges partial support from the INFN Grant PD51 and the PRIN-MIUR-2008 Grant 2008NR3EBK_003 "Matter-antimatter asymmetry, dark matter and dark energy in the LHC era." L. I. acknowledges support from a Conicyt FONDAP/BASAL grant. P. R. and S. S. acknowledge support from the DFG cluster of excellence Origin and Structure of the Universe program. NR 189 TC 57 Z9 57 U1 1 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2012 VL 757 IS 1 AR 22 DI 10.1088/0004-637X/757/1/22 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800022 ER PT J AU Currie, T Rodigas, TJ Debes, J Plavchan, P Kuchner, M Jang-Condell, H Wilner, D Andrews, S Kraus, A Dahm, S Robitaille, T AF Currie, Thayne Rodigas, Timothy J. Debes, John Plavchan, Peter Kuchner, Marc Jang-Condell, Hannah Wilner, David Andrews, Sean Kraus, Adam Dahm, Scott Robitaille, Thomas TI KECK/NIRC2 IMAGING OF THE WARPED, ASYMMETRIC DEBRIS DISK AROUND HD 32297 SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: early-type; stars: individual (HD 32297) ID SPITZER-SPACE-TELESCOPE; ORBITING HR 8799; BETA-PICTORIS B; MU-M; CIRCUMSTELLAR DISK; PLANET FORMATION; RESONANT SIGNATURES; OPTICAL-IMAGES; DUST DISK; HD-32297 AB We present Keck/NIRC2 K-s-band high-contrast coronagraphic imaging of the luminous debris disk around the nearby, young A star HD 32297 resolved at a projected separation of r = 0.'' 3-2.'' 5 (approximate to 35-280 AU). The disk is highly warped to the north and exhibits a complex, "wavy" surface brightness (SB) profile interior to r approximate to 110 AU, where the peaks/plateaus in the profiles are shifted between the NE and SW disk lobes. The SW side of the disk is 50%-100% brighter at r = 35-80 AU, and the location of its peak brightness roughly coincides with the disk's millimeter (mm) emission peak. Spectral energy distribution modeling suggests that HD 32297 has at least two dust populations that may originate from two separate belts, likely at different locations, possibly at distances coinciding with the SB peaks. A disk model for a single dust belt including a phase function with two components and a 5-10 AU pericenter offset explains the disk's warped structure and reproduces some of the SB profile's shape (e. g., the overall "wavy" profile, the SB peak/plateau shifts) but more poorly reproduces the disk's brightness asymmetry and the profile at wider separations (r > 110 AU). Although there may be alternate explanations, agreement between the SW disk brightness peak and disk's peak mm emission is consistent with an overdensity of very small, sub-blowout-sized dust and large, 0.1-1 mm sized grains at approximate to 45 AU tracing the same parent population of planetesimals. New near-IR and submillimeter observations may be able to clarify whether even more complex grain scattering properties or dynamical sculpting by an unseen planet are required to explain HD 32297's disk structure. C1 [Currie, Thayne; Kuchner, Marc] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Rodigas, Timothy J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Debes, John] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Plavchan, Peter] CALTECH, NEXSCI, Pasadena, CA 91125 USA. [Jang-Condell, Hannah] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Wilner, David; Andrews, Sean] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kraus, Adam] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Robitaille, Thomas] MPIA Heidelberg, D-69117 Heidelberg, Germany. RP Currie, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI Jang-Condell, Hannah/0000-0002-7639-1322; Rodigas, Timothy/0000-0002-7535-2997; Robitaille, Thomas/0000-0002-8642-1329 FU NASA; W. M. Keck Foundation FX We thank Richard Walters and Gregory Wirth for valuable help in setting up these observations, which were conducted remotely from the California Institute of Technology, and to Randy Campbell for indispensable NIRC2 support in helping the observer (T. C.) conduct his observations efficiently. Karl Stapelfeldt, Scott Kenyon, and Margaret Moerchen provided very useful discussions and the anonymous referee provided helpful comments. T. C. is supported by a NASA Postdoctoral Fellowship. The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We acknowledge the significant cultural role and reverence that the Mauna Kea summit has always had within the indigenous Hawaiian community. We are grateful to be able to conduct observations from this mountain. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 61 TC 21 Z9 21 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 20 PY 2012 VL 757 IS 1 AR 28 DI 10.1088/0004-637X/757/1/28 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800028 ER PT J AU Ozel, F Psaltis, D Narayan, R Villarreal, AS AF Oezel, Feryal Psaltis, Dimitrios Narayan, Ramesh Villarreal, Antonio Santos TI ON THE MASS DISTRIBUTION AND BIRTH MASSES OF NEUTRON STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; pulsars: general; stars: neutron; X-rays: binaries ID BINARY MILLISECOND PULSAR; PSR J1614-2230; ORBITAL DECAY; VELA X-1; RADIUS; EVOLUTION; DISTANCE; SYSTEM AB We investigate the distribution of neutron star masses in different populations of binaries, employing Bayesian statistical techniques. In particular, we explore the differences in neutron star masses between sources that have experienced distinct evolutionary paths and accretion episodes. We find that the distribution of neutron star masses in non-recycled eclipsing high-mass binaries as well as of slow pulsars, which are all believed to be near their birth masses, has a mean of 1.28 M-circle dot and a dispersion of 0.24 M-circle dot. These values are consistent with expectations for neutron star formation in core-collapse supernovae. On the other hand, double neutron stars, which are also believed to be near their birth masses, have a much narrower mass distribution, peaking at 1.33 M-circle dot, but with a dispersion of only 0.05 M-circle dot. Such a small dispersion cannot easily be understood and perhaps points to a particular and rare formation channel. The mass distribution of neutron stars that have been recycled has a mean of 1.48 M-circle dot and a dispersion of 0.2 M-circle dot, consistent with the expectation that they have experienced extended mass accretion episodes. The fact that only a very small fraction of recycled neutron stars in the inferred distribution have masses that exceed similar to 2 M-circle dot suggests that only a few of these neutron stars cross the mass threshold to form low-mass black holes. C1 [Oezel, Feryal; Psaltis, Dimitrios; Villarreal, Antonio Santos] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ozel, F (reprint author), Univ Arizona, Dept Astron, 933 N Cherry Ave, Tucson, AZ 85721 USA. OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST-1108753]; NASA ADAP [NNX10AE89G]; NSF CAREER award [NSF 0746549]; Chandra Theory grant [TMO-11003X] FX F.O., D.P., and R.N. thank the Institute of Astronomy, where a large fraction of this work was carried out, for their hospitality. We thank Scott Ransom for useful discussions as well as Ingrid Stairs, Michael Kramer, and Matthew Bailes for detailed comments on the manuscript. We thank Laura Kasian for sharing unpublished data. We gratefully acknowledge support from the NSF grant AST-1108753, the NASA ADAP grant NNX10AE89G, the NSF CAREER award NSF 0746549, and the Chandra Theory grant TMO-11003X for this work. NR 56 TC 85 Z9 87 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 SEP 20 PY 2012 VL 757 IS 1 AR 55 DI 10.1088/0004-637X/757/1/55 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009VG UT WOS:000309052800055 ER PT J AU Jorgensen, JK Favre, C Bisschop, SE Bourke, TL van Dishoeck, EF Schmalzl, M AF Jorgensen, Jes K. Favre, Cecile Bisschop, Suzanne E. Bourke, Tyler L. van Dishoeck, Ewine F. Schmalzl, Markus TI DETECTION OF THE SIMPLEST SUGAR, GLYCOLALDEHYDE, IN A SOLAR-TYPE PROTOSTAR WITH ALMA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE astrobiology; astrochemistry; ISM: abundances; ISM: individual objects (IRAS 16293-2422); ISM: molecules; stars: formation ID MASS STAR-FORMATION; IRAS 16293-2422; GALACTIC-CENTER; HOT CORE; INTERSTELLAR GLYCOLALDEHYDE; MOLECULAR-SPECTROSCOPY; COLOGNE DATABASE; MILLIMETER-WAVE; ETHYLENE-GLYCOL; IRAS-16293-2422 AB Glycolaldehyde (HCOCH2OH) is the simplest sugar and an important intermediate in the path toward forming more complex biologically relevant molecules. In this Letter we present the first detection of 13 transitions of glycolaldehyde around a solar-type young star, through Atacama Large Millimeter Array (ALMA) observations of the Class 0 protostellar binary IRAS 16293-2422 at 220 GHz (6 transitions) and 690 GHz (7 transitions). The glycolaldehyde lines have their origin in warm (200-300 K) gas close to the individual components of the binary. Glycolaldehyde co-exists with its isomer, methyl formate (HCOOCH3), which is a factor 10-15 more abundant toward the two sources. The data also show a tentative detection of ethylene glycol, the reduced alcohol of glycolaldehyde. In the 690 GHz data, the seven transitions predicted to have the highest optical depths based on modeling of the 220 GHz lines all show redshifted absorption profiles toward one of the components in the binary (IRAS 16293B) indicative of infall and emission at the systemic velocity offset from this by about 0 ''.2 (25 AU). We discuss the constraints on the chemical formation of glycolaldehyde and other organic species-in particular, in the context of laboratory experiments of photochemistry of methanol-containing ices. The relative abundances appear to be consistent with UV photochemistry of a CH3OH-CO mixed ice that has undergone mild heating. The order of magnitude increase in line density in these early ALMA data illustrates its huge potential to reveal the full chemical complexity associated with the formation of solar system analogs. C1 [Jorgensen, Jes K.; Bisschop, Suzanne E.] Univ Copenhagen, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.; Bisschop, Suzanne E.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, Jes K.; Bisschop, Suzanne E.] Univ Copenhagen, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Jorgensen, Jes K.; Bisschop, Suzanne E.] Univ Copenhagen, Nat Hist Museum Denmark, DK-1350 Copenhagen K, Denmark. [Favre, Cecile] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, Ewine F.; Schmalzl, Markus] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Jorgensen, JK (reprint author), Univ Copenhagen, Ctr Star & Planet Format, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. EM jeskj@nbi.dk; favre@phys.au.dk; suzanne@snm.ku.dk; tbourke@cfa.harvard.edu; ewine@strw.leidenuniv.nl; schmalzl@strw.leidenuniv.nl RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 FU Spinoza grant from the Netherlands Organization for Scientific Research (NWO); Netherlands Research School in Astronomy (NOVA); EU A-ERC grant [291141]; ALMA Regional Center node Allegro FX Instrument center for Danish Astrophysics (IDA) to Jes Jorgensen. Research at Centre for Star and Planet Formation is funded by the Danish National Research Foundation and the University of Copenhagen's programme of excellence. Astro-chemistry in Leiden is supported by a Spinoza grant from the Netherlands Organization for Scientific Research (NWO), the Netherlands Research School in Astronomy (NOVA), and by EU A-ERC grant 291141 CHEMPLAN. Markus Schmalzl is supported by the ALMA Regional Center node Allegro funded by NWO. NR 35 TC 69 Z9 69 U1 1 U2 35 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2012 VL 757 IS 1 AR L4 DI 10.1088/2041-8205/757/1/L4 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007VQ UT WOS:000308916900004 ER PT J AU Lu, RS Fish, VL Weintroub, J Doeleman, SS Bower, GC Freund, R Friberg, P Ho, PTP Honma, M Inoue, M Krichbaum, TP Marrone, DP Moran, JM Oyama, T Plambeck, R Primiani, R Shen, ZQ Tilanus, RPJ Wright, M Young, KH Ziurys, LM Zensus, JA AF Lu, Ru-Sen Fish, Vincent L. Weintroub, Jonathan Doeleman, Sheperd S. Bower, Geoffrey C. Freund, Robert Friberg, Per Ho, Paul T. P. Honma, Mareki Inoue, Makoto Krichbaum, Thomas P. Marrone, Daniel P. Moran, James M. Oyama, Tomoaki Plambeck, Richard Primiani, Rurik Shen, Zhi-Qiang Tilanus, Remo P. J. Wright, Melvyn Young, Ken H. Ziurys, Lucy M. Zensus, J. Anton TI RESOLVING THE INNER JET STRUCTURE OF 1924-292 WITH THE EVENT HORIZON TELESCOPE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (1924-292); radio continuum: general; techniques: high angular resolution; techniques: interferometric ID ACTIVE GALACTIC NUCLEI; COMPACT RADIO-SOURCES; SAGITTARIUS A-ASTERISK; GHZ VLBI SURVEY; BRIGHTNESS TEMPERATURES; SPECTRA; CATALOG AB We present the first 1.3 mm (230 GHz) very long baseline interferometry model image of an active galactic nucleus (AGN) jet using closure phase techniques with a four-element array. The model image of the quasar 1924-292 was obtained with four telescopes at three observatories: the James Clerk Maxwell Telescope on Mauna Kea in Hawaii, the Arizona Radio Observatory's Submillimeter Telescope in Arizona, and two telescopes of the Combined Array for Research in Millimeter-wave Astronomy in California in 2009 April. With the greatly improved resolution compared with previous observations and robust closure phase measurement, the inner jet structure of 1924-292 was spatially resolved. The inner jet extends to the northwest along a position angle of -53 degrees. at a distance of 0.38 mas from the tentatively identified core, in agreement with the inner jet structure inferred from lower frequencies, and making a position angle difference of similar to 80 degrees with respect to the centimeter jet. The size of the compact core is 0.15 pc with a brightness temperature of 1.2 x 10(11) K. Compared with those measured at lower frequencies, the low brightness temperature may argue in favor of the decelerating jet model or particle-cascade models. The successful measurement of closure phase paves the way for imaging and time resolving Sgr A* and nearby AGNs with the Event Horizon Telescope. C1 [Lu, Ru-Sen; Fish, Vincent L.; Doeleman, Sheperd S.] MIT, Haystack Observ, Westford, MA 01886 USA. [Weintroub, Jonathan; Moran, James M.; Primiani, Rurik; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bower, Geoffrey C.; Plambeck, Richard; Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Dept Astron, Berkeley, CA 94720 USA. [Freund, Robert; Marrone, Daniel P.; Ziurys, Lucy M.] Univ Arizona, Steward Observ, Arizona Radio Observ, Tucson, AZ 85721 USA. [Ho, Paul T. P.; Tilanus, Remo P. J.] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Ho, Paul T. P.; Inoue, Makoto] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Honma, Mareki; Oyama, Tomoaki] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Honma, Mareki] Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Krichbaum, Thomas P.; Zensus, J. Anton] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Shen, Zhi-Qiang] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Shen, Zhi-Qiang] Chinese Acad Sci, Key Lab Radio Astron, Shanghai 200030, Peoples R China. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. RP Lu, RS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM rslu@haystack.mit.edu RI he, shuyi/K-2082-2014; OI Marrone, Daniel/0000-0002-2367-1080; Moran, James/0000-0002-3882-4414 FU National Science Foundation (NSF); NSF University Radio Observatories (URO) program [AST 1140030]; Smithsonian Institution; Academia Sinica; NSF; CARMA partner universities FX We thank the referee for useful comments and suggestions. High-frequency VLBI work at MIT Haystack Observatory is supported by grants from the National Science Foundation (NSF). The Arizona Radio Observatory (ARO) is partially supported through the NSF University Radio Observatories (URO) program under grant No. AST 1140030. 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. Funding for ongoing CARMA development and operations is supported by the NSF and the CARMA partner universities. NR 30 TC 7 Z9 7 U1 0 U2 2 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 SEP 20 PY 2012 VL 757 IS 1 AR L14 DI 10.1088/2041-8205/757/1/L14 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007VQ UT WOS:000308916900014 ER PT J AU Molnar, L Kollath, Z Szabo, R Bryson, S Kolenberg, K Mullally, F Thompson, SE AF Molnar, L. Kollath, Z. Szabo, R. Bryson, S. Kolenberg, K. Mullally, F. Thompson, S. E. TI NONLINEAR ASTEROSEISMOLOGY OF RR LYRAE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: individual (RR Lyr); stars: oscillations; stars: variables: RR Lyrae ID KEPLER; STARS; PULSATION; CEPHEID; MODELS AB The observations of the Kepler Space Telescope revealed that fundamental-mode RR Lyrae stars may show various radial overtones. The presence of multiple radial modes may allow us to conduct nonlinear asteroseismology: comparison of mode amplitudes and frequency shifts between observations and models. Here we report the detection of three radial modes in the star RR Lyr, the eponym of the class, using the Kepler short cadence data: besides the fundamental mode, both the first and the ninth overtones can be derived from the data set. RR Lyrae shows period doubling, but switches occasionally to a state where a pattern of six pulsation cycles repeats instead of two. We found hydrodynamic models that show the same three modes and the period-six state, allowing for comparison with the observations. C1 [Molnar, L.; Kollath, Z.; Szabo, R.] MTA CSFK, Konkoly Observ, H-1121 Budapest, Hungary. [Bryson, S.; Mullally, F.; Thompson, S. E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Astron, B-3001 Heverlee, Belgium. [Mullally, F.; Thompson, S. E.] SETI Inst, Mountain View, CA 94043 USA. RP Molnar, L (reprint author), MTA CSFK, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary. EM molnar.laszlo@csfk.mta.hu OI Szabo, Robert/0000-0002-3258-1909; Molnar, Laszlo/0000-0002-8159-1599 FU NASA's Science Mission Directorate; Hungarian OTKA [K83790, K81421, MB08C 81013]; "Lendulet" programme, and the European Community's Seventh Framework Programme (FP7) [269194]; Hungarian Academy of Sciences; Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme; National Science Foundation [NSF PHY05-51164] FX Funding for this Discovery Mission is provided by NASA's Science Mission Directorate. The Kepler Team and the Kepler Guest Observer Office are recognized for helping to make the mission and these data possible. This work was supported by the Hungarian OTKA grants K83790, K81421, and MB08C 81013, as well as the "Lendulet" programme, and the European Community's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 269194. R.Sz. acknowledges the Bolyai Janos Scholarship of the Hungarian Academy of Sciences. K.K. is supported by a Marie Curie International Outgoing Fellowship within the 7th European Community Framework Programme. R.Sz. and K.K. warmly thank the KITP staff of UCSB for their hospitality during the "Asteroseismology in the Space Age" programme. This research was supported in part by the National Science Foundation under grant No. NSF PHY05-51164. NR 23 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 20 PY 2012 VL 757 IS 1 AR L13 DI 10.1088/2041-8205/757/1/L13 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 007VQ UT WOS:000308916900013 ER PT J AU Lyons, DC Perry, KJ Lesoway, MP Henry, JQ AF Lyons, Deirdre C. Perry, Kimberly J. Lesoway, Maryna P. Henry, Jonathan Q. TI Cleavage pattern and fate map of the mesentoblast, 4d, in the gastropod Crepidula: a hallmark of spiralian development SO EVODEVO LA English DT Article ID DENTALIUM-DENTALE SCAPHOPODA; TURBELLARIAN HOPLOPLANA-INQUILINA; OLIGOCHAETE ANNELID TUBIFEX; LATE LARVAL DEVELOPMENT; POSTERIOR GROWTH ZONE; PRIMORDIAL GERM-CELLS; SOMATIC STEM-CELLS; POLAR LOBE; ILYANASSA-OBSOLETA; DIVISION CHRONOLOGY AB Background: Animals with a spiral cleavage program, such as mollusks and annelids, make up the majority of the superphylum Lophotrochozoa. The great diversity of larval and adult body plans in this group emerges from this highly conserved developmental program. The 4d micromere is one of the most conserved aspects of spiralian development. Unlike the preceding pattern of spiral divisions, cleavages within the 4d teloblastic sublineages are bilateral, representing a critical transition towards constructing the bilaterian body plan. These cells give rise to the visceral mesoderm in virtually all spiralians examined and in many species they also contribute to the endodermal intestine. Hence, the 4d lineage is an ideal one for studying the evolution and diversification of the bipotential endomesodermal germ layer in protostomes at the level of individual cells. Little is known of how division patterns are controlled or how mesodermal and endodermal sublineages diverge in spiralians. Detailed modern fate maps for 4d exist in only a few species of clitellate annelids, specifically in glossiphoniid leeches and the sludge worm Tubifex. We investigated the 4d lineage in the gastropod Crepidula fornicata, an established model system for spiralian biology, and in a closely related direct-developing species, C. convexa. Results: High-resolution cell lineage tracing techniques were used to study the 4d lineage of C. fornicata and C. convexa. We present a new nomenclature to name the progeny of 4d, and report the fate map for the sublineages up through the birth of the first five pairs of teloblast daughter cells (when 28 cells are present in the 4d sublineage), and describe each clone's behavior during gastrulation and later stages as these undergo differentiation. We identify the precise origin of the intestine, two cells of the larval kidney complex, the larval retractor muscles and the presumptive germ cells, among others. Other tissues that arise later in the 4d lineage include the adult heart, internal foot tissues, and additional muscle and mesenchymal cells derived from later-born progeny of the left and right teloblasts. To test whether other cells can compensate for the loss of these tissues (that is, undergo regulation), specific cells were ablated in C. fornicata. Conclusions: Our results present the first fate map of the 4d micromere sublineages in a mollusk. The fate map reveals that endodermal and mesodermal fates segregate much later than previously thought. We observed little evidence of regulation between sublineages, consistent with a lineage-driven cell specification process. Our results provide a framework for comparisons with other spiralians and lay the groundwork for investigation of the molecular mechanisms of endomesoderm formation, germ line segregation and bilateral differentiation in Crepidula. C1 [Perry, Kimberly J.; Henry, Jonathan Q.] Univ Illinois, Dept Cell & Dev Biol, Urbana, IL 61801 USA. [Lyons, Deirdre C.] Duke Univ, Dept Biol, Durham, NC 27705 USA. [Lesoway, Maryna P.] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Lesoway, Maryna P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Henry, JQ (reprint author), Univ Illinois, Dept Cell & Dev Biol, 601 S Goodwin Ave, Urbana, IL 61801 USA. EM j-henry4@illinois.edu FU EDENRCN; NSF [105-0955517]; National Science Foundation [1121268] FX The authors thank the community of the Marine Biological Laboratory and especially Drs. Nipam Patel and Lee Niswander for their support. The authors also acknowledge generous assistance and advice from Hamilton-Thorne. DCL thanks DR McClay for his support. Professional Development for MPL was partially supported by EDENRCN, NSF Grant #105-0955517. This material is based upon work supported by the National Science Foundation under Grant No. 1121268 to JQH (JJH). Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation. NR 115 TC 25 Z9 25 U1 1 U2 14 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 2041-9139 J9 EVODEVO JI EvoDevo PD SEP 19 PY 2012 VL 3 AR 21 DI 10.1186/2041-9139-3-21 PG 26 WC Evolutionary Biology; Developmental Biology SC Evolutionary Biology; Developmental Biology GA 047FH UT WOS:000311822800001 PM 22992254 ER PT J AU Gotzek, D Brady, SG Kallal, RJ LaPolla, JS AF Gotzek, Dietrich Brady, Sean G. Kallal, Robert J. LaPolla, John S. TI The Importance of Using Multiple Approaches for Identifying Emerging Invasive Species: The Case of the Rasberry Crazy Ant in the United States SO PLOS ONE LA English DT Article ID NYLANDERIA HYMENOPTERA-FORMICIDAE; BAYESIAN PHYLOGENETIC INFERENCE; BIOLOGICAL INVASIONS; SOLENOPSIS-INVICTA; ARGENTINE ANTS; MOLECULAR SYSTEMATICS; POPULATION-GENETICS; MAXIMUM-LIKELIHOOD; GLOBAL CHANGE; FIRE ANTS AB In the past decade, Houston, Texas has been virtually overrun by an unidentified ant species, the sudden appearance and enormous population sizes and densities of which have received national media attention. The Rasberry Crazy Ant, as it has become known due to its uncertain species status, has since spread to neighboring states and is still a major concern to pest control officials. Previous attempts at identifying this species have resulted in widely different conclusions in regards to its native range, source, and biology. We identify this highly invasive pest species as Nylanderia fulva (Mayr) using morphometric data measured from 14 characters, molecular sequence data consisting of 4,669 aligned nucleotide sites from six independent loci and comparison with type specimens. This identification will allow for the study and control of this emerging pest species to proceed unencumbered by taxonomic uncertainty. We also show that N. fulva has a much wider distribution than previously thought and has most likely invaded all of the Gulf Coast states. C1 [Kallal, Robert J.; LaPolla, John S.] Towson Univ, Dept Biol Sci, Towson, MD 21252 USA. [Gotzek, Dietrich; Brady, Sean G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP LaPolla, JS (reprint author), Towson Univ, Dept Biol Sci, Towson, MD 21252 USA. EM JLapolla@towson.edu FU National Science Foundation [DEB-0743542] FX This research was supported by the National Science Foundation under grant DEB-0743542 awarded to S.G.B. and J.S.L. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 75 TC 26 Z9 30 U1 10 U2 77 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 19 PY 2012 VL 7 IS 9 AR e45314 DI 10.1371/journal.pone.0045314 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 014PP UT WOS:000309388400072 PM 23056657 ER PT J AU Hong, T AF Hong, Terry TI The Garden of Evening Mists 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 2 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 SEP 15 PY 2012 VL 137 IS 15 BP 64 EP 65 PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 008PU UT WOS:000308969800085 ER PT J AU Riley, S AF Riley, Sheila TI The Accomplice 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 SEP 15 PY 2012 VL 137 IS 15 BP 64 EP 64 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 008PU UT WOS:000308969800082 ER PT J AU Tscherbul, TV Grinev, TA Yu, HG Dalgarno, A Klos, J Ma, LF Alexander, MH AF Tscherbul, T. V. Grinev, T. A. Yu, H. -G. Dalgarno, A. Klos, Jacek Ma, Lifang Alexander, Millard H. TI Cold collisions of polyatomic molecular radicals with S-state atoms in a magnetic field: An ab initio study of He + CH2((X)over-tilde) collisions SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID RESONANCE-SPECTROSCOPY; ROTATIONAL-EXCITATION; AMMONIA MOLECULES; WAVE-FUNCTIONS; BASIS-SETS; SPIN; DEPOLARIZATION; TEMPERATURES; CONVERSION; METHYLENE AB We develop a rigorous quantum mechanical theory for collisions of polyatomic molecular radicals with S-state atoms in the presence of an external magnetic field. The theory is based on a fully uncoupled space-fixed basis set representation of the multichannel scattering wave function. Explicit expressions are presented for the matrix elements of the scattering Hamiltonian for spin-1/2 and spin-1 polyatomic molecular radicals interacting with structureless targets. The theory is applied to calculate the cross sections and thermal rate constants for spin relaxation in low-temperature collisions of the prototypical organic molecule methylene [CH2((S) over tilde (3) B-1)] with He atoms. To this end, two accurate three-dimensional potential energy surfaces (PESs) of the He-CH2((X) over tilde (3) B-1) complex are developed using the state-of-the-art coupled-cluster method including single and double excitations along with a perturbative correction for triple excitations and large basis sets. Both PESs exhibit shallow minima and are weakly anisotropic. Our calculations show that spin relaxation in collisions of CH2, CHD, and CD2 molecules with He atoms occurs at a much slower rate than elastic scattering over a large range of temperatures (1 mu K-1 K) and magnetic fields (0.01-1 T), suggesting excellent prospects for cryogenic helium buffer-gas cooling of ground-state ortho-CH2((X) over tilde (3) B-1) molecules in a magnetic trap. Furthermore, we find that ortho-CH2 undergoes collision-induced spin relaxation much more slowly than para-CH2, which indicates that magnetic trapping can be used to separate nuclear spin isomers of open-shell polyatomic molecules. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4748258] C1 [Tscherbul, T. V.; Grinev, T. A.] Univ Toronto, Dept Chem, Chem Phys Theory Grp, Toronto, ON M5S 3H6, Canada. [Yu, H. -G.] Brookhaven Natl Lab, Dept Chem, Upton, NY 11973 USA. [Dalgarno, A.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Dalgarno, A.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Klos, Jacek; Ma, Lifang; Alexander, Millard H.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Alexander, Millard H.] Univ Maryland, Inst Phys Sci & Technol, College Pk, MD 20742 USA. RP Tscherbul, TV (reprint author), Univ Toronto, Dept Chem, Chem Phys Theory Grp, Toronto, ON M5S 3H6, Canada. EM ttscherb@chem.utoronto.ca RI Tscherbul, Timur/K-3286-2014; Klos, Jacek/A-6457-2008; Yu, Hua-Gen/N-7339-2015 OI Tscherbul, Timur/0000-0001-5689-040X; Klos, Jacek/0000-0002-7407-303X; FU U.S. Department of Energy (DOE) Office of Basic Energy Science; National Science Foundation (NSF) [CHE-0848110, CHE-1213332] FX We thank Gregory E. Hall, John M. Doyle, and Paul J. Dagdigian for discussions and Roman Krems for helpful comments on the manuscript. This work was supported by the U.S. Department of Energy (DOE) Office of Basic Energy Science and the National Science Foundation (NSF) grants to the Harvard-MIT Center for Ultracold Atoms (CUA) and Institute for Theoretical Atomic, Molecular and Optical Physics (ITAMP) at Harvard University and the Smithsonian Astrophysical Observatory as well as to M. H. A. at the University of Maryland (Grant Nos. CHE-0848110 and CHE-1213332). NR 78 TC 6 Z9 6 U1 0 U2 17 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 0021-9606 EI 1089-7690 J9 J CHEM PHYS JI J. Chem. Phys. PD SEP 14 PY 2012 VL 137 IS 10 AR 104302 DI 10.1063/1.4748258 PG 14 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 010NF UT WOS:000309100400014 PM 22979854 ER PT J AU Morrow, KM Ritson-Williams, R Ross, C Liles, MR Paul, VJ AF Morrow, Kathleen M. Ritson-Williams, Raphael Ross, Cliff Liles, Mark R. Paul, Valerie J. TI Macroalgal Extracts Induce Bacterial Assemblage Shifts and Sublethal Tissue Stress in Caribbean Corals SO PLOS ONE LA English DT Article ID 16S RIBOSOMAL-RNA; ANTIFUNGAL CHEMICAL DEFENSE; LONG-TERM DYNAMICS; BROWN ALGA; HARD CORAL; ANTIMICROBIAL ACTIVITIES; SECONDARY METABOLITES; MICROBIAL-POPULATIONS; SURFACE COLONIZATION; CELLULAR DIAGNOSTICS AB Benthic macroalgae can be abundant on present-day coral reefs, especially where rates of herbivory are low and/or dissolved nutrients are high. This study investigated the impact of macroalgal extracts on both coral-associated bacterial assemblages and sublethal stress response of corals. Crude extracts and live algal thalli from common Caribbean macroalgae were applied onto the surface of Montastraea faveolata and Porites astreoides corals on reefs in both Florida and Belize. Denaturing gradient gel electrophoresis (DGGE) of 16S rRNA gene amplicons was used to examine changes in the surface mucus layer (SML) bacteria in both coral species. Some of the extracts and live algae induced detectable shifts in coral-associated bacterial assemblages. However, one aqueous extract caused the bacterial assemblages to shift to an entirely new state (Lobophora variegata), whereas other organic extracts had little to no impact (e.g. Dictyota sp.). Macroalgal extracts more frequently induced sublethal stress responses in M. faveolata than in P. astreoides corals, suggesting that cellular integrity can be negatively impacted in selected corals when comparing co-occurring species. As modern reefs experience phase-shifts to a higher abundance of macroalgae with potent chemical defenses, these macroalgae are likely impacting the composition of microbial assemblages associated with corals and affecting overall reef health in unpredicted and unprecedented ways. C1 [Morrow, Kathleen M.; Liles, Mark R.] Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. [Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Inst, Smithsonian Marine Stn, Ft Pierce, FL USA. [Ross, Cliff] Univ N Florida, Dept Biol, Jacksonville, FL USA. RP Morrow, KM (reprint author), Auburn Univ, Dept Biol Sci, Auburn, AL 36849 USA. EM morrow.kathleen@gmail.com RI Ross, Cliff/B-8291-2011 FU National Oceanic and Atmospheric Administration National Marine Sanctuary Program Nancy Foster Scholarship [NA08NOS4290448]; Mote Protect our Reefs grant [POR-2009-16] FX Daily stipend and tuition support to KMM from National Oceanic and Atmospheric Administration National Marine Sanctuary Program Nancy Foster Scholarship #NA08NOS4290448. http://fosterscholars.noaa.gov/aboutscholarship.html. Mote Protect our Reefs grant #POR-2009-16; supported travel to field sites and stress enzyme analysis. http://www.mote.org/index.php? src = gendocs&link = Reefplategrantapp&category = Main. The Hunterdon Oceanographic Research Fund and the Smithsonian Caribbean Coral Reef Ecosystems Program supported field work at Carrie Bow Cay Field Station. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 72 TC 22 Z9 22 U1 0 U2 47 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 13 PY 2012 VL 7 IS 9 AR e44859 DI 10.1371/journal.pone.0044859 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 005ZK UT WOS:000308788700046 PM 23028648 ER PT J AU Laurance, WF Useche, DC Rendeiro, J Kalka, M Bradshaw, CJA Sloan, SP Laurance, SG Campbell, M Abernethy, K Alvarez, P Arroyo-Rodriguez, V Ashton, P Benitez-Malvido, J Blom, A Bobo, KS Cannon, CH Cao, M Carroll, R Chapman, C Coates, R Cords, M Danielsen, F De Dijn, B Dinerstein, E Donnelly, MA Edwards, D Edwards, F Farwig, N Fashing, P Forget, PM Foster, M Gale, G Harris, D Harrison, R Hart, J Karpanty, S Kress, WJ Krishnaswamy, J Logsdon, W Lovett, J Magnusson, W Maisels, F Marshall, AR McClearn, D Mudappa, D Nielsen, MR Pearson, R Pitman, N van der Ploeg, J Plumptre, A Poulsen, J Quesada, M Rainey, H Robinson, D Roetgers, C Rovero, F Scatena, F Schulze, C Sheil, D Struhsaker, T Terborgh, J Thomas, D Timm, R Urbina-Cardona, JN Vasudevan, K Wright, SJ Arias-G, JC Arroyo, L Ashton, M Auzel, P Babaasa, D Babweteera, F Baker, P Banki, O Bass, M Bila-Isia, I Blake, S Brockelman, W Brokaw, N Bruhl, CA Bunyavejchewin, S Chao, JT Chave, J Chellam, R Clark, CJ Clavijo, J Congdon, R Corlett, R Dattaraja, HS Dave, C Davies, G Beisiegel, BD da Silva, RD Di Fiore, A Diesmos, A Dirzo, R Doran-Sheehy, D Eaton, M Emmons, L Estrada, A Ewango, C Fedigan, L Feer, F Fruth, B Willis, JG Goodale, U Goodman, S Guix, JC Guthiga, P Haber, W Hamer, K Herbinger, I Hill, J Huang, ZL Sun, IF Ickes, K Itoh, A Ivanauskas, N Jackes, B Janovec, J Janzen, D Jiangming, M Jin, C Jones, T Justiniano, H Kalko, E Kasangaki, A Killeen, T King, HB Klop, E Knott, C Kone, I Kudavidanage, E Ribeiro, JLD Lattke, J Laval, R Lawton, R Leal, M Leighton, M Lentino, M Leonel, C Lindsell, J Ling-Ling, L Linsenmair, KE Losos, E Lugo, A Lwanga, J Mack, AL Martins, M McGraw, WS McNab, R Montag, L Thompson, JM Nabe-Nielsen, J Nakagawa, M Nepal, S Norconk, M Novotny, V O'Donnell, S Opiang, M Ouboter, P Parker, K Parthasarathy, N Pisciotta, K Prawiradilaga, D Pringle, C Rajathurai, S Reichard, U Reinartz, G Renton, K Reynolds, G Reynolds, V Riley, E Rodel, MO Rothman, J Round, P Sakai, S Sanaiotti, T Savini, T Schaab, G Seidensticker, J Siaka, A Silman, MR Smith, TB de Almeida, SS Sodhi, N Stanford, C Stewart, K Stokes, E Stoner, KE Sukumar, R Surbeck, M Tobler, M Tscharntke, T Turkalo, A Umapathy, G van Weerd, M Rivera, JV Venkataraman, M Venn, L Verea, C de Castilho, CV Waltert, M Wang, B Watts, D Weber, W West, P Whitacre, D Whitney, K Wilkie, D Williams, S Wright, DD Wright, P Xiankai, L Yonzon, P Zamzani, F AF Laurance, William F. Useche, D. Carolina Rendeiro, Julio Kalka, Margareta Bradshaw, Corey J. A. Sloan, Sean P. Laurance, Susan G. Campbell, Mason Abernethy, Kate Alvarez, Patricia Arroyo-Rodriguez, Victor Ashton, Peter Benitez-Malvido, Julieta Blom, Allard Bobo, Kadiri S. Cannon, Charles H. Cao, Min Carroll, Richard Chapman, Colin Coates, Rosamond Cords, Marina Danielsen, Finn De Dijn, Bart Dinerstein, Eric Donnelly, Maureen A. Edwards, David Edwards, Felicity Farwig, Nina Fashing, Peter Forget, Pierre-Michel Foster, Mercedes Gale, George Harris, David Harrison, Rhett Hart, John Karpanty, Sarah Kress, W. John Krishnaswamy, Jagdish Logsdon, Willis Lovett, Jon Magnusson, William Maisels, Fiona Marshall, Andrew R. McClearn, Deedra Mudappa, Divya Nielsen, Martin R. Pearson, Richard Pitman, Nigel van der Ploeg, Jan Plumptre, Andrew Poulsen, John Quesada, Mauricio Rainey, Hugo Robinson, Douglas Roetgers, Christiane Rovero, Francesco Scatena, Frederick Schulze, Christian Sheil, Douglas Struhsaker, Thomas Terborgh, John Thomas, Duncan Timm, Robert Urbina-Cardona, J. Nicolas Vasudevan, Karthikeyan Wright, S. Joseph Arias-G, Juan Carlos Arroyo, Luzmila Ashton, Mark Auzel, Philippe Babaasa, Dennis Babweteera, Fred Baker, Patrick Banki, Olaf Bass, Margot Bila-Isia, Inogwabini Blake, Stephen Brockelman, Warren Brokaw, Nicholas Bruehl, Carsten A. Bunyavejchewin, Sarayudh Chao, Jung-Tai Chave, Jerome Chellam, Ravi Clark, Connie J. Clavijo, Jose Congdon, Robert Corlett, Richard Dattaraja, H. S. Dave, Chittaranjan Davies, Glyn Beisiegel, Beatriz de Mello da Silva, Rosa de Nazarepaes Di Fiore, Anthony Diesmos, Arvin Dirzo, Rodolfo Doran-Sheehy, Diane Eaton, Mitchell Emmons, Louise Estrada, Alejandro Ewango, Corneille Fedigan, Linda Feer, Francois Fruth, Barbara Willis, Jacalyn Giacalone Goodale, Uromi Goodman, Steven Guix, Juan C. Guthiga, Paul Haber, William Hamer, Keith Herbinger, Ilka Hill, Jane Huang, Zhongliang Sun, I. Fang Ickes, Kalan Itoh, Akira Ivanauskas, Natalia Jackes, Betsy Janovec, John Janzen, Daniel Jiangming, Mo Jin, Chen Jones, Trevor Justiniano, Hermes Kalko, Elisabeth Kasangaki, Aventino Killeen, Timothy King, Hen-biau Klop, Erik Knott, Cheryl Kone, Inza Kudavidanage, Enoka Ribeiro, Jose Lahoz da Silva Lattke, John Laval, Richard Lawton, Robert Leal, Miguel Leighton, Mark Lentino, Miguel Leonel, Cristiane Lindsell, Jeremy Ling-Ling, Lee Linsenmair, K. Eduard Losos, Elizabeth Lugo, Ariel Lwanga, Jeremiah Mack, Andrew L. Martins, Marlucia McGraw, W. Scott McNab, Roan Montag, Luciano Thompson, Jo Myers Nabe-Nielsen, Jacob Nakagawa, Michiko Nepal, Sanjay Norconk, Marilyn Novotny, Vojtech O'Donnell, Sean Opiang, Muse Ouboter, Paul Parker, Kenneth Parthasarathy, N. Pisciotta, Katia Prawiradilaga, Dewi Pringle, Catherine Rajathurai, Subaraj Reichard, Ulrich Reinartz, Gay Renton, Katherine Reynolds, Glen Reynolds, Vernon Riley, Erin Roedel, Mark-Oliver Rothman, Jessica Round, Philip Sakai, Shoko Sanaiotti, Tania Savini, Tommaso Schaab, Gertrud Seidensticker, John Siaka, Alhaji Silman, Miles R. Smith, Thomas B. de Almeida, Samuel Soares Sodhi, Navjot Stanford, Craig Stewart, Kristine Stokes, Emma Stoner, Kathryn E. Sukumar, Raman Surbeck, Martin Tobler, Mathias Tscharntke, Teja Turkalo, Andrea Umapathy, Govindaswamy van Weerd, Merlijn Rivera, Jorge Vega Venkataraman, Meena Venn, Linda Verea, Carlos de Castilho, Carolina Volkmer Waltert, Matthias Wang, Benjamin Watts, David Weber, William West, Paige Whitacre, David Whitney, Ken Wilkie, David Williams, Stephen Wright, Debra D. Wright, Patricia Xiankai, Lu Yonzon, Pralad Zamzani, Franky TI Averting biodiversity collapse in tropical forest protected areas SO NATURE LA English DT Article ID CLIMATE-CHANGE; EXTINCTION; FRAGMENTS; DEFORESTATION; RESERVES; AMAZON; WORLD AB The rapid disruption of tropical forests probably imperils global biodiversity more than any other contemporary phenomenon(1-3). With deforestation advancing quickly, protected areas are increasingly becoming final refuges for threatened species and natural ecosystem processes. However, many protected areas in the tropics are themselves vulnerable to human encroachment and other environmental stresses(4-9). As pressures mount, it is vital to know whether existing reserves can sustain their biodiversity. A critical constraint in addressing this question has been that data describing a broad array of biodiversity groups have been unavailable for a sufficiently large and representative sample of reserves. Here we present a uniquely comprehensive data set on changes over the past 20 to 30 years in 31 functional groups of species and 21 potential drivers of environmental change, for 60 protected areas stratified across the world's major tropical regions. Our analysis reveals great variation in reserve 'health': about half of all reserves have been effective or performed passably, but the rest are experiencing an erosion of biodiversity that is often alarmingly widespread taxonomically and functionally. Habitat disruption, hunting and forest-product exploitation were the strongest predictors of declining reserve health. Crucially, environmental changes immediately outside reserves seemed nearly as important as those inside in determining their ecological fate, with changes inside reserves strongly mirroring those occurring around them. These findings suggest that tropical protected areas are often intimately linked ecologically to their surrounding habitats, and that a failure to stem broad-scale loss and degradation of such habitats could sharply increase the likelihood of serious biodiversity declines. C1 [Laurance, William F.; Sloan, Sean P.; Laurance, Susan G.; Campbell, Mason; Edwards, David; Edwards, Felicity; Logsdon, Willis; Roetgers, Christiane] James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4878, Australia. [Laurance, William F.; Sloan, Sean P.; Laurance, Susan G.; Campbell, Mason; Edwards, David; Edwards, Felicity; Logsdon, Willis; Roetgers, Christiane] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [Laurance, William F.; Useche, D. Carolina; Rendeiro, Julio; Kalka, Margareta; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Bradshaw, Corey J. A.] Univ Adelaide, Sch Earth & Environm Sci, Adelaide, SA 5005, Australia. [Abernethy, Kate; Maisels, Fiona] Univ Stirling, Stirling FK9 4LA, Scotland. [Alvarez, Patricia; Pitman, Nigel; Struhsaker, Thomas; Terborgh, John; Clark, Connie J.] Duke Univ, Durham, NC 27705 USA. [Arroyo-Rodriguez, Victor; Benitez-Malvido, Julieta; Quesada, Mauricio] UNAM, Morelia, Michoacan, Mexico. [Ashton, Peter] Royal Bot Gardens, Richmond TW9 3AB, Surrey, England. [Blom, Allard; Carroll, Richard; Dinerstein, Eric; Itoh, Akira] World Wildlife Fund WWF, Washington, DC 20037 USA. [Bobo, Kadiri S.] Univ Dschang, Dschang, Cameroon. [Cannon, Charles H.; Cao, Min; Harrison, Rhett; Jin, Chen] Xishuangbanna Trop Bot Garden, Yunnan 666303, Peoples R China. [Chapman, Colin; Auzel, Philippe] McGill Univ, Montreal, PQ H3A 2T7, Canada. [Coates, Rosamond; Estrada, Alejandro] Univ Nacl Autonoma Mexico, Estn Biol Trop Los Tuxtlas, Veracruz 95701, Mexico. [Cords, Marina; West, Paige] Columbia Univ, New York, NY 10027 USA. [Danielsen, Finn] Nord Fdn Dev & Ecol, DK-1159 Copenhagen, Denmark. [De Dijn, Bart] Bart De Dijn Environm Consultancy, Paramaribo, Surinam. [Donnelly, Maureen A.] Florida Int Univ, Miami, FL 33199 USA. [Farwig, Nina] Univ Marburg, D-35043 Marburg, Germany. [Fashing, Peter] Calif State Univ Fullerton, Fullerton, CA 92834 USA. [Forget, Pierre-Michel; Feer, Francois] Museum Natl Hist Nat, F-91800 Brunoy, France. [Foster, Mercedes] US Geol Survey, Smithsonian Inst, Washington, DC 20013 USA. [Gale, George; Savini, Tommaso] King Mongkuts Univ Technol Thonburi, Bangkok 10150, Thailand. [Harris, David] Royal Bot Garden, Edinburgh EH3 5LR, Midlothian, Scotland. [Hart, John] Tshuapa Lomami Lualaba Project, Kinshasa, Congo. [Karpanty, Sarah] Virginia Tech Univ, Blacksburg, VA 24061 USA. [Kress, W. John; Emmons, Louise] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Krishnaswamy, Jagdish] Ashoka Trust Res Ecol & Environm ATREE, Bangalore 560064, Karnataka, India. [Lovett, Jon] Univ Twente, NL-7500 AE Enschede, Netherlands. [Magnusson, William; Sanaiotti, Tania] INPA, BR-69011970 Manaus, Amazonas, Brazil. [Maisels, Fiona; Rainey, Hugo; Blake, Stephen; Stokes, Emma; Weber, William; Wilkie, David] Wildlife Conservat Soc, Bronx, NY 10460 USA. [Marshall, Andrew R.; Hill, Jane] Univ York, York YO10 5DD, N Yorkshire, England. [McClearn, Deedra] La Selva Biol Stn, San Pedro, Costa Rica. [Mudappa, Divya] Nat Conservat Fdn, Mysore 570002, Karnataka, India. [Nielsen, Martin R.] Univ Copenhagen, Copenhagen, Denmark. [Pearson, Richard; Congdon, Robert; Jackes, Betsy; Williams, Stephen] James Cook Univ, Townsville, Qld 4811, Australia. [van der Ploeg, Jan; van Weerd, Merlijn] Leiden Univ, Leiden, Netherlands. [Plumptre, Andrew] Wildlife Conservat Soc, Kampala, Uganda. [Poulsen, John] Woods Hole Res Ctr, Falmouth, MA 02540 USA. [Robinson, Douglas; Thomas, Duncan] Oregon State Univ, Corvallis, OR 97331 USA. [Rovero, Francesco] Museo Sci, I-38122 Trento, Italy. [Scatena, Frederick; Janzen, Daniel] Univ Penn, Philadelphia, PA 19104 USA. [Schulze, Christian] Univ Vienna, A-1030 Vienna, Austria. [Sheil, Douglas] Bwindi Impenetrable Natl Pk, Kabale, Uganda. [Timm, Robert] Univ Kansas, Lawrence, KS 66045 USA. [Urbina-Cardona, J. Nicolas] Pontificia Univ Javeriana, Bogota, Colombia. [Vasudevan, Karthikeyan] Wildlife Inst India, Dehra Dun, India. [Arias-G, Juan Carlos] Unidad Parques Nacl Nat Colombia, Bogota, Colombia. 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[Clavijo, Jose] Cent Univ Venezuela, Aragua, Venezuela. [Corlett, Richard; Kudavidanage, Enoka; Sodhi, Navjot] Natl Univ Singapore, Singapore 117543, Singapore. [Dattaraja, H. S.] Indian Inst Sci, Bangalore 560012, Karnataka, India. [Dave, Chittaranjan] World Wide Fund Nat WWF, New Delhi 110003, India. [Davies, Glyn] World Wide Fund Nat WWF, Surrey GU7 1XR, England. [Beisiegel, Beatriz de Mello] Inst Chico Mendes Conservacao Biodiversidade, BR-12952011 Sao Paulo, Brazil. [da Silva, Rosa de Nazarepaes] Conselho Reg Engn Arquitetura & Agron Para, Belem, Para, Brazil. [Di Fiore, Anthony] Univ Texas Austin, Austin, TX 78712 USA. [Diesmos, Arvin] Natl Museum Philippines, Manila, Philippines. [Dirzo, Rodolfo] Stanford Univ, Stanford, CA 94305 USA. [Eaton, Mitchell] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Eaton, Mitchell] Univ Colorado, Boulder, CO 80309 USA. [Ewango, Corneille] Wildlife Conservat Soc, Kinshasa, Congo. [Fedigan, Linda] Univ Calgary, Calgary, AB T2N 1N4, Canada. [Fruth, Barbara; Surbeck, Martin] Max Planck Inst Evolutionary Anthropol, Leipzig, Germany. [Willis, Jacalyn Giacalone] Montclair State Univ, Montclair, NJ 07043 USA. [Goodale, Uromi] Univ Calif San Diego, San Diego, CA 92093 USA. [Goodman, Steven] Field Museum Nat Hist, Chicago, IL 60605 USA. [Guix, Juan C.] Univ Barcelona, E-08028 Barcelona, Spain. [Guthiga, Paul] Kenya Inst Publ Policy Res & Anal, Nairobi, Kenya. [Haber, William; Sun, I. Fang] Missouri Bot Garden, St Louis, MO 63166 USA. [Hamer, Keith] Univ Leeds, Leeds LS2 9JT, W Yorkshire, England. [Herbinger, Ilka] Wild Chimpanzee Fdn, Abidjan 23, Cote Ivoire. [Huang, Zhongliang] Dinghushan Biosphere Reserve, Zhaoqing, Peoples R China. Tunghai Univ, Taichung 407, Taiwan. [Ickes, Kalan] Clemson Univ, Clemson, SC 29634 USA. [Itoh, Akira] Osaka City Univ, Osaka 5588585, Japan. [Ivanauskas, Natalia] Inst Florestal, BR-02377000 Sao Paulo, Brazil. [Janovec, John; Tobler, Mathias] Bot Res Inst Texas, Ft Worth, TX 76107 USA. [Jiangming, Mo; Xiankai, Lu] S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Jones, Trevor] Anglia Ruskin Univ, Cambridge CB1 1PT, England. [Justiniano, Hermes] Fdn Conservac Bosque, Chiquitano, Bolivia. [Kalko, Elisabeth] Univ Ulm, D-89069 Ulm, Germany. [Kasangaki, Aventino] Mbarara Univ Sci & Technol, Mbarara, Uganda. [Killeen, Timothy] Conservat Int, Arlington, VA 22202 USA. [King, Hen-biau] Soc Subtrop Ecol, Taipei, Taiwan. [Klop, Erik] Royal Haskoning Water & Ecol Grp, Groningen, Netherlands. [Knott, Cheryl] Boston Univ, Boston, MA 02215 USA. [Kone, Inza] Ctr Suisse Rech Sci Cote Ivoire, Abidjan, Cote Ivoire. [Ribeiro, Jose Lahoz da Silva] Univ Estadual Londrina, Londrina, Parana, Brazil. [Lattke, John] Cent Univ Venezuela, Caracas, Venezuela. [Laval, Richard] Bat Jungle, Monteverde, Costa Rica. [Lawton, Robert] Univ Alabama, Huntsville, AL 35899 USA. [Lentino, Miguel] Colecc Ornitol Phelps, Caracas, Venezuela. [Leonel, Cristiane] Parque Estadual Horto Florestal, BR-02377000 Sao Paulo, Brazil. [Lindsell, Jeremy] Royal Soc Protect Birds, Sandy SG19 2DL, Beds, England. [Ling-Ling, Lee] Natl Taiwan Univ, Taipei 10764, Taiwan. [Linsenmair, K. Eduard] Univ Wurzburg, D-97074 Wurzburg, Germany. [Losos, Elizabeth] Org Trop Studies, Durham, NC 27705 USA. [Lugo, Ariel] USDA Int Inst Trop Forestry, Rio Piedras, PR 00926 USA. [Lwanga, Jeremiah] Makerere Univ, Kampala, Uganda. [Mack, Andrew L.; Wright, Debra D.] Green Capac Inc, New Florence, PA 15944 USA. [Martins, Marlucia] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [McGraw, W. Scott] Ohio State Univ, Columbus, OH 43210 USA. [McNab, Roan] Wildlife Conservat Soc, Flores, Guatemala. [Montag, Luciano] Fed Univ Para, BR-66040170 Belem, Para, Brazil. [Thompson, Jo Myers] Lukuru Wildlife Res Fdn, Kinshasa, Congo. [Nabe-Nielsen, Jacob] Aarhus Univ, DK-4000 Roskilde, Denmark. [Nepal, Sanjay] Univ Waterloo, Waterloo, ON N2L 3G1, Canada. [Nakagawa, Michiko] Nagoya Univ, Nagoya, Aichi 4648601, Japan. [Novotny, Vojtech] Acad Sci Czech Republic, Inst Entomol, CR-37005 Ceske Budejovice, Czech Republic. [O'Donnell, Sean] Univ Washington, Seattle, WA 98195 USA. [Opiang, Muse] PNG Inst Biol Res, Goroka, Papua N Guinea. [Ouboter, Paul] Univ Suriname, Paramaribo, Surinam. [Parthasarathy, N.] Pondicherry Univ, Pondicherry 605014, India. [Pisciotta, Katia] Fundacao Florestal, BR-02377000 Sao Paulo, Brazil. [Prawiradilaga, Dewi] Res Ctr Biol, Cibinong 16911, Indonesia. [Pringle, Catherine] Univ Georgia, Athens, GA 30602 USA. [Rajathurai, Subaraj] Strix Wildlife Consultancy, Singapore, Singapore. [Reichard, Ulrich] So Illinois Univ, Carbondale, IL 62901 USA. [Reinartz, Gay] Zool Soc Milwaukee, Milwaukee, WI 53226 USA. [Renton, Katherine; Rivera, Jorge Vega] Univ Nacl Autonoma Mexico, Estn Biol Chamela, Jalisco 48980, Mexico. [Reynolds, Glen] Danum Valley Field Ctr, Sabah, Malaysia. [Reynolds, Vernon] Univ Oxford, Oxford BN26 5UX, England. [Riley, Erin] San Diego State Univ, San Diego, CA 92182 USA. [Roedel, Mark-Oliver] Museum Naturkunde, Berlin, Germany. [Rothman, Jessica] CUNY, New York, NY 10065 USA. [Round, Philip] Mahidol Univ, Bangkok 10400, Thailand. [Sakai, Shoko] Res Inst Human & Nat, Kyoto, Japan. [Schaab, Gertrud] Karlsruhe Univ Appl Sci, Karlsruhe, Germany. [Seidensticker, John] Natl Zool Pk, Washington, DC 20013 USA. [Siaka, Alhaji] Gola Forest Programme, Kenema, Sierra Leone. [Silman, Miles R.] Wake Forest Univ, Winston Salem, NC 27106 USA. [Smith, Thomas B.; Wang, Benjamin] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Stanford, Craig] Univ So Calif, Los Angeles, CA 90089 USA. [Stewart, Kristine] Inst Appl Ethnobotany, Pompano Beach, FL 33069 USA. [Sukumar, Raman] Indian Inst Sci, Bangalore 560012, Karnataka, India. [Stoner, Kathryn E.] Texas A&M Univ, Kingsville, TX 78363 USA. [Tscharntke, Teja; Waltert, Matthias] Univ Gottingen, Gottingen, Germany. [Turkalo, Andrea] Wildlife Conservat Soc, Bangui, Cent Afr Republ. [Umapathy, Govindaswamy] Ctr Cellular & Mol Biol, Hyderabad, Andhra Pradesh, India. [Venn, Linda] Paluma Environm Educ Ctr, Paluma, Qld 4816, Australia. [Verea, Carlos] Cent Univ Venezuela, Maracay, Venezuela. [de Castilho, Carolina Volkmer] Embrapa Roraima, Boa Vista, Roraima, Brazil. [Whitacre, David] Treasure Valley Math & Sci Ctr, Boise, ID 83714 USA. [Whitney, Ken] Rice Univ, Houston, TX 77005 USA. [Wright, Patricia] SUNY Stony Brook, Stony Brook, NY 11794 USA. [Yonzon, Pralad] Resources Himalaya Fdn, Kathmandu, Nepal. RP Laurance, WF (reprint author), James Cook Univ, Ctr Trop Environm & Sustainabil Sci TESS, Cairns, Qld 4878, Australia. EM bill.laurance@jcu.edu.au RI Williams, Stephen/A-7250-2008; Pringle, Catherine/I-1841-2012; James Cook University, TESS/B-8171-2012; Arroyo-Rodriguez, Victor/C-9255-2009; Rainey, Hugo/I-6047-2012; Ivanauskas, Natalia/C-2224-2012; Whitney, Kenneth/B-2971-2011; Nabe-Nielsen, Jacob/A-5891-2010; Raman, Sukumar/C-9809-2013; Forget, Pierre-Michel/B-4355-2009; Cannon, Charles/D-7186-2012; van Weerd, Merlijn/K-6790-2013; Lahoz da Silva Ribeiro, Jose Eduardo/A-8574-2013; Sloan, Sean/A-8630-2012; Nielsen, Martin Reinhardt/E-1173-2015; Laurance, Susan/G-6021-2011; Lu, Xiankai/M-2127-2014; IBIS, INMUNOVIROLOGI/O-9246-2015; Waltert, Matthias/E-9134-2010; Lattke, John/K-2934-2015; Maisels, Fiona/E-7382-2015; publist, CMEC/C-3010-2012; Bradshaw, Corey/A-1311-2008; publicationpage, cmec/B-4405-2017; Urbina-Cardona, J. Nicolas/B-5447-2008; Wright, Stuart/M-3311-2013; Novotny, Vojtech/G-9434-2014; Tscharntke, Teja/N-5123-2014; Nabe-Nielsen, Jacob/A-3992-2014; Research ID, CTBCC /O-3564-2014; TropWATER, Research ID/P-1401-2014; Sheil, Douglas/A-3867-2015; Bruhl, Carsten/F-3385-2012; CSTFA, ResearcherID/P-1067-2014; Montag, Luciano/I-1485-2012; Stoner, Kathryn/E-1510-2015 OI Baker, Patrick/0000-0002-6560-7124; Corlett, Richard/0000-0002-2508-9465; Campbell, Mason/0000-0001-6803-271X; Williams, Stephen/0000-0002-2510-7408; Ivanauskas, Natalia/0000-0001-6643-8476; Whitney, Kenneth/0000-0002-2523-5469; Nabe-Nielsen, Jacob/0000-0002-0716-9525; Forget, Pierre-Michel/0000-0002-9252-974X; Cannon, Charles/0000-0003-1901-0420; Pearson, Richard/0000-0001-6047-031X; Abernethy, Katharine/0000-0002-0393-9342; Lahoz da Silva Ribeiro, Jose Eduardo/0000-0002-2389-5631; Harris, David/0000-0002-6801-2484; Bruhl, Carsten/0000-0003-1332-535X; Sloan, Sean/0000-0002-7834-0203; Nielsen, Martin Reinhardt/0000-0002-8941-6031; Laurance, Susan/0000-0002-2831-2933; Lattke, John/0000-0002-6793-3003; Maisels, Fiona/0000-0002-0778-0615; Bradshaw, Corey/0000-0002-5328-7741; Urbina-Cardona, J. Nicolas/0000-0002-4174-8467; Wright, Stuart/0000-0003-4260-5676; Novotny, Vojtech/0000-0001-7918-8023; Sheil, Douglas/0000-0002-1166-6591; Stoner, Kathryn/0000-0002-9964-1697 FU James Cook University; Smithsonian Tropical Research Institute; Australian Laureate Fellowship; NSF [RCN-0741956] FX The study was supported by James Cook University, the Smithsonian Tropical Research Institute, an Australian Laureate Fellowship (to W. F. L.) and NSF grant RCN-0741956. We thank A. Bruner, R. A. Butler, G. R. Clements, R. Condit, C. N. Cook, S. Goosem, J. Geldmann, L. Joppa, S. L. Pimm and O. Venter for comments. NR 30 TC 250 Z9 259 U1 66 U2 778 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 SEP 13 PY 2012 VL 489 IS 7415 BP 290 EP 294 DI 10.1038/nature11318 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 003UC UT WOS:000308635900041 PM 22832582 ER PT J AU Lemaitre, R Felder, DL AF Lemaitre, Rafael Felder, Darryl L. TI A new species of the hermit crab genus Areopaguristes Rahayu & McLaughlin, 2010 (Crustacea: Decapoda: Anomura: Diogenidae) discovered in the Mesoamerican Barrier Reef of Belize, Caribbean Sea SO ZOOTAXA LA English DT Article DE Crustacea; Anomura; Diogenidae; Areopaguristes; Paguristes tortugae complex; new species; Mesoamerican Barrier Reef; Belize ID PAGURISTES CRUSTACEA; WESTERN ATLANTIC; PAGUROIDEA; FAUNA AB A new species of hermit crab, Areopaguristes tudgei, family Diogenidae, is fully described and illustrated, including a color photograph. A dense population of this new species was discovered living intertidally in a concealed habitat under coral boulders covered with calcareous algae, on the crest to fore-reef zone in Carrie Bow Cay, a small island located on the western Caribbean Mesoamerican Barrier Reef of Belize. This new species, the 24rd of Areopaguristes Rahayu & McLaughlin, 2010, and fourth known in this genus from the western Atlantic, is superficially similar to those of the Paguristes tortugae complex. As in species of that complex, A. tudgei n. sp. has dense plumose setation on the chelipeds, and at least in females, a fringe of plumose setae on the dorsolateral margins of the chelae, and on the dorsal margins of the walking legs. The presence in A. tudgei n. sp. of this setal arrangement, previously considered the only defining character of the P. tortugae complex, can be attributed to convergence. The new species is contrasted with all other western Atlantic congeners, and a key is presented to aid in their identification. A list of all western Atlantic species of Paguristes sensu lato and their current generic assignments is included. C1 [Lemaitre, Rafael] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Suitland, MD 20746 USA. [Felder, Darryl L.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Felder, Darryl L.] Univ Louisiana Lafayette, Lab Crustacean Res, Lafayette, LA 70504 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM lemaitrr@si.edu; dlf4517@louisiana.edu FU U.S. National Science Foundation, NSF/AToL [EF-0531603]; Hunterdon Oceanographic Research Fund; University of Louisiana Laboratory for Crustacean Research [153] FX We thank CCRE station managers Jerry and Sandy Alonka for making sure that all lab, field equipment and accommodations worked perfectly; and our colleagues, J. Felder, S. Pecnick, and C.C. Tudge, for their enthusiasm and invaluable help in the field and lab. We are grateful to our colleagues: D. L. Rahayu, who kindly shared with us unpublished information about species of Paguristes sensu lato; and J. Poupin, for help in confirming morphological details of the type material of Paguristes iris Forest & de Saint Laurent, 1968 deposited in the MNHN. The assistance of R. Gulledge in the preparation of electronic versions of the figures, and processing of collections, is gratefully acknowledged. This study was supported, in part, by funding to D. L. Felder from U.S. National Science Foundation, NSF/AToL grant number EF-0531603, for the Decapod Tree of Life project. This work is contribution number 927 of the Caribbean Coral Reef Ecosystem Program (CCRE), Smithsonian Institution, supported in part by the Hunterdon Oceanographic Research Fund, and University of Louisiana Laboratory for Crustacean Research contribution number 153. NR 42 TC 3 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 SEP 12 PY 2012 IS 3480 BP 67 EP 79 PG 13 WC Zoology SC Zoology GA 004IS UT WOS:000308675700003 ER PT J AU Sulzner, K Johnson, CK Bonde, RK Gomez, NA Powell, J Nielsen, K Luttrell, MP Osterhaus, ADME Aguirre, AA AF Sulzner, Kathryn Johnson, Christine Kreuder Bonde, Robert K. Gomez, Nicole Auil Powell, James Nielsen, Klaus Luttrell, M. Page Osterhaus, A. D. M. E. Aguirre, A. Alonso TI Health Assessment and Seroepidemiologic Survey of Potential Pathogens in Wild Antillean Manatees (Trichechus manatus manatus) SO PLOS ONE LA English DT Article ID WEST-INDIAN MANATEE; TOXOPLASMA-GONDII INFECTION; DUGONGS DUGONG-DUGON; FLORIDA MANATEES; MARINE MAMMALS; ZALOPHUS-CALIFORNIANUS; SERUM CHEMISTRY; LATIROSTRIS; LEPTOSPIROSIS; ANTIBODIES AB The Antillean manatee (Trichechus manatus manatus), a subspecies of the West Indian manatee, inhabits fresh, brackish, and warm coastal waters distributed along the eastern border of Central America, the northern coast of South America, and throughout the Wider Caribbean Region. Threatened primarily by human encroachment, poaching, and habitat degradation, Antillean manatees are listed as endangered by the International Union for the Conservation of Nature. The impact of disease on population viability remains unknown in spite of concerns surrounding the species' ability to rebound from a population crash should an epizootic occur. To gain insight on the baseline health of this subspecies, a total of 191 blood samples were collected opportunistically from wild Antillean manatees in Belize between 1997 and 2009. Hematologic and biochemical reference intervals were established, and antibody prevalence to eight pathogens with zoonotic potential was determined. Age was found to be a significant factor of variation in mean blood values, whereas sex, capture site, and season contributed less to overall differences in parameter values. Negative antibody titers were reported for all pathogens surveyed except for Leptospira bratislava, L. canicola, and L. icterohemorrhagiae, Toxoplasma gondii, and morbillivirus. As part of comprehensive health assessment in manatees from Belize, this study will serve as a benchmark aiding in early disease detection and in the discernment of important epidemiologic patterns in the manatees of this region. Additionally, it will provide some of the initial tools to explore the broader application of manatees as sentinel species of nearshore ecosystem health. C1 [Sulzner, Kathryn; Johnson, Christine Kreuder] Univ Calif Davis, Wildlife Hlth Ctr, Sch Vet Med, Davis, CA 95616 USA. [Bonde, Robert K.] US Geol Survey, Sirenia Project, Gainesville, FL USA. [Gomez, Nicole Auil; Powell, James] Sea Shore Alliance, St Petersburg, FL USA. [Nielsen, Klaus] Canadian Food Inspect Agcy, Nepean, ON, Canada. [Luttrell, M. Page] Univ Georgia, Coll Vet Med, SE Cooperat Wildlife Dis Study, Dept Populat Hlth, Athens, GA USA. [Osterhaus, A. D. M. E.] Erasmus MC, Rotterdam, Netherlands. [Aguirre, A. Alonso] Smithsonian Mason Sch Conservat, Front Royal, VA USA. [Aguirre, A. Alonso] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Sulzner, K (reprint author), Univ Calif Davis, Wildlife Hlth Ctr, Sch Vet Med, Davis, CA 95616 USA. EM aaguirr3@gmu.edu OI Bonde, Robert/0000-0001-9179-4376 FU University of California, Davis, CA; Wildlife Health Center's Wildlife Fellowship Fund; Preventive Veterinary Department, University of California, Davis, CA FX Financial support for many of the serological assays performed in this study was provided in part by the University of California, Davis, CA, Wildlife Health Center's Wildlife Fellowship Fund and by a grant from the Preventive Veterinary Department, University of California, Davis, CA. Additional laboratory tests and services were offered in-kind by Dr. Pat Conrad, Department of Pathology, Microbiology and Immunology, School of Veterinary Medicine, University of California, Davis, CA; Dr. William Reisen, Center for Vectorborne Disease Research, University of California, Davis, CA; Dr. Dave Stallknecht and Page Luttrell, Department of Population Health, College of Veterinary Medicine, University of Georgia, Athens, GA; Dr. Klaus Nielsen, Canadian Food Inspection Agency, Nepean, Ontario, Canada; and Dr. A. D. M. E Osterhaus, Department of Virology, Erasmus Medical Centre, Rotterdam, The Netherlands. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 88 TC 6 Z9 6 U1 3 U2 42 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 12 PY 2012 VL 7 IS 9 AR e44517 DI 10.1371/journal.pone.0044517 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 005GJ UT WOS:000308738500062 PM 22984521 ER PT J AU Ho, HC Johnson, GD AF Ho, Hsuan-Ching Johnson, G. David TI Protoblepharon mccoskeri, a new flashlight fish from eastern Taiwan (Teleostei: Anomalopidae) SO ZOOTAXA LA English DT Article DE Pisces; Beryciformes; taxonomy; new species ID BERYCIFORMES AB A new flashlight fish of the genus Protoblepharon is described based on a large male specimen collected from eastern Taiwan, northwestern Pacific Ocean. It differs from the only congener, P. rosenblatti, in having the following characters: a smaller light organ with a larger cup; a deeper body; a strongly convex dorsal profile; a smaller and anterior placed pelvic fin, the appressed fin reaching to the midpoint between origins of pelvic and anal fins; a smaller pectoral fin, the apressed fin not reaching the lateral line; second dorsal-fin spine the longest; a shorter snout; a smaller eye; about 30 scale rows between first dorsal-fin base and lateral line; and more than 260 scale rows along the body axis. C1 [Ho, Hsuan-Ching] Natl Dong Hwa Univ, Inst Marine Biodivers & Evolutionary Biol, Natl Museum Marine Biol & Aquarium, Checheng 944, Pingtung, Taiwan. [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Ho, HC (reprint author), Natl Dong Hwa Univ, Inst Marine Biodivers & Evolutionary Biol, Natl Museum Marine Biol & Aquarium, 2 Houwan Rd, Checheng 944, Pingtung, Taiwan. EM ogcoho@gmail.com; johnsond@si.edu FU National Museum of Marine Biology and Aquarium [NMMBA100200254] FX The authors thank A. Hey (AMS) and S.-Y. Wang (NMMB-P) for curatorial assistance, Bruce Collette (NMFS), John Paxton (AMS) and Vic Springer (USNM) for comments on an early draft of the MS. This study is supported by the National Museum of Marine Biology and Aquarium (NMMBA100200254). NR 8 TC 2 Z9 3 U1 1 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 SEP 12 PY 2012 IS 3479 BP 77 EP 87 PG 11 WC Zoology SC Zoology GA 004IQ UT WOS:000308675500005 ER PT J AU Klimczak, C Watters, TR Ernst, CM Freed, AM Byrne, PK Solomon, SC Blair, DM Head, JW AF Klimczak, Christian Watters, Thomas R. Ernst, Carolyn M. Freed, Andrew M. Byrne, Paul K. Solomon, Sean C. Blair, David M. Head, James W. TI Deformation associated with ghost craters and basins in volcanic smooth plains on Mercury: Strain analysis and implications for plains evolution SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID BURIED IMPACT CRATERS; 1ST MESSENGER FLYBY; CALORIS BASIN; THERMAL-EXPANSION; NORMAL FAULTS; MARS; THICKNESS; TECTONISM; DEPOSITS; SURFACE AB Since its insertion into orbit about Mercury in March 2011, the MESSENGER spacecraft has imaged most previously unseen regions of the planet in unprecedented detail, revealing extensive regions of contiguous smooth plains at high northern latitudes and surrounding the Caloris basin. These smooth plains, thought to be emplaced by flood volcanism, are populated with several hundred ghost craters and basins, nearly to completely buried impact features having rims for which the surface expressions are now primarily rings of deformational landforms. Associated with some ghost craters are interior groups of graben displaying mostly polygonal patterns. The origin of these graben is not yet fully understood, but comparison with numerical models suggests that the majority of such features are the result of stresses from local thermal contraction. In this paper, we highlight a previously unreported category of ghost craters, quantify extensional strains across graben-bearing ghost craters, and make use of graben geometries to gain insights into the subsurface geology of smooth plains areas. In particular, the style and mechanisms of graben development imply that flooding of impact craters and basins led to substantial pooling of lavas, to thicknesses of similar to 1.5 km. In addition, surface strains derived from groups of graben are generally in agreement with theoretically and numerically derived strains for thermal contraction. C1 [Klimczak, Christian; Byrne, Paul K.; Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Ernst, Carolyn M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. [Freed, Andrew M.; Blair, David M.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Head, James W.] Brown Univ, Dept Geol Sci, Providence, RI 02912 USA. RP Klimczak, C (reprint author), Carnegie Inst Sci, Dept Terr Magnetism, 5241 Broad Branch Rd NW, Washington, DC 20015 USA. EM cklimczak@ciw.edu RI Ernst, Carolyn/I-4902-2012 FU NASA [NASW-00002, NAS5-97271] FX We thank Michelle Cooke and Chris Okubo for helpful comments on an earlier draft. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to the Johns Hopkins University Applied Physics Laboratory. NR 50 TC 23 Z9 23 U1 0 U2 13 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 SEP 11 PY 2012 VL 117 AR E00L03 DI 10.1029/2012JE004100 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 007LK UT WOS:000308889600001 ER PT J AU Giorgi, JA Vandenberg, NJ AF Giorgi, Jose Adriano Vandenberg, Natalia J. TI Review of the lady beetle genus Phaenochilus Weise (Coleoptera: Coccinellidae: Chilocorini) with description of a new species from Thailand that preys on cycad aulacaspis scale, Aulacaspis yasumatsui Takagi (Hemiptera: Sternorrhyncha: Diaspididae) SO ZOOTAXA LA English DT Review DE biological control; Cucujoidea; ladybird; pest; predator; sago palm; systematics; taxonomy ID FLORIDA AB Species of the genus Phaenochilus are reviewed, keyed, and illustrated, and an annotated checklist provided. A new species, Phaenochilus kashaya n. sp., is described from Thailand. This species feeds on an invasive pest of cycads, the cycad aulacaspis scale, Aulacaspis yasumatsui Takagi (Hemiptera: Sternorrhyncha: Diaspididae). The economic importance of cycads and cycad aulacaspis scale is discussed. A taxonomic history of Phaenochilus is provided. C1 [Giorgi, Jose Adriano] Fed Univ Para, Zool Lab, BR-68372040 Altamira, Para, Brazil. [Vandenberg, Natalia J.] Agr Res Serv, SEL, Inst Plant Sci, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Giorgi, JA (reprint author), Fed Univ Para, Zool Lab, BR-68372040 Altamira, Para, Brazil. EM Vandenberg@ars.usda.gov FU Smithsonian Department of Entomology (Casey Fund); FACEPE [APQ-0538-5.01/10] FX The visit of Adriano Giorgi to the USNM collection during the summer of 2011 was made possible through funds awarded by Smithsonian Department of Entomology (Casey Fund, administered through Terry Erwin) and FACEPE (APQ-0538-5.01/10, granted to Jorge Torres, Universidade Federal Rural de Pernambuco). NR 46 TC 3 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 SEP 11 PY 2012 IS 3478 SI SI BP 239 EP 255 PG 17 WC Zoology SC Zoology GA 004IO UT WOS:000308675200023 ER PT J AU Norrbom, AL Korytkowski, CA AF Norrbom, Allen L. Korytkowski, Cheslavo A. TI New species of Anastrepha (Diptera: Tephritidae), with a key for the species of the megacantha clade SO ZOOTAXA LA English DT Article DE fruit flies; taxonomy AB Thirteen new species of Anastrepha are described and illustrated: A. anopla (Brazil, Ecuador), A. grandicarina (Brazil, Ecuador, Per), A. hadracantha (Ecuador), A. haplacantha (Ecuador), A. hyperacantha (Ecuador), A. inaequalis (Trinidad), A. intermedia (Panama), A. lopezi (Guatemala), A. macracantha (Ecuador), A. magnicurva (Ecuador, Per), A. neogigantea (Ecuador, Venezuela), A. peneramosa (Per), and A. stangei (Venezuela). A key for the species of the megacantha clade is provided. Pouteria buenaventurensis (Sapotaceae) is reported as a host plant for A. intermedia. C1 [Norrbom, Allen L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst, Washington, DC 20013 USA. [Korytkowski, Cheslavo A.] Univ Panama, Programa Ctr Amer Maestria Entomol, Panama City, Panama. 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; cheslavok@cableonda.net FU USDA; APHIS; CPHST; IS FX We sincerely thank the curators and institutions who kindly loaned or provided specimens for study, particularly Gary Steck (FSCA), Norma Nolazco (SENASA), J.A. Rafael (INPA), Phil Perkins (MCZ) and Norman Penny (CAS), and Terry Erwin (Smithsonian) for access to the canopy material his project collected in Ecuador. George Venable, Jerrett McCormick and Lucrecia Rodriguez produced some of the illustrations, and Terrence Walters (USDA, APHIS, CPHST) secured funding for some of the illustration work. Annabella Reszczynski (USDA, APHIS, IS) helped obtain funding for ALN to travel to Per that facilitated collaboration with SENASA. We also thank Roberto Zucchi, Robert Kula, and Norman Woodley for their comments on previous drafts of the manuscript. USDA is an equal opportunity provider and employer. NR 16 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 SEP 11 PY 2012 IS 3478 SI SI BP 510 EP 552 PG 43 WC Zoology SC Zoology GA 004IO UT WOS:000308675200042 ER PT J AU Bamba, A Puhlhofer, G Acero, F Klochkov, D Tian, WW Yamazaki, R Li, ZY Horns, D Kosack, K Komin, N AF Bamba, Aya Puehlhofer, Gerd Acero, Fabio Klochkov, Dmitry Tian, Wenwu Yamazaki, Ryo Li, Zhiyuan Horns, Dieter Kosack, Karl Komin, Nukri TI SUZAKU OBSERVATIONS OF THE NON-THERMAL SUPERNOVA REMNANT HESS J1731-347 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; ISM: individual objects (HESS J1731-347); X-rays: ISM ID RAY-IMAGING SPECTROMETER; SNR RX J1713.7-3946; CHARGE-INJECTION; BOARD SUZAKU; BROAD-BAND; X-RAYS; EMISSION; SHELL; ACCELERATION; DISCOVERY AB A detailed analysis of the non-thermal X-ray emission from the northwestern and southern parts of the supernova remnant (SNR) HESS J1731-347 with Suzaku is presented. The shell portions covered by the observations emit hard and lineless X-rays. The spectrum can be reproduced by a simple absorbed power-law model with a photon index Gamma of 1.8-2.7 and an absorption column density N-H of (1.0-2.1) x 10(22) cm(-2). These quantities change significantly from region to region; the northwestern part of the SNR has the hardest and most absorbed spectrum. The western part of the X-ray shell has a smaller curvature than the northwestern and southern shell segments. A comparison of the X-ray morphology to the very high energy gamma-ray and radio images was performed. The efficiency of the electron acceleration and the emission mechanism in each portion of the shell are discussed. Thermal X-ray emission from the SNR was searched for but could not be detected at a significant level. C1 [Bamba, Aya; Yamazaki, Ryo] Aoyama Gakuin Univ, Dept Math & Phys, Chuo Ku, Sagamihara, Kanagawa 2525258, Japan. [Puehlhofer, Gerd; Klochkov, Dmitry] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Acero, Fabio] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier,CC 72, F-34095 Montpellier, France. [Tian, Wenwu] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Tian, Wenwu] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Li, Zhiyuan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Horns, Dieter] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. [Kosack, Karl] CEA Saclay, DSM IRFU, F-91191 Gif Sur Yvette, France. [Komin, Nukri] Univ Savoie, CNRS, IN2P3, Lab Annecy le Vieux Phys Particules, F-74941 Annecy Le Vieux, France. RP Bamba, A (reprint author), Aoyama Gakuin Univ, Dept Math & Phys, Chuo Ku, 5-10-1 Fuchinobe, Sagamihara, Kanagawa 2525258, Japan. RI XRAY, SUZAKU/A-1808-2009; Komin, Nukri/J-6781-2015 OI Komin, Nukri/0000-0003-3280-0582 FU Japanese Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan [22684012, 21740184]; NSFC, BeiRen Program of the CAS; 973 Program [2012CB821800] FX We thank the anonymous referee for useful comments. We thank all members of the Suzaku team who kindly scheduled these observations. We also thank S. Yamauchi and K. Ebisawa for helpful comments on the GXRE, and Y. Fukazawa, T. Mizuno, and Y. Terada for help with the HXD analysis, and S. Terada for help in writing this paper. This work was supported in part by Grant-in-Aid for Scientific Research of the Japanese Ministry of Education, Culture, Sports, Science, and Technology (MEXT) of Japan, No. 22684012 (A. B.) and No. 21740184 (R. Y.). W. W. T. acknowledges support from NSFC, BeiRen Program of the CAS, and the 973 Program (2012CB821800). NR 49 TC 14 Z9 14 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 149 DI 10.1088/0004-637X/756/2/149 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200045 ER PT J AU Bussmann, RS Gurwell, MA Fu, H Smith, DJB Dye, S Auld, R Baes, M Baker, AJ Bonfield, D Cava, A Clements, DL Cooray, A Coppin, K Dannerbauer, H Dariush, A De Zotti, G Dunne, L Eales, S Fritz, J Hopwood, R Ibar, E Ivison, RJ Jarvis, MJ Kim, S Leeuw, LL Maddox, S Michallowski, MJ Negrello, M Pascale, E Pohlen, M Riechers, DA Rigby, E Scott, D Temi, P Van der Werf, PP Wardlow, J Wilner, D Verma, A AF Bussmann, R. S. Gurwell, M. A. Fu, Hai Smith, D. J. B. Dye, S. Auld, R. Baes, M. Baker, A. J. Bonfield, D. Cava, A. Clements, D. L. Cooray, A. Coppin, K. Dannerbauer, H. Dariush, A. De Zotti, G. Dunne, L. Eales, S. Fritz, J. Hopwood, R. Ibar, E. Ivison, R. J. Jarvis, M. J. Kim, S. Leeuw, L. L. Maddox, S. Michallowski, M. J. Negrello, M. Pascale, E. Pohlen, M. Riechers, D. A. Rigby, E. Scott, Douglas Temi, P. Van der Werf, P. P. Wardlow, J. Wilner, D. Verma, A. TI A DETAILED GRAVITATIONAL LENS MODEL BASED ON SUBMILLIMETER ARRAY AND KECK ADAPTIVE OPTICS IMAGING OF A HERSCHEL-ATLAS SUBMILLIMETER GALAXY AT z=4.243 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; gravitational lensing: strong ID STAR-FORMATION HISTORY; SCIENCE DEMONSTRATION PHASE; ULTRALUMINOUS INFRARED GALAXIES; SPACE-TELESCOPE MORPHOLOGIES; DEGREE EXTRAGALACTIC SURVEY; DEEP-FIELD-SOUTH; ALL-SKY SURVEY; MOLECULAR GAS; BILLION YEARS; LUMINOSITY FUNCTIONS AB We present high-spatial resolution imaging obtained with the Submillimeter Array (SMA) at 880 mu m and the Keck adaptive optics (AO) system at the K-S-band of a gravitationally lensed submillimeter galaxy (SMG) at z = 4.243 discovered in the Herschel Astrophysical Terahertz Large Area Survey. The SMA data (angular resolution approximate to 0.'' 6) resolve the dust emission into multiple lensed images, while the Keck AO KS-band data (angular resolution approximate to 0.'' 1) resolve the lens into a pair of galaxies separated by 0.'' 3. We present an optical spectrum of the foreground lens obtained with the Gemini-South telescope that provides a lens redshift of z(lens) = 0.595 +/- 0.005. We develop and apply a new lens modeling technique in the visibility plane that shows that the SMG is magnified by a factor of mu = 4.1 +/- 0.2 and has an intrinsic infrared (IR) luminosity of L-IR = (2.1 +/- 0.2) x 10(13) L-circle dot. We measure a half-light radius of the background source of r(s) = 4.4 +/- 0.5 kpc which implies an IR luminosity surface density of Sigma(IR) = (3.4 +/- 0.9) x 10(11) L-circle dot kpc(-2), a value that is typical of z > 2 SMGs but significantly lower than IR luminous galaxies at z similar to 0. The two lens galaxies are compact (r(lens) approximate to 0.9 kpc) early-types with Einstein radii of theta(E1) = 0.57 +/- 0.01 and theta(E2) = 0.40 +/- 0.01 that imply masses of M-lens1 = (7.4 +/- 0.5) x 10(10) M-circle dot and M-lens2 = (3.7 +/- 0.3) x 10(10) M-circle dot. The two lensing galaxies are likely about to undergo a dissipationless merger, and the mass and size of the resultant system should be similar to other early-type galaxies at z similar to 0.6. This work highlights the importance of high spatial resolution imaging in developing models of strongly lensed galaxies discovered by Herschel. C1 [Bussmann, R. S.; Gurwell, M. A.; Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fu, Hai; Cooray, A.; Kim, S.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Smith, D. J. B.; Bonfield, D.; Dunne, L.; Jarvis, M. J.; Maddox, S.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys, Hatfield AL10 9AB, Herts, England. [Dye, S.; Eales, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Auld, R.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Cava, A.] Univ Complutense Madrid, Fac CC Fis, Dept Astrofis, E-28040 Madrid, Spain. [Clements, D. L.; Dariush, A.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, London SW7 2AZ, England. [Coppin, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Dannerbauer, H.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [De Zotti, G.; Negrello, M.] Univ Padua, Dipto Astron, IT-35122 Padua, Italy. [Hopwood, R.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Ibar, E.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa. [Leeuw, L. L.] Univ Johannesburg, Dept Phys, Auckland Pk 2006, South Africa. [Michallowski, M. J.] Univ Edinburgh, Inst Astron, Scottish Univ Phys Alliance, Edinburgh EH9 3HJ, Midlothian, Scotland. [Pascale, E.; Pohlen, M.] ESO, D-85748 Garching, Germany. [Riechers, D. A.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Rigby, E.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Temi, P.] NASA, Space Sci & Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [Van der Werf, P. P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Verma, A.] Univ Oxford, Oxford OX1 3RH, England. RP Bussmann, RS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rbussmann@cfa.harvard.edu RI Baes, Maarten/I-6985-2013; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Dye, Simon/0000-0002-1318-8343; Baes, Maarten/0000-0002-3930-2757; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840; Smith, Daniel/0000-0001-9708-253X; /0000-0002-0729-2988 FU Smithsonian Institution; Academia Sinica; W. M. Keck Foundation; NASA from JPL; SMA Fellowship program; NSF CAREER [AST-0645427] FX Some of the data presented herein were obtained at the Submillimeter Array, which 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.; 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.; The results described in this paper are based on observations obtained with Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The Herschel-ATLAS is a project with Herschel, which is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS Web site is http://www.h-atlas.org/. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL. R. S. B. acknowledges support from the SMA Fellowship program. H. F., A. C., J.L.W., and S. K. acknowledge support from NSF CAREER AST-0645427. We thank K. Rosenfeld and S. M. Andrews for assistance in implementing the lens modeling analysis in the visibility plane. We thank the referee for a thorough review of the manuscript which resulted in a stronger paper overall. NR 88 TC 17 Z9 17 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 SEP 10 PY 2012 VL 756 IS 2 AR 134 DI 10.1088/0004-637X/756/2/134 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200030 ER PT J AU Dawson, RI Johnson, JA AF Dawson, Rebekah I. Johnson, John Asher TI THE PHOTOECCENTRIC EFFECT AND PROTO-HOT JUPITERS. I. MEASURING PHOTOMETRIC ECCENTRICITIES OF INDIVIDUAL TRANSITING PLANETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; techniques: photometric ID KEPLER TARGET STARS; EXTRASOLAR PLANETS; LIGHT CURVES; ORBITAL ECCENTRICITIES; TIDAL EVOLUTION; PERIOD PLANETS; GIANT PLANET; HD 17156B; MIGRATION; CANDIDATES AB Exoplanet orbital eccentricities offer valuable clues about the history of planetary systems. Eccentric, Jupiter-sized planets are particularly interesting: they may link the "cold" Jupiters beyond the ice line to close-in hot Jupiters, which are unlikely to have formed in situ. To date, eccentricities of individual transiting planets primarily come from radial-velocity measurements. Kepler has discovered hundreds of transiting Jupiters spanning a range of periods, but the faintness of the host stars precludes radial-velocity follow-up of most. Here, we demonstrate a Bayesian method of measuring an individual planet's eccentricity solely from its transit light curve using prior knowledge of its host star's density. We show that eccentric Jupiters are readily identified by their short ingress/egress/total transit durations-part of the "photoeccentric" light curve signature of a planet's eccentricity-even with long-cadence Kepler photometry and loosely constrained stellar parameters. A Markov Chain Monte Carlo exploration of parameter posteriors naturally marginalizes over the periapse angle and automatically accounts for the transit probability. To demonstrate, we use three published transit light curves of HD 17156 b to measure an eccentricity of e = 0.71+(+0.16)(-0.09), in good agreement with the discovery value e = 0.67 +/- 0.08 based on 33 radial-velocity measurements. We present two additional tests using Kepler data. In each case, the technique proves to be a viable method of measuring exoplanet eccentricities and their confidence intervals. Finally, we argue that this method is the most efficient, effective means of identifying the extremely eccentric, proto-hot Jupiters predicted by Socrates et al. C1 [Dawson, Rebekah I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Johnson, John Asher] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Johnson, John Asher] NASA Exoplanet Sci Inst NExScI, Pasadena, CA 91125 USA. RP Dawson, RI (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. EM rdawson@cfa.harvard.edu FU National Science Foundation [DGE-1144152]; Bayesian Book Club; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G] FX We are thankful for the helpful and positive feedback from the anonymous referee. R. I. D. gratefully acknowledges support by the National Science Foundation Graduate Research Fellowship under grant DGE-1144152, clear and constant guidance from chapter Winn (2010), and the ministry and fellowship of the Bayesian Book Club. J.A.J. thanks Avi Loeb and the ITC for hosting him as part of their visitors program, thereby allowing the authors to work together in close proximity at the CfA during the completion of this work. We thank Sarah Ballard, Zachory Berta, Joshua Carter, Courtney Dressing, Subo Dong, Daniel Fabrycky, Jonathan Irwin, Boaz Katz, David Kipping, Timothy Morton, Norman Murray, Ruth Murray-Clay, Peter Plavchan, Gregory Snyder, Aristotle Socrates, and Joshua Winn for helpful discussions. Several colleagues provided helpful and inspiring comments on a manuscript draft: Joshua Carter (who, in addition to other helpful comments, suggested the procedure described in Section 3.4), Daniel Fabrycky, Eric Ford, David Kipping, and Ruth Murray-Clay. Special thanks to J. Zachary Gazak for helpful modifications to the TAP code.; This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. 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 74 TC 43 Z9 43 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 122 DI 10.1088/0004-637X/756/2/122 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200018 ER PT J AU Fong, W Berger, E Margutti, R Zauderer, BA Troja, E Czekala, I Chornock, R Gehrels, N Sakamoto, T Fox, DB Podsiadlowski, P AF Fong, W. Berger, E. Margutti, R. Zauderer, B. A. Troja, E. Czekala, I. Chornock, R. Gehrels, N. Sakamoto, T. Fox, D. B. Podsiadlowski, P. TI A JET BREAK IN THE X-RAY LIGHT CURVE OF SHORT GRB 111020A: IMPLICATIONS FOR ENERGETICS AND RATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual (111020A) ID NEUTRON-STAR BINARIES; COMPACT OBJECT MERGERS; LATE-TIME AFTERGLOW; SWIFT XRT DATA; GAMMA-RAY; BURST AFTERGLOWS; BLACK-HOLES; HOST GALAXIES; OBSERVATIONAL CONSTRAINTS; TELESCOPE OBSERVATIONS AB We present broadband observations of the afterglow and environment of the short GRB 111020A. An extensive X-ray light curve from Swift/XRT, XMM-Newton, and Chandra, spanning similar to 100 s to 10 days after the burst, reveals a significant break at delta t approximate to 2 days with pre- and post-break decline rates of alpha(X, 1) approximate to -0.78 and alpha(X, 2) less than or similar to -1.7, respectively. Interpreted as a jet break, we infer a collimated outflow with an opening angle of theta(j) approximate to 3 degrees-8 degrees. The resulting beaming-corrected gamma-ray (10-1000 keV band) and blast-wave kinetic energies are (2-3) x 10(48) erg and (0.3-2) x 10(49) erg, respectively, with the range depending on the unknown redshift of the burst. We report a radio afterglow limit of <39 mu Jy (3 sigma) from Expanded Very Large Array observations that, along with our finding that nu(c) < nu(X), constrains the circumburst density to n(0) similar to 0.01-0.1 cm(-3). Optical observations provide an afterglow limit of i greater than or similar to 24.4 mag at 18 hr after the burst and reveal a potential host galaxy with i approximate to 24.3 mag. The subarcsecond localization from Chandra provides a precise offset of 0 ''.80+/-0 ''.11 (1 sigma) from this galaxy corresponding to an offset of 5-7 kpc for z = 0.5-1.5. We find a high excess neutral hydrogen column density of (7.5 +/- 2.0) x 10(21) cm(-2) (z = 0). Our observations demonstrate that a growing fraction of short gamma-ray bursts (GRBs) are collimated, which may lead to a true event rate of greater than or similar to 100-1000 Gpc(-3) yr(-1), in good agreement with the NS-NS merger rate of approximate to 200-3000 Gpc(-3) yr(-1). This consistency is promising for coincident short GRB-gravitational wave searches in the forthcoming era of Advanced LIGO/VIRGO. C1 [Fong, W.; Berger, E.; Margutti, R.; Zauderer, B. A.; Czekala, I.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Troja, E.; Gehrels, N.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Podsiadlowski, P.] Univ Oxford, Dept Astron, Oxford OX1 3RH, England. RP Fong, W (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Czekala, Ian/0000-0002-1483-8811 FU National Science Foundation [AST-1107973]; National Aeronautics and Space Administration through Chandra X-Ray Observatory Center [GO1-12072X]; National Aeronautics Space Administration [NAS8-03060]; NASA/Swift AO6 grant [NNX10AI24G] FX We thank D. Finkbeiner for helpful discussions. The Berger GRB group at Harvard is supported by the National Science Foundation under grant AST-1107973. Partial support was also provided by the National Aeronautics and Space Administration through Chandra Award Number GO1-12072X 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. Additional support was provided by NASA/Swift AO6 grant NNX10AI24G. Observations were obtained with the EVLA (Program 10C-145) operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 109 TC 57 Z9 58 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 189 DI 10.1088/0004-637X/756/2/189 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200085 ER PT J AU Ford, EB Ragozzine, D Rowe, JF Steffen, JH Barclay, T Batalha, NM Borucki, WJ Bryson, ST Caldwell, DA Fabrycky, DC Gautier, TN Holman, MJ Ibrahim, KA Kjeldsen, H Kinemuchi, K Koch, DG Lissauer, JJ Still, M Tenenbaum, P Uddin, K Welsh, W AF Ford, Eric B. Ragozzine, Darin Rowe, Jason F. Steffen, Jason H. Barclay, Thomas Batalha, Natalie M. Borucki, William J. Bryson, Stephen T. Caldwell, Douglas A. Fabrycky, Daniel C. Gautier, Thomas N., III Holman, Matthew J. Ibrahim, Khadeejah A. Kjeldsen, Hans Kinemuchi, Karen Koch, David G. Lissauer, Jack J. Still, Martin Tenenbaum, Peter Uddin, Kamal Welsh, William TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. V. TRANSIT TIMING VARIATION CANDIDATES IN THE FIRST SIXTEEN MONTHS FROM POLYNOMIAL MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability; techniques: miscellaneous ID MULTIPLE-PLANET SYSTEMS; SUN-LIKE STAR; HIERARCHICAL TRIPLE; LOW-MASS; CONFIRMATION; ARCHITECTURE; PHOTOMETRY AB Transit timing variations provide a powerful tool for confirming and characterizing transiting planets, as well as detecting non-transiting planets. We report the results of an updated transit timing variation (TTV) analysis for 1481 planet candidates based on transit times measured during the first sixteen months of Kepler observations. We present 39 strong TTV candidates based on long-term trends (2.8% of suitable data sets). We present another 136 weaker TTV candidates (9.8% of suitable data sets) based on the excess scatter of TTV measurements about a linear ephemeris. We anticipate that several of these planet candidates could be confirmed and perhaps characterized with more detailed TTV analyses using publicly available Kepler observations. For many others, Kepler has observed a long-term TTV trend, but an extended Kepler mission will be required to characterize the system via TTVs. We find that the occurrence rate of planet candidates that show TTVs is significantly increased (similar to 68%) for planet candidates transiting stars with multiple transiting planet candidates when compared to planet candidates transiting stars with a single transiting planet candidate. C1 [Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. [Ragozzine, Darin; Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ibrahim, Khadeejah A.; Uddin, Kamal] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Caldwell, Douglas A.; Tenenbaum, Peter] SETI Inst, Mountain View, CA 94043 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Barclay, Thomas; Kinemuchi, Karen; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Welsh, William] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Ford, EB (reprint author), Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. EM eford@astro.ufl.edu RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; OI Barclay, Thomas/0000-0001-7139-2724; Fabrycky, Daniel/0000-0003-3750-0183; Caldwell, Douglas/0000-0003-1963-9616; /0000-0001-6545-639X FU NASA's Science Mission Directorate; National Aeronautics and Space Administration [NNX08AR04G] FX Funding for this mission is provided by NASA's Science Mission Directorate. We thank the entire Kepler team for the many years of work that is proving so successful. E.B.F. acknowledges support by the National Aeronautics and Space Administration under grant NNX08AR04G issued through the Kepler Participating Scientist Program. NR 25 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 185 DI 10.1088/0004-637X/756/2/185 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200081 ER PT J AU Foster, AR Ji, L Smith, RK Brickhouse, NS AF Foster, A. R. Ji, L. Smith, R. K. Brickhouse, N. S. TI UPDATED ATOMIC DATA AND CALCULATIONS FOR X-RAY SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic data; atomic processes; X-rays: general ID FINITE-DENSITY PLASMAS; DIELECTRONIC RECOMBINATION DATA; ELECTRON-IMPACT EXCITATION; COLLISIONAL IONIZATION EQUILIBRIUM; OPTICALLY THIN PLASMAS; INCLUDING N=4 LEVELS; R-MATRIX APPROACH; HELIUM-LIKE IONS; NA-LIKE IONS; ISOELECTRONIC SEQUENCE AB We describe the latest release of AtomDB, version 2.0.2, a database of atomic data and a plasma modeling code with a focus on X-ray astronomy. This release includes several major updates to the fundamental atomic structure and process data held within AtomDB, incorporating new ionization balance data, state-selective recombination data, and updated collisional excitation data for many ions, including the iron L-shell ions from Fe+16 to Fe+23 and all of the hydrogen-and helium-like sequences. We also describe some of the effects that these changes have on calculated emission and diagnostic line ratios, such as changes in the temperature implied by the He-like G-ratios of up to a factor of two. C1 [Foster, A. R.; Ji, L.; Smith, R. K.; Brickhouse, N. S.] Smithsonian Astrophys Observ, Cambridge, MA 02144 USA. RP Foster, AR (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02144 USA. OI Brickhouse, Nancy/0000-0002-8704-4473 FU NASA ADP [NNX09AC71G] FX We thank Paola Testa for discussion involving the line diagnostic issues. The authors gratefully acknowledge funding from NASA ADP grant NNX09AC71G. NR 84 TC 150 Z9 150 U1 1 U2 21 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 128 DI 10.1088/0004-637X/756/2/128 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200024 ER PT J AU France, K Schindhelm, E Herczeg, GJ Brown, A Abgrall, H Alexander, RD Bergin, EA Brown, JM Linsky, JL Roueff, E Yang, H AF France, Kevin Schindhelm, Eric Herczeg, Gregory J. Brown, Alexander Abgrall, Herve Alexander, Richard D. Bergin, Edwin A. Brown, Joanna M. Linsky, Jeffrey L. Roueff, Evelyne Yang, Hao TI A HUBBLE SPACE TELESCOPE SURVEY OF H-2 EMISSION IN THE CIRCUMSTELLAR ENVIRONMENTS OF YOUNG STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; stars: pre-main sequence; ultraviolet: planetary systems ID T-TAURI-STARS; MOLECULAR-HYDROGEN EMISSION; MAIN-SEQUENCE STARS; NE-II EMISSION; HIGH-RESOLUTION SPECTROSCOPY; ETA-CHAMAELEONTIS CLUSTER; FAR-ULTRAVIOLET CONTINUUM; CO FUNDAMENTAL EMISSION; 4TH POSITIVE EMISSION; PLANET-FORMING ZONES AB The formation timescale and final architecture of exoplanetary systems are closely related to the properties of the molecular disks from which they form. Observations of the spatial distribution and lifetime of the molecular gas at planet-forming radii (a < 10 AU) are important for understanding the formation and evolution of exoplanetary systems. Toward this end, we present the largest spectrally resolved survey of H-2 emission around low-mass pre-main-sequence stars compiled to date. We use a combination of new and archival far-ultraviolet spectra from the Cosmic Origins Spectrograph and Space Telescope Imaging Spectrograph instruments on the Hubble Space Telescope to sample 34 T Tauri stars (27 actively accreting Classical T Tauri Stars and 7 non-accreting Weak-lined T Tauri Stars) with ages ranging from similar to 1 to 10 Myr. We observe fluorescent H-2 emission, excited by Ly alpha photons, in 100% of the accreting sources, including all of the transitional disks in our sample (CS Cha, DM Tau, GM Aur, UX Tau A, LkCa 15, HD 135344B, and TW Hya). The spatial distribution of the emitting gas is inferred from spectrally resolved H-2 line profiles. Some of the emitting gas is produced in outflowing material, but the majority of H-2 emission appears to originate in a rotating disk. For the disk-dominated targets, the H-2 emission originates predominately at a less than or similar to 3 AU. The emission line widths and inner molecular radii are found to be roughly consistent with those measured from mid-IR CO spectra. C1 [France, Kevin; Schindhelm, Eric; Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Herczeg, Gregory J.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Abgrall, Herve; Roueff, Evelyne] Observ Paris, LUTH, Sect Meudon, F-92195 Meudon, France. [Abgrall, Herve; Roueff, Evelyne] Observ Paris, CNRS, UMR 8102, Sect Meudon, F-92195 Meudon, France. [Alexander, Richard D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Linsky, Jeffrey L.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, Jeffrey L.] NIST, Boulder, CO 80309 USA. [Yang, Hao] Cent China Normal Univ, Inst Astrophys, Wuhan 430079, Hubei, Peoples R China. 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; Herczeg, Gregory/0000-0002-7154-6065 FU Science & Technology Facilities Council (STFC) through an Advanced Fellowship [ST/G00711X/1]; NASA [NNX08AC146, NAS5-98043, 11533, 12036, NAS 5-26555]; HST GO [8041, 11616, 11828, 12361] FX We thank Tom Ayres for custom processing of the STIS observations and the DAO of Tau team for enjoyable discussions during the course of this work. K. F. thanks Phil Armitage for helpful discussion regarding gas giant migration. We acknowledge the technical efforts of Nico Nell and David Morris, and E. S. and K. F. thank Brian Wood for input on Ly alpha profile reconstruction. R. D. A. acknowledges support from the Science & Technology Facilities Council (STFC) through an Advanced Fellowship (ST/G00711X/1). This work was supported by NASA grants NNX08AC146 and NAS5-98043 to the University of Colorado at Boulder (HST programs 11533 and 12036) and made use of data from HST GO programs 8041, 11616, 11828, and 12361.; 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. NR 144 TC 32 Z9 32 U1 1 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 SEP 10 PY 2012 VL 756 IS 2 AR 171 DI 10.1088/0004-637X/756/2/171 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200067 ER PT J AU Ikeda, H Nagao, T Matsuoka, K Taniguchi, Y Shioya, Y Kajisawa, M Enoki, M Capak, P Civano, F Koekemoer, AM Masters, D Morokuma, T Salvato, M Schinnerer, E Scoville, NZ AF Ikeda, H. Nagao, T. Matsuoka, K. Taniguchi, Y. Shioya, Y. Kajisawa, M. Enoki, M. Capak, P. Civano, F. Koekemoer, A. M. Masters, D. Morokuma, T. Salvato, M. Schinnerer, E. Scoville, N. Z. TI CONSTRAINTS ON THE FAINT END OF THE QUASAR LUMINOSITY FUNCTION AT z similar to 5 IN THE COSMOS FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; quasars: general; surveys ID DIGITAL-SKY-SURVEY; BLACK-HOLE MASS; OPTICALLY SELECTED QSOS; EVOLUTION SURVEY COSMOS; ACTIVE GALACTIC NUCLEI; HOST GALAXIES; SUBARU TELESCOPE; STELLAR OBJECTS; ACCRETION RATE; BULGE MASS AB We present the result of our low-luminosity quasar survey in the redshift range of 4.5 less than or similar to z less than or similar to 5.5 in the COSMOS field. Using the COSMOS photometric catalog, we selected 15 quasar candidates with 22 < i' < 24 at z similar to 5 that are similar to 3 mag fainter than the Sloan Digital Sky Survey quasars in the same redshift range. We obtained optical spectra for 14 of the 15 candidates using FOCAS on the Subaru Telescope and did not identify any low-luminosity type-1 quasars at z similar to 5, while a low-luminosity type-2 quasar at z similar to 5.07 was discovered. In order to constrain the faint end of the quasar luminosity function at z similar to 5, we calculated the 1 sigma confidence upper limits of the space density of type-1 quasars. As a result, the 1 sigma confidence upper limits on the quasar space density are Phi < 1.33 x 10(-7) Mpc(-3) mag(-1) for -24.52 < M-1450 < -23.52 and Phi < 2.88 x 10(-7) Mpc(-3) mag(-1) for -23.52 < M-1450 < -22.52. The inferred 1s confidence upper limits of the space density are then used to provide constraints on the faint-end slope and the break absolute magnitude of the quasar luminosity function at z similar to 5. We find that the quasar space density decreases gradually as a function of redshift at low luminosity (M-1450 similar to -23), being similar to the trend found for quasars with high luminosity (M-1450 < -26). This result is consistent with the so-called downsizing evolution of quasars seen at lower redshifts. C1 [Ikeda, H.; Matsuoka, K.; Kajisawa, M.] Ehime Univ, Grad Sch Sci & Engn, Matsuyama, Ehime 7908577, Japan. [Ikeda, H.; Nagao, T.; Matsuoka, K.] Kyoto Univ, Dept Astron, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Nagao, T.] Kyoto Univ, Hakubi Ctr Adv Res, Sakyo Ku, Kyoto 6068302, Japan. [Taniguchi, Y.; Shioya, Y.; Kajisawa, M.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Enoki, M.] Tokyo Keizai Univ, Fac Business Adm, Kokubunji, Tokyo 1858502, Japan. [Capak, P.; Masters, D.; Scoville, N. Z.] 249 17 Caltech, Dept Astron, Pasadena, CA 91125 USA. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Masters, D.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Morokuma, T.] Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan. [Salvato, M.] Max Planck Inst Plasma Phys, D-85741 Garching, Germany. [Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Ikeda, H (reprint author), Ehime Univ, Grad Sch Sci & Engn, Bunkyo Cho, Matsuyama, Ehime 7908577, Japan. EM ikeda@cosmos.phys.sci.ehime-u.ac.jp OI Koekemoer, Anton/0000-0002-6610-2048; Schinnerer, Eva/0000-0002-3933-7677 FU Japan Society for the Promotion of Science (JSPS) [23244031, 23654068]; FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)"; Council for Science and Technology Policy (CSTP); JSPS through the JSPS Research Fellowship FX We thank the Subaru staff for their invaluable help and all members of the COSMOS team. This work was financially supported in part by the Japan Society for the Promotion of Science (JSPS; grant Nos. 23244031 and 23654068). This work was also partly supported by the FIRST program "Subaru Measurements of Images and Redshifts (SuMIRe)," which was initiated by the Council for Science and Technology Policy (CSTP). K. M. is financially supported by the JSPS through the JSPS Research Fellowship. NR 66 TC 17 Z9 17 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 SEP 10 PY 2012 VL 756 IS 2 AR 160 DI 10.1088/0004-637X/756/2/160 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200056 ER PT J AU Liu, HB Hsieh, PY Ho, PTP Su, YN Wright, M Sun, AL Minh, YC AF Liu, Hauyu Baobab Hsieh, Pei-Ying Ho, Paul T. P. Su, Yu-Nung Wright, Melvyn Sun, Ai-Lei Minh, Young Chol TI MILKY WAY SUPERMASSIVE BLACK HOLE: DYNAMICAL FEEDING FROM THE CIRCUMNUCLEAR ENVIRONMENT SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; Galaxy: kinematics and dynamics; Galaxy: structure; ISM: clouds ID GALACTIC-CENTER REGION; GIANT MOLECULAR CLOUDS; CLUSTER-FORMING REGION; STAR-FORMATION; SAGITTARIUS-A; IONIZED-GAS; EXPANDING SHELL; CENTRAL PARSEC; GALAXY; DISK AB The supermassive black hole (SMBH), Sgr A*, at the Galactic center is surrounded by a molecular circumnuclear disk (CND) lying between 1.5 and 4 pc radii. The irregular and clumpy structures of the CND suggest dynamical evolution and episodic feeding of gas toward the central SMBH. New sensitive data from the Submillimeter Array and Green Bank Telescope reveal several >5-10 pc scale molecular arms, which either directly connect to the CND or may penetrate inside the CND. The CND appears to be the convergence of the innermost parts of large-scale gas streamers, which are responding to the central gravitational potential well. Rather than being a quasi-stationary structure, the CND may be dynamically evolving, incorporating inflow via streamers, and feeding gas toward the center. C1 [Liu, Hauyu Baobab; Hsieh, Pei-Ying; Ho, Paul T. P.; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Liu, Hauyu Baobab; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Hauyu Baobab] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Hsieh, Pei-Ying] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan. [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Sun, Ai-Lei] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Minh, Young Chol] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM hlu@cfa.havard.edu FU Smithsonian Institution; Academia Sinica; ASIAA; NRAO; [GBT11B050]; [SMA2011AS085] FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica (Ho et al. 2004).; The GBT and SMA data are from projects GBT11B050 and SMA2011AS085, which are parts of the integrated state-of-art imaging project KISS: Kinematic Processes of the Extremely Turbulent ISM around the Supermassive Black Holes. We acknowledge financial support from ASIAA and NRAO. We thank Toney Minter, Glen Langston, and David T. Frayer for assisting the GBT observations. We thank Glen Petitpas and Nimesh Patel for supporting the SMA observations. We acknowledge Ray Blundell, Sergio Martin, and Jessica Lu for useful comments or suggestions. NR 54 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 SEP 10 PY 2012 VL 756 IS 2 AR 195 DI 10.1088/0004-637X/756/2/195 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200091 ER PT J AU Qiu, KP Zhang, QZ Beuther, H Fallscheer, C AF Qiu, Keping Zhang, Qizhou Beuther, Henrik Fallscheer, Cassandra TI FORMING AN O STAR VIA DISK ACCRETION? SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: jets and outflows; ISM: kinematics and dynamics; stars: early-type; stars: formation ID H-II REGIONS; ULTRACOMPACT HII-REGIONS; EXTREMELY HIGH-VELOCITY; W51 MASSIVE CORES; JET-LIKE OUTFLOW; DYNAMICAL COLLAPSE; MOLECULAR OUTFLOW; BIPOLAR OUTFLOW; STANDARD MODEL; EMISSION AB We present a study of outflow, infall, and rotation in a similar to 105 L-circle dot star-forming region, IRAS 18360-0537, with Submillimeter Array and IRAM 30 m observations. The 1.3 mm continuum map shows a 0.5 pc dust ridge, of which the central compact part has a mass of similar to 80 M-circle dot and harbors two condensations, MM1 and MM2. The CO (2-1) and SiO (5-4) maps reveal a biconical outflow centered at MM1, which is a hot molecular core (HMC) with a gas temperature of 320 +/- 50 K and a mass of similar to 13 M-circle dot. The outflow has a gas mass of 54 M-circle dot and a dynamical timescale of 8 x 10(3) yr. The kinematics of the HMC are probed by high-excitation CH3OH and CH3CN lines, which are detected at subarcsecond resolution and unveil a velocity gradient perpendicular to the outflow axis, suggesting a disk-like rotation of the HMC. An infalling envelope around the HMC is evidenced by CN lines exhibiting a profound inverse P Cygni profile, and the estimated mass infall rate, 1.5 x 10(-3) M-circle dot yr(-1), is well comparable to that inferred from the mass outflow rate. A more detailed investigation of the kinematics of the dense gas around the HMC is obtained from the (CO)-C-13 and (CO)-O-18 (2-1) lines; the position-velocity diagrams of the two lines are consistent with the model of a free-falling and Keplerian-like rotating envelope. The observations suggest that the protostar of a current mass similar to 10 M-circle dot embedded within MM1 will develop into an O star via disk accretion and envelope infall. C1 [Qiu, Keping] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Qiu, Keping] Nanjing Univ, Key Lab Modern Astron & Astrophys, Minist Educ, Nanjing 210093, Jiangsu, Peoples R China. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Beuther, Henrik; Fallscheer, Cassandra] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fallscheer, Cassandra] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. RP Qiu, KP (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM kqiu@mpifr-bonn.mpg.de OI Zhang, Qizhou/0000-0003-2384-6589 NR 41 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 SEP 10 PY 2012 VL 756 IS 2 AR 170 DI 10.1088/0004-637X/756/2/170 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200066 ER PT J AU Sanders, NE Soderberg, AM Valenti, S Foley, RJ Chornock, R Chomiuk, L Berger, E Smartt, S Hurley, K Barthelmy, SD Levesque, EM Narayan, G Botticella, MT Briggs, MS Connaughton, V Terada, Y Gehrels, N Golenetskii, S Mazets, E Cline, T von Kienlin, A Boynton, W Chambers, KC Grav, T Heasley, JN Hodapp, KW Jedicke, R Kaiser, N Kirshner, RP Kudritzki, RP Luppino, GA Lupton, RH Magnier, EA Monet, DG Morgan, JS Onaka, PM Price, PA Stubbs, CW Tonry, JL Wainscoat, RJ Waterson, MF AF Sanders, N. E. Soderberg, A. M. Valenti, S. Foley, R. J. Chornock, R. Chomiuk, L. Berger, E. Smartt, S. Hurley, K. Barthelmy, S. D. Levesque, E. M. Narayan, G. Botticella, M. T. Briggs, M. S. Connaughton, V. Terada, Y. Gehrels, N. Golenetskii, S. Mazets, E. Cline, T. von Kienlin, A. Boynton, W. Chambers, K. C. Grav, T. Heasley, J. N. Hodapp, K. W. Jedicke, R. Kaiser, N. Kirshner, R. P. Kudritzki, R-P. Luppino, G. A. Lupton, R. H. Magnier, E. A. Monet, D. G. Morgan, J. S. Onaka, P. M. Price, P. A. Stubbs, C. W. Tonry, J. L. Wainscoat, R. J. Waterson, M. F. TI SN 2010ay IS A LUMINOUS AND BROAD-LINED TYPE Ic SUPERNOVA WITHIN A LOW-METALLICITY HOST GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; supernovae: general; supernovae: individual (2010ay) ID GAMMA-RAY BURST; CORE-COLLAPSE SUPERNOVAE; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; 25 APRIL 1998; IBC SUPERNOVA; LIGHT CURVES; 100316D/SN 2010BH; PROGENITOR STARS; FORMATION RATES AB We report on our serendipitous pre-discovery detection and follow-up observations of the broad-lined Type Ic supernova (SN Ic) 2010ay at z = 0.067 imaged by the Pan-STARRS1 3 pi survey just similar to 4 days after explosion. The supernova (SN) had a peak luminosity, M-R approximate to -20.2 mag, significantly more luminous than known GRB-SNe and one of the most luminous SNe Ib/c ever discovered. The absorption velocity of SN 2010ay is v(Si) approximate to 19 x 10(3) km s(-1) at similar to 40 days after explosion, 2-5 times higher than other broad-lined SNe and similar to the GRB-SN 2010bh at comparable epochs. Moreover, the velocity declines similar to 2 times slower than other SNe Ic-BL and GRB-SNe. Assuming that the optical emission is powered by radioactive decay, the peak magnitude implies the synthesis of an unusually large mass of Ni-56, M-Ni = 0.9M(circle dot). Applying scaling relations to the light curve, we estimate a total ejecta mass, M-ej approximate to 4.7 M-circle dot, and total kinetic energy, E-K approximate to 11 x 10(51) erg. The ratio of M-Ni to M-ej is similar to 2 times as large for SN 2010ay as typical GRB-SNe and may suggest an additional energy reservoir. The metallicity (log(O/H)(PP04) + 12 = 8.19) of the explosion site within the host galaxy places SN 2010ay in the low-metallicity regime populated by GRB-SNe, and similar to 0.5(0.2) dex lower than that typically measured for the host environments of normal (broad-lined) SNe Ic. We constrain any gamma-ray emission with E-gamma less than or similar to 6 x 10(48) erg (25-150 keV), and our deep radio follow-up observations with the Expanded Very Large Array rule out relativistic ejecta with energy E greater than or similar to 10(48) erg. We therefore rule out the association of a relativistic outflow like those that accompanied SN 1998bw and traditional long-duration gamma-ray bursts (GRBs), but we place less-stringent constraints on a weak afterglow like that seen from XRF 060218. If this SN did not harbor a GRB, these observations challenge the importance of progenitor metallicity for the production of relativistic ejecta and suggest that other parameters also play a key role. C1 [Sanders, N. E.; Soderberg, A. M.; Foley, R. J.; Chornock, R.; Chomiuk, L.; Berger, E.; Kirshner, R. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Valenti, S.; Smartt, S.; Botticella, M. T.] Queens Univ Belfast, Astrophys Res Ctr, Sch Maths & Phys, Belfast BT7 1NN, Antrim, North Ireland. [Chomiuk, L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Hurley, K.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Barthelmy, S. D.; Gehrels, N.; Cline, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Levesque, E. M.] Univ Colorado, Dept Astrophys & Planetary Sci, CASA, Boulder, CO 80309 USA. [Narayan, G.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Briggs, M. S.; Connaughton, V.] Univ Alabama, CSPAR, Huntsville, AL 35899 USA. [Terada, Y.] Saitama Univ, Dept Phys, Sakura Ku, Saitama 3388570, Japan. [Golenetskii, S.; Mazets, E.] AF Ioffe Phys Tech Inst, Expt Astrophys Lab, St Petersburg 194021, Russia. [von Kienlin, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Boynton, W.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Chambers, K. C.; Heasley, J. N.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R-P.; Luppino, G. A.; Magnier, E. A.; Morgan, J. S.; Onaka, P. M.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ 85919 USA. [Lupton, R. H.; Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Monet, D. G.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Waterson, M. F.] Univ Western Australia, Int Ctr Radio Astron Res, Perth, WA 6009, Australia. RP Sanders, NE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nsanders@cfa.harvard.edu RI Terada, Yukikatsu/A-5879-2013; Waterson, Mark/B-7352-2013; Golenetskii, Sergey/B-3818-2015; Stubbs, Christopher/C-2829-2012 OI Chambers, Kenneth /0000-0001-6965-7789; Terada, Yukikatsu/0000-0002-2359-1857; Waterson, Mark/0000-0002-0192-2686; Stubbs, Christopher/0000-0003-0347-1724 FU RFBR [09-02-00166a]; NASA [NNX07AR71G, NNX08AN23G, NNX09AO97G, NNX08AX95G, NNX09AR28G, NNX09AU03G, NNX09AV61G]; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation FX We are grateful to the following people for their assistance with the IPN data: C. Meegan (Fermi GBM), K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, T. Murakami, and K. Makishima (Suzaku WAM), J. Goldsten (MESSENGER), S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer (Swift-BAT), R. Aptekar, V. Pal'shin, D. Frederiks, and D. Svinkin (Konus-Wind), X. Zhang and A. Rau (INTEGRAL SPI-ACS), and I. G. Mitrofanov, D. Golovin, M. L. Litvak, A. B. Sanin, C. Fellows, K. Harshman, H. Enos, and R. Starr (Odyssey). The Konus-Wind experiment is supported in the Russian Federation by RFBR Grant 09-02-00166a. K. H. acknowledges NASA support for the IPN under the following grants: NNX07AR71G (MESSENGER), NNX08AN23G and NNX09AO97G (Swift), NNX08AX95G and NNX09AR28G (INTEGRAL), NNX09AU03G (Fermi), and NNX09AV61G (Suzaku).; The PS1 Surveys have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, the Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under Grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate.; This work was supported by the National Science Foundation through a Graduate Research Fellowship provided to NES. NR 130 TC 24 Z9 24 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 184 DI 10.1088/0004-637X/756/2/184 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200080 ER PT J AU Schlafly, EF Finkbeiner, DP Juric, M Magnier, EA Burgett, WS Chambers, KC Grav, T Hodapp, KW Kaiser, N Kudritzki, RP Martin, NF Morgan, JS Price, PA Rix, HW Stubbs, CW Tonry, JL Wainscoat, RJ AF Schlafly, E. F. Finkbeiner, D. P. Juric, M. Magnier, E. A. Burgett, W. S. Chambers, K. C. Grav, T. Hodapp, K. W. Kaiser, N. Kudritzki, R. -P. Martin, N. F. Morgan, J. S. Price, P. A. Rix, H. -W. Stubbs, C. W. Tonry, J. L. Wainscoat, R. J. TI PHOTOMETRIC CALIBRATION OF THE FIRST 1.5 YEARS OF THE PAN-STARRS1 SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods: data analysis; surveys; techniques: photometric ID DIGITAL SKY SURVEY; ATMOSPHERIC EXTINCTION; TELESCOPE; PANSTARRS; GALAXIES; CATALOG; STAR AB We present a precise photometric calibration of the first 1.5 years of science imaging from the Pan-STARRS1 survey (PS1), an ongoing optical survey of the entire sky north of declination-30 degrees in five bands. Building on the techniques employed by Padmanabhan et al. in the Sloan Digital Sky Survey (SDSS), we use repeat PS1 observations of stars to perform the relative calibration of PS1 in each of its five bands, simultaneously solving for the system throughput, the atmospheric transparency, and the large-scale detector flat field. Both internal consistency tests and comparison against the SDSS indicate that we achieve relative precision of <10 mmag in g, r, and i(P1), and similar to 10 mmag in z and y(P1). The spatial structure of the differences with the SDSS indicates that errors in both the PS1 and SDSS photometric calibration contribute similarly to the differences. The analysis suggests that both the PS1 system and the Haleakala site will enable <1% photometry over much of the sky. C1 [Schlafly, E. F.; Finkbeiner, D. P.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Finkbeiner, D. P.; Juric, M.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Magnier, E. A.; Burgett, W. S.; Chambers, K. C.; Hodapp, K. W.; Kaiser, N.; Kudritzki, R. -P.; Morgan, J. S.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Grav, T.] Planetary Sci Inst, Tucson, AZ USA. [Martin, N. F.; Rix, H. -W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Martin, N. F.] CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Schlafly, EF (reprint author), Harvard Univ, Dept Phys, 17 Oxford St, Cambridge, MA 02138 USA. RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Schlafly, Edward Ford/0000-0002-3569-7421; Chambers, Kenneth /0000-0001-6965-7789 FU NASA [NNX10AD69G]; NASA by the Space Telescope Science Institute [HF-51255.01-A]; Association of Universities for Research in Astronomy, Inc. [NAS 5-26555]; German Research Foundation (DFG) [Sonderforschungsbereich SFB 881]; National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX D.F. and E. S. acknowledge support of NASA grant NNX10AD69G for this research. 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. N.F.M. acknowledges funding by Sonderforschungsbereich SFB 881 "The Milky Way System" (subproject A3) of the German Research Foundation (DFG); The Pan-STARRS1 survey has been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, and the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. NR 34 TC 110 Z9 110 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 SEP 10 PY 2012 VL 756 IS 2 AR 158 DI 10.1088/0004-637X/756/2/158 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200054 ER PT J AU Snyder, GF Brodwin, M Mancone, CM Zeimann, GR Stanford, SA Gonzalez, AH Stern, D Eisenhardt, PRM Brown, MJI Dey, A Jannuzi, B Perlmutter, S AF Snyder, Gregory F. Brodwin, Mark Mancone, Conor M. Zeimann, Gregory R. Stanford, S. A. Gonzalez, Anthony H. Stern, Daniel Eisenhardt, Peter R. M. Brown, Michael J. I. Dey, Arjun Jannuzi, Buell Perlmutter, Saul TI ASSEMBLY OF THE RED SEQUENCE IN INFRARED-SELECTED GALAXY CLUSTERS FROM THE IRAC SHALLOW CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: photometry ID COLOR-MAGNITUDE RELATION; HUBBLE-SPACE-TELESCOPE; SIMILAR-TO 1; STELLAR POPULATION SYNTHESIS; STAR-FORMATION HISTORIES; HIGH-REDSHIFT CLUSTERS; INITIAL MASS FUNCTION; IA SUPERNOVA RATE; WIDE-FIELD SURVEY; LUMINOSITY FUNCTION AB We present results for the assembly and star formation histories (SFHs) of massive (similar to L*) red sequence galaxies (RSGs) in 11 spectroscopically confirmed, infrared-selected galaxy clusters at 1.0 < z < 1.5, the precursors to present-day massive clusters with M similar to 10(15) M-circle dot. Using rest-frame optical photometry, we investigate evolution in the color and scatter of the RSG population, comparing with models of possible SFHs. In contrast to studies of central cluster galaxies at lower redshift (z < 1), these data are clearly inconsistent with the continued evolution of stars formed and assembled primarily at a single, much earlier time. Specifically, we find that the colors of massive cluster galaxies at z approximate to 1.5 imply that the bulk of star formation occurred at z similar to 3, whereas by z approximate to 1 their colors imply formation at z similar to 2; therefore these galaxies exhibit approximately the same luminosity-weighted stellar age at 1 < z < 1.5. This likely reflects star formation that occurs over an extended period, the effects of significant progenitor bias, or both. Our results generally indicate that massive cluster galaxy populations began forming a significant mass of stars at z greater than or similar to 4, contained some red spheroids by z approximate to 1.5, and were actively assembling much of their final mass during 1 < z < 2 in the form of younger stars. Qualitatively, the slopes of the cluster color-magnitude relations are consistent with no significant evolution relative to local clusters. C1 [Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Mancone, Conor M.; Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Zeimann, Gregory R.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Stern, Daniel; Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Dey, Arjun; Jannuzi, Buell] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Perlmutter, Saul] Univ Calif Berkeley, EO Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Perlmutter, Saul] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. RP Snyder, GF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Brown, Michael/B-1181-2015; Perlmutter, Saul/I-3505-2015 OI Brown, Michael/0000-0002-1207-9137; Perlmutter, Saul/0000-0002-4436-4661 FU NASA [NAS 5-26555]; NASA through grants from the STScI; W.M. Keck Foundation; NOAO; U.S. Department of Energy [W-7405-ENG-48]; [10496]; [11002]; [11597]; [11663] FX This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., (AURA) under NASA contract NAS 5-26555. These observations are associated with programs 10496, 11002, 11597, and 11663. Support for these programs was provided by NASA through grants from the STScI, which is operated by AURA under NASA contract NAS 5-26555. 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. This work is also based in part on data 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. This work makes use of image data from the NOAO Deep Wide-Field Survey (NDWFS) as distributed by the NOAO Science Archive. The research activities of A. D. and B.T.J. are also supported by NOAO, which is operated by the AURA under a cooperative agreement with the National Science Foundation. MultiDrizzle is a component of the STSDAS and PyRAF software, products of the STScI, which is operated by AURA for NASA.; This work relies on considerable efforts by the Spitzer, HST, and Keck Observatory support staff and instrument teams, and we thank the many hundreds of people who have contributed to these facilities over the years. We thank the anonymous referee for a number of useful suggestions, and Kyle Dawson for a helpful review of the manuscript. This research has made use of NASA's Astrophysics Data System. 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 89 TC 30 Z9 30 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 SEP 10 PY 2012 VL 756 IS 2 AR 114 DI 10.1088/0004-637X/756/2/114 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200010 ER PT J AU Steffen, JH Ford, EB Rowe, JF Fabrycky, DC Holman, MJ Welsh, WF Batalha, NM Borucki, WJ Bryson, S Caldwell, DA Ciardi, DR Jenkins, JM Kjeldsen, H Koch, DG Prsa, A Sanderfer, DT Seader, S Twicken, JD AF Steffen, Jason H. Ford, Eric B. Rowe, Jason F. Fabrycky, Daniel C. Holman, Matthew J. Welsh, William F. Batalha, Natalie M. Borucki, William J. Bryson, Steve Caldwell, Douglas A. Ciardi, David R. Jenkins, Jon M. Kjeldsen, Hans Koch, David G. Prsa, Andrej Sanderfer, Dwight T. Seader, Shawn Twicken, Joseph D. TI TRANSIT TIMING OBSERVATIONS FROM KEPLER. VI. POTENTIALLY INTERESTING CANDIDATE SYSTEMS FROM FOURIER-BASED STATISTICAL TESTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: dynamical evolution and stability; techniques: miscellaneous ID MULTIPLE-PLANET SYSTEMS; 1ST 4 MONTHS; TERRESTRIAL PLANETS; CONFIRMATION; MASS; PERTURBATIONS AB We analyze the deviations of transit times from a linear ephemeris for the Kepler Objects of Interest (KOI) through quarter six of science data. We conduct two statistical tests for all KOIs and a related statistical test for all pairs of KOIs in multi-transiting systems. These tests identify several systems which show potentially interesting transit timing variations (TTVs). Strong TTV systems have been valuable for the confirmation of planets and their mass measurements. Many of the systems identified in this study should prove fruitful for detailed TTV studies. C1 [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32111 USA. [Rowe, Jason F.; Borucki, William J.; Bryson, Steve; Caldwell, Douglas A.; Jenkins, Jon M.; Koch, David G.; Sanderfer, Dwight T.; Seader, Shawn; Twicken, Joseph D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Caldwell, Douglas A.; Jenkins, Jon M.; Twicken, Joseph D.] SETI Inst, Mountain View, CA 94043 USA. [Fabrycky, Daniel C.] Univ Calif Santa Cruz, UCO, Lick Observ, Santa Cruz, CA 95064 USA. [Holman, Matthew J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Ciardi, David R.] CALTECH, NASA Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. RP Steffen, JH (reprint author), Fermilab Ctr Particle Astrophys, POB 500,MS 127, Batavia, IL 60510 USA. EM jsteffen@fnal.gov RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [NNX08AR04G, HF-51272.01-A, HF-51267.01-A, NAS 5-26555]; NASA through Space Telescope Science Institute FX Funding for this mission is provided by NASA's Science Mission Directorate. J.H.S. acknowledges support by NASA under grant NNX08AR04G issued through the Kepler Participating Scientist Program. D.C.F. and J.A.C. acknowledge that support for this work was provided by NASA through Hubble Fellowship grants HF-51272.01-A and HF-51267.01-A awarded by the Space Telescope Science Institute, operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 22 TC 29 Z9 29 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 186 DI 10.1088/0004-637X/756/2/186 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200082 ER PT J AU van Engelen, A Keisler, R Zahn, O Aird, KA Benson, BA Bleem, LE Carlstrom, E Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hou, Z Hrubes, D Joy, M Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Natoli, T Padin, S Plagge, T Pryke, C Reichardt, CL Ruhl, JE Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, K Vanderlinde, K Vieira, JD Williamson, R AF van Engelen, A. Keisler, R. Zahn, O. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, E. Chang, C. L. Cho, H. M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, D. Joy, M. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Natoli, T. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. Vanderlinde, K. Vieira, J. D. Williamson, R. TI A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; cosmology: observations; gravitational lensing: weak; large-scale structure of universe ID ATACAMA COSMOLOGY TELESCOPE; PROBE WMAP OBSERVATIONS; POWER SPECTRUM; GALAXY CLUSTERS; EXTRAGALACTIC SOURCES; DARK-MATTER; DAMPING TAIL; 148 GHZ; CMB; ANISOTROPIES AB We use South Pole Telescope data from 2008 and 2009 to detect the non-Gaussian signature in the cosmic microwave background (CMB) produced by gravitational lensing and to measure the power spectrum of the projected gravitational potential. We constrain the ratio of the measured amplitude of the lensing signal to that expected in a fiducial Lambda CDM cosmological model to be 0.86 +/- 0.16, with no lensing disfavored at 6.3 sigma. Marginalizing over Lambda CDM cosmological models allowed by the Wilkinson Microwave Anisotropy Probe (WMAP7) results in a measurement of A(lens) = 0.90 +/- 0.19, indicating that the amplitude of matter fluctuations over the redshift range 0.5 less than or similar to z less than or similar to 5 probed by CMB lensing is in good agreement with predictions. We present the results of several consistency checks. These include a clear detection of the lensing signature in CMB maps filtered to have no overlap in Fourier space, as well as a "curl" diagnostic that is consistent with the signal expected for Lambda CDM. We perform a detailed study of bias in the measurement due to noise, foregrounds, and other effects and determine that these contributions are relatively small compared to the statistical uncertainty in the measurement. We combine this lensing measurement with results from WMAP7 to improve constraints on cosmological parameters when compared to those from WMAP7 alone: we find a factor of 3.9 improvement in the measurement of the spatial curvature of the universe, Omega(k) = -0.0014 +/- 0.0172; a 10% improvement in the amplitude of matter fluctuations within Lambda CDM, sigma(8) = 0.810 +/- 0.026; and a 5% improvement in the dark energy equation of state, w = -1.04 +/- 0.40. When compared with the measurement of w provided by the combination of WMAP7 and external constraints on the Hubble parameter, the addition of the lensing data improves the measurement of w by 15% to give w = -1.087 +/- 0.096. C1 [van Engelen, A.; de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Keisler, R.; Benson, B. A.; Bleem, L. E.; Carlstrom, E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Keisler, R.; Bleem, L. E.; Carlstrom, E.; Hoover, S.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. [Benson, B. A.; Carlstrom, E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.; Shirokoff, E.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Joy, M.] NASA Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Engelen, A (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8, Canada. RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics Frontier Center at the University of Chicago [0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Inaugural Berkeley Center for Cosmological Physics Fellowship; NASA Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan Research Fellowship; Yale University; NSF [AST-1009811]; Excellence Cluster Universe; DFG research program [TR33]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science FX The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Oliver Zahn acknowledges support from an Inaugural Berkeley Center for Cosmological Physics Fellowship. R. Keisler acknowledges support from the NASA Hubble Fellowship grant HF-51275.01. B. A. Benson is supported by a KICP Fellowship. M. Dobbs acknowledges support from an Alfred P. Sloan Research Fellowship. L. Shaw acknowledges the support of Yale University and the NSF grant AST-1009811. M. Millea and L. Knox acknowledge the support of the NSF grant 0709498. J. Mohr acknowledges support from the Excellence Cluster Universe and the DFG research program TR33 "Dark Universe." This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. It also used resources of the CLUMEQ supercomputing consortium, part of the Compute Canada network. 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. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. NR 96 TC 125 Z9 125 U1 2 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 142 DI 10.1088/0004-637X/756/2/142 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200038 ER PT J AU Wang, JF Fabbiano, G Karovska, M Elvis, M Risaliti, G AF Wang, Junfeng Fabbiano, Giuseppina Karovska, Margarita Elvis, Martin Risaliti, Guido TI THE CHANDRA HRC VIEW OF THE SUBARCSECOND STRUCTURES IN THE NUCLEAR REGION OF NGC 1068 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1068); galaxies: jets; galaxies: Seyfert; X-rays: galaxies ID NARROW-LINE REGION; X-RAY; RADIO STRUCTURE; CIRCUMNUCLEAR REGION; SEYFERT-GALAXIES; IONIZED-GAS; NGC-1068; KINEMATICS; SPECTROSCOPY; EMISSION AB We have obtained a high spatial resolution X-ray image of the nucleus of NGC 1068 using the High Resolution Camera (HRC-I) on board the Chandra X-ray Observatory, which provides an unprecedented view of the innermost 1 arcsec radius region of this galaxy. The HRC image resolves the narrow-line region into X-ray emission clumps matching bright emission-line clouds in the HST [OIII] lambda 5007 images and allows comparison with subarcsecond-scale radio jet for the first time. Two distinct X-ray knots are revealed at 1.3-1.4 arcsec northeast and southwest of the nucleus. Based on the combined X-ray, [O III], and radio continuum morphology, we identify the locations of intense radio jet-cloud interaction. The [O III] to soft X-ray ratios show that some of these clouds are strongly affected by shock heating, whereas in other locations the jet simply thrusts through with no signs of strong interaction. This is further strengthened by the presence of a kT similar to 1 keV collisionally ionized component in the ACIS spectrum of a shock-heated cloud HST-G. We estimate that the kinematic luminosity of the jet-driven shocks is 6 x 10(38) erg s(-1), a negligible fraction (10(-4)) of the estimated total jet power. C1 [Wang, Junfeng; Fabbiano, Giuseppina; Karovska, Margarita; Elvis, Martin; Risaliti, Guido] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Risaliti, Guido] INAF Arcetri Observ, I-50125 Florence, Italy. RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM juwang@cfa.harvard.edu OI Risaliti, Guido/0000-0002-3556-977X FU NASA [GO1-12120X, NAS8-03060, GO1-12009X, GO-12365.01-A]; CXC; National Science Foundation [1066293] FX We thank the anonymous referee for careful reading of the manuscript and helpful comments. We thank Jack Gallimore for kindly providing the VLA and MERLIN maps. This work is supported by NASA grant GO1-12120X (PI: Fabbiano). We acknowledge support from the CXC, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. This material is based upon work supported in part by the National Science Foundation grant No. 1066293 and the hospitality of the Aspen Center for Physics. J.W. acknowledges support from NASA grants GO1-12009X and GO-12365.01-A. M. K. is a member of CXC. This research has made use of data obtained from the Chandra Data Archive, and software provided by the CXC in the application packages CIAO. NR 41 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 10 PY 2012 VL 756 IS 2 AR 180 DI 10.1088/0004-637X/756/2/180 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200076 ER PT J AU Zeimann, GR Stanford, SA Brodwin, M Gonzalez, AH Snyder, GF Stern, D Eisenhardt, P Mancone, C Dey, A AF Zeimann, Gregory R. Stanford, S. A. Brodwin, Mark Gonzalez, Anthony H. Snyder, Gregory F. Stern, Daniel Eisenhardt, Peter Mancone, Conor Dey, Arjun TI IDCS J1433.2+3306: AN INFRARED-SELECTED GALAXY CLUSTER AT z=1.89 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (IDCS J1433.2+3306); galaxies: distances and redshifts; galaxies: evolution; galaxies: formation; galaxies: photometry; galaxies: star formation ID ACTIVE GALACTIC NUCLEI; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; X-RAY SURVEY; STAR-FORMATION; RED-SEQUENCE; DEEP; CONFIRMATION; EXTRACTION; RESOLUTION AB We report the discovery of an IR-selected galaxy cluster in the IRAC Distant Cluster Survey (IDCS). New data from the Hubble Space Telescope spectroscopically confirm IDCS J1433.2+3306 at z = 1.89 with robust spectroscopic redshifts for seven members, two of which are based on the 4000 angstrom break. Detected emission lines such as [O II] and H beta indicate star formation rates of greater than or similar to 20 M-circle dot yr(-1) for three galaxies within a 500 kpc projected radius of the cluster center. The cluster exhibits a red sequence with a scatter and color indicative of a formation redshift z(f) greater than or similar to 3.5. The stellar age of the early-type galaxy population is approximately consistent with those of clusters at lower redshift (1 < z < 1.5) suggesting that clusters at these redshifts are experiencing ongoing or increasing star formation. C1 [Zeimann, Gregory R.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Brodwin, Mark] Univ Missouri, Dept Phys, Kansas City, MO 64110 USA. [Gonzalez, Anthony H.; Mancone, Conor] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Snyder, Gregory F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stern, Daniel; Eisenhardt, Peter] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Zeimann, GR (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. FU National Science Foundation [AST-0708490]; NASA through JPL/Caltech; NASA from the Space Telescope Science Institute [11663, 12203]; NASA [NAS 5-26555]; W. M. Keck Foundation; U.S. Department of Energy [W-7405-ENG-48] FX A.H.G. acknowledges support from the National Science Foundation through grant AST-0708490. 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. Support for HST programs 11663 and 12203 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) 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.; We thank the anonymous referee for their constructive comments, Matt Ashby for creating the IRAC catalogs for SDWFS, Buell Jannuzi for his work on the NDWFS, Michael Brown for combining the NDWFS with SDWFS catalogs, and Steve Murray and the XBootes team for obtaining the Chandra data in the Bootes field. This paper would not have been possible without the efforts of the support staff of the Keck Observatory, Spitzer Space Telescope, Hubble Space Telescope, and Chandra X-ray Observatory. 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 48 TC 42 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 SEP 10 PY 2012 VL 756 IS 2 AR 115 DI 10.1088/0004-637X/756/2/115 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009TN UT WOS:000309048200011 ER PT J AU Arcavi, I Gal-Yam, A Cenko, SB Fox, DB Leonard, DC Moon, DS Sand, DJ Soderberg, AM Kiewe, M Yaron, O Becker, AB Scheps, R Birenbaum, G Chamudot, D Zhou, J AF Arcavi, Iair Gal-Yam, Avishay Cenko, S. Bradley Fox, Derek B. Leonard, Douglas C. Moon, Dae-Sik Sand, David J. Soderberg, Alicia M. Kiewe, Michael Yaron, Ofer Becker, Adam B. Scheps, Raphael Birenbaum, Gali Chamudot, Daniel Zhou, Jonathan TI CALTECH CORE-COLLAPSE PROJECT (CCCP) OBSERVATIONS OF TYPE II SUPERNOVAE: EVIDENCE FOR THREE DISTINCT PHOTOMETRIC SUBTYPES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general ID MODEL LIGHT CURVES; SN 2008AX; PROGENITOR; EVOLUTION; DISTANCE; COMPACT; 2009KR; 2005CS; 2011DH; 1993J AB We present R-band light curves of Type II supernovae (SNe) from the Caltech Core-Collapse Project (CCCP). With the exception of interacting (Type IIn) SNe and rare events with long rise times, we find that most light curve shapes belong to one of three apparently distinct classes: plateau, slowly declining, and rapidly declining events. The last class is composed solely of Type IIb SNe which present similar light curve shapes to those of SNe Ib, suggesting, perhaps, similar progenitor channels. We do not find any intermediate light curves, implying that these subclasses are unlikely to reflect variance of continuous parameters, but rather might result from physically distinct progenitor systems, strengthening the suggestion of a binary origin for at least some stripped SNe. We find a large plateau luminosity range for SNe IIP, while the plateau lengths seem rather uniform at approximately 100 days. As analysis of additional CCCP data goes on and larger samples are collected, demographic studies of core-collapse SNe will likely continue to provide new constraints on progenitor scenarios. C1 [Arcavi, Iair; Gal-Yam, Avishay; Yaron, Ofer] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. [Cenko, S. Bradley; Becker, Adam B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fox, Derek B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Moon, Dae-Sik] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sand, David J.] Global Telescope Network, Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Sand, David J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Soderberg, Alicia M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kiewe, Michael] Univ Wisconsin, Dept Phys, Madison, WI 53706 USA. [Scheps, Raphael] Univ Cambridge, Univ London Kings Coll, Cambridge CB2 1ST, England. RP Arcavi, I (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel. EM iair.arcavi@weizmann.ac.il OI Gal-Yam, Avishay/0000-0002-3653-5598 FU Israeli Science Foundation; German-Israeli Science Foundation; Lord Sieff of Brimpton fund; Richard & Rhoda Goldman Fund; NASA/Swift grants [NNX10AI21G, NNX12AD73G]; TABASGO Foundation; US National Science Foundation (NSF) grant [AST-0908886] FX We thank Mansi M. Kasliwal and Richard S. Walters for scheduling P60 reference imaging, and Yossi Shvartzvald for obtaining the required calibration data for SN2005an. A.G. and I.A. acknowledge support by the Israeli and German-Israeli Science Foundations, and the Lord Sieff of Brimpton fund. S.B.C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and NNX12AD73G, the TABASGO Foundation, and US National Science Foundation (NSF) grant AST-0908886. NR 44 TC 62 Z9 62 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 10 PY 2012 VL 756 IS 2 AR L30 DI 10.1088/2041-8205/756/2/L30 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 006CH UT WOS:000308796500006 ER PT J AU Beatty, TG Pepper, J Siverd, RJ Eastman, JD Bieryla, A Latham, DW Buchhave, LA Jensen, ELN Manner, M Stassun, KG Gaudi, BS Berlind, P Calkins, ML Collins, K DePoy, DL Esquerdo, GA Fulton, BJ Furesz, G Geary, JC Gould, A Hebb, L Kielkopf, JF Marshall, JL Pogge, R Stanek, KZ Stefanik, RP Street, R Szentgyorgyi, AH Trueblood, M Trueblood, P Stutz, AM AF Beatty, Thomas G. Pepper, Joshua Siverd, Robert J. Eastman, Jason D. Bieryla, Allyson Latham, David W. Buchhave, Lars A. Jensen, Eric L. N. Manner, Mark Stassun, Keivan G. Gaudi, B. Scott Berlind, Perry Calkins, Michael L. Collins, Karen DePoy, Darren L. Esquerdo, Gilbert A. Fulton, Benjamin J. Furesz, Gabor Geary, John C. Gould, Andrew Hebb, Leslie Kielkopf, John F. Marshall, Jennifer L. Pogge, Richard Stanek, K. Z. Stefanik, Robert P. Street, Rachel Szentgyorgyi, Andrew H. Trueblood, Mark Trueblood, Patricia Stutz, Amelia M. TI KELT-2Ab: A HOT JUPITER TRANSITING THE BRIGHT (V=8.77) PRIMARY STAR OF A BINARY SYSTEM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: visual; eclipses; planetary systems; stars: individual (HD 42176); techniques: photometric; techniques: radial velocities ID EXOPLANETS; ALGORITHM; RADII AB We report the discovery of KELT-2Ab, a hot Jupiter transiting the bright (V = 8.77) primary star of the HD 42176 binary system. The host is a slightly evolved late F-star likely in the very short-lived "blue-hook" stage of evolution, with T-eff = 6148 +/- 48 K, log g = 4.030(-0.026)(+0.015) and [Fe/H] = 0.034 +/- 0.78. The inferred stellar mass is M-* = 1.314(-0.060)(+0.063) M-circle dot and the star has a relatively large radius of R-* = 1.836(-0.046)(+0.066) R-circle dot. The planet is a typical hot Jupiter with period 4.1137913 +/- 0.00001 days and a mass of M-P = 1.524 +/- 0.088M(J) and radius of R-P = 1.290(-0.050)(+0.064) R-J. This is mildly inflated as compared to models of irradiated giant planets at the similar to 4 Gyr age of the system. KELT-2A is the third brightest star with a transiting planet identified by ground-based transit surveys, and the ninth brightest star overall with a transiting planet. KELT-2Ab's mass and radius are unique among the subset of planets with V < 9 host stars, and therefore increases the diversity of bright benchmark systems. We also measure the relative motion of KELT-2A and -2B over a baseline of 38 years, robustly demonstrating for the first time that the stars are bound. This allows us to infer that KELT-2B is an early K dwarf. We hypothesize that through the eccentric Kozai mechanism KELT-2B may have emplaced KELT-2Ab in its current orbit. This scenario is potentially testable with Rossiter-McLaughlin measurements, which should have an amplitude of similar to 44 m s(-1). C1 [Beatty, Thomas G.; Gaudi, B. Scott; Gould, Andrew; Pogge, Richard; Stanek, K. Z.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Pepper, Joshua; Siverd, Robert J.; Stassun, Keivan G.; Hebb, Leslie] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Eastman, Jason D.; Fulton, Benjamin J.; Street, Rachel] Global Telescope Network, Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Eastman, Jason D.] Univ Calif Santa Barbara, Dept Phys Broida Hall, Santa Barbara, CA 93106 USA. [Bieryla, Allyson; Latham, David W.; Berlind, Perry; Calkins, Michael L.; Esquerdo, Gilbert A.; Furesz, Gabor; Geary, John C.; Stefanik, Robert P.; Szentgyorgyi, Andrew H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-21500 Copenhagen, Denmark. [Buchhave, Lars A.] Geol Museum, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Manner, Mark] Spot Observ, Nunnelly, TN 37137 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Collins, Karen; Kielkopf, John F.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [DePoy, Darren L.; Marshall, Jennifer L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Trueblood, Mark; Trueblood, Patricia] Winer Observ, Sonoita, AZ 85637 USA. [Stutz, Amelia M.] Max Planck Inst Astron, D-6900 Heidelberg, Germany. [Stutz, Amelia M.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Stutz, Amelia M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Beatty, TG (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. RI Gaudi, Bernard/I-7732-2012; OI Eastman, Jason/0000-0003-3773-5142; Jensen, Eric/0000-0002-4625-7333; Buchhave, Lars A./0000-0003-1605-5666; Stutz, Amelia/0000-0003-2300-8200; Pepper, Joshua/0000-0002-3827-8417 FU NASA Grant [NNG04GO70G]; NSF CAREER Grant [AST-1056524]; National Science Foundation's PREST program [AST-0721386]; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics; National Science Foundation through PAARE Grant [AST-0849736]; National Science Foundation through AAG Grant [AST-1009810]; Kentucky Space Grant Consortium Graduate Fellowship; Kepler Mission through NASA [NNX11AB99A]; Smithsonian Astrophysical Observatory FX We particularly thank Bruce Gary for obtaining the HAO observations. Early work on KELT-North was supported by NASA Grant NNG04GO70G. Work by B.S.G., J.D.E., and T.G.B. was partially supported by NSF CAREER Grant AST-1056524. E.L.N.J. gratefully acknowledges the support of the National Science Foundation's PREST program, which helped to establish the Peter van de Kamp Observatory through grant AST-0721386. J.A.P. and K.G.S. acknowledge support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics. K.G.S. and L.H. acknowledge the support of the National Science Foundation through PAARE Grant AST-0849736 and AAG Grant AST-1009810. K.A.C. is supported by a Kentucky Space Grant Consortium Graduate Fellowship. The TRES and KeplerCam observations were obtained with partial support from the Kepler Mission through NASA Cooperative Agreement NNX11AB99A with the Smithsonian Astrophysical Observatory (PI: D.W.L.). NR 26 TC 19 Z9 19 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 SEP 10 PY 2012 VL 756 IS 2 AR L39 DI 10.1088/2041-8205/756/2/L39 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 006CH UT WOS:000308796500015 ER PT J AU Quinn, SN White, RJ Latham, DW Buchhave, LA Cantrell, JR Dahm, SE Furesz, G Szentgyorgyi, AH Geary, JC Torres, G Bieryla, A Berlind, P Calkins, MC Esquerdo, GA Stefanik, RP AF Quinn, Samuel N. White, Russel J. Latham, David W. Buchhave, Lars A. Cantrell, Justin R. Dahm, Scott E. Furesz, Gabor Szentgyorgyi, Andrew H. Geary, John C. Torres, Guillermo Bieryla, Allyson Berlind, Perry Calkins, Michael C. Esquerdo, Gilbert A. Stefanik, Robert P. TI TWO "b"s IN THE BEEHIVE: THE DISCOVERY OF THE FIRST HOT JUPITERS IN AN OPEN CLUSTER SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE open clusters and associations: individual (Praesepe, M44, NGC 2632, Beehive); planetary systems; stars: individual (BD+20 2184, 2MASS J08421149+1916373) ID TRANSIT SURVEYS; PLANETARY COMPANION; STELLAR POPULATIONS; PRAESEPE; SYSTEMS; HYADES; LIMITS; STARS; FIELD; ABUNDANCES AB We report the discovery of two giant planets orbiting stars in Praesepe ( also known as the Beehive Cluster). These are the first known hot Jupiters in an open cluster and the only planets known to orbit Sun-like, main-sequence stars in a cluster. The planets are detected from Doppler-shifted radial velocities; line bisector spans and activity indices show no correlation with orbital phase, confirming the variations are caused by planetary companions. Pr0201b orbits a V = 10.52 late F dwarf with a period of 4.4264 +/- 0.0070 days and has a minimum mass of 0.540 +/- 0.039 M-Jup, and Pr0211b orbits a V = 12.06 late G dwarf with a period of 2.1451 +/- 0.0012 days and has a minimum mass of 1.844 +/- 0.064 M-Jup. The detection of two planets among 53 single members surveyed establishes a lower limit of 3.8(2.4)(+5.0)% on the hot Jupiter frequency in this metal-rich open cluster. Given the precisely known age of the cluster, this discovery also demonstrates that, in at least two cases, giant planet migration occurred within 600 Myr after formation. As we endeavor to learn more about the frequency and formation history of planets, environments with well-determined properties-such as open clusters like Praesepe-may provide essential clues to this end. C1 [Quinn, Samuel N.; White, Russel J.; Cantrell, Justin R.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30302 USA. [Latham, David W.; Furesz, Gabor; Szentgyorgyi, Andrew H.; Geary, John C.; Torres, Guillermo; Bieryla, Allyson; Berlind, Perry; Calkins, Michael C.; Esquerdo, Gilbert A.; Stefanik, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Dahm, Scott E.] WM Keck Observ, Kamuela, HI 96743 USA. RP Quinn, SN (reprint author), Georgia State Univ, Dept Phys & Astron, POB 4106, Atlanta, GA 30302 USA. OI Buchhave, Lars A./0000-0003-1605-5666 FU National Aeronautics and Space Administration (NASA) through the Origins of Solar Systems program [NNX11AC32G]; NASA's Kepler mission under Cooperative Agreement [NNX11AB99A]; Smithsonian Astrophysical Observatory FX This material is based upon work supported by the National Aeronautics and Space Administration (NASA) under grant No. NNX11AC32G issued through the Origins of Solar Systems program. D.W.L. acknowledges partial support from NASA's Kepler mission under Cooperative Agreement NNX11AB99A with the Smithsonian Astrophysical Observatory. NR 35 TC 37 Z9 37 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 SEP 10 PY 2012 VL 756 IS 2 AR L33 DI 10.1088/2041-8205/756/2/L33 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 006CH UT WOS:000308796500009 ER PT J AU Smith, DG AF Smith, David G. TI A checklist of the moray eels of the world (Teleostei: Anguilliformes: Muraenidae) SO ZOOTAXA LA English DT Article ID WESTERN INDIAN-OCEAN; INDO-PACIFIC MORAYS; EASTERN TAIWAN; GYMNOTHORAX; PISCES; GENUS; REDESCRIPTION; IDENTITY; ISLANDS; UROPTERYGIINAE AB A checklist of the currently recognized species of moray eels (Muraenidae) is presented. One hundred ninety seven species are considered to be valid, in 15 genera, and two subfamilies. The account for each valid species contains bibliographic information for that species and all synonyms, including primary type specimens and type locality. Also given for each species is the number of vertebrae, the mean vertebral formula (MVF), the general geographic distribution, and any explanatory remarks that may be needed. A list of nominal genera and species is given, with the current status of each. Separate lists are provided for names that cannot be assigned to known species (incertae sedis) and those that are unavailable. C1 Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Smith, DG (reprint author), Smithsonian Inst, Museum Support Ctr, MRC-534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM smithd@si.edu NR 303 TC 6 Z9 7 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 SEP 7 PY 2012 IS 3474 BP 1 EP + PG 63 WC Zoology SC Zoology GA 004HS UT WOS:000308672900001 ER PT J AU Pham, LM Bar-Gill, N Le Sage, D Belthangady, C Stacey, A Markham, M Twitchen, DJ Lukin, MD Walsworth, RL AF Pham, L. M. Bar-Gill, N. Le Sage, D. Belthangady, C. Stacey, A. Markham, M. Twitchen, D. J. Lukin, M. D. Walsworth, R. L. TI Enhanced metrology using preferential orientation of nitrogen-vacancy centers in diamond SO PHYSICAL REVIEW B LA English DT Article ID SINGLE ELECTRONIC SPIN; NUCLEAR-SPIN; NANOSCALE RESOLUTION; COHERENCE; DYNAMICS; READOUT; QUBITS; CVD AB We demonstrate preferential orientation of nitrogen-vacancy (NV) color centers along two of four possible crystallographic axes in diamonds grown by chemical vapor deposition on the {100} face. We identify the relevant growth regime and present a possible explanation of this effect. We show that preferential orientation provides increased optical readout contrast for NV multispin measurements, including enhanced ac magnetic-field sensitivity, thus providing an important step towards high-fidelity multispin-qubit quantum information processing, sensing, and metrology. C1 [Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Bar-Gill, N.; Lukin, M. D.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bar-Gill, N.; Le Sage, D.; Belthangady, C.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stacey, A.; Markham, M.; Twitchen, D. J.] Element Six Ltd, Ascot SL5 8BP, Berks, England. RP Pham, LM (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. OI Le Sage, David/0000-0003-1678-9491; Stacey, Alastair/0000-0002-3794-0317 FU NSF; Defense Advanced Research Project Agency FX This work was supported by the NSF and Defense Advanced Research Project Agency (QuEST and QuASAR programs). We gratefully acknowledge helpful technical discussions with Keigo Arai, David Glenn, and Huiliang Zhang. Defense Advanced Research Project Agency NR 25 TC 20 Z9 20 U1 5 U2 36 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 SEP 6 PY 2012 VL 86 IS 12 AR 121202 DI 10.1103/PhysRevB.86.121202 PG 5 WC Physics, Condensed Matter SC Physics GA 000NM UT WOS:000308393000001 ER PT J AU Pendleton, L Donato, DC Murray, BC Crooks, S Jenkins, WA Sifleet, S Craft, C Fourqurean, JW Kauffman, JB Marba, N Megonigal, P Pidgeon, E Herr, D Gordon, D Baldera, A AF Pendleton, Linwood Donato, Daniel C. Murray, Brian C. Crooks, Stephen Jenkins, W. Aaron Sifleet, Samantha Craft, Christopher Fourqurean, James W. Kauffman, J. Boone Marba, Nuria Megonigal, Patrick Pidgeon, Emily Herr, Dorothee Gordon, David Baldera, Alexis TI Estimating Global "Blue Carbon" Emissions from Conversion and Degradation of Vegetated Coastal Ecosystems SO PLOS ONE LA English DT Article ID MANGROVE FOREST DISTRIBUTIONS; SEAGRASS ECOSYSTEMS; DYNAMICS; METHANE; CO2; SEQUESTRATION; DEFORESTATION; CONSERVATION; SEDIMENTS; ESTUARY AB Recent attention has focused on the high rates of annual carbon sequestration in vegetated coastal ecosystems-marshes, mangroves, and seagrasses-that may be lost with habitat destruction ('conversion'). Relatively unappreciated, however, is that conversion of these coastal ecosystems also impacts very large pools of previously-sequestered carbon. Residing mostly in sediments, this 'blue carbon' can be released to the atmosphere when these ecosystems are converted or degraded. Here we provide the first global estimates of this impact and evaluate its economic implications. Combining the best available data on global area, land-use conversion rates, and near-surface carbon stocks in each of the three ecosystems, using an uncertainty-propagation approach, we estimate that 0.15-1.02 Pg (billion tons) of carbon dioxide are being released annually, several times higher than previous estimates that account only for lost sequestration. These emissions are equivalent to 3-19% of those from deforestation globally, and result in economic damages of $US 6-42 billion annually. The largest sources of uncertainty in these estimates stems from limited certitude in global area and rates of land-use conversion, but research is also needed on the fates of ecosystem carbon upon conversion. Currently, carbon emissions from the conversion of vegetated coastal ecosystems are not included in emissions accounting or carbon market protocols, but this analysis suggests they may be disproportionally important to both. Although the relevant science supporting these initial estimates will need to be refined in coming years, it is clear that policies encouraging the sustainable management of coastal ecosystems could significantly reduce carbon emissions from the land-use sector, in addition to sustaining the well-recognized ecosystem services of coastal habitats. C1 [Pendleton, Linwood; Murray, Brian C.; Jenkins, W. Aaron; Gordon, David] Duke Univ, Nicholas Inst Environm Policy Solut, Durham, NC 27708 USA. [Donato, Daniel C.] Univ Wisconsin, Ecosyst & Landscape Ecol Lab, Madison, WI USA. [Crooks, Stephen] ESA Phillip Williams & Associates, San Francisco, CA USA. [Sifleet, Samantha] US EPA, Res Triangle Pk, NC 27711 USA. [Craft, Christopher] Indiana Univ, Sch Publ & Environm Affairs, Bloomington, IN USA. [Fourqurean, James W.] Florida Int Univ, Dept Biol Sci, N Miami, FL USA. [Fourqurean, James W.] Florida Int Univ, SE Environm Res Ctr, N Miami, FL USA. [Kauffman, J. Boone] Oregon State Univ, Dept Fisheries & Wildlife, Corvallis, OR 97331 USA. [Kauffman, J. Boone] Ctr Int Forest Res, Bogor, Indonesia. [Marba, Nuria] Mediterranean Inst Adv Studies, Dept Global Change Res, Esporles, Illes Balears, Spain. [Megonigal, Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Pidgeon, Emily] Conservat Int, Arlington, VA USA. [Herr, Dorothee] Int Union Conservat Nat, Washington, DC USA. [Baldera, Alexis] Ocean Conservancy, Baton Rouge, LA USA. RP Pendleton, L (reprint author), Duke Univ, Nicholas Inst Environm Policy Solut, Durham, NC 27708 USA. EM ddonato@wisc.edu RI Fourqurean, James/B-4606-2008; Marba, Nuria/H-8136-2015 OI Fourqurean, James/0000-0002-0811-8500; Marba, Nuria/0000-0002-8048-6789 FU Linden Trust for Conservation; Roger and Victoria Sant FX Funding for this effort was provided by the Linden Trust for Conservation (lindentrust.org) and Roger and Victoria Sant. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 141 Z9 148 U1 31 U2 347 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD SEP 4 PY 2012 VL 7 IS 9 AR e43542 DI 10.1371/journal.pone.0043542 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 002ZJ UT WOS:000308577600013 PM 22962585 ER PT J AU Clough, GW AF Clough, G. Wayne TI From the Castle 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 SEP PY 2012 VL 43 IS 5 SI SI BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 134KN UT WOS:000318209200002 ER PT J AU Tarr, K AF Tarr, Kimberly TI ROUND THE WORLD AND BACK AGAIN Mapping the Cultural and Historic Significance of the Adelaide Pearson Film Collection SO MOVING IMAGE LA English DT Article C1 [Tarr, Kimberly] NYU Libraries, New York, NY USA. [Tarr, Kimberly] Smithsonian Natl Museum Amer Hist, Multiyear Audiovisual Archiving Project, Washington, DC USA. RP Tarr, K (reprint author), NYU Libraries, New York, NY USA. NR 41 TC 0 Z9 0 U1 0 U2 0 PU UNIV MINNESOTA PRESS PI MINNEAPOLIS PA MILL PLACE, SUITE 290 111 THIRD AVE S, MINNEAPOLIS, MN 55401-2520 USA SN 1532-3978 J9 MOV IMAGE JI Mov. Image PD FAL PY 2012 VL 12 IS 2 BP 95 EP 120 PG 26 WC Film, Radio, Television SC Film, Radio & Television GA 087UO UT WOS:000314789600005 ER PT J AU Mawdsley, JR Sithole, H AF Mawdsley, J. R. Sithole, H. TI Tiger beetles (Coleoptera: Cicindelidae) of the Kruger National Park, South Africa: distribution, habitat associations and conservation status SO AFRICAN ENTOMOLOGY LA English DT Article DE tiger beetle; Cicindelidae; biodiversity; riverine areas; sand veld; microhabitats; South African Biodiversity Act of 2004 ID ECOLOGY AB Thirty-two species of tiger beetles (Coleoptera: Cicindelidae) have been recorded from the Kruger National Park, South Africa. Information about the distribution, habitat associations and seasonal activity patterns of tiger beetles in the Kruger National Park is summarized from data collected in field surveys conducted between 2006 and 2011, museum specimen records and literature records. Two ecological communities in the park support large and diverse assemblages of tiger beetle species: upland 'sand veld' communities and riverine/riparian areas. Information about adult and/or larval microhabitat associations is presented for 23 of the tiger beetle species occurring in the Kruger National Park. The park supports 25.8% of the species of Cicindelidae known to occur in South Africa. Eighteen species of tiger beetles recorded from the park (including three species of Manticora Fabricius, the species Megacephala regalis regalis Boheman, and 14 species of Dromica Dejean) are listed as 'protected species' under the South African Biodiversity Act of 2004. C1 [Mawdsley, J. R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. [Sithole, H.] S African Natl Pk, ZA-8306 Kimberley, South Africa. RP Mawdsley, JR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187,POB 37012, Washington, DC 20013 USA. EM mawdsley@heinzcenter.org NR 20 TC 0 Z9 0 U1 1 U2 9 PU ENTOMOLOGICAL SOC SOUTHERN AFRICA PI HATFIELD PA PO BOX 13162, HATFIELD 0028, SOUTH AFRICA SN 1021-3589 J9 AFR ENTOMOL JI Afr. Entomol. PD SEP PY 2012 VL 20 IS 2 BP 266 EP 275 PG 10 WC Entomology SC Entomology GA 068ZQ UT WOS:000313405100008 ER PT J AU Cordova, A AF Cordova, Amalia TI Indigenous Screen Cultures in Canada SO LABOUR-LE TRAVAIL LA English DT Book Review C1 [Cordova, Amalia] NYU, Smithsonian Natl Museum Amer Indian, New York, NY 10003 USA. RP Cordova, A (reprint author), NYU, Smithsonian Natl Museum Amer Indian, New York, NY 10003 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CANADIAN COMMITTEE LABOUR HISTORY PI ST JOHNS PA MEMORIAL UNIV NEWFOUNDLAND DEPT HISTORY, ST JOHNS, NEWFOUNDLAND A1C 5S7, CANADA SN 0700-3862 J9 LABOUR-TRAVAIL JI Labour-Trav. PD FAL PY 2012 IS 70 BP 299 EP 301 PG 3 WC History; Industrial Relations & Labor SC History; Business & Economics GA 069XO UT WOS:000313470600030 ER PT J AU Quinn, K AF Quinn, Kelly TI Public Housing as Preparation for Public Life SO JOURNAL OF THE AMERICAN PLANNING ASSOCIATION LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Quinn, K (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 3 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0194-4363 J9 J AM PLANN ASSOC JI J. Am. Plan. Assoc. PD SEP 1 PY 2012 VL 78 IS 4 SI SI BP 432 EP 433 DI 10.1080/01944363.2012.737978 PG 2 WC Planning & Development; Urban Studies SC Public Administration; Urban Studies GA 049BX UT WOS:000311958100008 ER PT J AU Balmaverde, B Capetti, A Grandi, P Torresi, E Chiaberge, M Zaurin, JR Tremblay, GR Axon, DJ Baum, SA Giovannini, G Kharb, P Macchetto, FD O'Dea, CP Sparks, W AF Balmaverde, B. Capetti, A. Grandi, P. Torresi, E. Chiaberge, M. Rodriguez Zaurin, J. Tremblay, G. R. Axon, D. J. Baum, S. A. Giovannini, G. Kharb, P. Macchetto, F. D. O'Dea, C. P. Sparks, W. TI Extended soft X-ray emission in 3CR radio galaxies at z < 0.3: high excitation and broad line galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; X-rays: galaxies; ISM: jets and outflows ID HUBBLE-SPACE-TELESCOPE; OPTICAL SPECTROSCOPIC SURVEY; HST SNAPSHOT SURVEY; XMM-NEWTON; IMAGING POLARIMETRY; SOURCE COUNTERPARTS; LOW-REDSHIFT; CHANDRA OBSERVATIONS; SPECTRAL-ANALYSIS; SEYFERT-GALAXIES AB We analyze Chandra observations of diffuse soft X-ray emission associated with a complete sample of 3CR radio galaxies at z < 0.3. We focus on the properties of the spectroscopic sub-classes of high excitation galaxies (HEGs) and broad line objects (BLOs). Among the 33 HEGs we detect extended (or possibly extended) emission in about 40% of the sources; the fraction is even higher (8/10) when restricting the analysis to the objects with exposure times larger than 10 ks. In the 18 BLOs, extended emission is seen only in two objects; this lower detection rate can be ascribed to the presence of their bright X-ray nuclei that easily outshine any genuine diffuse emission. A very close correspondence between the soft X-ray and optical line morphology emerges. We also find that the ratio between [O III] and extended soft X-ray luminosity is confined within a factor of 2 around a median value of 5. Both results are similar to what is seen in Seyfert galaxies. We discuss different processes that could explain the soft X-ray emission and conclude that the photoionization of extended gas, coincident with the narrow line region, is the favored mechanism. C1 [Balmaverde, B.; Capetti, A.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. [Grandi, P.; Torresi, E.] IASF Ist Astrofis & Fis Cosm Bologna, INAF, I-40129 Bologna, Italy. [Chiaberge, M.; Giovannini, G.] Ist Radioastron Bologna, INAF, I-40129 Bologna, Italy. [Chiaberge, M.; Macchetto, F. D.; Sparks, W.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Chiaberge, M.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Rodriguez Zaurin, J.] Inst Astrofis Canarias, Tenerife 38205, Spain. [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. [Axon, D. J.; Kharb, P.; O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Axon, D. J.] Univ Sussex, Sch Math & Phys Sci, Brighton BN2 9BH, E Sussex, England. [Baum, S. A.] Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Baum, S. A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Giovannini, G.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [O'Dea, C. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Balmaverde, B (reprint author), Osserv Astron Torino, INAF, Str Osservatorio 20, I-10025 Pino Torinese, Italy. EM balmaverde@oato.inaf.it OI Balmaverde, Barbara/0000-0002-0690-0638; Grandi, Paola/0000-0003-1848-6013; capetti, alessandro/0000-0003-3684-4275; Giovannini, Gabriele/0000-0003-4916-6362; Tremblay, Grant/0000-0002-5445-5401; TORRESI, ELEONORA/0000-0002-5201-010X FU Italian Space Agency [ASI-INAF I/009/10/0, ASI/GLAST I/017/07/0] FX We wish to honor the memory of our great friend and colleague David Axon, who has been the steadfast inspiration and participant in this and many other key papers that through many years of dedicated efforts have led to significant breakthroughs and greater understanding of the physics of active galaxies. He will be greatly missed by all of us. We are grateful to the anonymous referee for usuful comments that significantly improved the paper. We thank also S. Bianchi and G. Matt for helpful comments on the manuscript. This work was mainly supported by the Italian Space Agency through contract ASI-INAF I/009/10/0 and ASI/GLAST I/017/07/0. NR 77 TC 5 Z9 5 U1 1 U2 1 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 SEP PY 2012 VL 545 AR A143 DI 10.1051/0004-6361/201219561 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900143 ER PT J AU Buat, V Noll, S Burgarella, D Giovannoli, E Charmandaris, V Pannella, M Hwang, HS Elbaz, D Dickinson, M Magdis, G Reddy, N Murphy, EJ AF Buat, V. Noll, S. Burgarella, D. Giovannoli, E. Charmandaris, V. Pannella, M. Hwang, H. S. Elbaz, D. Dickinson, M. Magdis, G. Reddy, N. Murphy, E. J. TI GOODS-Herschel: dust attenuation properties of UV selected high redshift galaxies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: high-redshift; galaxies: ISM; galaxies: starburst; ultraviolet: galaxies; dust, extinction ID STAR-FORMING GALAXIES; SIMILAR-TO 2; LYMAN BREAK GALAXIES; STELLAR POPULATION SYNTHESIS; SPECTRAL ENERGY-DISTRIBUTION; FORMATION RATE DENSITY; INITIAL MASS FUNCTION; K-SELECTED GALAXIES; DEEP FIELD-SOUTH; STARBURST GALAXIES AB Context. Dust attenuation in galaxies is poorly known, especially at high redshift. And yet the amount of dust attenuation is a key parameter to deduce accurate star formation rates from ultraviolet (UV) rest-frame measurements. The wavelength dependence of the dust attenuation is also of fundamental importance to interpret the observed spectral energy distributions (SEDs) and to derive photometric redshifts or physical properties of galaxies. Aims. We want to study dust attenuation at UV wavelengths at high redshift, where the UV is redshifted to the observed visible light wavelength range. In particular, we search for a UV bump and related implications for dust attenuation determinations. Methods. We use photometric data in the Chandra Deep Field South (CDFS), obtained in intermediate and broad band filters by the MUSYC project, to sample the UV rest-frame of 751 galaxies with 0.95 < z < 2.2. When available, infrared (IR) Herschel/PACS** data from the GOODS-Herschel project, coupled with Spitzer/MIPS measurements, are used to estimate the dust emission and to constrain dust attenuation. The SED of each source is fit using the CIGALE code. The amount of dust attenuation and the characteristics of the dust attenuation curve are obtained as outputs of the SED fitting process, together with other physical parameters linked to the star formation history. Results. The global amount of dust attenuation at UV wavelengths is found to increase with stellar mass and to decrease as UV luminosity increases. A UV bump at 2175 angstrom is securely detected in 20% of the galaxies, and the mean amplitude of the bump for the sample is similar to that observed in the extinction curve of the LMC supershell region. This amplitude is found to be lower in galaxies with very high specific star formation rates, and 90% of the galaxies exhibiting a secure bump are at z < 1.5. The attenuation curve is confirmed to be steeper than that of local starburst galaxies for 20% of the galaxies. The large dispersion found for these two parameters describing the attenuation law is likely to reflect a wide diversity of attenuation laws among galaxies. The relations between dust attenuation, IR-to-UV flux ratio, and the slope of the UV continuum are derived for the mean attenuation curve found for our sample. Deviations from the average trends are found to correlate with the age of the young stellar population and the shape of the attenuation curve. C1 [Buat, V.; Burgarella, D.; Giovannoli, E.] Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France. [Noll, S.] Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Giovannoli, E.] Univ Western Cape, ZA-7535 Cape Town, South Africa. [Charmandaris, V.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, V.] Univ Crete, Inst Theoret & Computat Phys, Iraklion 71003, Greece. [Charmandaris, V.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece. [Charmandaris, V.] Observ Paris, LERMA, CNRS UMR 8112, F-75014 Paris, France. [Pannella, M.; Elbaz, D.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, CEA,DSM,Irfu,CNRS, F-91191 Gif Sur Yvette, France. [Hwang, H. S.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dickinson, M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Reddy, N.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Murphy, E. J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Buat, V (reprint author), Aix Marseille Univ, CNRS, LAM Lab Astrophys Marseille UMR 7326, F-13388 Marseille, France. EM veronique.buat@oamp.fr RI Charmandaris, Vassilis/A-7196-2008; Magdis, Georgios/C-7295-2014 OI Charmandaris, Vassilis/0000-0002-2688-1956; Magdis, Georgios/0000-0002-4872-2294 FU French National Agency for research [ANR-09-BLAN-0224]; NASA through JPL/Caltech; BMVIT (Austria); ESA-PRODEX (Belgium); CEA/CNES (France); DLR (Germany); ASI/INAF (Italy); CICYT/MCYT (Spain) FX This work is partially supported by the French National Agency for research (ANR-09-BLAN-0224). Support for the US-based coauthors was provided by NASA through an award issued by JPL/Caltech. PACS has been developed by a consortium of institutes led by MPE (Germany) and including UVIE (Austria); KU Leuven, CSL, IMEC (Belgium); CEA, LAM (France); MPIA (Germany); INAFIFSI/ OAA/OAP/OAT, LENS, SISSA (Italy); IAC (Spain). This development has been supported by the funding agencies BMVIT (Austria), ESA-PRODEX (Belgium), CEA/CNES (France), DLR (Germany), ASI/INAF (Italy), and CICYT/MCYT (Spain). NR 82 TC 55 Z9 55 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 SEP PY 2012 VL 545 AR A141 DI 10.1051/0004-6361/201219405 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900141 ER PT J AU Henrichs, HF Kolenberg, K Plaggenborg, B Marsden, SC Waite, IA Landstreet, JD Wade, GA Grunhut, JH Oksala, ME AF Henrichs, H. F. Kolenberg, K. Plaggenborg, B. Marsden, S. C. Waite, I. A. Landstreet, J. D. Wade, G. A. Grunhut, J. H. Oksala, M. E. CA MiMes Collaboration TI Discovery of a magnetic field in the early B-type star sigma Lupi SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: early-type; stars: magnetic field; stars: winds, outflows; stars: rotation; starspots; stars: abundances ID SLOWLY PULSATING-B; O-TYPE STARS; ACTIVE STARS; BETA-CEPHEI; ULTRAVIOLET PHOTOMETRY; PERIODIC VARIABLES; SPECTRAL TYPES; STELLAR WINDS; MASSIVE STARS; VARIABILITY AB Context. Magnetic early B-type stars are rare. Indirect indicators are needed to identify them before investing in time-intensive spectropolarimetric observations. Aims. We use the strongest indirect indicator of a magnetic field in B stars, which is periodic variability of ultraviolet (UV) stellar wind lines occurring symmetric about the approximate rest wavelength. Our aim is to identify probable magnetic candidates which would become targets for follow-up spectropolarimetry to search for a magnetic field. Methods. From the UV wind line variability the B1/B2V star sigma Lupi emerged as a new magnetic candidate star. AAT spectropolarimetric measurements with SEMPOL were obtained. The longitudinal component of the magnetic field integrated over the visible surface of the star was determined with the least-squares deconvolution method. Results. The UV line variations of sigma Lupi are similar to what is known in magnetic B stars, but no periodicity could be determined. We detected a varying longitudinal magnetic field with amplitude of about 100 G with error bars of typically 20 G, which supports an oblique magnetic-rotator configuration. The equivalent width variations of the UV lines, the magnetic and the optical-line variations are consistent with the photometric period of 3.02 d, which we identify with the rotation period of the star. Additional observations with ESPaDOnS attached to the CFHT confirmed this discovery, and allowed the determination of a precise magnetic period. Analysis revealed that sigma Lupi is a helium-strong star, with an enhanced nitrogen abundance and an underabundance of carbon, and has a chemically spotted surface. Conclusions. sigma Lupi is a magnetic oblique rotator, and is a He-strong star. Like in other magnetic B stars the UV wind emission appears to originate close to the magnetic equatorial plane, with maximum emission occurring when a magnetic pole points towards the Earth. The 3.01972 +/- 0.00043 d magnetic rotation period is consistent with the photometric period, with maximum light corresponding to maximum magnetic field. C1 [Henrichs, H. F.; Plaggenborg, B.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Henrichs, H. F.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Kolenberg, K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kolenberg, K.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Marsden, S. C.] Australian Astron Observ, Epping, NSW 1710, Australia. [Marsden, S. C.] James Cook Univ, Sch Engn & Phys Sci, Ctr Astron, Townsville, Qld 4811, Australia. [Waite, I. A.] Univ So Queensland, Fac Sci, Toowoomba, Qld 4350, Australia. [Landstreet, J. D.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Landstreet, J. D.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Wade, G. A.; Grunhut, J. H.] Royal Mil Coll Canada, Dept Phys, Kingston, ON, Canada. [Oksala, M. E.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. RP Henrichs, HF (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM h.f.henrichs@uva.nl RI Oksala, Mary/G-9902-2014 FU Natural Sciences and Engineering Research Council of Canada FX We are grateful to Coralie Neiner and Nolan Walborn for their comments on the manuscript. H. F. H. fondly acknowledge the warm hospitality of the Department of Astrophysics, Radboud University, Nijmegen, under the inspiring directorship of Prof. Paul Groot, where this work was initiated. The authors would like to thank the technical staff at the AAT for their helpful assistance during the acquisition of the spectroscopic data. G. A. W. and J.L. acknowledge Discovery Grant support from the Natural Sciences and Engineering Research Council of Canada. This project used the facilities of SIMBAD and Hipparcos. This research made use of INES data from the IUE satellite and of NASAs Astrophysics Data System. NR 64 TC 5 Z9 5 U1 0 U2 1 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 SEP PY 2012 VL 545 AR A119 DI 10.1051/0004-6361/201219632 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900119 ER PT J AU Piano, G Tavani, M Vittorini, V Trois, A Giuliani, A Bulgarelli, A Evangelista, Y Coppi, P Del Monte, E Sabatini, S Striani, E Donnarumma, I Hannikainen, D Koljonen, KII McCollough, M Pooley, G Trushkin, S Zanin, R Barbiellini, G Cardillo, M Cattaneo, PW Chen, AW Colafrancesco, S Feroci, M Fuschino, F Giusti, M Longo, F Morselli, A Pellizzoni, A Pittori, C Pucella, G Rapisarda, M Rappoldi, A Soffitta, P Trifoglio, M Vercellone, S Verrecchia, F AF Piano, G. Tavani, M. Vittorini, V. Trois, A. Giuliani, A. Bulgarelli, A. Evangelista, Y. Coppi, P. Del Monte, E. Sabatini, S. Striani, E. Donnarumma, I. Hannikainen, D. Koljonen, K. I. I. McCollough, M. Pooley, G. Trushkin, S. Zanin, R. Barbiellini, G. Cardillo, M. Cattaneo, P. W. Chen, A. W. Colafrancesco, S. Feroci, M. Fuschino, F. Giusti, M. Longo, F. Morselli, A. Pellizzoni, A. Pittori, C. Pucella, G. Rapisarda, M. Rappoldi, A. Soffitta, P. Trifoglio, M. Vercellone, S. Verrecchia, F. TI The AGILE monitoring of Cygnus X-3: transient gamma-ray emission and spectral constraints SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: Cygnus X-3; X-rays: binaries; radio continuum: general; radiation mechanisms: non-thermal; stars: winds, outflows; gamma rays: general ID HARD X-RAY; MICROQUASAR GRS 1915+105; CYG X-3; SILICON TRACKER; BINARY CYGNUS-X-3; RELATIVISTIC JET; STELLAR WIND; BLACK-HOLE; VARIABILITY; LINES AB We present the AGILE-GRID (Astro-rivelatore Gamma a Immagini LEggero - Gamma-Ray Imaging Detector) monitoring of Cygnus X-3, during the period between November 2007 and July 2009. We report here the whole AGILE-GRID monitoring of Cygnus X-3 in the AGILE "pointing" mode data-taking, to confirm that the gamma-ray activity coincides with the same repetitive pattern of multiwavelength emission and analyze in depth the overall gamma-ray spectrum by assuming both leptonic and hadronic scenarios. Seven intense gamma-ray events were detected in this period, with a typical event lasting one or two days. These durations are longer than the likely cooling times of the gamma-ray emitting particles, implying we see continuous acceleration rather than the result of an impulsive event such as the ejection of a single plasmoid that then cools as it propagates outwards. Cross-correlating the AGILE-GRID light curve with both X-ray and radio monitoring data, we find that the main events of gamma-ray activity were detected while the system was in soft spectral X-ray states (RXTE/ASM (Rossi X-ray Timing Explorer/All-Sky Monitor) count rate in the 3-5 keV band >= 3 counts s(-1)), that coincide with local and often sharp minima of the hard X-ray flux (Swift/BAT (Burst Alert Telescope) count rate less than or similar to 0.02 counts cm(-2) s(-1)), a few days before intense radio outbursts. This repetitive temporal coincidence between the gamma-ray transient emission and spectral state changes of the source turns out to be the spectral signature of gamma-ray activity from this microquasar. These gamma-ray events may thus reflect a sharp transition in the structure of the accretion disk and its corona, which leads to a rebirth of the microquasar jet and subsequent enhanced activity in the radio band. The gamma-ray differential spectrum of Cygnus X-3 (100 MeV-3 GeV), which was obtained by averaging the data collected by the AGILE-GRID during the gamma-ray events, is consistent with a power law of photon index alpha = 2.0 +/- 0.2. Finally, we examine leptonic and hadronic emission models for the gamma-ray events and find that both scenarios are valid. In the leptonic model - based on inverse Compton scatterings of mildly relativistic electrons on soft photons from both the Wolf-Rayet companion star and the accretion disk - the emitting particles may also contribute to the overall hard X-ray spectrum, possibly explaining the hard non-thermal power-law tail seen during special soft X-ray states in Cygnus X-3. C1 [Piano, G.; Tavani, M.; Vittorini, V.; Evangelista, Y.; Del Monte, E.; Sabatini, S.; Donnarumma, I.; Cardillo, M.; Feroci, M.; Giusti, M.; Soffitta, P.] INAF IAPS, I-00133 Rome, Italy. [Piano, G.; Tavani, M.; Sabatini, S.; Giusti, M.] CIFS Torino, I-10133 Turin, Italy. [Tavani, M.; Striani, E.; Cardillo, M.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Giuliani, A.; Chen, A. W.] INAF IASF Milano, I-20133 Milan, Italy. [Bulgarelli, A.; Fuschino, F.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy. [Barbiellini, G.; Longo, F.] Dipartimento Fis, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] INFN Trieste, I-34127 Trieste, Italy. [Cattaneo, P. W.; Rappoldi, A.] INFN Pavia, I-27100 Pavia, Italy. [Tavani, M.; Sabatini, S.; Striani, E.; Morselli, A.] INFN Roma Tor Vergata, I-00133 Rome, Italy. [Trois, A.; Pellizzoni, A.] INAF Osservatorio Astron Cagliari, I-09012 Capoterra, Italy. [Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy. [Pittori, C.; Verrecchia, F.] ASI Sci Data Ctr ASDC, Rome, Italy. [Colafrancesco, S.; Pittori, C.; Verrecchia, F.] INAF OAR, I-00040 Monte Porzio Catone, Italy. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, WITS, ZA-2050 Johannesburg, South Africa. [Vercellone, S.] INAF IASF Palermo, I-90146 Palermo, Italy. [Coppi, P.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Hannikainen, D.; Koljonen, K. I. I.] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland. [Hannikainen, D.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [McCollough, M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Pooley, G.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Trushkin, S.] Special Astrophys Observ RAS, Nizhnii Arkhyz 369169, Russia. [Zanin, R.] Univ Barcelona Marti & Franques 1, Fac Fis, Inst Ciencies Cosmos, Dept Astron & Meteorol, Barcelona 08028, Spain. RP Piano, G (reprint author), INAF IAPS, Via Fosso Cavaliere 100, I-00133 Rome, Italy. EM giovanni.piano@iaps.inaf.it; giovanni.piano@iaps.inaf.it RI Trifoglio, Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016; OI Donnarumma, Immacolata/0000-0002-4700-4549; Sabatini, Sabina/0000-0003-2076-5767; Koljonen, Karri/0000-0002-9677-1533; Tavani, Marco/0000-0003-2893-1459; Trifoglio, Massimo/0000-0002-2505-3630; trois, alessio/0000-0002-3180-6002; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Soffitta, Paolo/0000-0002-7781-4104; Vercellone, Stefano/0000-0003-1163-1396; Fuschino, Fabio/0000-0003-2139-3299; Pittori, Carlotta/0000-0001-6661-9779; Feroci, Marco/0000-0002-7617-3421; Bulgarelli, Andrea/0000-0001-6347-0649; Cardillo, Martina/0000-0001-8877-3996; Verrecchia, Francesco/0000-0003-3455-5082 FU ASI [I/089/06/2, I/042/10/0] FX The authors are grateful to the anonymous referee for her/his stimulating comments on the manuscript. We also thank A. Zdziarski for discussions about this work. This investigation was carried out with partial support under ASI contracts Nos. I/089/06/2, and I/042/10/0. NR 60 TC 15 Z9 15 U1 1 U2 12 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 SEP PY 2012 VL 545 AR A110 DI 10.1051/0004-6361/201219145 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900110 ER PT J AU Raiteri, CM Villata, M Smith, PS Larionov, VM Acosta-Pulido, JA Aller, MF D'Ammando, F Gurwell, MA Jorstad, SG Joshi, M Kurtanidze, OM Lahteenmaki, A Mirzaqulov, DO Agudo, I Aller, HD Arevalo, MJ Arkharov, AA Bach, U Benitez, E Berdyugin, A Blinov, DA Blumenthal, K Buemi, CS Bueno, A Carleton, TM Carnerero, MI Carosati, D Casadio, C Chen, WP Di Paola, A Dolci, M Efimova, NV Ehgamberdiev, SA Gomez, JL Gonzalez, AI Hagen-Thorn, VA Heidt, J Hiriart, D Holikov, S Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, SO Larionova, EG Larionova, LV Leon-Tavares, J Leto, P Lin, HC Lindfors, E Marscher, AP McHardy, IM Molina, SN Morozova, DA Mujica, R Nikolashvili, MG Nilsson, K Ovcharov, EP Panwar, N Pasanen, M Puerto-Gimenez, I Reinthal, R Richter, GM Ros, JA Sakamoto, T Schwartz, RD Sillanpaa, A Smith, N Takalo, LO Tammi, J Taylor, B Thum, C Tornikoski, M Trigilio, C Troitsky, IS Umana, G Valcheva, AT Wehrle, AE AF Raiteri, C. M. Villata, M. Smith, P. S. Larionov, V. M. Acosta-Pulido, J. A. Aller, M. F. D'Ammando, F. Gurwell, M. A. Jorstad, S. G. Joshi, M. Kurtanidze, O. M. Lahteenmaki, A. Mirzaqulov, D. O. Agudo, I. Aller, H. D. Arevalo, M. J. Arkharov, A. A. Bach, U. Benitez, E. Berdyugin, A. Blinov, D. A. Blumenthal, K. Buemi, C. S. Bueno, A. Carleton, T. M. Carnerero, M. I. Carosati, D. Casadio, C. Chen, W. P. Di Paola, A. Dolci, M. Efimova, N. V. Ehgamberdiev, Sh. A. Gomez, J. L. Gonzalez, A. I. Hagen-Thorn, V. A. Heidt, J. Hiriart, D. Holikov, Sh. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, S. O. Larionova, E. G. Larionova, L. V. Leon-Tavares, J. Leto, P. Lin, H. C. Lindfors, E. Marscher, A. P. McHardy, I. M. Molina, S. N. Morozova, D. A. Mujica, R. Nikolashvili, M. G. Nilsson, K. Ovcharov, E. P. Panwar, N. Pasanen, M. Puerto-Gimenez, I. Reinthal, R. Richter, G. M. Ros, J. A. Sakamoto, T. Schwartz, R. D. Sillanpaa, A. Smith, N. Takalo, L. O. Tammi, J. Taylor, B. Thum, C. Tornikoski, M. Trigilio, C. Troitsky, I. S. Umana, G. Valcheva, A. T. Wehrle, A. E. TI Variability of the blazar 4C 38.41 (B3 1633+382) from GHz frequencies to GeV energies SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; quasars: general; quasars: individual: 4C 38.41; galaxies: jets ID ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC RADIO-SOURCES; GAMMA-RAY OBSERVATIONS; BL LACERTAE OBJECTS; 3C 454.3; GASP-WEBT; MULTIFREQUENCY OBSERVATIONS; ELECTROMAGNETIC-SPECTRUM; NOVEMBER 1995; LOUD BLAZARS AB Context. After years of modest optical activity, the quasar-type blazar 4C 38.41 (B3 1633+382) experienced a large outburst in 2011, which was detected throughout the entire electromagnetic spectrum, renewing interest in this source. Aims. We present the results of low-energy multifrequency monitoring by the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT) consortium and collaborators, as well as those of spectropolarimetric/spectrophotometric monitoring at the Steward Observatory. We also analyse high-energy observations of the Swift and Fermi satellites. This combined study aims to provide insights into the source broad-band emission and variability properties. Methods. We assemble optical, near-infrared, millimetre, and radio light curves and investigate their features and correlations. In the optical, we also analyse the spectroscopic and polarimetric properties of the source. We then compare the low-energy emission behaviour with that at high energies. Results. In the optical-UV band, several results indicate that there is a contribution from a quasi-stellar-object (QSO) like emission component, in addition to both variable and polarised jet emission. In the optical, the source is redder-when-brighter, at least for R greater than or similar to 16. The optical spectra display broad emission lines, whose flux is constant in time. The observed degree of polarisation increases with flux and is higher in the red than the blue. The spectral energy distribution reveals a bump peaking around the U band. The unpolarised emission component is likely thermal radiation from the accretion disc that dilutes the jet polarisation. We estimate its brightness to be R-QSO similar to 17.85-18 and derive the intrinsic jet polarisation degree. We find no clear correlation between the optical and radio light curves, while the correlation between the optical and.-ray flux apparently fades in time, likely because of an increasing optical to gamma-ray flux ratio. Conclusions. As suggested for other blazars, the long-term variability of 4C 38.41 can be interpreted in terms of an inhomogeneous bent jet, where different emitting regions can change their alignment with respect to the line of sight, leading to variations in the Doppler factor delta. Under the hypothesis that in the period 2008-2011 all the gamma-ray and optical variability on a one-week timescale were due to changes in d, this would range between similar to 7 and similar to 21. If the variability were caused by changes in the viewing angle theta only, then theta would go from similar to 2.6 degrees to similar to 5 degrees. Variations in the viewing angle would also account for the dependence of the polarisation degree on the source brightness in the framework of a shock-in-jet model. C1 [Raiteri, C. M.; Villata, M.; Carnerero, M. I.] Osserv Astron Torino, INAF, Turin, Italy. [Smith, P. S.; Carleton, T. M.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Larionov, V. M.; Jorstad, S. G.; Blinov, D. A.; Efimova, N. V.; Hagen-Thorn, V. A.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Larionov, V. M.; Arkharov, A. A.; Efimova, N. V.] Pulkovo Observ, St Petersburg, Russia. [Larionov, V. M.; Hagen-Thorn, V. A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Acosta-Pulido, J. A.; Arevalo, M. J.; Bueno, A.; Carnerero, M. I.; Gonzalez, A. I.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Acosta-Pulido, J. A.; Arevalo, M. J.; Bueno, A.; Carnerero, M. I.; Gonzalez, A. I.] Univ La Laguna, Dept Astrofis, E-38207 San Cristobal la Laguna, Tenerife, Spain. [Aller, M. F.; Aller, H. D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [D'Ammando, F.] Univ Perugia, Dipartimento Fis, I-06100 Perugia, Italy. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jorstad, S. G.; Joshi, M.; Agudo, I.; Blumenthal, K.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Kurtanidze, O. M.; Kurtanidze, S. O.; Nikolashvili, M. G.] Abastumani Observ, Abastumani, GA USA. [Kurtanidze, O. M.; Richter, G. M.] Astrophys Inst Potsdam, Potsdam, Germany. [Kurtanidze, O. M.; Heidt, J.] Landessternwarte Heidelberg Konigstuhl, Heidelberg, Germany. [Kurtanidze, O. M.] Kazan Fed Univ, Engelhardt Astron Observ, Tatarstan, Russia. [Lahteenmaki, A.; Leon-Tavares, J.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, Kylmala, Finland. [Agudo, I.; Casadio, C.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Bach, U.] Max Planck Inst Radioastron, Bonn, Germany. [Benitez, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Berdyugin, A.; Lindfors, E.; Pasanen, M.; Reinthal, R.; Sillanpaa, A.; Takalo, L. O.] Univ Turku, Dept Phys & Astron, Tuorla Observ, Piikkio, Finland. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, Catania, Italy. [Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain. [Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain. [Chen, W. P.; Koptelova, E.; Lin, H. C.; Panwar, N.] Natl Cent Univ, Grad Inst Astron, Jhongli, Taiwan. [Di Paola, A.] Osserv Astron Roma, INAF, Rome, Italy. [Dolci, M.] Osservatorio Astron Collurania Teramo, INAF, Teramo, Italy. [Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Mexico. [Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei 10764, Taiwan. [McHardy, I. M.] Univ Southampton, Dept Phys & Astron, Southampton, Hants, England. [Mujica, R.] Inst Nacl Astrofis Opt & Electr, Puebla, Mexico. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, Piikkio, Finland. [Ovcharov, E. P.; Valcheva, A. T.] Univ Sofia, Dept Astron, BU-1126 Sofia, Bulgaria. [Puerto-Gimenez, I.] European Space Astron Ctr INSA ESAC, Madrid, Spain. [Sakamoto, T.] CRESST, Greenbelt, MD USA. [Sakamoto, T.] Astroparticle Phys Lab NASA GSFC, Greenbelt, MD USA. [Sakamoto, T.] Univ Maryland, Dept Phys, Baltimore, MD 21201 USA. [Schwartz, R. D.] Galaxy View Observ, Sequim, WA USA. [Smith, N.] Cork Inst Technol, Cork, Ireland. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. [Thum, C.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Wehrle, A. E.] Space Sci Inst, Boulder, CO USA. RP Raiteri, CM (reprint author), Osserv Astron Torino, INAF, Turin, Italy. EM villata@oato.inaf.it RI Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Larionova, Elena/H-7287-2013; Efimova, Natalia/I-2196-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013 OI Umana, Grazia/0000-0002-6972-8388; Leto, Paolo/0000-0003-4864-2806; Raiteri, Claudia Maria/0000-0003-1784-2784; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Buemi, Carla Simona/0000-0002-7288-4613; Villata, Massimo/0000-0003-1743-6946; Carleton, Timothy/0000-0001-6650-2853; Dolci, Mauro/0000-0001-8000-5642; Larionova, Liudmila/0000-0002-0274-1481; Di Paola, Andrea/0000-0002-2189-8644; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Larionova, Elena/0000-0002-2471-6500; Efimova, Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784; FU ASI-INAF [I/009/10/0]; NSF [AST-0607523]; NASA/Fermi GI [NNX09AU16G, NNX10AP16G, NNX11AO13G]; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); CEIC (Andalucia) [P09-FQM-4784]; MINECO (Spain) [AYA2010-14844]; Georgian National Science foundation [GNSF/ST09/4-521]; Observatorio del Teide; Fermi Guest Investigator [NNX08AW56G, NNX09AU10G]; PAPIIT [IN116211]; Academy of Finland [212656, 210338, 121148]; NASA [NNX08AV61G, NNX10AU15G, NNX11AQ03G]; NSF; BU; Lowell Observatory; UK Science and Technology Facilities Council; Russian RFBR foundation [12-02-00452]; BSF [DO02 340/08]; National Aeronautics and Space Administration FX We thank the referee, Robert Hartman, for his useful comments and suggestions. We are grateful to Stefano Vercellone for information about the AGILE detection of 4C 38.41. We acknowledge financial contribution from the agreement ASI-INAF I/009/10/0. Partly based on observations with the Medicina and Noto telescopes operated by INAF - Istituto di Radioastronomia. The work at U. Michigan was supported by NSF grant AST-0607523 and NASA/Fermi GI grants NNX09AU16G, NNX10AP16G and NNX11AO13G. 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. 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. This paper is partly based on observations carried out at the IRAM-30 m Telescope, which is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). Acquisition of the MAPCAT, POLAMI, and MAPI data is partly supported by CEIC (Andalucia) grant P09-FQM-4784 and by MINECO (Spain) grant and AYA2010-14844. This work is partly supported by the Georgian National Science foundation grant GNSF/ST09/4-521. This article is partly based on observations made with the telescopes IAC80 and TCS operated by the Instituto de Astrofisica de Canarias in the Spanish Observatorio del Teide on the island of Tenerife. Most of the observations were taken under the rutinary observation programme. The IAC team acknowledges the support from the group of support astronomers and telescope operators of the Observatorio del Teide. The Steward Observatory spectropolarimetric monitoring project is supported by the Fermi Guest Investigator grants NNX08AW56G and NNX09AU10G. Data at SPM observatory were obtained through the support given by PAPIIT grant IN116211. The Metsahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The BU group acknowledges support by NASA grants NNX08AV61G, NNX10AU15G, and NNX11AQ03G. 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 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 St. Petersburg University team acknowledges support from Russian RFBR foundation via grant 12-02-00452. AZT-24 observations are made within an agreement between Pulkovo, Rome, and Teramo observatories. Data at NAO Rozhen were obtained through the support given by the BSF grant DO02 340/08. We acknowledge the use of public data from the Swift data archive. This research has made of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This research has made use of the SAO/NASA's Astrophysics Data System (ADS) and of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data obtained through the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. NR 80 TC 23 Z9 23 U1 0 U2 8 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 SEP PY 2012 VL 545 DI 10.1051/0004-6361/201219492 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900048 ER PT J AU Robitaille, TP Churchwell, E Benjamin, RA Whitney, BA Wood, K Babler, BL Meade, MR AF Robitaille, T. P. Churchwell, E. Benjamin, R. A. Whitney, B. A. Wood, K. Babler, B. L. Meade, M. R. TI A self-consistent model of Galactic stellar and dust infrared emission and the abundance of polycyclic aromatic hydrocarbons SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiative transfer; galaxies: structure; infrared: ISM ID MILKY-WAY; INTERSTELLAR DUST; STAR COUNTS; GALAXY; SKY; DISTRIBUTIONS; EXTINCTION; PLANE; IRAS; VIEW AB We present a self-consistent three-dimensional Monte-Carlo radiative transfer model of the stellar and dust emission in the Milky-Way, and have computed synthetic observations of the 3.6 to 100 mu m emission in the Galactic mid-plane. To compare the model to observations, we use the GLIMPSE, MIPSGAL, and IRAS s\urveys to construct total emission spectra, as well as longitude and latitude profiles for the emission. The distribution of stars and dust is taken from the SKY model, and the dust emissivities include an approximation of the emission from polycyclic aromatic hydrocarbons (PAHs) in addition to thermal emission. The model emission is in broad agreement with the observations, but a few modifications are needed to obtain a good fit. Firstly, by adjusting the model to include two major and two minor spiral arms rather than four equal spiral arms, the fit to the longitude profiles for vertical bar l vertical bar > 30 degrees. can be improved. Secondly, introducing a deficit in the dust distribution in the inner Galaxy results in a better fit to the shape of the IRAS longitude profiles at 60 and 100 mu m. With these modifications, the model fits the observed profiles well, although it systematically under-estimates the 5.8 and 8.0 mu m fluxes. One way to resolve this discrepancy is to increase the abundance of PAH molecules by 50% compared to the original model, although we note that changes to the dust distribution or radiation field may provide alternative solutions. Finally, we use the model to quantify which stellar populations contribute the most to the heating of different dust types and which stellar populations and dust types contribute the most to the emission at different wavelengths. C1 [Robitaille, T. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Robitaille, T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Churchwell, E.; Whitney, B. A.; Babler, B. L.; Meade, M. R.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Benjamin, R. A.] Univ Wisconsin, Dept Phys, Whitewater, WI 53190 USA. [Whitney, B. A.] Space Sci Inst, Boulder, CO 80301 USA. [Wood, K.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. RP Robitaille, TP (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM robitaille@mpia.de OI Babler, Brian/0000-0002-6984-5752; Robitaille, Thomas/0000-0002-8642-1329 FU NASA through the Spitzer Space Telescope Fellowship Program [1368699, 1367334] FX We wish to thank the referee for a careful review and for comments that helped improve this paper. We thank Bruce Draine and Aigen Li for useful discussions relating to PAH emission. 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. T.R. was supported by NASA through the Spitzer Space Telescope Fellowship Program, and B.W., E.C., M.M., and B.B. gratefuly acknowledge support from NASA through awards issued by JPL/Caltech (1368699 and 1367334). The models in this paper were run using Hyperion 0.9.0, and the scripts used to produce the results presented here are available as supplementary online material. NR 33 TC 16 Z9 16 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 SEP PY 2012 VL 545 AR A39 DI 10.1051/0004-6361/201219073 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900039 ER PT J AU Teyssier, D Quintana-Lacaci, G Marston, AP Bujarrabal, V Alcolea, J Cernicharo, J Decin, L Dominik, C Justtanont, K de Koter, A Melnick, G Menten, KM Neufeld, DA Olofsson, H Planesas, P Schmidt, M Soria-Ruiz, R Schoier, FL Szczerba, R Waters, LBFM AF Teyssier, D. Quintana-Lacaci, G. Marston, A. P. Bujarrabal, V. Alcolea, J. Cernicharo, J. Decin, L. Dominik, C. Justtanont, K. de Koter, A. Melnick, G. Menten, K. M. Neufeld, D. A. Olofsson, H. Planesas, P. Schmidt, M. Soria-Ruiz, R. Schoier, F. L. Szczerba, R. Waters, L. B. F. M. TI Herschel/HIFI observations of red supergiants and yellow hypergiants I. Molecular inventory SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: AGB and post-AGB; supergiants; circumstellar matter; submillimeter: stars ID ROTATIONAL LINE-PROFILES; GIANT BRANCH STARS; MASS-LOSS HISTORY; EVOLVED STARS; ALPHA-ORIONIS; NML-CYGNI; CIRCUMSTELLAR ENVELOPES; PROTOPLANETARY NEBULAE; EMISSION; AFGL-2343 AB Context. Red supergiant stars (RSGs) and yellow hypergiant stars (YHGs) are believed to be the high-mass counterparts of stars in the asymptotic giant branch (AGB) and early post-AGB phases. As such, they are scarcer and the properties and evolution of their envelopes are still poorly understood. Aims. We study the mass-loss in the post main-sequence evolution of massive stars, through the properties of their envelopes in the intermediate and warm gas layers. These are the regions where the acceleration of the gas takes place and the most recent mass-loss episodes can be seen. Methods. We used the HIFI instrument on-board the Herschel Space Observatory to observe sub-millimetre and far-infrared (FIR) transitions of CO, water, and their isotopologues in a sample of two RSGs (NML Cyg and Betelgeuse) and two YHGs (IRC + 10420 and AFGL 2343) stars. We present an inventory of the detected lines and analyse the information revealed by their spectral profiles. A comparison of the line intensity and shape in various transitions is used to qualitatively derive a picture of the envelope physical structure. On the basis of the results presented in an earlier study, we model the CO and (CO)-C-13 emission in IRC + 10420 and compare it to a set of lines ranging from the millimetre to the FIR. Results. Red supergiants have stronger high-excitation lines than the YHGs, indicating that they harbour dense and hot inner shells contributing to these transitions. Consequently, these high-J lines in RSGs originate from acceleration layers that have not yet reached the circumstellar terminal velocity and have narrower profiles than their flat-topped lower-J counterparts. The YHGs tend to lack this inner component, in line with the picture of detached, hollow envelopes derived from studies at longer wavelengths. NH3 is only detected in two sources (NML Cyg and IRC + 10420), which are also observed to be the strongest water-line emitters of the studied sample. In contrast, OH is detected in all sources and does not seem to correlate with the water line intensities. We show that the IRC + 10420 model derived solely from millimetre low-J CO transitions is capable of reproducing the high-J transitions when the temperature in the inner shell is simply lowered by about 30%. C1 [Teyssier, D.; Marston, A. P.] European Space Astron Ctr, Madrid 28080, Spain. [Quintana-Lacaci, G.] Inst Radio Astron Millimetr, Granada 18012, Spain. [Bujarrabal, V.] Observ Astron Nacl IGN, Alcala De Henares 28803, Spain. [Alcolea, J.; Planesas, P.; Soria-Ruiz, R.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Quintana-Lacaci, G.; Cernicharo, J.] INTA CSIC, CAB, Madrid 28850, Spain. [Decin, L.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Decin, L.; Dominik, C.; de Koter, A.; Waters, L. B. F. M.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekoek, NL-1098 Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands. [Justtanont, K.; Olofsson, H.; Schoier, F. L.] Chalmers, Onsala Space Observ, Dept Radio & Space Sci, S-43992 Onsala, Sweden. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Melnick, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Neufeld, D. A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Olofsson, H.] Univ Stockholm, AlbaNova Univ Ctr, Dept Astron, S-10691 Stockholm, Sweden. [Schmidt, M.; Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Waters, L. B. F. M.] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. RP Teyssier, D (reprint author), European Space Astron Ctr, POB 50727, Madrid 28080, Spain. EM David.Teyssier@esa.int RI Planesas, Pere/G-7950-2015; OI Planesas, Pere/0000-0002-7808-3040; /0000-0003-1689-9201; Quintana-Lacaci, Guillermo/0000-0002-5417-1943 FU German Deutsche Forschungsgemeinschaft, DFG [Os 177/1-1]; National Science Center [N203 581040] FX The authors would like to thank the anonymous referee for constructive comments, allowing in particular this paper to become more concise. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the US. Consortium members are: Canada, CSA, U. Waterloo; France, CESR, LAB, LERMA, IRAM; Germany, KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy, ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri - INAF; The Netherlands, SRON, TUD; Poland, CAMK, CBK; Spain, Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden, Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland, ETH Zurich, FHNW; USA, Caltech, JPL, NHSC. This work was supported by the German Deutsche Forschungsgemeinschaft, DFG project number Os 177/1-1. A portion of this research was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. RSz and MSch ackowledge support from grant N203 581040 of National Science Center. NR 38 TC 7 Z9 7 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 SEP PY 2012 VL 545 AR A99 DI 10.1051/0004-6361/201219545 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 012RT UT WOS:000309254900099 ER PT J AU DeVorkin, D AF DeVorkin, David TI Opening Space Research: Dreams, Technology, and Scientific Discovery SO ISIS LA English DT Book Review C1 [DeVorkin, David] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP DeVorkin, D (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD SEP PY 2012 VL 103 IS 3 BP 617 EP 618 DI 10.1086/669018 PG 4 WC History & Philosophy Of Science SC History & Philosophy of Science GA 036PI UT WOS:000311040100065 ER PT J AU Munoz, FN Saavedra, ACS AF Najera Munoz, Fernando Suarez Saavedra, Alfredo Carlos TI Horner's Syndrome Associated with Escherichia Coli Infection in a Raccoon (Procyon lotor) - A Case Report SO THAI JOURNAL OF VETERINARY MEDICINE LA English DT Article DE bite wounds; Escherichia coli; Horner's syndrome; Procyon lotor; raccoon ID DOG-BITE WOUNDS; CATS; FLORA; BACTERIOLOGY; TIGRIS AB This clinical case describes a three-year-old male raccoon (Procyon tutor), castrated, from La Lajita Oasis Park Zoological Park (Spain) which showed lack of appetite, state of mental depression and mild dehydration. During clinical examination an abscess was detected in the left ventrolateral area of the neck as well as clinical signs compatible with Homer's Syndrome in the left eye. A hypersensitivity test was carried out by sympathetic innervation with topical epinephrine 0.0001% and results suggested the presence of second-order Homer's Syndrome formed by pressure from the abscess on the sympathetic innervation of the left eye. A radiologic study of the neck was performed and blood and samples of the abscess exudates were obtained. A culture of the exudates revealed the presence of Escherichia coli. Initial treatment was introduced according to indications resulting from the previously obtained antibiogram. Symptoms disappeared six days after the initial treatment. While Homer's Syndrome is a common clinical finding in small animal clinics, it is more complicated to observe in wild carnivores, yet diagnostic and therapeutic techniques applicable to domestic animals can be used as a reference for small carnivores of the Procyonidae family. C1 [Najera Munoz, Fernando] Smithsonian Inst, Washington, DC 20560 USA. [Suarez Saavedra, Alfredo Carlos] Univ Las Palmas Gran Canaria, Sch Vet, Arucas 35416, Las Palmas, Spain. EM nanonaj@hotmail.com NR 42 TC 0 Z9 0 U1 3 U2 4 PU CHULALONGKORN UNIV PI BANGKOK PA FAC VETERINARY SCI, HENRI DUNANT RD, BANGKOK, 10330, THAILAND SN 0125-6491 J9 THAI J VET MED JI Thai J. Vet. Med. PD SEP PY 2012 VL 42 IS 3 BP 367 EP 372 PG 6 WC Veterinary Sciences SC Veterinary Sciences GA 035EO UT WOS:000310926200016 ER PT J AU Stokes, D AF Stokes, Deborah TI The African Art Gallery SO AFRICAN ARTS LA English DT Art Exhibit Review C1 Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. RP Stokes, D (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. EM StokesD@si.edu NR 1 TC 0 Z9 0 U1 0 U2 1 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD FAL PY 2012 VL 45 IS 3 SI SI BP 84 EP 86 PG 3 WC Art SC Art GA 987KK UT WOS:000307415600011 ER PT J AU Anderson, HR Butland, BK van Donkelaar, A Brauer, M Strachan, DP Clayton, T van Dingenen, R Amann, M Brunekreef, B Cohen, A Dentener, F Lai, C Lamsal, LN Martin, RV AF Anderson, H. Ross Butland, Barbara K. van Donkelaar, Aaron Brauer, Michael Strachan, David P. Clayton, Tadd van Dingenen, Rita Amann, Marcus Brunekreef, Bert Cohen, Aaron Dentener, Frank Lai, Christopher Lamsal, Lok N. Martin, Randall V. CA ISAAC Phase One Study Grp ISAAC Phase Three Study Grp TI Satellite-based Estimates of Ambient Air Pollution and Global Variations in Childhood Asthma Prevalence SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article DE air pollution; asthma prevalence; children; epidemiology; global; nitrogen dioxide; ozone; particulate matter; satellite observations ID PARTICULATE POLLUTION; MODEL TM5; ISAAC; ALLERGIES; AEROSOL; MORTALITY; SYMPTOMS; EXPOSURE; CHILDREN AB BACKGROUND: The effect of ambient air pollution on global variations and trends in asthma prevalence is unclear. OBJECTIVES: Our goal was to investigate community-level associations between asthma prevalence data from the International Study of Asthma and Allergies in Childhood (ISAAC) and satellite-based estimates of particulate matter with aerodynamic diameter < 2.5 mu m (PM2.5) and nitrogen dioxide (NO2), and modelled estimates of ozone. METHODS: We assigned satellite-based estimates of PM2.5 and NO2 at a spatial resolution of 0.1 degrees x 0.1 degrees and modeled estimates of ozone at a resolution of 1 degrees x 1 degrees to 183 ISAAC centers. We used center-level prevalence of severe asthma as the outcome and multilevel models to adjust for gross national income (GM) and center- and country-level sex, climate, and population density. We examined associations (adjusting for GNI) between air pollution and asthma prevalence over time in centers with data from ISAAC Phase One (mid-1900s) and Phase Three (2001-2003). RESULTS: For the 13- to 14-year age group (128 centers in 28 countries), the estimated average within-country change in center-level asthma prevalence per 100 children per 10% increase in center-level PM2.5 and NO2 was -0.043 [95% confidence interval (Cl): 0.139, 0.053] and 0.017 (95% Cl: 0.030, 0.064) respectively. For ozone the estimated change in prevalence per parts per billion by volume was -0.116 (95% Cl: -0.234, 0.001). Equivalent results for the 6- to 7-year age group (83 centers in 20 countries), though slightly different, were not significantly positive. For the 13- to 14-year age group, change in center-level asthma prevalence over time per 100 children per 10% increase in PM2.5 from Phase One to Phase Three was -0.139 (95% Cl: -0.347, 0.068). The corresponding association with ozone (per ppbV) was -0.171(95% Cl: -0.275, -0.067). CONCLUSION: In contrast to reports from within-community studies of individuals exposed to traffic pollution, we did not find evidence of a positive association between ambient air pollution and asthma prevalence as measured at the community level. C1 [Anderson, H. Ross] Univ London, Div Populat Hlth Sci & Educ, MRC HPA Ctr Environm & Hlth, London SW17 0RE, England. [Anderson, H. Ross] Kings Coll London, MRC HPA Ctr Environm & Hlth, London, England. [Brauer, Michael] Univ British Columbia, Vancouver, BC V5Z 1M9, Canada. [van Donkelaar, Aaron; Lamsal, Lok N.; Martin, Randall V.] Dalhousie Univ, Halifax, NS, Canada. [Clayton, Tadd] Univ Auckland, Auckland 1, New Zealand. [van Dingenen, Rita; Dentener, Frank] Commiss European Communities, Joint Res Ctr, I-21020 Ispra, Italy. [Amann, Marcus] Int Inst Appl Syst Anal, A-2361 Laxenburg, Austria. [Brunekreef, Bert] Inst Risk Assessment Sci, Utrecht, Netherlands. [Brunekreef, Bert] Julius Ctr Hlth Sci & Primary Care, Utrecht, Netherlands. [Cohen, Aaron] Hlth Effects Inst, Boston, MA USA. [Lai, Christopher] Chinese Univ Hong Kong, Hong Kong, Hong Kong, Peoples R China. [Lamsal, Lok N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD USA. [Lamsal, Lok N.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Anderson, HR (reprint author), Univ London, Div Populat Hlth Sci & Educ, MRC HPA Ctr Environm & Hlth, Cranmer Terrace, London SW17 0RE, England. EM r.anderson@sgul.ac.uk RI Lamsal, Lok/G-4781-2012; Martin, Randall/C-1205-2014; Ellwood, Philippa/G-7555-2015; OI Martin, Randall/0000-0003-2632-8402; Ellwood, Philippa/0000-0002-1994-4023; brunekreef, bert/0000-0001-9908-0060; Brauer, Michael/0000-0002-9103-9343 FU ISAAC; U.S. Environmental Protection Agency; worldwide motor industry FX We thank the children and parents who participated in ISAAC Phase One and Phase Three, the school staff for their assistance and help with coordination, the ISAAC principal investigators and their colleagues, and the many funding bodies throughout the world that supported the individual ISAAC centers and collaborators and their meetings. We also thank M. Field-Smith for her assistance with the preparation of this paper. All investigators in the Phase One and Phase Three study groups are listed in Supplemental Material, p. 3.; M.A. is employed by the International Institute for Applied Systems Analysis, Austria. A.C. is employed by the Health Effects Institute (HEI), Boston, MA, USA. The HEI receives about half of its core funds from the U.S. Environmental Protection Agency and half from the worldwide motor industry. The views expressed in this paper are those of the authors and do not necessarily reflect the views of the HEI or its sponsors. NR 36 TC 25 Z9 26 U1 3 U2 40 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD SEP PY 2012 VL 120 IS 9 BP 1333 EP 1339 DI 10.1289/ehp.1104724 PG 7 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 005YV UT WOS:000308786900034 PM 22548921 ER PT J AU Boedeker, NC Hayek, LAC Murray, S de Avila, DM Brown, JL AF Boedeker, Nancy C. Hayek, Lee-Ann C. Murray, Suzan de Avila, David M. Brown, Janine L. TI EFFECTS OF A GONADOTROPIN-RELEASING HORMONE VACCINE ON OVARIAN CYCLICITY AND UTERINE MORPHOLOGY OF AN ASIAN ELEPHANT (ELEPHAS MAXIMUS) SO JOURNAL OF ZOO AND WILDLIFE MEDICINE LA English DT Article DE Contraception; elephant; Elephas maxims; gonadotropin-releasing; progestagen; vaccine ID FREUNDS COMPLETE ADJUVANT; MOTIF-BASED ADJUVANT; WHITE-TAILED DEER; LUTEINIZING-HORMONE; GNRH VACCINE; LOXODONTA-AFRICANA; ACTIVE IMMUNIZATION; REPRODUCTIVE CYCLICITY; ESTROUS-CYCLE; BEEF HEIFERS AB This report describes the successful use of a gonadotropin-releasing hormone (GnRH) vaccine to suppress ovarian steroidogenic activity and to treat hemorrhage and anemia associated with reproductive tract pathology in a 59-year-old Asian elephant (Elephas maximus). The Repro-BLOC (R) GnRH vaccine was administered subcutaneously as a series of 4 boosters of increasing dose from 3 to 30 mg of recombinant ovalbumin-GnRH fusion protein given at variable intervals after initial vaccination with 3 mg protein. Efficacy was confirmed over a year after initial vaccination based on complete ovarian cycle suppression determined by serum progestagen analyses. Estrous cycle suppression was associated with a significant increase in GnRH. antibody binding and subsequent decrease in serum luteinizing hormone and follicle-stimulating hormone concentrations. Ultrasonographic examinations of the reproductive tract documented a reduction in uterine size and vascularity after immunization. The hematocrit level normalized soon after the initial intrauterine hemorrhage, and no recurrence of anemia has been detected. No substantive adverse effects were associated with GnRH vaccination. The results indicate that GnRH vaccination in elephants shows potential for contraception and management of uterine pathology in older elephants. C1 [Boedeker, Nancy C.; Murray, Suzan] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20008 USA. [Hayek, Lee-Ann C.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [de Avila, David M.] Washington State Univ, Dept Anim Sci, Pullman, WA 99164 USA. [Brown, Janine L.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. RP Boedeker, NC (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, 3001 Connecticut Ave NW, Washington, DC 20008 USA. EM boedekern@si.edu NR 57 TC 6 Z9 6 U1 4 U2 17 PU AMER ASSOC ZOO VETERINARIANS PI YULEE PA 581705 WHITE OAK ROAD, YULEE, FL 32097 USA SN 1042-7260 EI 1937-2825 J9 J ZOO WILDLIFE MED JI J. Zoo Wildl. Med. PD SEP PY 2012 VL 43 IS 3 BP 603 EP 614 PG 12 WC Veterinary Sciences SC Veterinary Sciences GA 018WM UT WOS:000309697600021 PM 23082526 ER PT J AU Mair, JM Cipriani, R Guzman, HM Usan, D AF Mair, James M. Cipriani, Roberto Guzman, Hector M. Usan, David TI Fishery of the Green Jack Caranx caballus (Osteichytes: Carangidae) in Las Perlas Archipelago, Pacific Panama SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE Caranx caballus; cojinua; green jack; fishery assessment; Eastern Pacific; Panama ID POPULATION ASSESSMENT; NATURAL MORTALITY; LENGTH; LARVAE; EVENT; BAY AB Green Jacks, Caranx caballus, are distributed along the Eastern Pacific coast. In Panama, C. caballus was heavily fished around Las Perlas Archipelago to sustain local markets until 2007, when the archipelago was declared a marine protected area. This first study in Panama, analyzed a sample of 4 990 individuals from Las Perlas, obtained monthly from June 2005 to June 2006, from landings at the central fish market. Average total length was 36.1 +/- 6.4cm and optimum length 38.9cm. Approximately 68% of fish lengths were within +/- 10% of the optimal length but only six (15%) were considered mega-spawners. The von Bertalanffy parameters describe a long-lived and fast growing species, while mortality rates revealed that C. caballus is under high fishing pressure. Standard length at which half of the population is mature was 38.8cm, and the size at which individuals matured massively, 33cm. Only 10-13% of the fish were immature. C. caballus reproduces two to three times per year, with peaks in December, April, and probably September, and recruits to the population at least twice per year. Catch per unit effort (CPUE) was best predicted by minimum annual values of the Multivariate ENSO/LNSO Index (MEI) (R-2=0.54). Results show that C. caballus in Pacific Panama is overfished. We recommend the raising of the minimum capture/landing size of this species in order to increase the proportion of mega-spawners in the population and guarantee the sustainability of this resource. Rev. Biol. Trop. 60(3): 1271-1288. Epub 2012 September 01. C1 [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Cipriani, Roberto] Calif State Univ Fullerton, Dept Biol Sci, Fullerton, CA 92634 USA. [Mair, James M.; Usan, David] Heriot Watt Univ, Sch Life Sci, Ctr Marine Biodivers & Biotechnol, Edinburgh EH14 4AS, Midlothian, Scotland. RP Guzman, HM (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM j.m.mair@hw.ac.uk; rcipriani@fullerton.edu; guzmanh@si.edu; dausan@hotmail.com FU DEFRA's Darwin Initiative Fund (UK); Heriot-Watt University; Smithsonian Tropical Research Institute, Panama; Universidad Simon Bolivar, Caracas, Venezuela [GID-67] FX The authors thank Carlos Guevara and Carlos Vega for processing samples and Julio Agujetas for providing access to satellite data and all fishermen who provided information about the fisheries in Las Perlas. The Government of Panama provided permits to work in the area. This research was partially sponsored by DEFRA's Darwin Initiative Fund (UK), Heriot-Watt University, Smithsonian Tropical Research Institute, Panama, and Universidad Simon Bolivar (GID-67), Caracas, Venezuela. NR 54 TC 1 Z9 1 U1 0 U2 8 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA RICA SN 0034-7744 EI 2215-2075 J9 REV BIOL TROP JI Rev. Biol. Trop. PD SEP PY 2012 VL 60 IS 3 BP 1271 EP 1288 PG 18 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 020BY UT WOS:000309784800026 PM 23025097 ER PT J AU van der Linden, FR AF van der Linden, F. Robert TI Government, Business, and Technology: U.S. Airliner Development, 1927-2012 SO WORLD NEUROSURGERY LA English DT Article DE Aeronautics; Airliner; Aviation; Boeing; Business; Government; Jet; NASA; Technology; Whitcomb C1 Smithsonian Inst, Natl Air & Space Museum, Aeronaut Div, Washington, DC 20560 USA. RP van der Linden, FR (reprint author), Smithsonian Inst, Natl Air & Space Museum, Aeronaut Div, Washington, DC 20560 USA. EM vanderlindenb@si.edu NR 12 TC 1 Z9 1 U1 0 U2 2 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1878-8750 J9 WORLD NEUROSURG JI World Neurosurg. PD SEP-OCT PY 2012 VL 78 IS 3-4 BP 206 EP 213 DI 10.1016/j.wneu.2012.06.040 PG 8 WC Clinical Neurology; Surgery SC Neurosciences & Neurology; Surgery GA 021TK UT WOS:000309908100006 PM 22749960 ER PT J AU Sheets, P Lentz, D Piperno, D Jones, J Dixon, C Maloof, G Hood, A AF Sheets, Payson Lentz, David Piperno, Dolores Jones, John Dixon, Christine Maloof, George Hood, Angela TI ANCIENT MANIOC AGRICULTURE SOUTH OF THE CEREN VILLAGE, EL SALVADOR SO LATIN AMERICAN ANTIQUITY LA English DT Article ID MANIHOT-ESCULENTA; STARCH GRAINS; MAYA; PHYTOLITHS; MAIZE; ROOT; MESOAMERICA; SUBSISTENCE; HISTORY; CASSAVA AB The role of seed crops in the Maya diet is well understood. The role of root crops in the ancient Maya diet has been controversial, with some scholars suggesting they were staples, and others arguing they were not cultivated at all. Research in the 1990s found occasional manioc plants in kitchen gardens within the Classic period Ceren village, leading to the interpretation that manioc did contribute to the diet, but was not a staple. Recent research outside the village encountered sophisticated raised-bed monocropping of manioc over an extensive area. This area vas harvested essentially all at once, about a week prior to the eruption. An estimated ten tons of tubers were harvested. The various uses of manioc include consumption as food, exchange with other settlements, fermentation, drying and storage as a powder, and as an adhesive. It is possible that many or all these alternatives were being followed. At Ceren manioc was a staple, not just an occasional adjunct to the diet. Because Ceren is toward the wet end of the ideal range for manioc cultivation, other areas of the Neotropics that receive less than 1,700 nun of precipitation may be more suitable for manioc cultivation than Ceren. C1 [Sheets, Payson] Univ Colorado, Dept Anthropol, Boulder, CO 80309 USA. [Lentz, David] Univ Cincinnati, Dept Biol Sci, Cincinnati, OH 45221 USA. [Piperno, Dolores] Smithsonian Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Piperno, Dolores] Smithsonian Trop Res Inst, Balboa, Panama. [Jones, John] Washington State Univ, Dept Anthropol, Pullman, WA 99164 USA. [Dixon, Christine] Univ Colorado, Dept Anthropol, Boulder, CO 80309 USA. [Maloof, George] Inst Costariccense Elect, San Jose, Costa Rica. [Hood, Angela] Univ Cincinnati, Dept Anthropol, Cincinnati, OH 45221 USA. RP Sheets, P (reprint author), Univ Colorado, Dept Anthropol, Boulder, CO 80309 USA. EM sheetsp@colorado.edu NR 60 TC 10 Z9 10 U1 2 U2 14 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD SEP PY 2012 VL 23 IS 3 BP 259 EP 281 PG 23 WC Archaeology SC Archaeology GA 018EZ UT WOS:000309644200002 ER PT J AU Goulding, AD Forman, WR Hickox, RC Jones, C Kraft, R Murray, SS Vikhlinin, A Coil, AL Cooper, MC Davis, M Newman, JA AF Goulding, A. D. Forman, W. R. Hickox, R. C. Jones, C. Kraft, R. Murray, S. S. Vikhlinin, A. Coil, A. L. Cooper, M. C. Davis, M. Newman, J. A. TI THE CHANDRA X-RAY POINT-SOURCE CATALOG IN THE DEEP2 GALAXY REDSHIFT SURVEY FIELDS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; surveys; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; QUASAR LUMINOSITY FUNCTION; MEDIUM-SENSITIVITY SURVEY; MS SOURCE CATALOGS; SEYFERT 2 GALAXIES; SIMILAR-TO 1; COSMOS FIELD; STAR-FORMATION; NORTH SURVEY AB We present the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined similar to 3.2 deg(2) DEEP2 (XDEEP2) survey fields, which consist of four similar to 0.7-1.1 deg(2) fields. The combined total exposures across all four XDEEP2 fields range from similar to 10 ks to 1.1 Ms. We detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. We find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of approximate to 30 sources (less than or similar to 1%). We present the combined logN - log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f(X,0.5-2 keV) similar to 2 x 10(-16) erg cm(-2) s(-1). Given the large survey area of XDEEP2, we additionally place relatively strong constraints on the logN - log S distribution at high fluxes (f(X,0.5-2 keV) similar to 3 x 10(-14) erg cm(-2) s(-1)), and find a small systematic offset (a factor similar to 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, we present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R-AB < 25.2) and find that 2126 (approximate to 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a less than or similar to 6% contamination fraction. We provide the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog. C1 [Goulding, A. D.; Forman, W. R.; Hickox, R. C.; Jones, C.; Kraft, R.; Murray, S. S.; Vikhlinin, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Hickox, R. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Coil, A. L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, La Jolla, CA 92093 USA. [Cooper, M. C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Davis, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Newman, J. A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. RP Goulding, AD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM agoulding@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 NR 92 TC 17 Z9 17 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 SEP PY 2012 VL 202 IS 1 AR 6 DI 10.1088/0067-0049/202/1/6 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016ZB UT WOS:000309557300006 ER PT J AU Usinowicz, J Wright, SJ Ives, AR AF Usinowicz, Jacob Wright, S. Joseph Ives, Anthony R. TI Coexistence in tropical forests through asynchronous variation in annual seed production SO ECOLOGY LA English DT Article DE asynchrony; Barro Colorado Island, Panama; community dynamics; competition; phylogenetic analysis; resource partitioning; seed production; storage effect; tree recruitment; tropical forest diversity ID EL-NINO; RECRUITMENT LIMITATION; DEPENDENT RECRUITMENT; VARIABLE ENVIRONMENTS; SPECIES COEXISTENCE; CLIMATE VARIABILITY; RELATIVE ABUNDANCE; NEOTROPICAL FOREST; CENTRAL-AMERICA; TREE SEEDLINGS AB The storage effect is a mechanism that can facilitate the coexistence of competing species through temporal fluctuations in reproductive output. Numerous natural systems have the prerequisites for the storage effect, yet it has rarely been quantitatively assessed. Here, we investigate the possible importance of the storage effect in explaining the coexistence of tree species in the diverse tropical forest on Barro Colorado Island, Panama. This tropical forest has been monitored for more than 20 years, and annual seed production is asynchronous among species, a primary requirement for the storage effect. We constructed a model of forest regeneration that includes species-specific recruitment through seed, sapling, and adult stages, and we parameterized the model using data for 28 species for which information is known about seedling germination and survival. Simulations of the model demonstrated that the storage effect alone can be a strong mechanism allowing long-term persistence of species. We also developed a metric to quantify the strength of the storage effect in a way comparable to classical resource partitioning. Applying this metric to seed production data from 108 species, the storage effect reduces the strength of pairwise interspecific competition to 11-43% of the strength of intraspecific competition, thereby demonstrating strong potential to facilitate coexistence. Finally, for a subset of 51 species whose phylogenetic relationships are known, we compared the strength of the storage effect between pairs of species to their phylogenetic similarity. The strength of the storage effect between closely related species was on average no different from distantly related species, implying that the storage effect can be important in promoting the coexistence of even closely related species. C1 [Usinowicz, Jacob; Ives, Anthony R.] Univ Wisconsin, Dept Zool, Madison, WI 53706 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. RP Usinowicz, J (reprint author), Univ Wisconsin, Dept Zool, 250 N Mills St, Madison, WI 53706 USA. EM usinowicz@wisc.edu RI Ives, Anthony/A-5698-2008; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU NSF [DEB 0816613]; Smithsonian Institution FX We thank Osvaldo Calderon and Andres Hernandez for collecting seed and seedling data for many, many years and the Smithsonian Institution for funding. John Kress kindly provided the barcode phylogeny we used for the phylogenetic analyses. This work was funded in part by NSF grant DEB 0816613 to A. R. Ives. NR 62 TC 7 Z9 10 U1 3 U2 51 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 SEP PY 2012 VL 93 IS 9 BP 2073 EP 2084 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 016KO UT WOS:000309517200011 PM 23094379 ER PT J AU Coverdale, TC Altieri, AH Bertness, MD AF Coverdale, Tyler C. Altieri, Andrew H. Bertness, Mark D. TI Belowground herbivory increases vulnerability of New England salt marshes to die-off SO ECOLOGY LA English DT Article DE aboveground herbivory; belowground grazing; burrowing; cordgrass die-off; herbivory; salt marsh; Sesarma reticulatum; Spartina alterniflora ID SPARTINA-ALTERNIFLORA; CONSUMER CONTROL; BELOWGROUND HERBIVORY; TROPHIC CASCADE; CRAB HERBIVORY; CAPE-COD; DEFENSES; PREDICTIONS; BURROWS; IMPACT AB Belowground herbivory is commonly overlooked as a mechanism of top-down control in vegetated habitats, particularly in aquatic ecosystems. Recent research has revealed that increased densities of the herbivorous crab Sesarma reticulatum have led to runaway herbivory and widespread salt marsh die-off on Cape Cod, Massachusetts, USA. Aboveground herbivory is a major driver of this cordgrass habitat loss, but the role of belowground grazing is poorly understood. Sesarma live in communal burrows typically consisting of 1-2 openings and containing 2-3 crabs. However, at die-off sites, burrow complexes can cover >90% of the low marsh zone, with crab densities as high as 50 crabs/m(2) and burrow opening densities of 170 openings/m(2). The magnitude of belowground Sesarma activity in association with salt marsh die-off provides an excellent opportunity to extend our knowledge of belowground herbivory impacts in coastal wetlands. Since Sesarma burrows allow access to cordgrass roots and rhizomes, and Sesarma are frequently restricted to burrows by thermal stress and predation, we hypothesized that belowground herbivory would be widespread in die-off areas. We experimentally demonstrate that Sesarma readily eat belowground roots and rhizomes in addition to aboveground cordgrass leaves. We then partitioned above-and belowground herbivory with field manipulations and found that belowground grazing is not only common, but can cause total plant mortality. Additional experiments revealed that plants remain vulnerable to belowground herbivory even after reaching a size refuge from aboveground grazing. This suggests that belowground herbivory contributes to salt marsh die-offs and adds to growing evidence that belowground herbivory is a widespread structuring force in plant communities that can limit habitat persistence. C1 [Coverdale, Tyler C.; Bertness, Mark D.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Panama. RP Coverdale, TC (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Box G-W, Providence, RI 02912 USA. EM Tyler_Coverdale@Brown.edu OI Coverdale, Tyler/0000-0003-0910-9187 FU NSF Biological Oceanography Program FX We thank Massachusetts Audubon, The Cape Cod National Seashore, and numerous municipal and conservation agencies for access to and use of field sites. N. Herrmann, E. Axelman, P. Szathmary, and S. Yin provided assistance in the laboratory and field. Q. He provided valuable comments on the manuscript and help in the field. This work was funded by the NSF Biological Oceanography Program. NR 41 TC 21 Z9 21 U1 7 U2 78 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 SEP PY 2012 VL 93 IS 9 BP 2085 EP 2094 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 016KO UT WOS:000309517200012 PM 23094380 ER PT J AU Hvidberg, CS Fishbaugh, KE Winstrup, M Svensson, A Byrne, S Herkenhoff, KE AF Hvidberg, C. S. Fishbaugh, K. E. Winstrup, M. Svensson, A. Byrne, S. Herkenhoff, K. E. TI Reading the climate record of the martian polar layered deposits SO ICARUS LA English DT Article DE Mars, polar caps; Mars, climate; Mars, atmosphere; Mars, polar geology ID ICE AGES; MARS; CAP; STRATIGRAPHY; CIRCULATION; EXPLORATION; SCIENCE; REGION AB The martian polar regions have layered deposits of ice and dust. The stratigraphy of these deposits is exposed within scarps and trough walls and is thought to have formed due to climate variations in the past. Insolation has varied significantly over time and caused dramatic changes in climate, but it has remained unclear whether insolation variations could be linked to the stratigraphic record. We present a model of layer formation based on physical processes that expresses polar deposition rates of ice and dust in terms of insolation. In this model, layer formation is controlled by the insolation record, and dust-rich layers form by two mechanisms: (1) increased summer sublimation during high obliquity, and (2) variations in the polar deposition of dust modulated by obliquity variations. The model is simple, yet physically plausible, and allows for investigations of the climate control of the polar layered deposits (PLD). We compare the model to a stratigraphic column obtained from the north polar layered deposits (NPLD) (Fishbaugh, K.E., Hvidberg, CS., Byrne, S., Russel, P.S., Herkenhoff, K.E., Winstrup, M., Kirk, R. 120104 Geophys. Res. Lett., 37, L07201) and show that the model can be tuned to reproduce complex layer sequences. The comparison with observations cannot uniquely constrain the PLD chronology, and it is limited by our interpretation of the observed stratigraphic column as a proxy for NPLD composition. We identified, however, a set of parameters that provides a chronology of the NPLD tied to the insolation record and consistently explains layer formation in accordance with observations of NPLD stratigraphy. This model dates the top 500 m of the NPLD back to similar to 1 million years with an average net deposition rate of ice and dust of 0.55 mm a(-1). The model stratigraphy contains a quasi-periodic similar to 30 m cycle, similar to a previously suggested cycle in brightness profiles from the NPLD (Laskar, J., Levrard, B., Mustard, F.[2002]. Nature, 419, 375-377; Milkovich, S., Head, J.W. [2005]. J. Geophys. Res. 110), but here related to half of the obliquity cycles of 120 and 99 kyr and resulting from a combination of the two layer formation mechanisms. Further investigations of the non-linear Insolation control of PLD formation should consider data from other geographical locations and include radar data and other stratigraphic datasets that can constrain the composition and stratigraphy of the NPLD layers. (C) 2012 Elsevier Inc. All rights reserved. C1 [Hvidberg, C. S.; Winstrup, M.; Svensson, A.] Univ Copenhagen, Ctr Ice & Climate, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Fishbaugh, K. E.] Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Byrne, S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Herkenhoff, K. E.] US Geol Survey, Flagstaff, AZ 86001 USA. RP Hvidberg, CS (reprint author), Univ Copenhagen, Ctr Ice & Climate, Niels Bohr Inst, Juliane Mules Vej 30, DK-2100 Copenhagen, Denmark. EM ch@gfy.ku.dk RI Svensson, Anders/A-2643-2010; Winstrup, Mai/M-5844-2014; Hvidberg, Christine/E-8934-2015 OI Svensson, Anders/0000-0002-4364-6085; Winstrup, Mai/0000-0002-4794-4004; Hvidberg, Christine/0000-0002-9665-1339 FU Danish National Research Foundation under Centre for Ice and Climate at University of Copenhagen; International Space Science Institute (ISSI) in Bern FX This work was supported by the Danish National Research Foundation under Centre for Ice and Climate at University of Copenhagen. Thanks to the International Space Science Institute (ISSI) in Bern for supporting workshops under the KEF-led team "Are the martian Polar Deposits a Rosetta Stone for the climate?" We thank Taylor Perron and two anonymous reviewers for constructive reviews that greatly improved the manuscript. NR 34 TC 12 Z9 12 U1 2 U2 17 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 SEP-OCT PY 2012 VL 221 IS 1 BP 405 EP 419 DI 10.1016/j.icarus.2012.08.009 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 017VV UT WOS:000309620200035 ER PT J AU Foley, DH Wilkerson, RC Dornak, LL Pecor, DB Nyari, AS Rueda, LM Long, LS Richardson, JH AF Foley, Desmond H. Wilkerson, Richard C. Dornak, L. Lynnette Pecor, David B. Nyari, Arpad S. Rueda, Leopoldo M. Long, Lewis S. Richardson, Jason H. TI SandflyMap: leveraging spatial data on sand fly vector distribution for disease risk assessments SO GEOSPATIAL HEALTH LA English DT Article DE database; distribution; SandflyMap; VectorMap; leishmaniasis; georeferencing; geographical information system AB We feature SandflyMap (www.sandflymap.org), a new map service within VectorMap (www.vectormap.org) that allows free public online access to global sand fly, tick and mosquito collection records and habitat suitability models. Given the short home range of sand flies, combining remote sensing and collection point data give a powerful insight into the environmental determinants of sand fly distribution. SandflyMap is aimed at medical entomologists, vector disease control workers, public health officials and health planners. Data are checked for geographical and taxonomic errors, and are comprised of vouchered specimen information, and both published and unpublished observation data. SandflyMap uses Microsoft Silverlight and ESRI's ArcGIS Server 10 software platform to present disease vector data and relevant remote sensing layers in an online geographical information system format. Users can view the locations of past vector collections and the results of models that predict the geographic extent of individual species. Collection records are searchable and downloadable, and Excel collection forms with drop down lists, and Excel charts to country, are available for data contributors to map and quality control their data. SandflyMap makes accessible, and adds value to, the results of past sand fly collecting efforts. We detail the workflow for entering occurrence data from the literature to SandflyMap, using an example for sand flies from South America. We discuss the utility of SandflyMap as a focal point to increase collaboration and to explore the nexus between geography and vector-borne disease transmission. C1 [Foley, Desmond H.; Wilkerson, Richard C.; Dornak, L. Lynnette; Pecor, David B.; Nyari, Arpad S.; Rueda, Leopoldo M.; Long, Lewis S.; Richardson, Jason H.] Walter Reed Army Inst Res, Entomol Branch, Silver Spring, MD 20910 USA. RP Foley, DH (reprint author), Smithsonian Inst, Walter Reed Army Inst Res, MSC MRC534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM foleydes@si.edu RI Richardson, Jason/A-9441-2011; Valle, Ruben/A-7512-2013 FU Global Emerging Infections Surveillance and Response System, a Division of the Armed Forces Health Surveillance Center; Global Biodiversity Information Facility FX Funding for this work was provided by the Global Emerging Infections Surveillance and Response System, a Division of the Armed Forces Health Surveillance Center, and from the Global Biodiversity Information Facility. This research was performed under a Memorandum of Understanding between the Walter Reed Army Institute of Research and the Smithsonian Institution, with institutional support provided by both organizations. The opinions and assertions contained herein are those of the authors and are not to be construed as official or reflecting the views of the Department of the Army or the Department of Defense. NR 9 TC 5 Z9 5 U1 1 U2 6 PU UNIV NAPLES FEDERICO II PI NAPLES PA FAC VET MED, DEP PATHOLOGY & ANIMAL HEALTH, VET PARASITOLOGY, VIA DELLA VETERINARIA 1, NAPLES, 80137, ITALY SN 1827-1987 J9 GEOSPATIAL HEALTH JI Geospatial Health PD SEP PY 2012 VL 6 IS 3 SI SI BP S25 EP S30 PG 6 WC Health Care Sciences & Services; Public, Environmental & Occupational Health SC Health Care Sciences & Services; Public, Environmental & Occupational Health GA 011JC UT WOS:000309159900005 PM 23032280 ER PT J AU Lee, RML Lam-Phua, SG Tan, WCH Pang, SC Vythilingam, I Ng, LC Rueda, LM AF Lee, Ruth Mee Lian Lam-Phua, Sai Gek Tan, Wilson Cheong Huat Pang, Sook Cheng Vythilingam, Indra Ng, Lee Ching Rueda, Leopoldo M. TI MOSQUITO FAUNA OF UBIN ISLAND, SINGAPORE SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE Diptera; Culicidae; mosquitoes; Ubin; Singapore AB We report the mosquito species and their distribution records for Ubin Island, Singapore, based on our field collections in February 2010, routine adult and larval surveys from 1993 to 2009 by Singapore operational officers, and accessioned specimens deposited in the Environmental Health Institute, Singapore, and the US National Museum of Natural History, Washington, DC. A total of 25 species and 6 unidentified species belonging to 9 genera (Aedes, Anopheles, Armigeres, Coquillettidia, Culex, Lutzia, Mansonia, Uranotaenia, and Verrallina) were identified and recorded from Ubin Island, based on specimens collected from 1993 to 2010. C1 [Lee, Ruth Mee Lian; Lam-Phua, Sai Gek; Tan, Wilson Cheong Huat; Pang, Sook Cheng; Vythilingam, Indra; Ng, Lee Ching] Natl Environm Agcy, Environm Hlth Inst, Singapore 138667, Singapore. [Rueda, Leopoldo M.] Walter Reed Army Inst Res, Walter Reed Biosystemat Unit, Entomol Branch, Silver Spring, MD 20910 USA. [Vythilingam, Indra] Univ Malaya, Fac Med, Parasitol Dept, Kuala Lumpur 50603, Malaysia. RP Rueda, LM (reprint author), Smithsonian Inst, Walter Reed Biosystemat Unit, MSC MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. RI Vythilingam, Indra/Q-5019-2016 FU Singapore EHI FX We would like to thank researchers of the Singapore EHI and field officers of the Environmental Health Department for their help in collecting mosquito specimens, especially C. S. B. Lee, N. Maideen, and O. Mohd Ali. We also thank C. S. Chong, B. A. Harrison, Y. M. Huang, and B. P. Rueda for reviewing the manuscript. Funding for this work was provided by the Singapore EHI. The opinions and assertions contained herein are those of the authors and are not to be construed as official or reflecting the views of the US Department of the Army or the US Department of Defense. NR 13 TC 1 Z9 1 U1 0 U2 2 PU AMER MOSQUITO CONTROL ASSOC PI MOUNT LAUREL PA 15000 COMMERCE PARKWAY, SUITE C, MOUNT LAUREL, NJ 08054 USA SN 8756-971X J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD SEP PY 2012 VL 28 IS 3 BP 248 EP 254 PG 7 WC Entomology SC Entomology GA 013HH UT WOS:000309296000013 PM 23833906 ER PT J AU Martinez-Luis, S Gomez, JF Spadafora, C Guzman, HM Gutierrez, M AF Martinez-Luis, Sergio Felix Gomez, Jose Spadafora, Carmenza Guzman, Hector M. Gutierrez, Marcelino TI Antitrypanosomal Alkaloids from the Marine Bacterium Bacillus pumilus SO MOLECULES LA English DT Article DE indole alkaloids; Trypanosoma cruzi; Bacillus pumilus; Chagas disease ID TRYPANOSOMA-CRUZI; NATURAL-PRODUCTS; ANTIPROTOZOAL ACTIVITY; IN-VIVO; DERIVATIVES AB Fractionation of the ethyl acetate extract of the marine bacterium Bacillus pumilus isolated from the black coral Antipathes sp. led to the isolation of five compounds: cyclo-(L-Leu-L-Pro) (1), 3-hydroxyacetylindole (2), N-acetyl-beta-oxotryptamine (3), cyclo-(L-Phe-L-Pro) (4), and 3-formylindole (5). The structures of compounds 1-5 were established by spectroscopic analyses, including HRESITOF-MS and NMR (H-1, C-13, HSQC, HMBC and COSY). Compounds 2, 3 and 5 caused the inhibition on the growth of Trypanosoma cruzi (T. cruzi), with IC50 values of 20.6, 19.4 and 26.9 mu M, respectively, with moderate cytotoxicity against Vero cells. Compounds 1-5 were found to be inactive when tested against Plasmodium falciparum and Leishmania donovani, therefore showing selectivity against T. cruzi parasites. C1 [Martinez-Luis, Sergio; Felix Gomez, Jose; Gutierrez, Marcelino] Inst Sci Res & High Technol Serv, Ctr Biodivers & Drug Discovery, City Of Knowledge, Panama. [Felix Gomez, Jose] IPN, Ctr Invest & Estudios Avanzados, Dept Quim, Mexico City 07360, DF, Mexico. [Spadafora, Carmenza] Inst Sci Res & High Technol Serv, Ctr Cellular & Mol Biol Dis, City Of Knowledge, Panama. [Guzman, Hector M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Gutierrez, M (reprint author), Inst Sci Res & High Technol Serv, Ctr Biodivers & Drug Discovery, POB 0843-01103, City Of Knowledge, Panama. EM smartinez@indicasat.org.pa; jfgomez@cinvestav.mx; cspadafora@indicasat.org.pa; guzmanh@si.edu; mgutierrez@indicasat.org.pa OI Spadafora, Carmenza/0000-0002-3002-9467 FU National Secretariat for Science and Technology of Panama (SENACYT) [COL08-061, COL09-047]; INDICASAT-AIP; Fogarty International Center's International Cooperative Biodeversity Groups program [TW006634] FX We gratefully acknowledge the Government of Panama (ANAM, ARAP) for granting permission to make these collections; to J. Sanchez, J. Martinez and R. Gavilan for the taxonomic identification of the bacterium. We thank M. Ng and L. Herrera for performing Chagas' and malaria assays and W. H. Gerwick for HRMS measurements. This work was partially supported by the National Secretariat for Science and Technology of Panama (SENACYT, grant numbers COL08-061 and COL09-047), INDICASAT-AIP, and Fogarty International Center's International Cooperative Biodeversity Groups program (grant number TW006634). NR 35 TC 11 Z9 12 U1 0 U2 21 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1420-3049 J9 MOLECULES JI Molecules PD SEP PY 2012 VL 17 IS 9 BP 11146 EP 11155 DI 10.3390/molecules170911146 PG 10 WC Chemistry, Organic SC Chemistry GA 012XJ UT WOS:000309269700081 PM 22990456 ER PT J AU Murray-Clay, RA Loeb, A AF Murray-Clay, Ruth A. Loeb, Abraham TI Disruption of a proto-planetary disc by the black hole at the milky way centre SO NATURE COMMUNICATIONS LA English DT Article ID SGR-A-ASTERISK; GALACTIC-CENTER; CIRCUMSTELLAR DISKS; STELLAR ORBITS; ORION NEBULA; 5 MYR; GALAXY; ACCRETION; CLUSTERS; SHOCKS AB Recently, an ionized cloud of gas was discovered plunging towards the supermassive black hole, SgrA(star), at the centre of the Milky Way. The cloud is being tidally disrupted along its path to closest approach at similar to 3,100 Schwarzschild radii from the black hole. Here we show that the observed properties of this cloud of gas can naturally be produced by a proto-planetary disc surrounding a low-mass star, which was scattered from the observed ring of young stars orbiting SgrA(star). As the young star approaches the black hole, its disc experiences both photoevaporation and tidal disruption, producing a cloud. Our model implies that planets form in the Galactic centre, and that tidal debris from proto-planetary discs can flag low-mass stars, which are otherwise too faint to be detected. C1 [Murray-Clay, Ruth A.; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Murray-Clay, RA (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM rmurray-clay@cfa.harvard.edu FU NSF grant [AST-0907890]; NASA grants [NNX08AL43G, NNA09DB30A] FX We thank Andi Burkert, Reinhard Genzel and Chris McKee for stimulating discussions. AL was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 23 TC 33 Z9 33 U1 0 U2 2 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD SEP PY 2012 VL 3 AR 1049 DI 10.1038/ncomms2044 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 013XA UT WOS:000309338100016 PM 22968695 ER PT J AU Leonard-Pingel, JS Jackson, JBC O'Dea, A AF Leonard-Pingel, Jill S. Jackson, Jeremy B. C. O'Dea, Aaron TI Changes in bivalve functional and assemblage ecology in response to environmental change in the Caribbean Neogene SO PALEOBIOLOGY LA English DT Article ID BOCAS-DEL-TORO; TROPICAL AMERICAN MOLLUSKS; PANAMA LAND-BRIDGE; WESTERN ATLANTIC; THALASSIA COMMUNITIES; SHELL ORNAMENTATION; DEATH ASSEMBLAGES; REEF DEVELOPMENT; FAUNAL TURNOVER; MASS EXTINCTION AB We documented changes in the relative abundance of bivalve genera and functional groups in the southwest Caribbean over the past 11 Myr to determine their response to oceanographic changes associated with the closure of the Central American Seaway ca. 3.5 Ma. Quantitative bulk samples from 29 localities yielded 106,000 specimens in 145 genera. All genera were assigned to functional groups based on diet, relationship to the substrate, and mobility. Ordinations of assemblages based on quantitative data for functional groups demonstrated strong shifts in community structure, with a stark contrast between assemblages older than 5 Ma and those younger than 3.5 Ma. These changes are primarily due to an increase in the abundance of attached epifaunal bivalves (e.g., Chama, Arcopsis, and Barbatia) and a decrease in infaunal bivalves (e.g., Varicorbula and Caryocorbula). Taxa associated with seagrasses, including deposit-feeding and chemosymbiotic bivalves (e.g., Lucina), also increased in relative abundance compared to suspension feeders. The composition of bivalve assemblages is correlated with the carbonate content of sediments and the percentage of skeletal biomass that is coral. Our results strongly support the hypothesis that increases in the extent of coral reefs and Thalassia communities were important drivers of biologic turnover in Neogene Caribbean benthic communities. C1 [Leonard-Pingel, Jill S.; Jackson, Jeremy B. C.] Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Jackson, Jeremy B. C.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. RP Leonard-Pingel, JS (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, La Jolla, CA 92093 USA. EM jsleonar@ucsd.edu RI O'Dea, Aaron/D-4114-2011 FU National Research System (SNI) of the National Secretariat of Science, Technology and Innovation of Panama (SENACYT); NSF [0921924] FX F. Rodriguez and B. De Gracia assisted in the field and laboratory and J. Todd helped to identify the myriad bivalve genera. C. Lennert-Cody, K. Cramer, and R. Norris provided valuable discussion and assistance. L. Anderson, A. Bush, T. Olszewski, and two anonymous reviewers provided helpful commentary on the manuscript. M. Leonard provided the artwork featured in Figure 5. To all we are grateful. O'Dea would like to thank the National Research System (SNI) of the National Secretariat of Science, Technology and Innovation of Panama (SENACYT) for financial support. NSF grant 0921924. NR 87 TC 13 Z9 13 U1 0 U2 20 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 FAL PY 2012 VL 38 IS 4 BP 509 EP 524 DI 10.1666/10050.1 PG 16 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 011WR UT WOS:000309197500001 ER PT J AU Barnard, R Galache, JL Garcia, MR Nooraee, N Callanan, PJ Zezas, A Murray, SS AF Barnard, R. Galache, J. L. Garcia, M. R. Nooraee, N. Callanan, P. J. Zezas, A. Murray, S. S. TI A PERIOD DISTRIBUTION OF X-RAY BINARIES OBSERVED IN THE CENTRAL REGION OF M31 WITH CHANDRA AND THE HUBBLE SPACE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: general ID LIGHT CURVES; SPECTRAL TRANSITIONS; OPTICAL COUNTERPART; TRANSIENT; STARS; HST; NGC-6712; CATALOG; BURSTER; NOVAE AB Almost all Galactic black hole (BH) binaries with low-mass donor stars are transient X-ray sources; we expect most of the X-ray transients observed in external galaxies to be BH binaries also. Obtaining period estimates for extragalactic transients is challenging, but the resulting period distribution is an important tool for modeling the evolution history of the host galaxy. We have obtained periods, or upper limits, for 12 transients in M31, using an updated relation between the optical and X-ray luminosities. We have monitored the central region of M31 with Chandra for the last similar to 12 years, and followed up promising transients with the Hubble Space Telescope; 4 sigma B-magnitude limits for optical counterparts are 26-29, depending on crowding. We obtain period estimates for each transient for both neutron star and BH accretors. Periods range from <0.4 to 490 +/- 90 hr (<0.97 to <175 hr if all are BH systems). These M31 transients appear to be somewhat skewed toward shorter periods than the Milky Way (MW) transients; indeed, comparing the M31 and MW transients with survival analysis techniques used to account for some data with only upper limits yields probabilities of similar to 0.02-0.08 that the two populations are drawn from the same distribution. We also checked for a correlation between orbital period and distance from the nucleus, finding a 12% probability of no correlation. Further observations of M31 transients will strengthen these results. C1 [Barnard, R.; Galache, J. L.; Garcia, M. R.; Zezas, A.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nooraee, N.; Callanan, P. J.] Dublin Inst Adv Studies, Dublin 4, Ireland. [Nooraee, N.; Callanan, P. J.] Natl Univ Ireland Univ Coll Cork, Cork, Ireland. [Zezas, A.] Univ Crete, Iraklion 71409, Crete, Greece. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MD 21218 USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Zezas, Andreas/C-7543-2011 OI Zezas, Andreas/0000-0001-8952-676X FU Chandra grant [GO9-0100X]; HST grant [GO-11013]; NASA [NAS8-03060] FX We thank the referee for thoughtful comments that helped clarify this work. This research has made use of data obtained from the Chandra data archive, and software provided by the Chandra X-ray Center (CXC). R. B. is funded by Chandra grant GO9-0100X and HST grant GO-11013. M. R. G. and S. S. M are both partially supported by NASA contract NAS8-03060. NR 31 TC 11 Z9 11 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 32 DI 10.1088/0004-637X/756/1/32 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300032 ER PT J AU Castro, D Slane, P Ellison, DC Patnaude, DJ AF Castro, Daniel Slane, Patrick Ellison, Donald C. Patnaude, Daniel J. TI FERMI-LAT OBSERVATIONS AND A BROADBAND STUDY OF SUPERNOVA REMNANT CTB 109 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma rays: ISM; ISM: individual objects (CTB 109); ISM: supernova remnants ID LARGE-AREA TELESCOPE; DIFFUSIVE SHOCK ACCELERATION; COSMIC-RAY ACCELERATION; SNR RX J1713.7-3946; GALACTIC PLANE SURVEY; PARTICLE-ACCELERATION; HIGH-ENERGY; X-RAYS; NONEQUILIBRIUM IONIZATION; CTB-109 G109.1-1.0 AB CTB 109 (G109.1-1.0) is a Galactic supernova remnant (SNR) with a hemispherical shell morphology in X-rays and in the radio band. In this work, we report the detection of gamma-ray emission coincident with CTB 109, using 37 months of data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. We study the broadband characteristics of the remnant using a model that includes hydrodynamics, efficient cosmic-ray (CR) acceleration, nonthermal emission, and a self-consistent calculation of the X-ray thermal emission. We find that the observations can be successfully fit with two distinct parameter sets, one where the gamma-ray emission is produced primarily by leptons accelerated at the SNR forward shock and the other where gamma-rays produced by forward shock accelerated CR ions dominate the high-energy emission. Consideration of thermal X-ray emission introduces a novel element to the broadband fitting process, and while it does not rule out either the leptonic or the hadronic scenarios, it constrains the parameter sets required by the model to fit the observations. Moreover, the model that best fits the thermal and nonthermal emission observations is an intermediate case, where both radiation from accelerated electrons and hadrons contribute almost equally to the gamma-ray flux observed. C1 [Castro, Daniel] MIT, Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Slane, Patrick; Patnaude, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ellison, Donald C.] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA. RP Castro, D (reprint author), MIT, Kavli Ctr Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. FU NASA [NNX10AP70G, NAS8-03060]; National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract [SV3-73016]; National Aeronautics Space Administration [NAS8-03060]; NASA ATP [NNX11AE03G] FX The authors thank Yasunobu Uchiyama, Stefan Funk, Joshua Lande, Elizabeth Hays, and Marianne Lemoine-Goumard for their advise on this work, especially with regard to Fermi-LAT data analysis. Additionally, we thank the referee for his/her feedback. This work was partially funded by NASA Fermi grant NNX10AP70G. D.C. also acknowledges support for this work 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. P.O.S. acknowledges partial support from NASA contract NAS8-03060. D.C.E. acknowledges support from NASA ATP grant NNX11AE03G. NR 67 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 SEP 1 PY 2012 VL 756 IS 1 AR 88 DI 10.1088/0004-637X/756/1/88 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300088 ER PT J AU Greve, TR Vieira, JD Weiss, A Aguirre, JE Aird, KA Ashby, MLN Benson, BA Bleem, LE Bradford, CM Brodwin, M Carlstrom, JE Chang, CL Chapman, SC Crawford, TM de Breuck, C de Haan, T Dobbs, MA Downes, T Fassnacht, CD Fazio, G George, EM Gladders, M Gonzalez, AH Halverson, NW Hezaveh, Y High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Johnson, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D Malkan, M Marrone, DP McIntyre, V McMahon, JJ Mehl, J Menten, KM Meyer, SS Montroy, T Murphy, EJ Natoli, T Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Rosenman, M Ruel, J Ruhl, JE Schaffer, KK Sharon, K Shaw, L Shirokoff, E Stalder, B Stanford, SA Staniszewski, Z Stark, AA Story, K Vanderlinde, K Walsh, W Welikala, N Williamson, R AF Greve, T. R. Vieira, J. D. Weiss, A. Aguirre, J. E. Aird, K. A. Ashby, M. L. N. Benson, B. A. Bleem, L. E. Bradford, C. M. Brodwin, M. Carlstrom, J. E. Chang, C. L. Chapman, S. C. Crawford, T. M. de Breuck, C. de Haan, T. Dobbs, M. A. Downes, T. Fassnacht, C. D. Fazio, G. George, E. M. Gladders, M. Gonzalez, A. H. Halverson, N. W. Hezaveh, Y. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Johnson, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Malkan, M. Marrone, D. P. McIntyre, V. McMahon, J. J. Mehl, J. Menten, K. M. Meyer, S. S. Montroy, T. Murphy, E. J. Natoli, T. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Rosenman, M. Ruel, J. Ruhl, J. E. Schaffer, K. K. Sharon, K. Shaw, L. Shirokoff, E. Stalder, B. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. Vanderlinde, K. Walsh, W. Welikala, N. Williamson, R. TI SUBMILLIMETER OBSERVATIONS OF MILLIMETER BRIGHT GALAXIES DISCOVERED BY THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; submillimeter: galaxies ID SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; FAR-INFRARED PROPERTIES; STAR-FORMATION RATE; MU-M OBSERVATIONS; HIGH-REDSHIFT; HERSCHEL-ATLAS; BULLET CLUSTER; NUMBER COUNTS; MOLECULAR GAS AB We present APEX SABOCA 350 mu m and LABOCA 870 mu m observations of 11 representative examples of the rare, extremely bright (S-1.4mm > 15 mJy), dust-dominated millimeter-selected galaxies recently discovered by the South Pole Telescope. All 11 sources are robustly detected with LABOCA with 40 mJy < S-870 mu m < 130 mJy, approximately an order of magnitude higher than the canonical submillimeter galaxy (SMG) population. Six of the sources are also detected by SABOCA at > 3 sigma, with the detections or upper limits providing a key constraint on the shape of the spectral energy distribution (SED) near its peak. We model the SEDs of these galaxies using a simple modified blackbody and perform the same analysis on samples of SMGs of known redshift from the literature. These calibration samples inform the distribution of dust temperature for similar SMG populations, and this dust temperature prior allows us to derive photometric redshift estimates and far-infrared luminosities for the sources. We find a median redshift of (z) over bar = 3.0, higher than the (z) over bar = 2.2 inferred for the normal SMG population. We also derive the apparent size of the sources from the temperature and apparent luminosity, finding them to appear larger than our unlensed calibration sample, which supports the idea that these sources are gravitationally magnified by massive structures along the line of sight. C1 [Greve, T. R.] Univ London Univ Coll, Dept Phys & Astron, London WC1E 6BT, England. [Vieira, J. D.; Downes, T.; Lueker, M.; Staniszewski, Z.] CALTECH, Pasadena, CA 91125 USA. [Weiss, A.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Aguirre, J. E.; Rosenman, M.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Aird, K. A.; Carlstrom, J. E.; Crawford, T. M.; Gladders, M.; High, F. W.; Hrubes, J. D.; Leitch, E. M.; Luong-Van, D.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Ashby, M. L. N.; Brodwin, M.; Fazio, G.; Stalder, B.; Stark, A. A.; Walsh, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Gladders, M.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Sharon, K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; Meyer, S. S.; Natoli, T.; Pryke, C.; Story, K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bradford, C. M.] Jet Prop Lab, Pasadena, CA 91109 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [de Breuck, C.] European So Observ, D-85748 Garching, Germany. [de Haan, T.; Dobbs, M. A.; Hezaveh, Y.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Fassnacht, C. D.; Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; 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. [Johnson, M.; Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Montroy, T.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Rest, A.; Ruel, J.; Stalder, B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Welikala, N.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Welikala, N.] CNRS, F-91405 Orsay, France. RP Greve, TR (reprint author), Univ London Univ Coll, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM tgreve@star.ucl.ac.uk RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; IDA; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; Alfred P. Sloan Research Fellowship; Becker Fund of the Smithsonian Institution; National Aeronautics and Space Administration FX The authors thank A. Blain and N. Scoville for stimulating discussions and guidance. We are grateful to the competent staff at the APEX base camp in Sequitor, Chile. The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. T. R. G. acknowledges support from IDA. 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. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship. A. A. S. acknowledges support by the Becker Fund of the Smithsonian Institution. 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. Finally, we are grateful to the directors of ESO and the SMA for granting us director's discretionary time. NR 76 TC 36 Z9 36 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 SEP 1 PY 2012 VL 756 IS 1 AR 101 DI 10.1088/0004-637X/756/1/101 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300101 ER PT J AU Kim, S Wardlow, JL Cooray, A Fleuren, S Sutherland, W Khostovan, AA Auld, R Baes, M Bussmann, RS Buttiglione, S Cava, A Clements, D Dariush, A De Zotti, G Dunne, L Dye, S Eales, S Fritz, J Hopwood, R Ibar, E Ivison, R Jarvis, M Maddox, S Michalowski, MJ Pascale, E Pohlen, M Rigby, E Scott, D Smith, DJB Temi, P van der Werf, P AF Kim, Sam Wardlow, Julie L. Cooray, Asantha Fleuren, S. Sutherland, W. Khostovan, A. A. Auld, R. Baes, M. Bussmann, R. S. Buttiglione, S. Cava, A. Clements, D. Dariush, A. De Zotti, G. Dunne, L. Dye, S. Eales, S. Fritz, J. Hopwood, R. Ibar, E. Ivison, R. Jarvis, M. Maddox, S. Michalowski, M. J. Pascale, E. Pohlen, M. Rigby, E. Scott, D. Smith, D. J. B. Temi, P. van der Werf, P. TI SPITZER-IRAC IDENTIFICATION OF HERSCHEL-ATLAS SPIRE SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies ID DEEP-FIELD-SOUTH; DEGREE EXTRAGALACTIC SURVEY; SCIENCE DEMONSTRATION PHASE; DIGITAL SKY SURVEY; REDSHIFT SUBMILLIMETER GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; NEAR-INFRARED COUNTERPARTS; STAR-FORMING GALAXIES; ARRAY CAMERA IRAC; SCUBA SUPER-MAP AB We use Spitzer-IRAC data to identify near-infrared counterparts to submillimeter galaxies detected with Herschel-SPIRE at 250 mu m in the Herschel Astrophysical Terahertz Large Area Survey. Using a likelihood ratio analysis we identify 146 reliable IRAC counterparts to 123 SPIRE sources out of the 159 in the survey area. We find that, compared to the field population, the SPIRE counterparts occupy a distinct region of the 3.6 and 4.5 mu m color-magnitude space, and we use this property to identify 23 further counterparts to 13 SPIRE sources. The IRAC identification rate of 86% is significantly higher than those that have been demonstrated with wide-field ground-based optical and near-IR imaging of Herschel fields. We estimate a false identification rate of 3.6%, corresponding to 4-5 sources. Among the 73 counterparts that are undetected in Sloan Digital Sky Survey, 57 have both 3.6 and 4.5 mu m coverage. Of these, 43 have [3.6]-[4.5] > 0, indicating that they are likely to be at z greater than or similar to 1.4. Thus, similar to 40% of identified SPIRE galaxies are likely to be high-redshift (z greater than or similar to 1.4) sources. We discuss the statistical properties of the IRAC-identified SPIRE galaxy sample including far-IR luminosities, dust temperatures, star formation rates, and stellar masses. The majority of our detected galaxies have 10(10)-10(11) L-circle dot total IR luminosities and are not intense starbursting galaxies as those found at z similar to 2, but they have a factor of 2-3 above average specific star formation rates compared to near-IR selected galaxy samples. C1 [Kim, Sam; Wardlow, Julie L.; Cooray, Asantha; Khostovan, A. A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Fleuren, S.; Sutherland, W.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Auld, R.; Eales, S.; Pascale, E.; Pohlen, M.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Baes, M.; Fritz, J.] Univ Ghent, Sterrenkundig Observ, B-9000 Ghent, Belgium. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buttiglione, S.; De Zotti, G.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Clements, D.; Dariush, A.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Dunne, L.; Maddox, S.; Rigby, E.] Univ Canterbury, Dept Phys & Astron, Christchurch 8041, New Zealand. [Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Ibar, E.; Ivison, R.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Jarvis, M.; Smith, D. J. B.] Univ Hertfordshire, Ctr Astrophys Res, Sci & Technol Res Inst, Hatfield AL10 9AB, Herts, England. [Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Cape Town, South Africa. [Michalowski, M. J.] Univ Edinburgh, Royal Observ, Scottish Univ Phys Alliance, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Temi, P.] NASA, Astrophys Branch, Ames Res Ctr, Moffett Field, CA 94035 USA. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Kim, S (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. RI Baes, Maarten/I-6985-2013; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Cava, Antonio/C-5274-2017; OI Smith, Daniel/0000-0001-9708-253X; Baes, Maarten/0000-0002-3930-2757; Wardlow, Julie/0000-0003-2376-8971; Ivison, R./0000-0001-5118-1313; Cava, Antonio/0000-0002-4821-1275; De Zotti, Gianfranco/0000-0003-2868-2595; Maddox, Stephen/0000-0001-5549-195X; Scott, Douglas/0000-0002-6878-9840; Dye, Simon/0000-0002-1318-8343 FU NASA; JPL/Caltech; NASA Herschel Science Center; 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; NSF CAREER [AST-0645427]; NASA [NNX10AD42G]; Caltech/JPL for US participation in Herschel-ATLAS FX Herschel-ATLAS is a project which uses Herschel, an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS Web site is http://www.h-atlas.org/. 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. US participants in H-ATLAS also acknowledge support from the NASA Herschel Science Center through a contract from JPL/Caltech.; 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.; We thank Giulia Rodighiero for providing us electronic tables of COSMOS and GOODS SED fitting results. The UCI group acknowledges support from NSF CAREER AST-0645427, NASA NNX10AD42G, and an award from Caltech/JPL for US participation in Herschel-ATLAS. NR 109 TC 6 Z9 6 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 28 DI 10.1088/0004-637X/756/1/28 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300028 ER PT J AU Lee, JC Hwang, HS Lee, MG Kim, M Lee, JH AF Lee, Jong Chul Hwang, Ho Seong Lee, Myung Gyoon Kim, Minjin Lee, Joon Hyeop TI AKARI NEAR-INFRARED SPECTROSCOPY OF LUMINOUS INFRARED GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: ISM; galaxies: starburst; infrared: galaxies ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; MU-M SPECTROSCOPY; STAR-FORMING GALAXIES; ULTRALUMINOUS IRAS GALAXIES; BROAD-LINE REGIONS; DATA RELEASE; REDSHIFT SURVEY; EXTINCTION LAW; LARGE-SAMPLE AB We present the AKARI near-infrared (NIR; 2.5-5 mu m) spectroscopic study of 36 (ultra) luminous infrared galaxies ((U) LIRGs) at z = 0.01-0.4. We measure the NIR spectral features including the strengths of 3.3 mu m polycyclic aromatic hydrocarbon emission and hydrogen recombination lines (Br alpha and Br beta), optical depths at 3.1 and 3.4 mu m, and NIR continuum slope. These spectral features are used to identify optically elusive, buried active galactic nuclei (AGNs). We find that half of the (U) LIRGs optically classified as non-Seyferts show AGN signatures in their NIR spectra. Using a combined sample of (U) LIRGs with NIR spectra in the literature, we measure the contribution of buried AGNs to the infrared luminosity from the spectral energy distribution fitting to the IRAS photometry. The contribution of these buried AGNs to the infrared luminosity is 5%-10%, smaller than the typical AGN contribution of (U) LIRGs including Seyfert galaxies (10%-40%). We show that NIR continuum slopes correlate well with WISE [3.4]-[4.6] colors, which would be useful for identifying a large number of buried AGNs using the WISE data. C1 [Lee, Jong Chul; Lee, Myung Gyoon] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Lee, Jong Chul; Kim, Minjin; Lee, Joon Hyeop] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hwang, Ho Seong] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kim, Minjin] Natl Radio Astron Observ, Charlottesville, VA USA. RP Lee, JC (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. EM jclee@kasi.re.kr; hhwang@cfa.harvard.edu; mglee@astro.snu.ac.kr; mkim@kasi.re.kr; jhl@kasi.re.kr FU Mid-career Research Program through NRF; MEST [2010-0013875]; Centre National d'Etudes Spatiales (CNES); Smithsonian Institution; 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; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck-Institute for Astronomy (MPIA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We are grateful to an anonymous referee for comments that helped to improve the manuscript. This work was supported by Mid-career Research Program through NRF grant funded by the MEST (No.2010-0013875). J.C.L., M. K., and J.H.L. are members of the Dedicated Researchers for Extragalactic AstronoMy (DREAM) in the Korea Astronomy and Space Science Institute (KASI). H. S. H. acknowledges the Centre National d'Etudes Spatiales (CNES) and the Smithsonian Institution for the support of his post-doctoral fellowship. This research is based on observations with AKARI, a JAXA project with the participation of ESA. 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. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 125 TC 20 Z9 19 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 95 DI 10.1088/0004-637X/756/1/95 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300095 ER PT J AU Lewkow, NR Kharchenko, V Zhang, P AF Lewkow, N. R. Kharchenko, V. Zhang, P. TI ENERGY RELAXATION OF HELIUM ATOMS IN ASTROPHYSICAL GASES SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; atomic processes; astronomical databases: miscellaneous; ISM: atoms; planets and satellites: atmospheres; scattering ID DIFFERENTIAL CROSS-SECTIONS; NONTHERMAL ESCAPE; UPPER-ATMOSPHERE; HYDROGEN-ATOMS; HOT OXYGEN; SCATTERING; MARS; VENUS; HE; COLLISIONS AB We report accurate parameters describing energy relaxation of He atoms in atomic gases, important for astrophysics and atmospheric science. Collisional energy exchange between helium atoms and atomic constituents of the interstellar gas, heliosphere, and upper planetary atmosphere has been investigated. Energy transfer rates, number of collisions required for thermalization, energy distributions of recoil atoms, and other major parameters of energy relaxation for fast He atoms in thermal H, He, and O gases have been computed in a broad interval of energies from 10 meV to 10 keV. This energy interval is important for astrophysical applications involving the energy deposition of energetic atoms and ions into atmospheres of planets and exoplanets, atmospheric evolution, and analysis of non-equilibrium processes in the interstellar gas and heliosphere. Angular-and energy-dependent cross sections, required for an accurate description of the momentum-energy transfer, are obtained using ab initio interaction potentials and quantum mechanical calculations for scattering processes. Calculation methods used include partial wave analysis for collisional energies below 2 keV and the eikonal approximation at energies higher than 100 eV, keeping a significant energy region of overlap, 0.1-2 keV, between these two methods for their mutual verification. The partial wave method and the eikonal approximation excellently match results obtained with each other as well as experimental data, providing reliable cross sections in the astrophysically important interval of energies from 10 meV to 10 keV. Analytical formulae, interpolating obtained energy-and angular-dependent cross sections, are presented to simplify potential applications of the reported database. Thermalization of fast He atoms in the interstellar gas and energy relaxation of hot He and O atoms in the upper atmosphere of Mars are considered as illustrative examples of potential applications of the new database. C1 [Lewkow, N. R.; Kharchenko, V.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Lewkow, N. R.; Kharchenko, V.; Zhang, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhang, P.] Duke Univ, Dept Chem, Durham, NC 27708 USA. RP Lewkow, NR (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. FU NASA [NNX09AF13G, NNX10AB88G] FX We are grateful to Dr. I. Simbotin for reading and suggestions. N. Lewkow and V. Kharchenko are grateful to NASA supporting our research via grants NNX09AF13G and NNX10AB88G. NR 49 TC 3 Z9 3 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 57 DI 10.1088/0004-637X/756/1/57 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300057 ER PT J AU Liu, HYBB Jimenez-Serra, I Ho, PTP Chen, HR Zhang, QZ Li, ZY AF Liu, Hauyu Baobab Jimenez-Serra, Izaskun Ho, Paul T. P. Chen, Huei-Ru Zhang, Qizhou Li, Zhi-Yun TI FRAGMENTATION AND OB STAR FORMATION IN HIGH-MASS MOLECULAR HUB-FILAMENT SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE evolution; ISM: individual objects (G33.92+0.11); stars: formation ID INFRARED-DARK CLOUD; CLUSTER-FORMING REGION; S-BEARING MOLECULES; STELLAR CLUSTERS; HOT-CORE; INITIAL CONDITIONS; SULFUR CHEMISTRY; DENSE CORES; SUBMILLIMETER ARRAY; PROTOSTELLAR CORES AB Filamentary structures are ubiquitously seen in the interstellar medium. The concentrated molecular mass in the filaments allows fragmentation to occur in a shorter timescale than the timescale of the global collapse. Such hierarchical fragmentation may further assist the dissipation of excessive angular momentum. It is crucial to resolve the morphology and the internal velocity structures of the molecular filaments observationally. We perform 0 ''.5-2 ''.5 angular resolution interferometric observations toward the nearly face-on OB cluster-forming region G33.92+0.11. Observations of various spectral lines, as well as the millimeter dust continuum emission, consistently trace several similar to 1 pc scale, clumpy molecular arms. Some of the molecular arms geometrically merge to an inner 3.0(-1.4)(+2.8)x10(3) M-circle dot, 0.6 pc scale central molecular clump, and may directly channel the molecular gas to the warm (similar to 50 K) molecular gas immediately surrounding the centrally embedded OB stars. The NH3 spectra suggest a medium turbulence line width of FWHM less than or similar to 2 km s(-1) in the central molecular clump, implying a greater than or similar to 10 times larger molecular mass than the virial mass. Feedbacks from shocks and the centrally embedded OB stars and localized (proto) stellar clusters likely play a key role in the heating of molecular gas and could lead to the observed chemical stratification. Although (proto) stellar feedbacks are already present, G33.92+0.11 chemically appears to be at an early evolutionary stage given by the low abundance limit of SO2 observed in this region. C1 [Liu, Hauyu Baobab] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Liu, Hauyu Baobab; Ho, Paul T. P.; Chen, Huei-Ru] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Liu, Hauyu Baobab; Jimenez-Serra, Izaskun; Ho, Paul T. P.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, Huei-Ru] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. [Chen, Huei-Ru] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. [Li, Zhi-Yun] Dept Astrophys, Charlottesville, VA 22904 USA. RP Liu, HYBB (reprint author), Natl Taiwan Univ, Dept Phys, 1,Sec 4,Roosevelt Rd, Taipei 106, Taiwan. 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 112 TC 18 Z9 18 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 SEP 1 PY 2012 VL 756 IS 1 AR 10 DI 10.1088/0004-637X/756/1/10 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300010 ER PT J AU Long, KS Blair, WP Godfrey, LEH Kuntz, KD Plucinsky, PP Soria, R Stockdale, CJ Whitmore, BC Winkler, PF AF Long, Knox S. Blair, William P. Godfrey, L. E. H. Kuntz, K. D. Plucinsky, Paul P. Soria, Roberto Stockdale, Christopher J. Whitmore, Bradley C. Winkler, P. Frank TI RECOVERY OF THE HISTORICAL SN1957D IN X-RAYS WITH CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M83); galaxies: ISM; ISM: supernova remnants; radio continuum: galaxies; supernovae: individual (SN 1957D); X-rays: general; X-rays: individual (SN 1957D, M83) ID RICH SUPERNOVA-REMNANTS; HUBBLE-SPACE-TELESCOPE; OPTICAL-EMISSION; LIGHT CURVES; SN 1957D; RADIO; M83; DUST; CRAB; EVOLUTION AB SN1957D, located in one of the spiral arms of M83, is one of the small number of extragalactic supernovae (SNe) that has remained detectable at radio and optical wavelengths during the decades after its explosion. Here, we report the first detection of SN1957D in X-rays, as part of a 729 ks observation of M83 with Chandra. The X-ray luminosity (0.3-8 keV) is 1.7(-0.3)(+ 2.4) x10(37) erg s(-1). The spectrum is hard and highly self-absorbed compared to most sources in M83 and to other young supernova remnants (SNRs), suggesting that the system is dominated at X-ray wavelengths by an energetic pulsar and its pulsar wind nebula. The high column density may be due to absorption within the SN ejecta. Hubble Space Telescope WFC3 images resolve the SNR from the surrounding emission and the local star field. Photometry of stars around SN1957D, using WFC3 images, indicates an age of less than 10(7) years and a main-sequence turnoff mass more than 17M(circle dot). New spectra obtained with Gemini-South show that the optical spectrum continues to be dominated by broad [O III] emission lines, the signature of fast-moving SN ejecta. The width of the broad lines has remained about 2700 km s(-1) (FWHM). The [O III] flux dropped precipitously between 1989 and 1991, but continued monitoring shows the flux has been almost constant since. In contrast, radio observations over the period 1990-2011 show a decline rate S-nu similar to t(-4.0), far steeper than the rate observed earlier, suggesting that the primary shock has overrun the edge of a pre-SN wind. C1 [Long, Knox S.; Whitmore, Bradley C.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Blair, William P.; Kuntz, K. D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Godfrey, L. E. H.; Soria, Roberto] Curtin Univ Technol, Curtin Inst Radio Astron, Bentley, WA 6102, Australia. [Plucinsky, Paul P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stockdale, Christopher J.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Stockdale, Christopher J.] Australian Astron Observ, Epping, NSW 1710, Australia. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Long, KS (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM long@stsci.edu; wpb@pha.jhu.edu; leith.godfrey@icrar.org; kuntz@pha.jhu.edu; plucinsky@cfa.harvard.edu; roberto.soria@icrar.org; Christopher.Stockdale@marquette.edu; whitmore@stsci.edu; winkler@middlebury.edu RI Godfrey, Leith/B-5283-2013 FU National Aeronautics and Space Administration [G01-12115, NAS8-03060, NAS 5-26555]; National Science Foundation [AST-0908566]; Smithsonian Astrophysical Observatory [NAS83060]; [GO-12513]; [GO-12683] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Grant No. G01-12115, 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. P. F. W. and W. P. B. are grateful for both observing and travel support for the Gemini observations from the Gemini office at NOAO. P. F. W. also acknowledges financial support from the National Science Foundation through grant AST-0908566, and the hospitality of the Research School of Astronomy and Astrophysics, Australian National University, during a portion of the work presented here.; Based on observations made with NASA's Chandra X-ray Observatory, the NASA/ESA Hubble Space Telescope (HST), the 6.5 m Magellan Telescopes located at Las Campanas Observatory, and the Gemini Observatory. NASA's Chandra Observatory is operated by Smithsonian Astrophysical Observatory under contract NAS83060 and the data were obtained through program GO1-12115. The HST observations were obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS 5-26555. The new HST observations were obtained through programs GO-12513 and GO-12683. Data in the HST archive from program GO-11360 were also used. The ground-based observations were obtained through NOAO, which is operated by Association of Universities for Research in Astronomy, Inc., for the National Science Foundation. NR 51 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 18 DI 10.1088/0004-637X/756/1/18 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300018 ER PT J AU Margutti, R Berger, E Fong, W Zauderer, BA Cenko, SB Greiner, J Soderberg, AM Cucchiara, A Rossi, A Klose, S Schmidl, S Milisavljevic, D Sanders, N AF Margutti, R. Berger, E. Fong, W. Zauderer, B. A. Cenko, S. B. Greiner, J. Soderberg, A. M. Cucchiara, A. Rossi, A. Klose, S. Schmidl, S. Milisavljevic, D. Sanders, N. TI THE AFTERGLOW AND ENVIRONMENT OF THE SHORT GRB 111117A SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: individual (GRB111117A) ID GAMMA-RAY BURST; DIGITAL SKY SURVEY; HOST GALAXIES; STAR-FORMATION; TELESCOPE OBSERVATIONS; OPTICAL AFTERGLOW; EXTENDED EMISSION; COMPACT OBJECTS; FORMATION RATES; HIGH-REDSHIFT AB We present multi-wavelength observations of the afterglow of the short GRB 111117A, and follow-up observations of its host galaxy. From rapid optical and radio observations, we place limits of r greater than or similar to 25.5 mag at delta t approximate to 0.55 days and F-nu(5.8 GHz) less than or similar to 18 mu Jy at delta t approximate to 0.50 days, respectively. However, using a Chandra observation at delta t approximate to 3.0 days we locate the absolute position of the X-ray afterglow to an accuracy of 0 ''.22 (1 sigma), a factor of about six times better than the Swift/XRT position. This allows us to robustly identify the host galaxy and to locate the burst at a projected offset of 1 ''.25 +/- 0 ''.20 from the host centroid. Using optical and near-IR observations of the host galaxy we determine a photometric redshift of z = 1.3(-0.2)(+0.3), one of the highest for any short gamma-ray burst (GRB), leading to a projected physical offset for the burst of 10.5 +/- 1.7 kpc, typical of previous short GRBs. At this redshift, the isotropic gamma-ray energy is E-gamma,E-iso approximate to 3.0 x 10(51) erg (rest-frame 23-2300 keV) with a peak energy of E-pk approximate to 850-2300 keV (rest-frame). In conjunction with the isotropic X-ray energy, GRB 111117A appears to follow our recently reported E-x,E-iso-E-gamma,E-iso-E-pk universal scaling. Using the X-ray data along with the optical and radio non-detections, we find that for a blastwave kinetic energy of E-K,E-iso approximate to E-gamma,E-iso erg, the circumburst density is n(0) approximate to 3x10(-4) - 1 cm(-3) (for a range of epsilon(B) = 0.001-0.1). Similarly, from the non-detection of a break in the X-ray light curve at delta t less than or similar to 3 days, we infer a minimum opening angle for the outflow of theta(j) greater than or similar to 3-10 degrees (depending on the circumburst density). We conclude that Chandra observations of short GRBs are effective at determining precise positions and robust host galaxy associations in the absence of optical and radio detections. C1 [Margutti, R.; Berger, E.; Fong, W.; Zauderer, B. A.; Soderberg, A. M.; Milisavljevic, D.; Sanders, N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cenko, S. B.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Greiner, J.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Cucchiara, A.] Univ Calif Santa Cruz, UCO Lick Observ, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Rossi, A.; Klose, S.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. RP Margutti, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Rossi, Andrea/N-4674-2015 OI Rossi, Andrea/0000-0002-8860-6538 FU National Science Foundation [AST-1107973]; NASA/Swift AO6 grant [NNX10AI24G]; David and Lucile Packard Foundation; Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund; NASA/Swift [NNX10AI21G, NNX12AD73G]; TABASGO Foundation; US National Science Foundation (NSF) [AST-0908886]; DFG Kl 766/16-1; Landesstipendium; DFG [HA 1850/28-1]; JVLA [10C-145] FX R.M. thanks Rodolfo Barniol Duran and Cristiano Guidorzi for useful discussions. We thank Francesco di Mille for carrying out the Magellan FourStar observations, and Andy Monson for assistance with the data reduction. The Berger GRB group at Harvard is supported by the National Science Foundation under grant AST-1107973. Partial support was also provided by NASA/Swift AO6 grant NNX10AI24G. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A. M. S. S. B. C. acknowledges generous financial assistance from Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, NASA/Swift grants NNX10AI21G and NNX12AD73G, the TABASGO Foundation, and US National Science Foundation (NSF) grant AST-0908886. A. R. and S. K. acknowledge support by grant DFG Kl 766/16-1. S. S. acknowledges support by a Landesstipendium. Part of the funding for GROND (both hardware and personnel) was generously granted by the Leibniz-Prize to G. Hasinger (DFG grant HA 1850/28-1). Observations were obtained with the JVLA (program 10C-145) 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 paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This work is based in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 70 TC 13 Z9 14 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 SEP 1 PY 2012 VL 756 IS 1 AR 63 DI 10.1088/0004-637X/756/1/63 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300063 ER PT J AU Paggi, A Wang, JF Fabbiano, G Elvis, M Karovska, M AF Paggi, Alessandro Wang, Junfeng Fabbiano, Giuseppina Elvis, Martin Karovska, Margarita TI CHEERS RESULTS ON Mrk 573: A STUDY OF DEEP CHANDRA OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (Mrk 573); galaxies: jets; galaxies: Seyfert; X-rays: galaxies ID NARROW-LINE REGION; X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; GALAXY MARKARIAN 573; AGN DUSTY TORI; SEYFERT-GALAXIES; XMM-NEWTON; NGC 1068; IMAGE-RESTORATION AB We present results on Mrk 573 obtained as part of the CHandra survey of Extended Emission-line Regions in nearby Seyfert galaxies (CHEERS). Previous studies showed that this source features a biconical emission in the soft X-ray band closely related to the narrow-line region as mapped by the [OIII] emission line and the radio emission, though on a smaller scale; we investigate the properties of soft X-ray emission from this source with new deep Chandra observations. Making use of the subpixel resolution of the Chandra/ACIS image and point-spread function deconvolution, we resolve and study substructures in each ionizing cone. The two cone spectra are fitted with a photoionization model, showing a mildly photoionized phase diffused over the bicone. Thermal collisional gas at about similar to 1.1 keV and similar to 0.8 keV appears to be located between the nucleus and the "knots" resolved in radio observations, and between the "arcs" resolved in the optical images, respectively; this can be interpreted in terms of shock interaction with the host galactic plane. The nucleus shows a significant flux decrease across the observations indicating variability of the active galactic nucleus (AGN), with the nuclear region featuring a higher ionization parameter with respect to the bicone region. The long exposure allows us to find extended emission up to similar to 7 kpc from the nucleus along the bicone axis. Significant emission is also detected in the direction perpendicular to the ionizing cones, disagreeing with the fully obscuring torus prescribed in the AGN unified model and suggesting instead the presence of a clumpy structure. C1 [Paggi, Alessandro; Wang, Junfeng; Fabbiano, Giuseppina; Elvis, Martin; Karovska, Margarita] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Paggi, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM apaggi@cfa.harvard.edu RI Paggi, Alessandro/C-1219-2017 OI Paggi, Alessandro/0000-0002-5646-2410 FU NASA [GO1-12009X, HST GO-12365.01-A, NAS8-03060]; CXC; National Science Foundation [1066293]; hospitality of the Aspen Center for Physics; Association of Universities for Research in Astronomy, Inc. under NASA [NAS5-26555] FX We acknowledge useful comments and suggestions by our anonymous referee. This work is supported by NASA grant GO1-12009X and HST GO-12365.01-A (PI: Wang). We acknowledge support from the CXC, which is operated by the Smithsonian Astrophysical Observatory (SAO) for and on behalf of NASA under contract NAS8-03060. This material is based upon work supported in part by the National Science Foundation Grant No. 1066293 and the hospitality of the Aspen Center for Physics. A. P. thanks Andrea Marinucci, Francesco Massaro, and Guido Risaliti for useful discussions. This research has made use of data obtained from the Chandra Data Archive, and software provided by the CXC in the application packages CIAO and Sherpa. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. NR 60 TC 8 Z9 8 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 39 DI 10.1088/0004-637X/756/1/39 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300039 ER PT J AU Patnaude, DJ Badenes, C Park, S Laming, JM AF Patnaude, Daniel J. Badenes, Carles Park, Sangwook Laming, J. Martin TI THE ORIGIN OF KEPLER'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE hydrodynamics; ISM: individual objects (SN 1604); ISM: supernova remnants; nuclear reactions, nucleosynthesis, abundances; supernovae: general; X-rays: ISM ID X-RAY-EMISSION; MASS-LOSS RATES; DIFFUSIVE SHOCK ACCELERATION; IA SUPERNOVA; BLAST WAVE; RS OPHIUCHI; SN 2011FE; NONEQUILIBRIUM IONIZATION; CIRCUMSTELLAR MATERIAL; EXPLOSION MECHANISM AB It is now well established that Kepler's supernova remnant (SNR) is the result of a Type Ia explosion. With an age of 407 yr and an angular diameter of similar to 4', Kepler is estimated to be between 3.0 and 7.0 kpc distant. Unlike other Galactic Type Ia SNRs such as Tycho and SN 1006, and SNR 0509-67.5 in the Large Magellanic Cloud, Kepler shows evidence for a strong circumstellar interaction. A bowshock structure in the north is thought to originate from the motion of a mass-losing system through the interstellar medium prior to the supernova. We present results of hydrodynamical and spectral modeling aimed at constraining the circumstellar environment of the system and the amount of Ni-56 produced in the explosion. Using models that contain either 0.3M(circle dot) (subenergetic) or 1.0M(circle dot) (energetic) of Ni-56, we simulate the interaction between supernova Ia ejecta and various circumstellar density models. Based on dynamical considerations alone, we find that the subenergetic models favor a distance to the SNR of <6.4 kpc, while the model that produces 1M(circle dot) of Ni-56 requires a distance to the SNR of >7 kpc. The X-ray spectrum is consistent with an explosion that produced similar to 1M(circle dot) of Ni-56, ruling out the subenergetic models, and suggesting that Kepler's SNR was an SN 1991T-like event. Additionally, the X-ray spectrum rules out a pure r(-2) wind profile expected from isotropic mass loss up to the time of the supernova. Introducing a small cavity around the progenitor system results in modeled X-ray spectra that are consistent with the observed spectrum. If a wind-shaped circumstellar environment is necessary to explain the dynamics and X-ray emission from the shocked ejecta in Kepler's SNR, then we require that the distance to the remnant be greater than 7 kpc. C1 [Patnaude, Daniel J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Badenes, Carles] Univ Pittsburgh, Pittsburgh, PA 15260 USA. [Badenes, Carles] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Badenes, Carles] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Park, Sangwook] Univ Texas Arlington, Dept Phys, Arlington, TX 76019 USA. [Laming, J. Martin] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RP Patnaude, DJ (reprint author), Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. OI Badenes, Carles/0000-0003-3494-343X FU Chandra Theory program [GO0-11094X]; NASA [NAS8-03060] FX D.J.P. acknowledges support from the Chandra Theory program through grant GO0-11094X as well as support from NASA contract NAS8-03060. D.J.P. is grateful for the hospitality of the Weizmann Institute for hosting him so that the groundwork for this paper could be performed. We thank Alexa Hart at SAO for useful discussions regarding the abundances and wind luminosities of asymptotic giant branch stars. Additionally, we thank Paul Plucinsky for discussions regarding the measurement of line centroids in ACIS spectra. NR 56 TC 19 Z9 19 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 6 DI 10.1088/0004-637X/756/1/6 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300006 ER PT J AU Sand, DJ Strader, J Willman, B Zaritsky, D McLeod, B Caldwell, N Seth, A Olszewski, E AF Sand, David J. Strader, Jay Willman, Beth Zaritsky, Dennis McLeod, Brian Caldwell, Nelson Seth, Anil Olszewski, Edward TI TIDAL SIGNATURES IN THE FAINTEST MILKY WAY SATELLITES: THE DETAILED PROPERTIES OF LEO V, PISCES II, AND CANES VENATICI II SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; Local Group ID DWARF SPHEROIDAL GALAXY; STAR-FORMATION HISTORY; GLOBULAR-CLUSTER PALOMAR-5; COLOR-MAGNITUDE DIAGRAM; SMALL-MAGELLANIC-CLOUD; METAL-POOR STARS; GIANT BRANCH TIP; LOCAL GROUP; URSA-MAJOR; STELLAR POPULATION AB We present deep wide-field photometry of three recently discovered faint Milky Way (MW) satellites: Leo V, Pisces II, and Canes Venatici II. Our main goals are to study the structure and star formation history of these dwarfs; we also search for signs of tidal disturbance. The three satellites have similar half-light radii (similar to 60-90 pc) but a wide range of ellipticities. Both Leo V and CVn II show hints of stream-like overdensities at large radii. An analysis of the satellite color-magnitude diagrams shows that all three objects are old (>10 Gyr) and metal-poor ([Fe/H] similar to-2), though neither the models nor the data have sufficient precision to assess when the satellites formed with respect to cosmic reionization. The lack of an observed younger stellar population (less than or similar to 10 Gyr) possibly sets them apart from the other satellites at Galactocentric distances greater than or similar to 150 kpc. We present a new compilation of structural data for all MW satellite galaxies and use it to compare the properties of classical dwarfs to the ultra-faints. The ellipticity distribution of the two groups is consistent at the similar to 2 sigma level. However, the faintest satellites tend to be more aligned toward the Galactic Center, and those satellites with the highest ellipticity (greater than or similar to 0.4) have orientations (Delta theta(GC)) in the range 20 degrees less than or similar to Delta theta(GC) less than or similar to 40 degrees. This latter observation is in rough agreement with predictions from simulations of dwarf galaxies that have lost a significant fraction of their dark matter halos and are being tidally stripped. C1 [Sand, David J.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Sand, David J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Strader, Jay; McLeod, Brian; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Willman, Beth] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Zaritsky, Dennis; Olszewski, Edward] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Seth, Anil] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Sand, DJ (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Santa Barbara, CA 93117 USA. EM dsand@lcogt.net FU NSF [AST-0908193, AST-0807498, AST-0907771] FX Many thanks to Maureen Conroy and John Roll for their tireless efforts related to Megacam, and their focus on getting scientific results. This work is 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. B.W. acknowledges financial support from the NSF grant AST-0908193 for support. E.O. acknowledges partial support from the NSF grant AST-0807498. D.Z. acknowledges financial support from the NSF grant AST-0907771. NR 94 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 SEP 1 PY 2012 VL 756 IS 1 AR 79 DI 10.1088/0004-637X/756/1/79 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300079 ER PT J AU Sanhueza, P Jackson, JM Foster, JB Garay, G Silva, A Finn, SC AF Sanhueza, Patricio Jackson, James M. Foster, Jonathan B. Garay, Guido Silva, Andrea Finn, Susanna C. TI CHEMISTRY IN INFRARED DARK CLOUD CLUMPS: A MOLECULAR LINE SURVEY AT 3 mm SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: clouds; ISM: molecules; stars: formation ID MASSIVE-STAR-FORMATION; EARLY EVOLUTIONARY STAGES; ELECTRIC-DIPOLE MOMENT; EXTENDED GREEN OBJECTS; AB-INITIO; DEUTERIUM FRACTIONATION; GALACTIC DISTRIBUTION; PHYSICAL PARAMETERS; ARRAY OBSERVATIONS; COLOGNE DATABASE AB We have observed 37 Infrared Dark Clouds (IRDCs), containing a total of 159 clumps, in high-density molecular tracers at 3 mm using the 22 m ATNF Mopra Telescope located in Australia. After determining kinematic distances, we eliminated clumps that are not located in IRDCs and clumps with a separation between them of less than one Mopra beam. Our final sample consists of 92 IRDC clumps. The most commonly detected molecular lines are (detection rates higher than 8%) N2H+, HNC, (HNC)-C-13, HCO+, H13CO+, HCN, C2H, HC3N, HNCO, and SiO. We investigate the behavior of the different molecular tracers and look for chemical variations as a function of an evolutionary sequence based on Spitzer IRAC and MIPS emission. We find that the molecular tracers behave differently through the evolutionary sequence and some of them can be used to yield useful relative age information. The presence of HNC and N2H+ lines does not depend on the star formation activity. On the other hand, HC3N, HNCO, and SiO are predominantly detected in later stages of evolution. Optical depth calculations show that in IRDC clumps the N2H+ line is optically thin, the C2H line is moderately optically thick, and HNC and HCO+ are optically thick. The HCN hyperfine transitions are blended, and, in addition, show self-absorbed line profiles and extended wing emission. These factors combined prevent the use of HCN hyperfine transitions for the calculation of physical parameters. Total column densities of the different molecules, except C2H, increase with the evolutionary stage of the clumps. Molecular abundances increase with the evolutionary stage for N2H+ and HCO+. The N2H+/HCO+ and N2H+/HNC abundance ratios act as chemical clocks, increasing with the evolution of the clumps. C1 [Sanhueza, Patricio; Jackson, James M.; Foster, Jonathan B.; Finn, Susanna C.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Garay, Guido] Univ Chile, Dept Astron, Santiago, Chile. [Silva, Andrea] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sanhueza, P (reprint author), Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. RI Garay, Guido/H-8840-2013 OI Garay, Guido/0000-0003-1649-7958 FU NSF [AST-0808001]; CONICYT project FONDAP [15010003]; CONICYT project BASAL [PFB-06] FX J.M.J. gratefully acknowledges funding support from NSF Grant No. AST-0808001. G. G. acknowledges support from CONICYT projects FONDAP No. 15010003 and BASAL PFB-06. We also thank the anonymous referee for helpful comments. NR 94 TC 56 Z9 56 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 SEP 1 PY 2012 VL 756 IS 1 AR 60 DI 10.1088/0004-637X/756/1/60 PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300060 ER PT J AU Stassun, KG Kratter, KM Scholz, A Dupuy, TJ AF Stassun, Keivan G. Kratter, Kaitlin M. Scholz, Aleks Dupuy, Trent J. TI AN EMPIRICAL CORRECTION FOR ACTIVITY EFFECTS ON THE TEMPERATURES, RADII, AND ESTIMATED MASSES OF LOW-MASS STARS AND BROWN DWARFS SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; stars: activity; stars: fundamental parameters; stars: low-mass ID ORION NEBULA CLUSTER; SIMULTANEOUS MULTIWAVELENGTH OBSERVATIONS; BINARY 2MASS J05352184-0546085; AUTOMATED SURVEY CATALOG; SKY SURVEY DATA; ECLIPSING BINARIES; MAGNETIC ACTIVITY; H-ALPHA; SPECTROSCOPIC SURVEY; PHYSICAL PARAMETERS AB We present empirical relations for determining the amount by which the effective temperatures and radii-and therefore the estimated masses-of low-mass stars and brown dwarfs are altered due to chromospheric activity. We base our relations on a large set of low-mass stars in the field with H alpha activity measurements, and on a set of low-mass eclipsing binaries with X-ray activity measurements from which we indirectly infer the H alpha activity. Both samples yield consistent relations linking the amount by which an active object's temperature is suppressed, and its radius inflated, to the strength of its H alpha emission. These relations are found to approximately preserve bolometric luminosity. We apply these relations to the peculiar brown dwarf eclipsing binary 2M0535-05, in which the active, higher-mass brown dwarf has a cooler temperature than its inactive, lower-mass companion. The relations correctly reproduce the observed temperatures and radii of 2M0535-05 after accounting for the Ha emission; 2M0535-05 would be in precise agreement with theoretical isochrones were it is inactive. The relations that we present are applicable to brown dwarfs and low-mass stars with masses below 0.8 M-circle dot and for which the activity, as measured by the fractional H alpha luminosity, is in the range -4.6 less than or similar to log LH alpha/L-bol less than or similar to -3.3. We expect these relations to be most useful for correcting radius and mass estimates of low-mass stars and brown dwarfs over their active lifetimes (few Gyr) and when the ages or distances (and therefore luminosities) are unknown. We also discuss the implications of this work for improved determinations of young cluster initial mass functions. C1 [Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Kratter, Kaitlin M.; Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Scholz, Aleks] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. RP Stassun, KG (reprint author), Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. EM keivan.stassun@vanderbilt.edu OI Scholz, Aleks/0000-0001-8993-5053 FU NSF [AST-0607773, AST-1009810]; Science Foundation Ireland [10/RFP/AST2780]; Hubble Fellowship [HST-HF-51271.01-A]; Space Telescope Science Institute; AURA for NASA [NAS 5-26555] FX We thank Beate Stelzer for helpful discussions. K. G. S. acknowledges NSF grants AST-0607773 and AST-1009810. Part of this work was funded by the Science Foundation Ireland through grant No. 10/RFP/AST2780 to A. S. 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. NR 57 TC 45 Z9 46 U1 2 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 SEP 1 PY 2012 VL 756 IS 1 AR 47 DI 10.1088/0004-637X/756/1/47 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300047 ER PT J AU Wang, YY Khardon, R Protopapas, P AF Wang, Yuyang Khardon, Roni Protopapas, Pavlos TI NONPARAMETRIC BAYESIAN ESTIMATION OF PERIODIC LIGHT CURVES SO ASTROPHYSICAL JOURNAL LA English DT Article DE methods: data analysis; methods: statistical; stars: variables: general ID TIME-SERIES ANALYSIS; FAST EFFICIENT TECHNIQUE; UNEQUALLY-SPACED DATA; SPECTRAL-ANALYSIS; FREQUENCY; PERIODOGRAM; STARS AB Many astronomical phenomena exhibit patterns that have periodic behavior. An important step when analyzing data from such processes is the problem of identifying the period: estimating the period of a periodic function based on noisy observations made at irregularly spaced time points. This problem is still a difficult challenge despite extensive study in different disciplines. This paper makes several contributions toward solving this problem. First, we present a nonparametric Bayesian model for period finding, based on Gaussian Processes (GPs), that does not make assumptions on the shape of the periodic function. As our experiments demonstrate, the new model leads to significantly better results in period estimation especially when the light curve does not exhibit sinusoidal shape. Second, we develop a new algorithm for parameter optimization for GP which is useful when the likelihood function is very sensitive to the parameters with numerous local minima, as in the case of period estimation. The algorithm combines gradient optimization with grid search and incorporates several mechanisms to overcome the high computational complexity of GP. Third, we develop a novel approach for using domain knowledge, in the form of a probabilistic generative model, and incorporate it into the period estimation algorithm. Experimental results validate our approach showing significant improvement over existing methods. C1 [Wang, Yuyang; Khardon, Roni] Tufts Univ, Dept Comp Sci, Medford, MA 02155 USA. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Protopapas, Pavlos] Harvard Univ, Inst Appl Computat Sci, Cambridge, MA 02138 USA. RP Wang, YY (reprint author), Tufts Univ, Dept Comp Sci, Medford, MA 02155 USA. FU NSF [IIS-0803409] FX This research was partly supported by NSF grant IIS-0803409. The experiments in this paper were performed on the Odyssey cluster supported by the FAS Research Computing Group at Harvard and the Tufts Linux Research Cluster supported by Tufts UIT Research Computing. NR 39 TC 5 Z9 5 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 SEP 1 PY 2012 VL 756 IS 1 AR 67 DI 10.1088/0004-637X/756/1/67 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300067 ER PT J AU Willner, SP Ashby, MLN Barmby, P Chapman, SC Coil, AL Cooper, MC Huang, JS Ivison, R Koo, DC AF Willner, S. P. Ashby, M. L. N. Barmby, P. Chapman, S. C. Coil, A. L. Cooper, M. C. Huang, J. -S. Ivison, R. Koo, D. C. TI A FULLY IDENTIFIED SAMPLE OF AEGIS20 MICROJANSKY RADIO SOURCES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; galaxies: photometry; infrared: galaxies; radio continuum: galaxies ID EXTENDED GROTH-STRIP; ACTIVE GALACTIC NUCLEI; STAR-FORMING GALAXIES; DEEP-FIELD-SOUTH; TO-FIR ANALYSIS; X-RAY SOURCES; K-Z RELATION; SOURCE POPULATION; REDSHIFT SURVEY; VLA SURVEY AB Infrared 3.6-8 mu m images of the Extended Groth Strip yield plausible counterpart identifications for all but one of 510 radio sources in the AEGIS20 S(1.4 GHz) > 50 mu Jy sample. This is the first such deep sample that has been effectively 100% identified. Achieving the same identification rate at R band would require observations reaching R-AB > 27. Spectroscopic redshifts are available for 46% of the sample and photometric redshifts for an additional 47%. Almost all of the sources with 3.6 mu m AB magnitudes brighter than 19 have spectroscopic redshifts z < 1.1, while fainter objects predominantly have photometric redshifts with 1 less than or similar to z less than or similar to 3. Unlike more powerful radio sources that are hosted by galaxies having large stellar masses within a relatively narrow range, the AEGIS20 counterparts have stellar masses spanning more than a factor of 10 at z similar to 1. The sources are roughly 10%-15% starbursts at z less than or similar to 0.5 and 20%-25% active galactic nuclei mostly at z > 1 with the remainder of uncertain nature. C1 [Willner, S. P.; Ashby, M. L. N.; Huang, J. -S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Chapman, S. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Cooper, M. C.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Ivison, R.] Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Koo, D. C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Coil, A. L.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. RP Willner, SP (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011 OI Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313 FU NASA; JPL/Caltech; NSF [AST-1055081, AST-0071198, AST-0507483, AST-0808133] FX The authors thank Jennifer Donley for valuable discussions on interpretation of IRAC color-color plots and Kate Whittaker for drawing our attention to and help with the NMBS survey. We thank Satoshi Miyazaki for providing the Subaru R images. We also thank Pablo Perez Gonzalez for help using the Rainbow Navigator query system and especially for his and Guillermo Barro'swork to create the Rainbow database. 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. A.L.C. acknowledges funding from NSF CAREER grant AST-1055081. DEEP spectroscopy is supported by the National Science Foundation grants AST-0071198, AST-0507483, and AST-0808133. This study makes use of data from AEGIS, a multiwavelength sky survey conducted with the Chandra, GALEX, Hubble, Keck, CFHT, MMT, Subaru, Palomar, Spitzer, VLA, and other telescopes and supported in part by the NSF, NASA, and the STFC. This work has made use of the Rainbow Cosmological Surveys Database, which is operated by the Universidad Complutense de Madrid (UCM). IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under cooperative agreement with the National Science Foundation. NR 57 TC 6 Z9 6 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 72 DI 10.1088/0004-637X/756/1/72 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300072 ER PT J AU Wu, JW Tsai, CW Sayers, J Benford, D Bridge, C Blain, A Eisenhardt, PRM Stern, D Petty, S Assef, R Bussmann, S Comerford, JM Cutri, R Evans, NJ Griffith, R Jarrett, T Lake, S Lonsdale, C Rho, J Stanford, SA Weiner, B Wright, EL Yan, L AF Wu, Jingwen Tsai, Chao-Wei Sayers, Jack Benford, Dominic Bridge, Carrie Blain, Andrew Eisenhardt, Peter R. M. Stern, Daniel Petty, Sara Assef, Roberto Bussmann, Shane Comerford, Julia M. Cutri, Roc Evans, Neal J., II Griffith, Roger Jarrett, Thomas Lake, Sean Lonsdale, Carol Rho, Jeonghee Stanford, S. Adam Weiner, Benjamin Wright, Edward L. Yan, Lin TI SUBMILLIMETER FOLLOW-UP OF WISE-SELECTED HYPERLUMINOUS GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: starburst; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; DUST-OBSCURED GALAXIES; STAR-FORMATION HISTORY; INFRARED LUMINOUS GALAXIES; SPITZER MIDINFRARED SPECTROSCOPY; POLYCYCLIC AROMATIC-HYDROCARBON; SPECTRAL ENERGY-DISTRIBUTIONS; SUPERMASSIVE BLACK-HOLES; DIGITAL SKY SURVEY; MU-M OBSERVATIONS AB We have used the Caltech Submillimeter Observatory (CSO) to follow-up a sample of Wide-field Infrared Survey Explorer (WISE) selected, hyperluminous galaxies, the so-called W1W2-dropout galaxies. This is a rare (similar to 1000 all-sky) population of galaxies at high redshift (peaks at z = 2-3), which are faint or undetected by WISE at 3.4 and 4.6 mu m, yet are clearly detected at 12 and 22 mu m. The optical spectra of most of these galaxies show significant active galactic nucleus activity. We observed 14 high-redshift (z > 1.7) W1W2-dropout galaxies with SHARC-II at 350-850 mu m, with nine detections, and observed 18 with Bolocam at 1.1 mm, with five detections. Warm Spitzer follow-up of 25 targets at 3.6 and 4.5 mu m, as well as optical spectra of 12 targets, are also presented in the paper. Combining WISE data with observations from warm Spitzer and CSO, we constructed their mid-IR to millimeter spectral energy distributions (SEDs). These SEDs have a consistent shape, showing significantly higher mid-IR to submillimeter ratios than other galaxy templates, suggesting a hotter dust temperature. We estimate their dust temperatures to be 60-120 K using a single-temperature model. Their infrared luminosities are well over 10(13) L-circle dot. These SEDs are not well fitted with existing galaxy templates, suggesting they are a new population with very high luminosity and hot dust. They are likely among the most luminous galaxies in the universe. We argue that they are extreme cases of luminous, hot dust-obscured galaxies (DOGs), possibly representing a short evolutionary phase during galaxy merging and evolution. A better understanding of their long-wavelength properties needs ALMA as well as Herschel data. C1 [Wu, Jingwen; Eisenhardt, Peter R. M.; Stern, Daniel; Assef, Roberto] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Tsai, Chao-Wei; Cutri, Roc; Griffith, Roger; Jarrett, Thomas; Yan, Lin] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Sayers, Jack; Bridge, Carrie] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Benford, Dominic] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Blain, Andrew] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Petty, Sara; Lake, Sean; Wright, Edward L.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Bussmann, Shane] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Comerford, Julia M.; Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78731 USA. [Lonsdale, Carol] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Rho, Jeonghee] SETI Inst, Mountain View, CA 94043 USA. [Rho, Jeonghee] NASA, Ames Res Ctr, SOFIA Sci Ctr, Moffett Field, CA 94035 USA. [Stanford, S. Adam] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Weiner, Benjamin] Steward Observ, Tucson, AZ 85721 USA. RP Wu, JW (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jingwen.wu@jpl.nasa.gov RI Benford, Dominic/D-4760-2012; OI Benford, Dominic/0000-0002-9884-4206; Weiner, Benjamin/0000-0001-6065-7483 FU NASA; NSF [AST-1109116]; National Aeronautics and Space Administration; National Science Foundation [AST 90-15755]; W. M. Keck Foundation; Alfred P. Sloan Foundation; U.S. Department of Energy Office of Science FX J.W. and R. A. were supported by an appointment to the NASA Postdoctoral Program at the Jet Propulsion Laboratory, administered by Oak Ridge Associated Universities through a contract with NASA. N.E. acknowledges support from NSF Grant AST-1109116. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This work is based on observations made with the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under funding from the National Science Foundation, contract AST 90-15755. This work uses data obtained from the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under contract with NASA. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California, and NASA. The Keck Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Some data reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution. This paper uses data from SDSS (DR 8). Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. NR 78 TC 44 Z9 44 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 SEP 1 PY 2012 VL 756 IS 1 AR 96 DI 10.1088/0004-637X/756/1/96 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300096 ER PT J AU Zahn, O Reichardt, CL Shaw, L Lidz, A Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dore, O Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Natoli, T Padin, S Plagge, T Pryke, C Ruhl, JE Schaffer, KK Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, K van Engelen, A Vanderlinde, K Vieira, JD Williamson, R AF Zahn, O. Reichardt, C. L. Shaw, L. Lidz, A. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dore, O. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, J. D. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Natoli, T. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Schaffer, K. K. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. TI COSMIC MICROWAVE BACKGROUND CONSTRAINTS ON THE DURATION AND TIMING OF REIONIZATION FROM THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; intergalactic medium; large-scale structure of universe ID LY-ALPHA EMITTERS; PROBE WMAP OBSERVATIONS; RADIATIVE-TRANSFER SIMULATIONS; ZELDOVICH POWER SPECTRUM; HYDROGEN REIONIZATION; PATCHY REIONIZATION; INTERGALACTIC MEDIUM; NEUTRAL HYDROGEN; BUBBLE-GROWTH; HII-REGIONS AB The epoch of reionization is a milestone of cosmological structure formation, marking the birth of the first objects massive enough to yield large numbers of ionizing photons. However, the mechanism and timescale of reionization remain largely unknown. Measurements of the cosmic microwave background (CMB) Doppler effect from ionizing bubbles embedded in large-scale velocity streams-known as the patchy kinetic Sunyaev-Zel'dovich (kSZ) effect-can be used to constrain the duration of reionization. When combined with large-scale CMB polarization measurements, the evolution of the ionized fraction, (x) over bar (e), can be inferred. Using new multi-frequency data from the South Pole Telescope (SPT), we show that the ionized fraction evolved relatively rapidly. For our basic foreground model, we find the kSZ power sourced by reionization at l = 3000 to be D-3000(patchy) <= 2.1 mu K-2 at 95% confidence. Using reionization simulations, we translate this to a limit on the duration of reionization of Delta z equivalent to z((x) over bare-0.20) - z((x) over bare-0.99) <= 4.4 (95% confidence). We find that this constraint depends on assumptions about the angular correlation between the thermal SZ power and the cosmic infrared background (CIB). Introducing the degree of correlation as a free parameter, we find that the limit on kSZ power weakens to D-3000(patchy) <= 4.9 mu K-2, implying Delta z <= 7.9 (95% confidence). We combine the SPT constraint on the duration of reionization with the Wilkinson Microwave Anisotropy Probe measurement of the integrated optical depth to probe the cosmic ionization history. We find that reionization ended with 95% confidence at z > 7.2 under the assumption of no tSZ-CIB correlation, and z > 5.8 when correlations are allowed. Improved constraints from the full SPT data set in conjunction with upcoming Herschel and Planck data should detect extended reionization at >95% confidence provided Delta z >= 2. These CMB observations complement other observational probes of the epoch of reionization such as the redshifted 21 cm line and narrowband surveys for Ly alpha-emitting galaxies. C1 [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Shaw, L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Lidz, A.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Dore, O.; Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 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. [Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Joy, M.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Lee, A. T.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.; Staniszewski, Z.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zahn, O (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. EM zahn@berkeley.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; Berkeley Center for Cosmological Physics fellowship; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan Research Fellowship; Yale University; NSF [AST-1009811, 0709498]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231] FX We thank Matt George, Guilaine Lagache, Cien Shang, David Spergel, Marco Viero, and Matias Zaldarriaga for useful discussions. The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation and the Gordon and Betty Moore Foundation. O. Zahn acknowledges support from a Berkeley Center for Cosmological Physics fellowship. 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. R. Keisler acknowledges support from NASA Hubble Fellowship grant HF-51275.01. B. A. Benson is supported by a KICP Fellowship. M. Dobbs acknowledges support from an Alfred P. Sloan Research Fellowship. L. Shaw acknowledges the support of Yale University and NSF grant AST-1009811. M. Millea and L. Knox acknowledge the support of NSF grant 0709498. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U. S. Department of Energy under Contract No. DE-AC02-05CH11231. 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. We also acknowledge usage of the FFTW and TeXShop software packages. NR 111 TC 83 Z9 83 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2012 VL 756 IS 1 AR 65 DI 10.1088/0004-637X/756/1/65 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 009SA UT WOS:000309044300065 ER PT J AU Itoh, A Nanami, S Harata, T Ohkubo, T Tan, S Chong, L Davies, SJ Yamakura, T AF Itoh, Akira Nanami, Satoshi Harata, Tsuyoshi Ohkubo, Tatsuhiro Tan, Sylvester Chong, Lucy Davies, Stuart J. Yamakura, Takuo TI The Effect of Habitat Association and Edaphic Conditions on Tree Mortality during El Nino-induced Drought in a Bornean Dipterocarp Forest SO BIOTROPICA LA English DT Article DE Borneo; El Nino drought; habitat association; lowland dipterocarp forest; mortality rates; Sarawak ID TROPICAL RAIN-FOREST; POPULATION-DYNAMICS; SENSITIVITY; IMPACT; PREFERENCE; SURVIVAL; SARAWAK; FIRE AB The effects of El Nino-induced droughts on dipterocarp forests must be quantified to evaluate the implications of future global climatic changes for the tropical forests of Southeast Asia. We studied the mortality of trees =1cm in diameter in a lowland dipterocarp forest in Borneo before, during, and after the 1997/1998 El Nino drought. The annual mortality rates were 1.30, 1.75, and 1.66percent/yr for the pre-drought, drought, and post-drought periods, respectively. The effect of drought was tree size-dependent being greater for larger trees. Modified logistic regression analysis revealed a significant interaction effect between species' habitat association and edaphic condition on mortality rates in all periods. For species associated with wet habitat, drought effect was greater in dry conditions than in wet conditions, in both the drought and post-drought periods. The mortality rates of dry-habitat species were less affected by the drought both in dry and wet conditions. A similar pattern was also found in common Dipterocarpaceae species; mortality rates increased more in species associated with wet-habitat in the drought and post-drought periods. Species and families with higher mortality in the pre-drought period tended to experience greater mortality increases during the drought and post-drought periods. These results suggest that changes in drought regimes alter the species composition and spatial distribution of dipterocarp forests. C1 [Itoh, Akira; Nanami, Satoshi; Harata, Tsuyoshi; Yamakura, Takuo] Osaka City Univ, Grad Sch Sci, Osaka 5588585, Japan. [Ohkubo, Tatsuhiro] Utsunomiya Univ, Fac Agr, Utsunomiya, Tochigi 3210943, Japan. [Tan, Sylvester; Chong, Lucy] Sarawak Forestry Corp, Kuching, Sarawak, Malaysia. [Tan, Sylvester; Davies, Stuart J.] Harvard Univ, Smithsonian Trop Res Inst, Cambridge, MA 02138 USA. [Tan, Sylvester; Davies, Stuart J.] Harvard Univ, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. RP Itoh, A (reprint author), Osaka City Univ, Grad Sch Sci, Osaka 5588585, Japan. EM itoha@sci.osaka-cu.ac.jp FU Global Environment Research Fund of the Ministry of the Environment, Japan [D-0901]; MEXT; JSPS, Japan [NP0201, NP0901, 20405011] FX We thank Drs. H. S. Lee, K. Ogino, I. Yamada, and P. S. Ashton for their support during this long-term ecological study of the Lambir forest. The 52-ha study plot was established in collaboration with the Forest Department of Sarawak, Sarawak Forestry Corporation, Harvard University, The Center for Tropical Forest Science of the Smithsonian Tropical Research Institute, and several Japanese universities. We also thank Dr. J. LaFrankie for species identification and the staff members of the Forest Department of Sarawak and Sarawak Forestry Corporation for their field assistance. This study was supported in part by the Global Environment Research Fund of the Ministry of the Environment, Japan (D-0901), and Grants-in-Aid for Scientific Research from MEXT and JSPS, Japan (NP0201, NP0901, 20405011). NR 42 TC 13 Z9 13 U1 4 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD SEP PY 2012 VL 44 IS 5 BP 606 EP 617 DI 10.1111/j.1744-7429.2012.00867.x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 000QW UT WOS:000308403400005 ER PT J AU Flechas, SV Sarmiento, C Amezquita, A AF Victoria Flechas, Sandra Sarmiento, Carolina Amezquita, Adolfo TI Bd on the Beach: High Prevalence of Batrachochytrium dendrobatidis in the Lowland Forests of Gorgona Island (Colombia, South America) SO ECOHEALTH LA English DT Article DE Batrachochytrium dendrobatidis; Atelopus; lowland rainforests; Gorgona Island; prevalence of infection ID AMPHIBIAN POPULATION DECLINES; CHYTRID FUNGUS; INFECTIOUS-DISEASE; GLOBAL DECLINE; FROGS; EXTINCTIONS; CHYTRIDIOMYCOSIS; HABITATS; PANAMA AB The amphibian chytrid fungus, Batrachochytrium dendrobatidis, Bd, has been implicated in the decimation and extinction of many amphibian populations worldwide, especially at mid and high elevations. Recent studies have demonstrated the presence of the pathogen in the lowlands from Australia and Central America. We extend here its elevational range by demonstrating its presence at the sea level, in the lowland forests of Gorgona Island, off the Pacific coast of Colombia. We conducted two field surveys, separated by four years, and diagnosed Bd by performing polymerase chain reactions on swab samples from the skin of five amphibian species. All species, including the Critically Endangered Atelopus elegans, tested positive for the pathogen, with prevalences between 3.9 % in A. elegans (in 2010) and 52 % in Pristimantis achatinus. Clinical signs of chytridiomycosis were not detected in any species. To our knowledge, this is the first report of B. dendrobatidis in tropical lowlands at sea level, where temperatures may exceed optimal growth temperatures of this pathogen. This finding highlights the need to understand the mechanisms allowing the interaction between frogs and pathogen in lowland ecosystems. C1 [Victoria Flechas, Sandra; Sarmiento, Carolina; Amezquita, Adolfo] Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. [Sarmiento, Carolina] Smithsonian Trop Res Inst, Ancon, Panama. RP Flechas, SV (reprint author), Univ Los Andes, Dept Biol Sci, Bogota 4976, Colombia. EM vickyflechas@gmail.com OI Sarmiento, Carolina/0000-0002-8575-7170 FU Conservation International's Critically Endangered Species Fund; Association of Zoos and Aquariums' Conservation Endowment Fund FX This study was completed with financial support from Conservation International's Critically Endangered Species Fund and the Association of Zoos and Aquariums' Conservation Endowment Fund. For assistance in the field, we thank A. J. Crawford, C. Silva, J. Mendez, and J. A. Hernandez. Thanks to A. J. Crawford, D. M. Hudson, S. LOtters and R. Ibanez for helpful comments and suggestions that greatly improved this manuscript. Research permits were provided by the Unidad Administrativa del Sistema de Parques Nacionales Naturales (PIDB DTSO 001-09 and PIDB DTSO 019-09). NR 43 TC 9 Z9 9 U1 0 U2 19 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1612-9202 EI 1612-9210 J9 ECOHEALTH JI EcoHealth PD SEP PY 2012 VL 9 IS 3 BP 298 EP 302 DI 10.1007/s10393-012-0771-9 PG 5 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 006KK UT WOS:000308817900011 PM 22669408 ER PT J AU Loss, SR Will, T Marra, PP AF Loss, Scott R. Will, Tom Marra, Peter P. TI Direct human-caused mortality of birds: improving quantification of magnitude and assessment of population impact SO FRONTIERS IN ECOLOGY AND THE ENVIRONMENT LA English DT Review ID COMMUNICATION TOWERS; AVIAN COLLISIONS; DOMESTIC CATS; GUY WIRES; DECLINES; REMOVAL; MANAGEMENT; SCAVENGERS; PREDATION; HEIGHT AB Hundreds of millions to greater than one billion North American birds are directly killed each year by human stressors, including collisions with man-made structures, predation by feral and pet cats, intentional and accidental poisoning, and pollution. Because these causes of mortality are increasingly abundant and because some result in large bird die-offs, they have received both increased scientific attention and general media coverage. However, quantifying bird mortality remains imprecise and methods to assess whether these losses cause important biological impacts remain underdeveloped. If local mortality studies followed rigorous design and sampling schemes, allowing comparison of data and scaling up of mortality estimates to broad regions, this could lead to improved analyses. Several analytical techniques - including hierarchical and population models - show potential for improving quantification of anthropogenic mortality of birds and inference of population-level effects. Results arising from improved study designs and analytical techniques will more effectively inform decision making about policies and regulations aimed at reducing avian mortality and minimizing population impacts. C1 [Loss, Scott R.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC USA. [Will, Tom] US Fish & Wildlife Serv, Div Migratory Birds, Midwest Reg Off, Bloomington, MN USA. RP Loss, SR (reprint author), Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC USA. EM losss@si.edu RI Loss, Scott/B-1504-2014 FU US Fish and Wildlife Service through the Smithsonian Conservation Biology Institute FX SRL was supported by a postdoctoral fellowship funded by the US Fish and Wildlife Service through the Smithsonian Conservation Biology Institute's Postdoctoral Fellowship program. We thank TW Arnold, DH Johnson, AD Rodewald, JA Royle, and MC Runge for comments that greatly improved the manuscript. The findings and conclusions in this article are those of the authors and do not necessarily represent the views of the US Fish and Wildlife Service. NR 38 TC 39 Z9 39 U1 5 U2 107 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1540-9295 EI 1540-9309 J9 FRONT ECOL ENVIRON JI Front. Ecol. Environ. PD SEP PY 2012 VL 10 IS 7 BP 357 EP 364 DI 10.1890/110251 PG 8 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 010KG UT WOS:000309092700014 ER PT J AU Meisner, K Zotz, G AF Meisner, Kerstin Zotz, Gerhard TI HETEROBLASTY IN BROMELIADS: ITS FREQUENCY IN A LOCAL FLORA AND THE TIMING OF THE TRANSITION FROM ATMOSPHERIC TO TANK FORM IN THE FIELD SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE growth; leaf index; ontogeny; relative growth rate; vascular epiphytes ID TILLANDSIA-DEPPEANA BROMELIACEAE; HUMID MONTANE FOREST; EPIPHYTIC BROMELIADS; GROWTH-RATE; PLANTS; ALLOCATION; SURVIVAL; ONTOGENY AB The prevalence and functional relevance of heteroblasty, i.e., abrupt morphological changes in ontogeny in many angiosperms, remain obscure. To obtain a first estimate of the number of heteroblastic bromeliads, we used a simple metric to distinguish unambiguously heteroblastic from homoblastic species. We addressed ecological relevance by determining the time for transition between ontogenetic stages (atmospheric and tank) and by comparing the prevalence of heteroblasty in different habitats. Epiphytic Tillandsioideae were studied in a lowland and a montane forest in Panama. Repeated censuses allowed estimates of relative growth rates and the construction of ontogenetic trajectories for 14 species. Data on leaf index (leaf length/width) were taken for 23 species. Ontogenetic changes in leaf index reliably separate homoblastic and heteroblastic species. The early atmospheric stage in heteroblastic species lasts, on average, 3 yr, equivalent to 20% of the average generation time. Heteroblastic species are as common in the understory as at exposed growing sites. This finding challenges the notion of heteroblasty as an adaptation to drought, because there are no differences in the proportion of heteroblastic species in wet and dry habitats. An alternative hypothesis is proposed. C1 [Meisner, Kerstin; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, AG Funkt Okol, Inst Biol & Umweltwissensch, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Meisner, K (reprint author), Carl von Ossietzky Univ Oldenburg, AG Funkt Okol, Inst Biol & Umweltwissensch, Postfach 2503, D-26111 Oldenburg, Germany. EM kerstin.meisner@uni-oldenburg.de FU Deutsche Forschungsgemeinschaft [GZ ZO 94/4-1]; Panamanian authorities (ANAM) [SE/P-17-09, SE/P-5-10, SE/P-5-11] FX Financial support from the Deutsche Forschungsgemeinschaft (GZ ZO 94/4-1) for our current studies on heteroblasty in bromeliads is acknowledged. We thank the Panamanian authorities (ANAM, SE/P-17-09, SE/P-5-10, and SE/P-5-11) and the Smithsonian Tropical Research Institute (STRI, Panama) for permission to carry out this study. For assistance in the field, we acknowledge Yader Sageth, who was supported by a STRI internship. NR 40 TC 8 Z9 8 U1 0 U2 19 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1058-5893 J9 INT J PLANT SCI JI Int. J. Plant Sci. PD SEP PY 2012 VL 173 IS 7 BP 780 EP 788 DI 10.1086/666665 PG 9 WC Plant Sciences SC Plant Sciences GA 997KQ UT WOS:000308164600004 ER PT J AU Waller, TR AF Waller, Thomas R. TI MORPHOLOGY, PHYLOGENY, AND SYSTEMATIC REVISION OF GENERA IN THE DIMYIDAE (MOLLUSCA, BIVALVIA, PTERIOMORPHIA) SO JOURNAL OF PALEONTOLOGY LA English DT Article ID NEW-ZEALAND; PECTINIDAE; CLASSIFICATION; OSTREIDAE; HINGE; GENUS AB Differences in the mineralogy of hinge teeth and inner shell layers in the family Dimyidae form the basis for a revision of genera. The stem genus Atreta (Late Triassic to Late Cretaceous) has aragonitic denticulate hinge teeth on the right valve articulating with pitted sockets on the left valve. The same arrangement is present in Neoatreta n. gen. (Paleocene? Miocene to Recent) but with the appearance of extensive calcitic overarching of the resilifer. In Dimyella (Eocene to Recent), aragonitic teeth and sockets are still present but are modified into hook shaped denticulate teeth with corresponding sockets. All three of these genera have inner aragonitic crossed-lamellar shell layers that extend well outside the pallial line. In contrast, Dimya (Eocene to Recent) and Basiliomya),a (Pliocene to Recent) comprise a second clade in which aragonitic hinge teeth are absent and hinge articulation is calcitic, derived from the calcitic rim. Dimya has only weak hinge articulation and has an aragonitic inner shell layer delimited by the pallial line; in Basiliomya calcitic hinge teeth are more prominent and the entire inner shell layer inside the pallial line is foliated calcite. Diploschiza (Cretaceous, Albian to Maastrichtian), here reinstated from synonymy with Atreta, is probably a precursor of the Dimya-Basiliomya clade based on incipient calcitic hinge teeth. Predation pressures probably drove the evolution of this cemented family from its original habitat on hardgrounds in moderately deep water into much greater depths or into cryptic habitats, including submarine caves. New combinations are Dimyella malnatrensis (Corselli and Bernocchi), D. molokaia (Dall, Bartsch, and Rehder), D. similis (v. Koenen), Neoatreta dissimilis (Tate), N. filipina (Bartsch), N. kaiparaensis (Laws), N. phaidra (Woodring), and N. plana (Martin). C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Waller, TR (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. EM wallert@si.edu NR 119 TC 1 Z9 3 U1 0 U2 3 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD SEP PY 2012 VL 86 IS 5 BP 829 EP 851 PG 23 WC Paleontology SC Paleontology GA 002XV UT WOS:000308573200006 ER PT J AU Davidson, TM AF Davidson, Timothy M. TI Boring crustaceans damage polystyrene floats under docks polluting marine waters with microplastic SO MARINE POLLUTION BULLETIN LA English DT Article DE Burrowing isopod; Invasive species; Marine borers; Microplastic; Plastic pollution; Sphaeroma quoianum ID ISOPOD SPHAEROMA-QUOIANUM; BURROWING ISOPOD; PLASTIC DEBRIS; SALT-MARSHES; ENVIRONMENT; CONTAMINANTS; INGESTION; SEABIRDS; FLABELLIFERA; CALIFORNIA AB Boring isopods damage expanded polystyrene floats under docks and, in the process, expel copious numbers of microplastic particles. This paper describes the impacts of boring isopods in aquaculture facilities and docks, quantifies and discusses the implications of these microplastics, and tests if an alternate foam type prevents boring. Floats from aquaculture facilities and docks were heavily damaged by thousands of isopods and their burrows. Multiple sites in Asia, Australia, Panama, and the USA exhibited evidence of isopod damage. One isopod creates thousands of microplastic particles when excavating a burrow; colonies can expel millions of particles. Microplastics similar in size to these particles may facilitate the spread of non-native species or be ingested by organisms causing physical or toxicological harm. Extruded polystyrene inhibited boring, suggesting this foam may prevent damage in the field. These results reveal boring isopods cause widespread damage to docks and are a novel source of microplastic pollution. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Davidson, Timothy M.] Portland State Univ ESM, Aquat Bioinvas Res & Policy Inst, Portland, OR 97207 USA. RP Davidson, TM (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM DavidsonT@si.edu OI Davidson, Timothy/0000-0001-9535-7982 FU Western Regional Panel on Aquatic Nuisance Species (under United States Fish & Wildlife Service Grant) [60181-7G256]; Estuarine Reserves Division, Office of Ocean and Coastal Resource Management, National Ocean Service, National Oceanic and Atmospheric Administration; National Science Foundation East Asia and South Pacific Summer Institute fellowship in Taiwan FX I thank James Carlton, Andy Chang, Simon Cragg, Catherine de Rivera, Glenn Dolphin, Ernie Estevez, George Rotramel, Gregory Ruiz, Kerstin Wasson, and Elizabeth Wells for providing technical advice, information on the distribution of borers, and helpful conversations. The comments from the reviewers helped improve a previous version of this manuscript. I am grateful to Hwey Lian Hsieh for providing lab space and transportation assistance while in Taiwan. Aspects of this research were supported by the Western Regional Panel on Aquatic Nuisance Species (under United States Fish & Wildlife Service Grant Agreement number 60181-7G256 to C.E. de Rivera), the Estuarine Reserves Division, Office of Ocean and Coastal Resource Management, National Ocean Service, National Oceanic and Atmospheric Administration (fellowship to T.M. Davidson), and the National Science Foundation East Asia and South Pacific Summer Institute fellowship in Taiwan (fellowship to T.M. Davidson). NR 70 TC 11 Z9 15 U1 12 U2 108 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0025-326X EI 1879-3363 J9 MAR POLLUT BULL JI Mar. Pollut. Bull. PD SEP PY 2012 VL 64 IS 9 BP 1821 EP 1828 DI 10.1016/j.marpolbul.2012.06.005 PG 8 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 006WV UT WOS:000308851400022 PM 22763283 ER PT J AU Beardsley, AP Hazelton, BJ Morales, MF Capallo, RJ Goeke, R Emrich, D Lonsdale, CJ Arcus, W Barnes, D Bernardi, G Bowman, JD Bunton, JD Corey, BE Deshpande, A deSouza, L Gaensler, BM Greenhill, LJ Herne, D Hewitt, JN Kaplan, DL Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lynch, MJ McWhirter, SR Mitchell, DA Morgan, E Oberoi, D Ord, SM Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, A Salah, JE Sault, RJ Shankar, NU Srivani, KS Stevens, J Subrahmanyan, R Tingay, SJ Wayth, RB Waterson, M Webster, RL Whitney, AR Williams, A Williams, CL Wyithe, JSB AF Beardsley, A. P. Hazelton, B. J. Morales, M. F. Capallo, R. J. Goeke, R. Emrich, D. Lonsdale, C. J. Arcus, W. Barnes, D. Bernardi, G. Bowman, J. D. Bunton, J. D. Corey, B. E. Deshpande, A. deSouza, L. Gaensler, B. M. Greenhill, L. J. Herne, D. Hewitt, J. N. Kaplan, D. L. Kasper, J. C. Kincaid, B. B. Koenig, R. Kratzenberg, E. Lynch, M. J. McWhirter, S. R. Mitchell, D. A. Morgan, E. Oberoi, D. Ord, S. M. Pathikulangara, J. Prabu, T. Remillard, R. A. Rogers, A. E. E. Roshi, A. Salah, J. E. Sault, R. J. Shankar, N. Udaya Srivani, K. S. Stevens, J. Subrahmanyan, R. Tingay, S. J. Wayth, R. B. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Williams, C. L. Wyithe, J. S. B. TI A new layout optimization technique for interferometric arrays, applied to the Murchison Widefield Array SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; cosmology: miscellaneous ID REIONIZATION OBSERVATORIES; EPOCH; DESIGN; SUBTRACTION; SENSITIVITY AB Antenna layout is an important design consideration for radio interferometers because it determines the quality of the snapshot point spread function (PSF, or array beam). This is particularly true for experiments targeting the 21-cm Epoch of Reionization signal as the quality of the foreground subtraction depends directly on the spatial dynamic range and thus the smoothness of the baseline distribution. Nearly all sites have constraints on where antennas can be placed even at the remote Australian location of the Murchison Widefield Array (MWA) there are rock outcrops, flood zones, heritages areas, emergency runways and trees. These exclusion areas can introduce spatial structure into the baseline distribution that enhances the PSF sidelobes and reduces the angular dynamic range. In this paper we present a new method of constrained antenna placement that reduces the spatial structure in the baseline distribution. This method not only outperforms random placement algorithms that avoid exclusion zones, but surprisingly outperforms random placement algorithms without constraints to provide what we believe are the smoothest constrained baseline distributions developed to date. We use our new algorithm to determine antenna placements for the originally planned MWA, and present the antenna locations, baseline distribution and snapshot PSF for this array choice. C1 [Beardsley, A. P.; Hazelton, B. J.; Morales, M. F.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Capallo, R. J.; Lonsdale, C. J.; Corey, B. E.; Kincaid, B. B.; Kratzenberg, E.; McWhirter, S. R.; Oberoi, D.; Rogers, A. E. E.; Salah, J. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Goeke, R.; Hewitt, J. N.; Morgan, E.; Remillard, R. A.; Williams, C. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Emrich, D.; Arcus, W.; Herne, D.; Lynch, M. J.; Tingay, S. J.; Wayth, R. B.; Waterson, M.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Barnes, D.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Bernardi, G.; Greenhill, L. J.; Kasper, J. C.; Mitchell, D. A.; Ord, S. M.; Wayth, R. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, J. D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Bunton, J. D.; deSouza, L.; Koenig, R.; Pathikulangara, J.; Stevens, J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Deshpande, A.; Prabu, T.; Roshi, A.; Shankar, N. Udaya; Srivani, K. S.; Subrahmanyan, R.] Raman Res Inst, Bangalore 560080, Karnataka, India. [deSouza, L.; Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Gaensler, B. M.; Mitchell, D. A.; Tingay, S. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Kaplan, D. L.] Univ Wisconsin, Dept Phys, Milwaukee, WI 53201 USA. [Sault, R. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Sch Phys, Parkville, Vic 3010, Australia. [Stevens, J.] Univ Tasmania, Hobart, Tas 7001, Australia. [Waterson, M.] Australian Natl Univ, Weston, ACT 2611, Australia. [Williams, A.] Perth Observ, Bickley, WA 6076, Australia. [Williams, A.] Univ Western Australia, Nedlands, WA 6009, Australia. RP Beardsley, AP (reprint author), Univ Washington, Dept Phys, Seattle, WA 98195 USA. EM mmorales@phys.washington.edu RI Bunton, John/A-4944-2008; Deshpande, Avinash/D-4868-2012; Williams, Andrew/K-2931-2013; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; Subrahmanyan, Ravi/D-4889-2012; Wayth, Randall/B-2444-2013; Tingay, Steven/B-5271-2013; Emrich, David/B-7002-2013; Waterson, Mark/B-7352-2013; Ord, Stephen/C-6138-2013; Kasper, Justin/D-1152-2010; Gaensler, Bryan/F-8655-2010 OI Wyithe, Stuart/0000-0001-7956-9758; Gaensler, Bryan/0000-0002-3382-9558; Williams, Andrew/0000-0001-9080-0105; M, Manjunath/0000-0001-8710-0730; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; Waterson, Mark/0000-0002-0192-2686; Kasper, Justin/0000-0002-7077-930X; FU U.S. National Science Foundation [AST CAREER-0847753, AST-0457585, AST-0908884, PHY-0835713]; Australian Research Council [LE0775621, LE0882938]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Smithsonian Astrophysical Observatory; MIT School of Science; Raman Research Institute; Australian National University; iVEC Petabyte Data Store; Initiative in Innovative Computing; NVIDIA; International Centre for Radio Astronomy Research; Curtin University of Technology; University of Western Australia; Western Australian State government FX Support came from the U.S. National Science Foundation (grants AST CAREER-0847753, AST-0457585, AST-0908884 and PHY-0835713), the Australian Research Council (grants LE0775621 and LE0882938), the U.S. Air Force Office of Scientific Research (grant FA9550-0510247), the Smithsonian Astrophysical Observatory, the MIT School of Science, the Raman Research Institute, the Australian National University, the iVEC Petabyte Data Store, the Initiative in Innovative Computing and NVIDIA sponsored Center for Excellence at Harvard, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University of Technology and The University of Western Australia, funded by the Western Australian State government. NR 17 TC 9 Z9 9 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 SEP PY 2012 VL 425 IS 3 BP 1781 EP 1788 DI 10.1111/j.1365-2966.2012.20878.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996KC UT WOS:000308084100015 ER PT J AU Silverman, JM Foley, RJ Filippenko, AV Ganeshalingam, M Barth, AJ Chornock, R Griffith, CV Kong, JJ Lee, N Leonard, DC Matheson, T Miller, EG Steele, TN Barris, BJ Bloom, JS Cobb, BE Coil, AL Desroches, LB Gates, EL Ho, LC Jha, SW Kandrashoff, MT Li, WD Mandel, KS Modjaz, M Moore, MR Mostardi, RE Papenkova, MS Park, S Perley, DA Poznanski, D Reuter, CA Scala, J Serduke, FJD Shields, JC Swift, BJ Tonry, JL Van Dyk, SD Wang, XF Wong, DS AF Silverman, Jeffrey M. Foley, Ryan J. Filippenko, Alexei V. Ganeshalingam, Mohan Barth, Aaron J. Chornock, Ryan Griffith, Christopher V. Kong, Jason J. Lee, Nicholas Leonard, Douglas C. Matheson, Thomas Miller, Emily G. Steele, Thea N. Barris, Brian J. Bloom, Joshua S. Cobb, Bethany E. Coil, Alison L. Desroches, Louis-Benoit Gates, Elinor L. Ho, Luis C. Jha, Saurabh W. Kandrashoff, Michael T. Li, Weidong Mandel, Kaisey S. Modjaz, Maryam Moore, Matthew R. Mostardi, Robin E. Papenkova, Marina S. Park, Sung Perley, Daniel A. Poznanski, Dovi Reuter, Cassie A. Scala, James Serduke, Franklin J. D. Shields, Joseph C. Swift, Brandon J. Tonry, John L. Van Dyk, Schuyler D. Wang, Xiaofeng Wong, Diane S. TI Berkeley Supernova Ia Program - I. Observations, data reduction and spectroscopic sample of 582 low-redshift Type Ia supernovae SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE surveys; supernovae: general; cosmology: observations; distance scale ID DIGITAL SKY SURVEY; BVRI LIGHT CURVES; DARK-ENERGY CONSTRAINTS; PHOTOMETRY DATA RELEASE; LEGACY SURVEY; TIME DILATION; ULTRAVIOLET EXTINCTION; OPTICAL SPECTROSCOPY; IMPROVED DISTANCES; ESSENCE PROJECT AB In this first paper in a series, we present 1298 low-redshift (z ? 0.2) optical spectra of 582 Type Ia supernovae (SNe Ia) observed from 1989 to 2008 as part of the Berkeley Supernova Ia Program (BSNIP). 584 spectra of 199 SNe Ia have well-calibrated light curves with measured distance moduli, and many of the spectra have been corrected for host-galaxy contamination. Most of the data were obtained using the Kast double spectrograph mounted on the Shane 3 m telescope at Lick Observatory and have a typical wavelength range of 330010?400 angstrom, roughly twice as wide as spectra from most previously published data sets. We present our observing and reduction procedures, and we describe the resulting SN Database, which will be an online, public, searchable data base containing all of our fully reduced spectra and companion photometry. In addition, we discuss our spectral classification scheme (using the SuperNova IDentification code, snid; Blondin & Tonry), utilizing our newly constructed set of snid spectral templates. These templates allow us to accurately classify our entire data set, and by doing so we are able to reclassify a handful of objects as bona fide SNe Ia and a few other objects as members of some of the peculiar SN Ia subtypes. In fact, our data set includes spectra of nearly 90 spectroscopically peculiar SNe Ia. We also present spectroscopic host-galaxy redshifts of some SNe Ia where these values were previously unknown. The sheer size of the BSNIP data set and the consistency of our observation and reduction methods make this sample unique among all other published SN Ia data sets and complementary in many ways to the large, low-redshift SN Ia spectra presented by Matheson et al. and Blondin et al. In other BSNIP papers in this series, we use these data to examine the relationships between spectroscopic characteristics and various observables such as photometric and host-galaxy properties. C1 [Silverman, Jeffrey M.; Filippenko, Alexei V.; Ganeshalingam, Mohan; Griffith, Christopher V.; Kong, Jason J.; Steele, Thea N.; Bloom, Joshua S.; Desroches, Louis-Benoit; Kandrashoff, Michael T.; Li, Weidong; Modjaz, Maryam; Moore, Matthew R.; Mostardi, Robin E.; Park, Sung; Perley, Daniel A.; Poznanski, Dovi; Reuter, Cassie A.; Scala, James; Serduke, Franklin J. D.; Wong, Diane S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Foley, Ryan J.; Chornock, Ryan; Mandel, Kaisey S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barth, Aaron J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Griffith, Christopher V.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Lee, Nicholas; Barris, Brian J.; Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Miller, Emily G.] Univ Penn, Philadelphia, PA 19104 USA. [Steele, Thea N.] Kutztown Univ Penn, Dept Comp Sci, Kutztown, PA 19530 USA. [Cobb, Bethany E.] George Washington Univ, Dept Phys, Washington, DC 20052 USA. [Coil, Alison L.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Desroches, Louis-Benoit] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Gates, Elinor L.] Univ Calif Observ, Lick Observ, Mt Hamilton, CA 95140 USA. [Ho, Luis C.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Jha, Saurabh W.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Modjaz, Maryam] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Mostardi, Robin E.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Papenkova, Marina S.] E Los Angeles Coll, Dept Phys & Astron, Monterey Pk, CA 91754 USA. [Perley, Daniel A.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Reuter, Cassie A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Shields, Joseph C.] Ohio Univ, Dept Phys & Astron, Athens, OH 45701 USA. [Swift, Brandon J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Van Dyk, Schuyler D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Wang, Xiaofeng] Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China. [Wang, Xiaofeng] Tsinghua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China. RP Silverman, JM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM JSilverman@astro.berkeley.edu RI Wang, Xiaofeng/J-5390-2015; OI Barth, Aaron/0000-0002-3026-0562; Van Dyk, Schuyler/0000-0001-9038-9950 FU W. M. Keck Foundation; NSF [AST-0908886]; DOE [DE-FC02-06ER41453, DE-FG02-08ER41563]; TABASGO Foundation; Hubble Fellowship [HST-HF-51277.01-A]; STScI; NASA [NAS5-26555] FX We would like to thank K. Alatalo, L. Armus, M. Baker, M. Bentz, E. Berger, M. Bershady, A. Blum, A. Burgasser, N. Butler, G. Canalizo, H. Chen, M. Cooper, C. DeBreuck, M. Dickinson, R. Eastman, M. Eracleous, S. Faber, X. Fan, C. Fassnacht, P. Garnavich, M. George, D. Gilbank, A. Gilbert, K. Glazebrook, J. Graham, G. Graves, R. Green, J. Greene, M. Gregg, M. Hidas, K. Hiner, W. Ho, J. Hoffman, I. Hook, D. Hutchings, V. Junkkarinen, L. Kewley, R. Kirshner, D. Kocevski, S. Kulkarni, M. Lehnert, B. Leibundgut, M. Malkan, A. Martel, M. McCourt, A. Miller, E. Moran, P. Nandra, J. Newman, K. Noeske, C. Papovich, C. Peng, S. Perlmutter, M. Phillips, D. Pooley, H. Pugh, E. Quataert, M. Rich, M. Richmond, A. Riess, S. Rodney, K. Sandstrom, W. Sargent, K. Shimasaki, R. Simcoe, T. Small, G. Smith, H. Smith, H. Spinrad, G. Squires, C. Steidel, D. Stern, D. Stevens, R. Street, C. Thornton, T. Treu, B. Tucker, D. Tytler, W. van Breugel, V. Virgilio, V. Viscomi, N. Vogt, J. Walsh, D. Weisz, C. Willmer, A. Wolfe and J.-H. Woo for their assistance with some of the observations over the last two decades. We would also like to thank J. Choi, M. Ellison, L. Jewett, A. Morton, X. Parisky and P. Thrasher for helping to verify some of the information in the SNDB. Moreover, we thank the referee for comments and suggestions that improved the manuscript. We are grateful to the staff at the Lick and Keck Observatories for their support. 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 (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. 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 NASA. AVF's group is supported by the NSF grant AST-0908886, DOE grants DE-FC02-06ER41453 (SciDAC) and DE-FG02-08ER41563, and the TABASGO Foundation. MM acknowledges support from Hubble Fellowship grant HST-HF-51277.01-A, awarded by STScI, which is operated by AURA under NASA contract NAS5-26555, for the time during which some of this work was conducted. 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. We would like to dedicate this paper to the memory of Marc J. Staley, who never stopped asking the Great Questions. NR 118 TC 79 Z9 79 U1 0 U2 3 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 SEP PY 2012 VL 425 IS 3 BP 1789 EP 1818 DI 10.1111/j.1365-2966.2012.21270.x PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996KC UT WOS:000308084100016 ER PT J AU Keres, D Vogelsberger, M Sijacki, D Springel, V Hernquist, L AF Keres, Dusan Vogelsberger, Mark Sijacki, Debora Springel, Volker Hernquist, Lars TI Moving-mesh cosmology: characteristics of galaxies and haloes SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE methods: numerical; galaxies: evolution; galaxies: formation; galaxies: haloes; galaxies: interactions; dark matter ID SMOOTHED PARTICLE HYDRODYNAMICS; COLD DARK-MATTER; STAR-FORMING GALAXIES; LAMBDA-CDM UNIVERSE; LYMAN-ALPHA FOREST; ANGULAR-MOMENTUM; DISK GALAXIES; NUMERICAL SIMULATIONS; COMPARISON PROJECT; BARYON FRACTION AB We discuss cosmological hydrodynamic simulations of galaxy formation performed with the new moving-mesh code arepo, which promises higher accuracy compared with the traditional smoothed particle hydrodynamics (SPH) technique that has been widely employed for this problem. In this exploratory study, we deliberately limit the complexity of the physical processes followed by the code for ease of comparison with previous calculations, and include only cooling of gas with a primordial composition, heating by a spatially uniform ultraviolet background, and a simple subresolution model for regulating star formation in the dense interstellar medium. We use an identical set of physics in corresponding simulations carried out with the well-tested SPH code gadget, adopting also the same high-resolution gravity solver. We are thus able to compare both simulation sets on an object-by-object basis, allowing us to cleanly isolate the impact of different hydrodynamical methods on galaxy and halo properties. In accompanying papers, Vogelsberger et al. and Sijacki et al., we focus on an analysis of the global baryonic statistics predicted by the simulation codes, and complementary idealized simulations that highlight the differences between the hydrodynamical schemes. Here we investigate their influence on the baryonic properties of simulated galaxies and their surrounding haloes. We find that arepo leads to significantly higher star formation rates for galaxies in massive haloes and to more extended gaseous discs in galaxies, which also feature a thinner and smoother morphology than their gadget counterparts. Consequently, galaxies formed in arepo have larger sizes and higher specific angular momentum than their SPH correspondents. Interestingly, the more efficient cooling flows in arepo yield higher densities and lower entropies in halo centres compared to gadget, whereas the opposite trend is found in halo outskirts. The cooling differences leading to higher star formation rates of massive galaxies in arepo also slightly increase the baryon content within the virial radius of massive haloes. We show that these differences persist as a function of numerical resolution. While both codes agree to acceptable accuracy on a number of baryonic properties of cosmic structures, our results thus clearly demonstrate that galaxy formation simulations greatly benefit from the use of more accurate hydrodynamical techniques such as arepo and call into question the reliability of galaxy formation studies in a cosmological context using traditional standard formulations of SPH, such as the one implemented in gadget. Our new moving-mesh simulations demonstrate that a population of extended gaseous discs of galaxies in large volume cosmological simulations can be formed even without energetic feedback in the form of galactic winds, although such outflows appear required to obtain realistic stellar masses. C1 [Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Vogelsberger, Mark; Sijacki, Debora; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Heidelberg Univ, Zentrum Astron, ARI, D-69120 Heidelberg, Germany. RP Keres, D (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM dkeres@physics.ucsd.edu FU NASA [HSTHF-51276.01-A]; NASA ATP [NNX11AI97G]; NASA Hubble Fellowship [HST-HF-51282.01-A] FX We would like to thank the referee, Fabio Governato, for constructive comments. The simulations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. DK acknowledges support from NASA through Hubble Fellowship grant HSTHF-51276.01-A and NASA ATP NNX11AI97G. DS acknowledges NASA Hubble Fellowship through grant HST-HF-51282.01-A. NR 117 TC 81 Z9 82 U1 0 U2 5 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 SEP PY 2012 VL 425 IS 3 BP 2027 EP 2048 DI 10.1111/j.1365-2966.2012.21548.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996KC UT WOS:000308084100027 ER PT J AU Leverkus, AB Puerta-Pinero, C Guzman-Alvarez, JR Navarro, J Castro, J AF Leverkus, Alexandro B. Puerta-Pinero, Carolina Ramon Guzman-Alvarez, Jose Navarro, Javier Castro, Jorge TI Post-fire salvage logging increases restoration costs in a Mediterranean mountain ecosystem SO NEW FORESTS LA English DT Article DE Forest economics; Nurse objects; Post-fire restoration; Salvage logging ID FOREST MANAGEMENT; SEED PREDATION; BARK BEETLES; PINE FORESTS; FIRE; SERVICES; WILDFIRE; CONSERVATION; REGENERATION; RECRUITMENT AB Post-fire salvage logging (i.e. felling and removing burnt trees, often eliminating the remaining woody debris) is a practice routinely performed by forest managers worldwide. In Mediterranean-type ecosystems, salvage logging is considered a measure to reduce future reforestation costs, but this assumption remains largely untested. We made a cost analysis of different management schemes, addressing the immediate post-fire burnt-wood management as well as the costs and success of subsequent reforestation efforts. Two experimental 25-ha plots were established in a burnt pine reforestation of SE Spain, in which three replicates of three post-fire treatments were applied: non-intervention (NI), partial cut plus lopping (PCL; felling and lopping off the branches from most of the trees, leaving all biomass in situ), and salvage logging (SL). After 4 years, a mechanised reforestation was undertaken, and seedling mortality was monitored for 2 years. The cost of all management operations was recorded in situ, and the cost of re-planting the dead seedlings was estimated according to the expenses of previous reforestation. Initial cost of wood management was greatest in SL and zero in NI. Reforestation cost was highest in NI and lowest in SL, and seedling-mortality rates proved lowest in PCL (43 % vs. 51 % and 52 % in SL and NI, respectively). Considering all the post-fire management operations, salvage logging did not provide particular economic advantages for forest restoration, and had an overall cost of 3,436 +/- A 340 a,not sign/ha. By contrast, NI and PCL reduced total restoration costs by 50 and 35 %, respectively, and PCL indeed promoted restoration success. We suggest that the full cost of management operations needs to be considered when evaluating the economic implications of post-fire salvage logging. C1 [Leverkus, Alexandro B.; Castro, Jorge] Univ Granada, Fac Ciencias, Dept Ecol, E-18071 Granada, Spain. [Puerta-Pinero, Carolina] Smithsonian Trop Res Inst, APO AA, Unit 0948, Miami, FL 34002 USA. [Ramon Guzman-Alvarez, Jose] Univ Cordoba, Grp Invest Silvopascicultura, Cordoba, Spain. [Navarro, Javier] Consejeri Medio Ambiente, Sierra Nevada Natl Pk, Granada, Spain. RP Leverkus, AB (reprint author), Univ Granada, Fac Ciencias, Dept Ecol, E-18071 Granada, Spain. EM leverkus@ugr.es RI Puerta Pinero, Carolina/B-3186-2012; Castro, Jorge/M-1509-2014; Leverkus, Alexandro/C-4752-2016 OI Puerta Pinero, Carolina/0000-0002-0584-7548; Castro, Jorge/0000-0002-6362-2240; Leverkus, Alexandro/0000-0001-5452-3614 FU Spanish Ministerio de Ciencia e Innovacion [CGL2008-01671]; Organismo Autonomo de Parques Nacionales [10/2005]; Spanish Ministerio de Educacion, Cultura y Deporte [EX2009-0703, AP2010-0272] FX We thank the Consejeria de Medio Ambiente, Junta de Andalucia, and the Direction of the Natural and National Park of Sierra Nevada for fieldwork permission, treatment implementation, and facilities. We thank Francisco Vilchez Alvarez and Ernesto Punzano Nieto (Andalusian Water and Environment Agency) for cost data provision. Angela Sanchez Miranda and Carlos Serrano Hermo provided invaluable fieldwork. This study was supported by Project CGL2008-01671 from the Spanish Ministerio de Ciencia e Innovacion and Project 10/2005 from the Organismo Autonomo de Parques Nacionales. CP-P had a postdoctoral fellowship (EX2009-0703) and AL had a Ph. D. grant from the Spanish Ministerio de Educacion, Cultura y Deporte (Ref: AP2010-0272). NR 52 TC 9 Z9 9 U1 4 U2 35 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-4286 J9 NEW FOREST JI New For. PD SEP PY 2012 VL 43 IS 5-6 SI SI BP 601 EP 613 DI 10.1007/s11056-012-9327-7 PG 13 WC Forestry SC Forestry GA 992YY UT WOS:000307819000005 ER PT J AU Krayesky, DM Norris, JN West, JA Kamiya, M Viguerie, M Wysor, BS Fredericq, S AF Krayesky, David M. Norris, James N. West, John A. Kamiya, Mitsunobu Viguerie, Matt Wysor, Brian S. Fredericq, Suzanne TI Two new species of Caloglossa (Delesseriaceae, Rhodophyta) from the Americas, C. confusa and C. fluviatilis spp. nov. SO PHYCOLOGIA LA English DT Article DE Atlantic Ocean; Caloglossa; Ceramiales; Delesseriaceae; LSU rDNA; Pacific Ocean; Panama Canal; rbcL; Rhodophyta; Systematics ID LEPRIEURII COMPLEX DELESSERIACEAE; CONTINUA DELESSERIACEAE; MORPHOLOGICAL EVIDENCE; PACIFIC MEXICO; RED ALGAE; CERAMIALES; MONOSTICHA; GUATEMALA; SEQUENCES; RDNA AB Although the systematics of Caloglossa has been intensely investigated, the species diversity of the genus is not yet fully understood. Comparative chloroplast-encoded rbcL and nuclear LSU rDNA sequence analyses, combined with morphological observations, reveal new records and two new species for the Americas. The species, previously identified as Caloglossa monosticha from the western Atlantic, is newly described as C confusa sp. nov. It differs from Pacific Ocean C monosticha primarily by its strongly constricted thallus nodes, and the sequence data presented here show that it is most closely allied with other taxa of the C. continua species complex, but its relationship with these taxa is not fully resolved. The freshwater C. fluviatilis sp. nov. from the Panama Canal is characterised by thalli arranged in tufts, adventitious branching, strong constrictions at the thallus nodes and lanceolate blades. Caloglossa fluviatilis forms a monophyletic group along with the species having only adventitious secondary branching. A dichotomous key highlights the diagnostic vegetative characters for separating the nine species of Caloglossa occurring in the Americas. C1 [Krayesky, David M.] Slippery Rock Univ, Dept Biol, Slippery Rock, PA 16057 USA. [Norris, James N.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. [West, John A.] Univ Melbourne, Sch Bot, Parkville, Vic 3010, Australia. [Kamiya, Mitsunobu] Fukui Prefectural Univ, Dept Marine Biosci, Obama, Fukui 9170003, Japan. [Viguerie, Matt; Fredericq, Suzanne] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Wysor, Brian S.] Roger Williams Univ, Dept Biol & Marine Biol, Bristol, RI 02809 USA. RP Krayesky, DM (reprint author), Slippery Rock Univ, Dept Biol, Slippery Rock, PA 16057 USA. EM david.krayesky@sru.edu FU National Science Foundation [DEB PEET 0328491, DEB 091905, DEB 0936216, OISE 0819205] FX The National Science Foundation Grants DEB PEET 0328491, DEB 091905, DEB 0936216 and OISE 0819205 who supported parts of this study. We would like to thank all collectors cited in Table I and National Museum of Natural History (US) for sending material used in this study. In addition, we would also like to thank Giuseppe C. Zuccarello, Craig, W. Schneider and Jerry G. Chmielewski for their helpful remarks on this manuscript. NR 34 TC 3 Z9 4 U1 0 U2 11 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD SEP PY 2012 VL 51 IS 5 BP 513 EP 530 DI 10.2216/11-57.1 PG 18 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 004LI UT WOS:000308682800004 ER PT J AU Golombek, M Grant, J Kipp, D Vasavada, A Kirk, R Fergason, R Bellutta, P Calef, F Larsen, K Katayama, Y Huertas, A Beyer, R Chen, A Parker, T Pollard, B Lee, S Sun, Y Hoover, R Sladek, H Grotzinger, J Welch, R Dobrea, EN Michalski, J Watkins, M AF Golombek, M. Grant, J. Kipp, D. Vasavada, A. Kirk, R. Fergason, R. Bellutta, P. Calef, F. Larsen, K. Katayama, Y. Huertas, A. Beyer, R. Chen, A. Parker, T. Pollard, B. Lee, S. Sun, Y. Hoover, R. Sladek, H. Grotzinger, J. Welch, R. Dobrea, E. Noe Michalski, J. Watkins, M. TI Selection of the Mars Science Laboratory Landing Site SO SPACE SCIENCE REVIEWS LA English DT Review DE Landing sites; Mars; Surface materials; Surface characteristics; Mars Science Laboratory ID THERMAL EMISSION SPECTROMETER; ORBITER LASER ALTIMETER; SIZE-FREQUENCY DISTRIBUTIONS; MAWRTH-VALLIS REGION; REMOTE-SENSING DATA; GALE-CRATER; PHYSICAL-PROPERTIES; EXPLORATION ROVERS; MELAS-CHASMA; LAYERED DEPOSITS AB The selection of Gale crater as the Mars Science Laboratory landing site took over five years, involved broad participation of the science community via five open workshops, and narrowed an initial > 50 sites (25 by 20 km) to four finalists (Eberswalde, Gale, Holden and Mawrth) based on science and safety. Engineering constraints important to the selection included: (1) latitude (+/- 30A degrees) for thermal management of the rover and instruments, (2) elevation (<-1 km) for sufficient atmosphere to slow the spacecraft, (3) relief of < 100-130 m at baselines of 1-1000 m for control authority and sufficient fuel during powered descent, (4) slopes of < 30A degrees at baselines of 2-5 m for rover stability at touchdown, (5) moderate rock abundance to avoid impacting the belly pan during touchdown, and (6) a radar-reflective, load-bearing, and trafficable surface that is safe for landing and roving and not dominated by fine-grained dust. Science criteria important for the selection include the ability to assess past habitable environments, which include diversity, context, and biosignature (including organics) preservation. Sites were evaluated in detail using targeted data from instruments on all active orbiters, and especially Mars Reconnaissance Orbiter. All of the final four sites have layered sedimentary rocks with spectral evidence for phyllosilicates that clearly address the science objectives of the mission. Sophisticated entry, descent and landing simulations that include detailed information on all of the engineering constraints indicate all of the final four sites are safe for landing. Evaluation of the traversabilty of the landing sites and target "go to" areas outside of the ellipse using slope and material properties information indicates that all are trafficable and "go to" sites can be accessed within the lifetime of the mission. In the final selection, Gale crater was favored over Eberswalde based on its greater diversity and potential habitability. C1 [Golombek, M.; Kipp, D.; Vasavada, A.; Bellutta, P.; Calef, F.; Katayama, Y.; Huertas, A.; Chen, A.; Parker, T.; Pollard, B.; Lee, S.; Sun, Y.; Hoover, R.; Sladek, H.; Welch, R.; Dobrea, E. Noe; Michalski, J.; Watkins, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Grant, J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. [Kirk, R.; Fergason, R.] US Geol Survey, Flagstaff, AZ 86001 USA. [Larsen, K.] Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA. [Katayama, Y.] Japan Aerosp Explorat Agcy, Lunar & Planetary Explorat Program Grp, Tokyo, Japan. [Beyer, R.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Sun, Y.; Grotzinger, J.] CALTECH, Pasadena, CA 91125 USA. [Hoover, R.] Univ Colorado, Boulder, CO 80309 USA. [Sladek, H.] Univ Montana Western, Dillon, MT 59725 USA. [Dobrea, E. Noe; Michalski, J.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Golombek, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mgolombek@jpl.nasa.gov OI Beyer, Ross/0000-0003-4503-3335 FU Mars Data Analysis Program; Critical Data Products program FX Research described in this paper was partially done by the MSL project, Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration and was supported by the Mars Data Analysis Program. Derived data products were sponsored by the Critical Data Products program administered by the JPL Mars Exploration Program office. We especially thank members of the Council of Atmospheres and Council of Terrains for work on characterizing MSL landing sites. We thank L. Redmond and N. Warner for help with the figures. NR 201 TC 55 Z9 58 U1 5 U2 45 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PD SEP PY 2012 VL 170 IS 1-4 BP 641 EP 737 DI 10.1007/s11214-012-9916-y PG 97 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 008JF UT WOS:000308952500017 ER PT J AU Frazier, J Ishihara-Brito, R AF Frazier, Jack Ishihara-Brito, Reiko TI The occurrence of tortoiseshell on a pre-Hispanic Maya mosaic mask SO ANTIQUITY LA English DT Article DE Mesoamerica; Maya; K'inich Ajaw; Postclassic; thirteenth-fourteenth century AD; marine turtle; tortoiseshell; mask; sea symbolism; taphonomy; keratin ID SPECTROSCOPY AB The Dumbarton Oaks Maya mosaic mask is shown to have included tortoiseshell on an earlobe-remarkable since this is the only demonstrated use of this material in pre-Hispanic Mesoamerica. The authors present diagnostic evidence for the presence of tortoiseshell, account for its absence in pre-Hispanic artefacts because of decay, and propose its use (in the mask) as being symbolic of the ocean. C1 [Frazier, Jack] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool Amphibians & Reptiles, Washington, DC 20013 USA. [Ishihara-Brito, Reiko] Dumbarton Oaks Res Lib & Collect, Washington, DC 20007 USA. RP Frazier, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool Amphibians & Reptiles, POB 37012, Washington, DC 20013 USA. EM kurma@shentel.net; reikoish@gmail.com NR 82 TC 0 Z9 0 U1 0 U2 5 PU ANTIQUITY PI YORK PA KINGS MANOR, YORK YO1 7EP, ENGLAND SN 0003-598X J9 ANTIQUITY JI Antiquity PD SEP PY 2012 VL 86 IS 333 BP 825 EP 837 PG 13 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 002EN UT WOS:000308514600016 ER PT J AU Hetzinger, S Halfar, J Mecking, JV Keenlyside, NS Kronz, A Steneck, RS Adey, WH Lebednik, PA AF Hetzinger, S. Halfar, J. Mecking, J. V. Keenlyside, N. S. Kronz, A. Steneck, R. S. Adey, W. H. Lebednik, P. A. TI Marine proxy evidence linking decadal North Pacific and Atlantic climate SO CLIMATE DYNAMICS LA English DT Article DE Aleutian Low; North Atlantic Oscillation; North Pacific; Atlantic Multidecadal Variability; Mg/Ca; Coralline algae ID BERING-SEA; INTERDECADAL VARIABILITY; GEOPOTENTIAL HEIGHT; ELECTRON-MICROPROBE; OSCILLATION; TEMPERATURE; OCEAN; 20TH-CENTURY; LINKAGES; IMPACTS AB Decadal- to multidecadal variability in the extra-tropical North Pacific is evident in 20th century instrumental records and has significant impacts on Northern Hemisphere climate and marine ecosystems. Several studies have discussed a potential linkage between North Pacific and Atlantic climate on various time scales. On decadal time scales no relationship could be confirmed, potentially due to sparse instrumental observations before 1950. Proxy data are limited and no multi-centennial high-resolution marine geochemical proxy records are available from the subarctic North Pacific. Here we present an annually-resolved record (1818-1967) of Mg/Ca variations from a North Pacific/Bering Sea coralline alga that extends our knowledge in this region beyond available data. It shows for the first time a statistically significant link between decadal fluctuations in sea-level pressure in the North Pacific and North Atlantic. The record is a lagged proxy for decadal-scale variations of the Aleutian Low. It is significantly related to regional sea surface temperature and the North Atlantic Oscillation (NAO) index in late boreal winter on these time scales. Our data show that on decadal time scales a weaker Aleutian Low precedes a negative NAO by several years. This atmospheric link can explain the coherence of decadal North Pacific and Atlantic Multidecadal Variability, as suggested by earlier studies using climate models and limited instrumental data. C1 [Hetzinger, S.; Halfar, J.] Univ Toronto, CPS Dept, Mississauga, ON L5L 1C6, Canada. [Hetzinger, S.] Leibniz Inst Marine Sci, IFM GEOMAR, D-24148 Kiel, Germany. [Mecking, J. V.; Keenlyside, N. S.] Leibniz Inst Marine Sci, IFM GEOMAR, D-24105 Kiel, Germany. [Mecking, J. V.; Keenlyside, N. S.] Univ Bergen, Inst Geophys, Bergen, Norway. [Mecking, J. V.; Keenlyside, N. S.] Univ Bergen, Bjerknes Ctr Climate Res, Bergen, Norway. [Kronz, A.] Univ Gottingen, Geowissensch Zentrum, D-37077 Gottingen, Germany. [Steneck, R. S.] Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. [Adey, W. H.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. [Lebednik, P. A.] ARCADIS US Inc, Walnut Creek, CA 94596 USA. RP Hetzinger, S (reprint author), Univ Toronto, CPS Dept, 3359 Mississauga Rd N, Mississauga, ON L5L 1C6, Canada. EM shetzinger@ifm-geomar.de RI Keenlyside, Noel/E-8303-2013; Halfar, Jochen/C-7317-2014; Hetzinger, Steffen/B-5778-2016 OI Keenlyside, Noel/0000-0002-8708-6868; FU Alexander von Humboldt Foundation; Deutsche Forschungsgemeinschaft [HA 3238/2-1. 2-2, KE 1471/2-1]; Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation and Research; Ontario Research Fund FX We thank B. Williams, R. Greatbatch, and M. Latif for discussion and helpful comments. This research was funded by the Alexander von Humboldt Foundation (Feodor Lynen Fellowship to S. H.), the Deutsche Forschungsgemeinschaft (grant HA 3238/2-1. 2-2 to J. H. and A. K.; and Emmy Noether grant KE 1471/2-1 to N. S. K and J. V. M), a Natural Sciences and Engineering Research Council of Canada Discovery Grant and a Canadian Foundation for Innovation and Research and Ontario Research Fund Grant (all J. H.). Two anonymous reviewers are thanked for their valuable comments that greatly improved this manuscript. NR 38 TC 12 Z9 12 U1 3 U2 29 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0930-7575 EI 1432-0894 J9 CLIM DYNAM JI Clim. Dyn. PD SEP PY 2012 VL 39 IS 6 BP 1447 EP 1455 DI 10.1007/s00382-011-1229-4 PG 9 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 005AO UT WOS:000308722900014 ER PT J AU Deichmann, JL Toft, CA Deichmann, PM Lima, AP Williamson, GB AF Deichmann, Jessica L. Toft, Catherine A. Deichmann, Peter M. Lima, Albertina P. Bruce Williamson, G. TI Neotropical primary productivity affects biomass of the leaf-litter herpetofaunal assemblage SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Amazonia; amphibians; biomass; geomorphology; lizards; primary productivity; species richness ID FOREST; FROGS; ECOLOGY; HISTORY; AMAZON; PANAMA; SITES; SOILS AB Soil fertility and plant productivity are known to vary across the Amazon Basin partially as a function of geomorphology and age of soils. Using data on herpetofaunal abundance collected from 5 x 5 m and 6 x 6 m plots in mature tropical forests, we tested whether variation in community biomass of litter frogs and lizards across ten Neotropical sites could be explained by cation exchange capacity. primary productivity or stem turnover rate. About half of the variation in frog biomass (48%) could be attributed to stem turnover rate, while over two-thirds of the variation in lizard biomass (69%) was explained by primary productivity. Biomass variation in frogs resulted from variation in abundance and size, and abundance was related to cation exchange capacity (45% of variation explained), but size was not. Lizard biomass across sites varied mostly with individual lizard size, but not with abundance, and size was highly dependent on primary productivity (85% of variation explained). Soil fertility and plant productivity apparently affect secondary consumers like frogs and lizards through food webs, as biomass is transferred from plants to herbivorous arthropods to secondary consumers. C1 [Deichmann, Jessica L.; Bruce Williamson, G.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, AM, Brazil. [Deichmann, Jessica L.; Bruce Williamson, G.] Smithsonian Trop Res Inst, BR-69011970 Manaus, AM, Brazil. [Toft, Catherine A.] Univ Calif Davis, Coll Biol Sci, Dept Ecol & Evolut, Davis, CA 95616 USA. [Deichmann, Peter M.] Mass Audubon, Allens Pond Wildlife Sanctuary, Westport, MA 02790 USA. [Lima, Albertina P.] Inst Nacl de Pesquisas da Amazonia, BR-69060001 Manaus, AM, Brazil. [Deichmann, Jessica L.; Bruce Williamson, G.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Deichmann, JL (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk,POB 37012,MRC 705, Washington, DC 20013 USA. EM jessiedeichmann@gmail.com FU Conservation, Food and Health Foundation; Louisiana Governor's Office of Environmental Education; Louisiana State University Biograds; US National Science Foundation [DEB-0639144, DEB-1147434] FX We thank the staff at all of our field sites, particularly P. Gaucher at Nouragues. K. Swing, D. Romo and C. Barriga de Romo at Tiputini, L. Baldeon at Yasuni and R. Hipolito at the BDFFP for their help with logistics. We are grateful to S. Whitfield for allowing access to herpetofauna data from La Selva. We also thank M. Rodriguez, A. Enomenga. I. Nenquimo, H. Ahua and J. Fragata for assistance in the field. This work was supported by grants from the Conservation, Food and Health Foundation, Louisiana Governor's Office of Environmental Education, the Louisiana State University Biograds, and the US National Science Foundation (DEB-0639144 and DEB-1147434). Herpetofauna sampling procedures were approved by Louisiana State University Animal Care and Use Committee (Protocol 04-132). Fieldwork was conducted in Ecuador with permission of the Ministerio del Ambiente (004-IC-FA-PNY-RSO) and in Brazil with permits from CNPq (EXC 006-06-C) and MAMA (no 222/2006). This is publication #600 in the Technical Series of the Biological Dynamics of Forest Fragments Project (INPA-STRI). NR 29 TC 2 Z9 2 U1 3 U2 27 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD SEP PY 2012 VL 28 BP 427 EP 435 DI 10.1017/S0266467412000430 PN 5 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 006RY UT WOS:000308837700001 ER PT J AU Pravosudov, VV Roth, TC Forister, ML Ladage, LD Burg, TM Braun, MJ Davidson, BS AF Pravosudov, V. V. Roth, T. C., II Forister, M. L. Ladage, L. D. Burg, T. M. Braun, M. J. Davidson, B. S. TI Population genetic structure and its implications for adaptive variation in memory and the hippocampus on a continental scale in food-caching black-capped chickadees SO MOLECULAR ECOLOGY LA English DT Article DE adaptation; chickadee; food caching; gene flow; hippocampus; memory; population structure ID MULTILOCUS GENOTYPE DATA; ENVIRONMENTAL HARSHNESS; STORING BIRDS; AFLP MARKERS; SOFTWARE; SPECIALIZATION; INFERENCE; GRADIENT; ECOLOGY; LENGTH AB Food-caching birds rely on stored food to survive the winter, and spatial memory has been shown to be critical in successful cache recovery. Both spatial memory and the hippocampus, an area of the brain involved in spatial memory, exhibit significant geographic variation linked to climate-based environmental harshness and the potential reliance on food caches for survival. Such geographic variation has been suggested to have a heritable basis associated with differential selection. Here, we ask whether population genetic differentiation and potential isolation among multiple populations of food-caching black-capped chickadees is associated with differences in memory and hippocampal morphology by exploring population genetic structure within and among groups of populations that are divergent to different degrees in hippocampal morphology. Using mitochondrial DNA and 583 AFLP loci, we found that population divergence in hippocampal morphology is not significantly associated with neutral genetic divergence or geographic distance, but instead is significantly associated with differences in winter climate. These results are consistent with variation in a history of natural selection on memory and hippocampal morphology that creates and maintains differences in these traits regardless of population genetic structure and likely associated gene flow. C1 [Pravosudov, V. V.; Roth, T. C., II; Forister, M. L.; Ladage, L. D.] Univ Nevada, Dept Biol, Reno, NV 89557 USA. [Roth, T. C., II] Kenyon Coll, Dept Biol, Gambier, OH 43022 USA. [Burg, T. M.] Univ Lethbridge, Dept Biol Sci, Lethbridge, AB T1K 3M4, Canada. [Braun, M. J.; Davidson, B. S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Pravosudov, VV (reprint author), Univ Nevada, Dept Biol, M5314, Reno, NV 89557 USA. EM vpravosu@unr.edu FU NSF [IOB-0615021, IOB-0918268]; NSERC DG FX The project was partially funded by NSF IOB-0615021 to VVP and NSF IOB-0918268 to LDA and VVP. Work was approved by the University of Nevada IACUC #A05/06-35 and followed all federal and local guidelines for the use of animals in research. We thank Ken Otter and Angelique Grava for samples from UNBC. TMB would like to thank John Hindley and Linda Lait for assistance in the laboratory, and Heather Bird, Karley Campbell, Brendan Graham, John Hindley, Elysha Koran, Linda Lait, Christine Michell and Paulo Pulgarin for the field work obtaining samples. TMB was funded by NSERC DG. NR 33 TC 10 Z9 10 U1 1 U2 34 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 SEP PY 2012 VL 21 IS 18 BP 4486 EP 4497 DI 10.1111/j.1365-294X.2012.05721.x PG 12 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 003TN UT WOS:000308634300008 PM 22882305 ER PT J AU Needell, AA AF Needell, Allan A. TI Science-Mart: Privatizing American Science SO REVIEWS IN AMERICAN HISTORY LA English DT Book Review C1 [Needell, Allan A.] Smithsonian Inst, Space Hist Div, Washington, DC 20560 USA. RP Needell, AA (reprint author), Smithsonian Inst, Space Hist Div, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0048-7511 J9 REV AM HIST JI Rev. Am. Hist. PD SEP PY 2012 VL 40 IS 3 BP 512 EP 517 PG 6 WC History SC History GA 009OR UT WOS:000309035600036 ER PT J AU Zecchini, F Vecchione, M Belcari, P Roper, CFE AF Zecchini, Fulvio Vecchione, Michael Belcari, Paola Roper, Clyde F. E. TI Development of the hectocotylus in Illex coindetii (Verany, 1837) (Cephalopoda: Ommastrephidae) SO SCIENTIA MARINA LA English DT Article DE squid; development; maturity; arm modification; identification; taxonomic character ID SQUID AB Species of the genus Illex (Family Ommastrephidae) are distinguished morphologically mainly based on differences in the hectocotylus, the modified arm that males of many cephalopod species use to transfer spermatophores to females during mating We examined the developmental details of the hectocotylus in Illex coindetii, the species of Illex with the most highly modified hectocotylized arm, to determine whether it has an ontogeny that passes through stages that are similar to the less modified hectocotyli of sympatric I. illecebrosus and I. oxygonius The development of modifications of one of the ventral arms is essentially synchronous on all portions. The hectocotylus of I. coindetii is therefore morphologically distinctive even at early maturity stages, and therefore should not be easily confused with that of its sympatric congeners. C1 [Zecchini, Fulvio] Consorzio Interuniv Nazl Chim Ambiente, Venezia Marghera, Italy. [Vecchione, Michael] Natl Museum Nat Hist, Natl Marine Fisheries Serv, Systemat Lab, Washington, DC 20013 USA. [Belcari, Paola] Dipartimento Sci Uomo & Ambiente, I-56126 Pisa, Italy. [Belcari, Paola] UCL, Dept Phys & Astron, London, England. [Roper, Clyde F. E.] Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. RP Zecchini, F (reprint author), Consorzio Interuniv Nazl Chim Ambiente, Venezia Marghera, Italy. EM vecchiom@si.edu NR 24 TC 3 Z9 3 U1 2 U2 8 PU INST CIENCIAS MAR BARCELONA PI BARCELONA PA PG MARITIM DE LA BARCELONETA, 37-49, 08003 BARCELONA, SPAIN SN 0214-8358 J9 SCI MAR JI Sci. Mar. PD SEP PY 2012 VL 76 IS 3 BP 463 EP 472 DI 10.3989/scimar.03305.07D PG 10 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 010RQ UT WOS:000309112200006 ER PT J AU Rick, TC Wah, JS Erlandson, JM AF Rick, Torben C. Wah, John S. Erlandson, Jon M. TI Re-evaluating the origins of late Pleistocene fire areas on Santa Rosa Island, California, USA SO QUATERNARY RESEARCH LA English DT Article DE Fire history; Anthropogenic burning; X-ray diffraction; Soils; Macrobotanical remains; Charcoal; Smectite ID NORTHERN CHANNEL-ISLANDS; DAISY CAVE CA-SMI-261; X-RAY-DIFFRACTION; ENVIRONMENTAL-CHANGE; SOUTHERN CALIFORNIA; MIGUEL ISLAND; IRON-OXIDES; FOREST-FIRE; SOIL; TEMPERATURE AB At the close of the Pleistocene, fire regimes in North America changed significantly in response to climate change, megafaunal extinctions, anthropogenic burning and, possibly, even an extraterrestrial impact. On California's Channel Islands, researchers have long debated the nature of late Pleistocene "fire areas," discrete red zones in sedimentary deposits, interpreted by some as prehistoric mammoth-roasting pits created by humans. Further research found no evidence that these red zones were cultural in origin, and two hypotheses were advanced to explain their origin: natural fires and groundwater processes. Radiocarbon dating, X-ray diffraction analysis, and identification of charcoal from six red zones on Santa Rosa Island suggest that the studied features date between similar to 27,500 and 11,400 cal yr BP and resulted from burning or heating, not from groundwater processes. Our results show that fire was a component of late Pleistocene Channel Island ecology prior to and after human colonization of the islands, with no clear evidence for increased fire frequency coincident with Paleoindian settlement, extinction of pygmy mammoths, or a proposed Younger Dryas impact event. Published by Elsevier Inc. on behalf of University of Washington. C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Wah, John S.] Matapeake Soil & Environm Consultants, Shippensburg, PA 17257 USA. [Erlandson, Jon M.] Univ Oregon, Dept Anthropol, Eugene, OR 97403 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 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 OI Erlandson, Jon/0000-0002-4705-4319 FU NSF grant [BCS 0917677]; University of Oregon; Smithsonian Institution FX This research was supported by NSF grant BCS 0917677 awarded to Erlandson and Rick, with additional funding from the University of Oregon and the Smithsonian Institution. Ann Huston, Kelly Minas, and Mark Senning facilitated our research conducted under ARPA permit PWR-1979-09-CA-04. We are also grateful to Todd Braje, Tracy Garcia, Nick Jew, Paula Pugh, Quintan Shup, Leslie Reeder, and Lauren Willis for help in the field, K. Puseman and Linda Scott-Cummings of PaleoResearch, Brendan Culleton and Doug Kennett for preliminary processing of several 14C samples, and Dr. Martin Rabenhorst and the University of Maryland Pedology Lab. Finally, we thank Drs. Scott Anderson, Alan Gillespie, Dan Muhs, and Jeff Pigati for comments that greatly improved this manuscript. NR 66 TC 2 Z9 2 U1 1 U2 26 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0033-5894 J9 QUATERNARY RES JI Quat. Res. PD SEP PY 2012 VL 78 IS 2 BP 353 EP 362 DI 10.1016/j.yqres.2012.06.006 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 002EY UT WOS:000308516000021 ER PT J AU Yoon, J Sillett, TS Morrison, SA Ghalambor, CK AF Yoon, Jongmin Sillett, T. Scott Morrison, Scott A. Ghalambor, Cameron K. TI Breeding density, not life history, predicts interpopulation differences in territorial aggression in a passerine bird SO ANIMAL BEHAVIOUR LA English DT Article DE breeding density; dear enemy; individual recognition; life history; male aggression; nasty neighbour; simulated territorial intrusion ID DEAR-ENEMY PHENOMENON; MIGRATORY SONGBIRD; ASYMMETRIC WAR; CLUTCH SIZE; TRADE-OFFS; NEIGHBORS; BEHAVIOR; TESTOSTERONE; HYPOTHESIS; EVOLUTION AB Interpopulation variation in territorial aggression can reflect differences in life history or competitive environments. Life history theory predicts that males with more opportunities for future reproduction should avoid risk-taking behaviour to minimize the cost of current reproduction, whereas competitive environments should favour higher aggression to defend limited resources. Additionally, male aggression can be modulated by familiarity with competitors to be either lower (dear enemies) or higher (nasty neighbours) towards neighbours. We conducted a territory intrusion experiment using neighbour-stranger songs to examine how territorial aggression differed in two populations of orange-crowned warblers, Oreothlypis celata, breeding in California and Alaska. The California population breeds at very high densities and has a higher annual survival relative to the Alaska population, which breeds at significantly lower densities and has a lower annual survival rate. We found that California males showed higher amounts of territorial aggression in response to simulated territory intrusions than did Alaska males, supporting the hypothesis that competitive environments, as indicated by breeding density, rather than life history, shape geographical variation in levels of aggression. Both populations discriminated between song stimuli of neighbours and strangers, but California males responded more strongly towards neighbours, whereas Alaska males responded more strongly towards strangers. We discuss these results in light of the mechanisms for overall aggression and neighbour-stranger discrimination. (c) 2012 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Yoon, Jongmin; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Yoon, Jongmin; Ghalambor, Cameron K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC USA. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA USA. RP Ghalambor, CK (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM cameron.ghalambor@colostate.edu FU The Nature Conservancy; Smithsonian Institution; Colorado State University FX Our research was supported by The Nature Conservancy, the Smithsonian Institution and Colorado State University. We thank the many field technicians who assisted with data collection, especially J. Coumoutso, H. Montag and L. Caldwell, and The Catalina Island Conservancy for providing logistical support. This study was improved by the advice and comments of L. Angeloni, P. Doherty, K. Langin and H. Sofaer. NR 59 TC 13 Z9 13 U1 3 U2 62 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 SEP PY 2012 VL 84 IS 3 BP 515 EP 521 DI 10.1016/j.anbehav.2012.05.024 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 996VU UT WOS:000308123700005 ER PT J AU Cheung, CC Stawarz, L Siemiginowska, A Gobeille, D Wardle, JFC Harris, DE Schwartz, DA AF Cheung, C. C. Stawarz, L. Siemiginowska, A. Gobeille, D. Wardle, J. F. C. Harris, D. E. Schwartz, D. A. TI DISCOVERY OF A KILOPARSEC-SCALE X-RAY/RADIO JET IN THE z=4.72 QUASAR GB 1428+4217 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (GB 1428+4217); radiation mechanisms: non-thermal; radio continuum: galaxies; X-rays: galaxies ID RAY-EMISSION; HIGH-REDSHIFT; RADIO GALAXIES; BLAZAR; CHANDRA; LOBES AB We report the discovery of a one-sided 3.'' 6 (24 kpc, projected) long jet in the high-redshift, z = 4.72, quasar GB 1428+4217 in new Chandra X-ray and Very Large Array (VLA) radio observations. This is the highest redshift kiloparsec-scale X-ray/radio jet known. Analysis of archival very long baseline interferometry 2.3 and 8.6 GHz data reveal a faint one-sided jet extending out to similar to 200 pc and aligned to within similar to 30 degrees of the Chandra/VLA emission. The 3.'' 6 distant knot is not detected in an archival Hubble Space Telescope image, and its broadband spectral energy distribution is consistent with an origin from inverse Compton scattering of cosmic microwave background photons for the X-rays. Assuming also equipartition between the radiating particles and magnetic field, the implied jet Lorentz factor is approximate to 5. This is similar to the other two known z similar to 4 kpc scale X-ray jet cases and smaller than typically inferred in lower-redshift cases. Although there are still but a few such very high redshift quasar X-ray jets known, for an inverse Compton origin, the present data suggest that they are less relativistic on large scales than their lower-redshift counterparts. C1 [Cheung, C. C.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Stawarz, L.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Siemiginowska, A.; Harris, D. E.; Schwartz, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gobeille, D.; Wardle, J. F. C.] Brandeis Univ, Dept Phys, Waltham, MA 02454 USA. [Gobeille, D.] Univ S Florida, Dept Phys, Tampa, FL 33620 USA. RP Cheung, CC (reprint author), USN, Res Lab, Washington, DC 20375 USA. EM Teddy.Cheung.ctr@nrl.navy.mil FU NASA [NAS8-39073, GO7-8114]; Chandra X-Ray Observatory Center; NSF [NSF1009261]; NRAO; NASA DPR [S-15633-Y] FX This research was supported in part by NASA through contract NAS8-39073 (A. S., D. E. H., and D. A. S.) and Chandra Award number GO7-8114 issued to NRAO and Eureka Scientific (C. C. C.) and Brandeis University (D. G. and J.F.C.W.) by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-39073. Radio astronomy at Brandeis University is supported by NSF Grant NSF1009261. This work began while C. C. C. was supported by a Jansky fellowship from NRAO; his work at NRL is supported in part by NASA DPR S-15633-Y. NR 28 TC 5 Z9 5 U1 0 U2 2 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 SEP 1 PY 2012 VL 756 IS 1 AR L20 DI 10.1088/2041-8205/756/1/L20 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996HF UT WOS:000308074800020 ER PT J AU Espada, D Matsushita, S Peck, AB Henkel, C Israel, F Iono, D AF Espada, D. Matsushita, S. Peck, A. B. Henkel, C. Israel, F. Iono, D. TI DISENTANGLING THE CIRCUMNUCLEAR ENVIRONS OF CENTAURUS A: GASEOUS SPIRAL ARMS IN A GIANT ELLIPTICAL GALAXY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: individual (NGC 5128); galaxies: ISM; galaxies: structure ID NGC 5128 CENTAURUS; MOLECULAR GAS; DISC GALAXIES; WARPED DISK; KINEMATICS; LINE AB We report the existence of spiral arms in the recently formed gaseous and dusty disk of the closest giant elliptical, NGC 5128 (Centaurus A), using high-resolution (CO)-C-12(2-1) observations of the central 3' (3 kpc) obtained with the Submillimeter Array. This provides evidence that spiral-like features can develop within ellipticals if enough cold gas exists. We elucidate the distribution and kinematics of the molecular gas in this region with a resolution of 4.'' 4 x 1.'' 9 (80 pc x 40 pc). The spiral arms extend from the circumnuclear gas at a radius of 200 pc to at least 1 kpc. The general properties of the arms are similar to those in spiral galaxies: they are trailing, the width is similar to 500 +/- 200 pc, and the pitch angle is 20 degrees. From independent estimates of the time when the Hi-rich galaxy merger occurred, we infer that the formation of spiral arms happened on a timescale of less than similar to 10(8) yr. The formation of spiral arms increases the gas density and thus the star formation efficiency in the early stages of the formation of a disk. C1 [Espada, D.] Natl Astron Observ Japan NAOJ, Mitaka, Tokyo 1818588, Japan. [Espada, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Espada, D.; Matsushita, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Matsushita, S.; Peck, A. B.] Joint ALMA Observ, Santiago, Chile. [Peck, A. B.] NRAO, Charlottesville, VA 22903 USA. [Henkel, C.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Henkel, C.] King Abdulaziz Univ, Dept Astron, Jeddah 21413, Saudi Arabia. [Israel, F.] Leiden Univ, Sterrewach Leiden, NL-2333 CA Leiden, Netherlands. [Iono, D.] NAOJ, Nobeyama Radio Observ, Minamisa Ku, Minamimaki, Nagano 3841305, Japan. RP Espada, D (reprint author), Natl Astron Observ Japan NAOJ, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. EM daniel.espada@nao.ac.jp FU Marie Curie International Fellowship within the 6th European Community Framework Programme FX We thank the referee for useful comments that improved the focus of this Letter. This research has made use of NASA's Astrophysics Data System Bibliographic Services, and 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. This research was partially supported by a Marie Curie International Fellowship within the 6th European Community Framework Programme. NR 32 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2012 VL 756 IS 1 AR L10 DI 10.1088/2041-8205/756/1/L10 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996HF UT WOS:000308074800010 ER PT J AU Gupta, A Mathur, S Krongold, Y Nicastro, F Galeazzi, M AF Gupta, A. Mathur, S. Krongold, Y. Nicastro, F. Galeazzi, M. TI A HUGE RESERVOIR OF IONIZED GAS AROUND THE MILKY WAY: ACCOUNTING FOR THE MISSING MASS? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; Galaxy: halo; intergalactic medium; quasars: absorption lines; X-rays: galaxies ID X-RAY-ABSORPTION; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; XMM-NEWTON OBSERVATIONS; GALACTIC HALO; LOCAL GROUP; HOT GAS; INTERGALACTIC MEDIUM; DISC GALAXIES; LOW-REDSHIFT; ABUNDANCES AB Most of the baryons from galaxies have been "missing" and several studies have attempted to map the circumgalactic medium (CGM) of galaxies in their quest. We report on X-ray observations made with the Chandra X-Ray Observatory probing the warm-hot phase of the CGM of our Milky Way at about 10(6) K. We detect O VII and O VIII absorption lines at z = 0 in extragalactic sight lines and measure accurate column densities using both K alpha and K beta lines of O VII. We then combine these measurements with the emission measure of the Galactic halo from literature to derive the density and the path length of the CGM. We show that the warm-hot phase of the CGM is massive, extending over a large region around the Milky Way, with a radius of over 100 kpc. The mass content of this phase is over 10 billion solar masses, many times more than that in cooler gas phases and comparable to the total baryonic mass in the disk of the Galaxy. The missing mass of the Galaxy appears to be in this warm-hot gas phase. C1 [Gupta, A.; Mathur, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, F.] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, RM, Italy. [Galeazzi, M.] Univ Miami, Dept Phys, Coral Gables, FL 33124 USA. [Mathur, S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Gupta, A (reprint author), Ohio State Univ, Dept Astron, 174 W 18Th Ave, Columbus, OH 43210 USA. EM agupta@astronomy.ohio-state.edu OI Nicastro, Fabrizio/0000-0002-6896-1364 FU National Aeronautics and Space Administration through Chandra X-ray Observatory Center [TM9-0010X]; National Aeronautics Space Administration [NAS8-03060] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number TM9-0010X 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 36 TC 77 Z9 77 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2012 VL 756 IS 1 AR L8 DI 10.1088/2041-8205/756/1/L8 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996HF UT WOS:000308074800008 ER PT J AU Hernandez, AK Tan, JC Kainulainen, J Caselli, P Butler, MJ Jimenez-Serra, I Fontani, F AF Hernandez, Audra K. Tan, Jonathan C. Kainulainen, Jouni Caselli, Paola Butler, Michael J. Jimenez-Serra, Izaskun Fontani, Francesco TI A VIRIALIZED FILAMENTARY INFRARED DARK CLOUD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; ISM: clouds; stars: formation ID MASSIVE STAR-FORMATION; MOLECULAR CLOUDS; CORES; TURBULENT; CLUSTERS; CLUMPS; RADIO; RING AB The initial conditions of massive star and star cluster formation are expected to be cold, dense, and high column density regions of the interstellar medium, which can reveal themselves via near-, mid-, and even far-infrared absorption as infrared dark clouds (IRDCs). Elucidating the dynamical state of IRDCs thus constrains theoretical models of these complex processes. In particular, it is important to assess whether IRDCs have reached virial equilibrium, where the internal pressure balances that due to the self-gravitating weight of the cloud plus the pressure of the external environmental. We study this question for the filamentary IRDC G035.39-00.33 by deriving mass from combined NIR and MIR extinction maps and velocity dispersion from (CO)-O-18 (1-0) and (2-1) line emission. In contrast to our previous moderately super-virial results based on (CO)-C-13 emission and MIR-only extinction mapping, with improved mass measurements we now find that the filament is consistent with being in virial equilibrium, at least in its central parsec-wide region where similar to 1000 M-circle dot snakes along several parsecs. This equilibrium state does not require large-scale net support or confinement by magnetic fields. C1 [Hernandez, Audra K.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Tan, Jonathan C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Tan, Jonathan C.] Univ Florida, Dept Phys, Gainesville, FL 32611 USA. [Kainulainen, Jouni] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Caselli, Paola] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butler, Michael J.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Jimenez-Serra, Izaskun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fontani, Francesco] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. RP Hernandez, AK (reprint author), Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. EM hernande@astro.wisc.edu OI Fontani, Francesco/0000-0003-0348-3418 FU NSF [AST-0645412]; NASA [ATP09-0094, ADAP10-0110]; HST [HST-GO-112275, HST-GO-12276] FX We thank Bruce Draine and an anonymous referee for helpful comments and discussions that improved the Letter. J.C.T. acknowledges support from NSF CAREER grant AST-0645412, NASA Astrophysics Theory and Fundamental Physics grant ATP09-0094, and NASA Astrophysics Data Analysis Program ADAP10-0110. A. K. H. acknowledges support from HST grants HST-GO-112275 and HST-GO-12276 to Bart Wakker at the University of Wisconsin. Finally, we would like to acknowledge the IRAM facilities and staff. NR 26 TC 17 Z9 17 U1 0 U2 5 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 SEP 1 PY 2012 VL 756 IS 1 AR L13 DI 10.1088/2041-8205/756/1/L13 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996HF UT WOS:000308074800013 ER PT J AU Schindhelm, E France, K Herczeg, GJ Bergin, E Yang, H Brown, A Brown, JM Linsky, JL Valenti, J AF Schindhelm, Eric France, Kevin Herczeg, Gregory J. Bergin, Edwin Yang, Hao Brown, Alexander Brown, Joanna M. Linsky, Jeffrey L. Valenti, Jeff TI Ly alpha DOMINANCE OF THE CLASSICAL T TAURI FAR-ULTRAVIOLET RADIATION FIELD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE protoplanetary disks; stars: pre-main sequence; ultraviolet: planetary systems ID FLUORESCENT H-2 EMISSION; MOLECULAR-HYDROGEN EMISSION; PLANET-FORMING REGION; X-RAY; PROTOPLANETARY DISKS; SPACE-TELESCOPE; MIRA-B; STARS; SPECTRA; EVOLUTION AB Far-ultraviolet (FUV) radiation plays an important role in determining chemical abundances in protoplanetary disks. H I Lyman alpha (Ly alpha) is suspected to be the dominant component of the FUV emission from Classical T Tauri Stars (CTTSs), but is difficult to measure directly due to circumstellar and interstellar H I absorption. To better characterize the intrinsic Ly alpha radiation, we present FUV spectra of 14 CTTSs taken with the Hubble Space Telescope Cosmic Origins Spectrograph and Space Telescope Imaging Spectrograph instruments. H-2 fluorescence, commonly seen in the spectra of CTTSs, is excited by Ly alpha photons, providing an indirect measure of the Ly alpha flux incident upon the warm disk surface. We use observed H-2 progression fluxes to reconstruct the CTTS Ly alpha profiles. The Ly alpha flux correlates with total measured FUV flux, in agreement with an accretion-related source of FUV emission. With a geometry-independent analysis, we confirm that in accreting T Tauri systems Ly alpha radiation dominates the FUV flux (similar to 1150 angstrom -1700 angstrom). In the systems surveyed this one line comprises 70%-90% of the total FUV flux. C1 [Schindhelm, Eric] SW Res Inst, Boulder, CO 80303 USA. [France, Kevin; Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Bergin, Edwin] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Yang, Hao] Cent China Normal Univ, Inst Astrophys, Wuhan 430079, Hubei, Peoples R China. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Linsky, Jeffrey L.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, Jeffrey L.] NIST, Boulder, CO 80309 USA. [Valenti, Jeff] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Schindhelm, E (reprint author), SW Res Inst, 1050 Walnut St,Suite 300, Boulder, CO 80303 USA. EM eric@boulder.swri.edu RI Yang, Hao/F-8396-2014 OI Yang, Hao/0000-0002-9423-2333 FU NASA [NNX08AC146, NAS5-98043] FX E.S. and K. F. thank Brian Wood for input on Ly alpha profile reconstruction. This work was supported by NASA grants NNX08AC146 and NAS5-98043 to the University of Colorado at Boulder (HST programs 11533 and 12036) and made use of data from HST GO programs 8041 and 11616. NR 30 TC 19 Z9 19 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2012 VL 756 IS 1 AR L23 DI 10.1088/2041-8205/756/1/L23 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996HF UT WOS:000308074800023 ER PT J AU Silverman, JM Ganeshalingam, M Cenko, SB Filippenko, AV Li, WD Barth, AJ Carson, DJ Childress, M Clubb, KI Cucchiara, A Graham, ML Marion, GH Nguyen, ML Pei, LY Tucker, BE Vinko, J Wheeler, JC Worseck, G AF Silverman, Jeffrey M. Ganeshalingam, Mohan Cenko, S. Bradley Filippenko, Alexei V. Li, Weidong Barth, Aaron J. Carson, Daniel J. Childress, Michael Clubb, Kelsey I. Cucchiara, Antonino Graham, Melissa L. Marion, G. H. Nguyen, My L. Pei, Liuyi Tucker, Brad E. Vinko, Jozsef Wheeler, J. Craig Worseck, Gabor TI THE VERY YOUNG TYPE Ia SUPERNOVA 2012cg: DISCOVERY AND EARLY-TIME FOLLOW-UP OBSERVATIONS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual: SN 2012cg ID SN 2011FE; TELESCOPE; STAR; SPECTROGRAPH; CONSTRAINTS; REDSHIFT; GALAXIES; SPECTRA AB On 2012 May 17.2 UT, only 1.5 +/- 0.2 days after explosion, we discovered SN 2012cg, a Type Ia supernova (SN Ia) in NGC 4424 (d approximate to 15 Mpc). As a result of the newly modified strategy employed by the Lick Observatory Supernova Search, a sequence of filtered images was obtained starting 161 s after discovery. Utilizing recent models describing the interaction of supernova (SN) ejecta with a companion star, we rule out a similar to 1 M-circle dot companion for half of all viewing angles and a red-giant companion for nearly all orientations. SN 2012cg reached a B-band maximum of 12.09 +/- 0.02 mag on 2012 June 2.0 and took similar to 17.3 days from explosion to reach this, typical for SNe Ia. Our pre-maximum-brightness photometry shows a narrower-than-average B-band light curve for SN 2012cg, though slightly overluminous at maximum brightness and with normal color evolution (including some of the earliest SN Ia filtered photometry ever obtained). Spectral fits to SN 2012cg reveal ions typically found in SNe Ia at early times, with expansion velocities greater than or similar to 14,000 km s(-1) at 2.5 days past explosion. Absorption from C II is detected early, as well as high-velocity components of both Si II lambda 6355 and Ca II. Our last spectrum (13.5 days past explosion) resembles that of the somewhat peculiar SN Ia 1999aa. This suggests that SN 2012cg will have a slower-than-average declining light curve, which may be surprising given the faster-than-average rising light curve. C1 [Silverman, Jeffrey M.; Ganeshalingam, Mohan; Cenko, S. Bradley; Filippenko, Alexei V.; Li, Weidong; Clubb, Kelsey I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Barth, Aaron J.; Carson, Daniel J.; Nguyen, My L.; Pei, Liuyi] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Childress, Michael; Tucker, Brad E.; Worseck, Gabor] Australian Natl Univ, Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Cucchiara, Antonino] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Graham, Melissa L.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Graham, Melissa L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Marion, G. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Vinko, Jozsef; Wheeler, J. Craig] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Silverman, JM (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM jsilverman@astro.berkeley.edu OI Worseck, Gabor/0000-0003-0960-3580; Barth, Aaron/0000-0002-3026-0562 FU NSF [AST-1109801, AST-0908886]; Hungarian grant [OTKA K76816]; Sylvia & Jim Katzman Foundation; Richard & Rhoda Goldman Fund; TABASGO Foundation FX We thank J. Caldwell, J. R. Mould, S. Odewahn, J. X. Prochaska, S. Rostopchin, M. Shetrone, and I. Shivvers for their assistance with some of the observations. We are grateful to the staff at Lick Observatory for their support and are indebted to the benefactors, builders, and partners of the HET and LRS. This work was supported in part by NSF grant AST-1109801 and Hungarian grant OTKA K76816. A.V.F.'s group at UC Berkeley, and KAIT and its ongoing operation, have received financial assistance from the Sylvia & Jim Katzman Foundation, Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the TABASGO Foundation, and NSF grant AST-0908886. NR 37 TC 32 Z9 32 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 SEP 1 PY 2012 VL 756 IS 1 AR L7 DI 10.1088/2041-8205/756/1/L7 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996HF UT WOS:000308074800007 ER PT J AU Moffett, MW AF Moffett, Mark W. TI Supercolonies of billions in an invasive ant: What is a society? SO BEHAVIORAL ECOLOGY LA English DT Review DE Argentine ant; polydomy; recognition system; reproductive isolation; society; speciation; supercolony; unicolonial ID ARGENTINE ANT; LINEPITHEMA-HUMILE; NESTMATE RECOGNITION; COLONY STRUCTURE; SOCIAL INSECTS; INTRASPECIFIC AGGRESSION; CUTICULAR HYDROCARBONS; INDIVIDUAL RECOGNITION; IRIDOMYRMEX-HUMILIS; FORAGING ECOLOGY AB All societies are characterized by the capacity of their members to distinguish one another from outsiders. Ants are among the species that form "anonymous societies": members are not required to tell each other apart as individuals for the group to remain unified. Rather, each society depends on shared cues recognized by all its members. These cues permit societies to reach populations in the low millions in certain ant and termite species, and to grow indefinitely populous, expansive, and possibly long lasting in a few other ant species, which are described as having supercolonies. Anonymous societies are contrasted with "individual recognition societies" such as those of most vertebrates, which are limited to a few individuals by the necessity that the members individually recognize each other. The shared recognition cues of ants provide clear criteria for defining colonies and are what enables a supercolony to remain a single society no matter how large it becomes. I examine the often conflicting ideas about the best studied ant with supercolonies, the Argentine ant (Linepithema humile). Its invasive supercolonies, containing in some cases billions of workers and queens spread over hundreds of square kilometers, can be most parsimoniously understood as single colonies that have had an opportunity to expand across regions of suitable habitat because of a lack of well-matched competitors. This capacity for unrestricted growth is the defining characteristic of supercolonies. There is no evidence that the local patchiness of nests and patterns of worker and food traffic within these wide-ranging populations are so invariant that supercolonies do not exist but instead are collections of numerous independent nest clusters that should be called "colonies." Nor is there evidence for the hypothesis that invasive supercolonies have been able to grow large and successful overseas only as a result of evolving through genetic drift or selection to become fundamentally different from the smaller colonies typical of the species' region of origin around northern Argentina. The most unique feature of the Argentine ant, however, is not that its colonies are anonymous or that they can grow indefinitely large-though the last trait is found only in a few ant species and humans. Rather, it is that Argentine ant colonies do not interbreed. Indeed, the only fighting among Argentine ants occurs along colony borders, which even reproductives seldom, if ever, cross and survive. For this reason, each Argentine ant supercolony acts as virtually a sibling species. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Moffett, MW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, 10th St & Constitut Ave, Washington, DC 20013 USA. EM naturalist@erols.com FU National Geographic Society [EC0312-07] FX National Geographic Society (EC0312-07). NR 84 TC 19 Z9 19 U1 9 U2 81 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 SEP-OCT PY 2012 VL 23 IS 5 BP 925 EP 933 DI 10.1093/beheco/ars043 PG 9 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 998HL UT WOS:000308228200001 ER PT J AU Moffett, MW AF Moffett, Mark W. TI Supercolonies, nests, and societies: distinguishing the forests from the trees SO BEHAVIORAL ECOLOGY LA English DT Editorial Material DE Argentine ant; Linepithema humile; kin selection; polydomous; supercolony; unicolonial ID ARGENTINE ANTS C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Moffett, MW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, 10th St & Constitut Ave, Washington, DC 20013 USA. EM naturalist@erols.com NR 13 TC 5 Z9 5 U1 4 U2 18 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 SEP-OCT PY 2012 VL 23 IS 5 BP 938 EP 939 DI 10.1093/beheco/ars042 PG 3 WC Behavioral Sciences; Biology; Ecology; Zoology SC Behavioral Sciences; Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Zoology GA 998HL UT WOS:000308228200006 ER PT J AU Frankham, R Ballou, JD Dudash, MR Eldridge, MDB Fenster, CB Lacy, RC Mendelson, JR Porton, IJ Ralls, K Ryder, OA AF Frankham, Richard Ballou, Jonathan D. Dudash, Michele R. Eldridge, Mark D. B. Fenster, Charles B. Lacy, Robert C. Mendelson, Joseph R., III Porton, Ingrid J. Ralls, Katherine Ryder, Oliver A. TI Implications of different species concepts for conserving biodiversity SO BIOLOGICAL CONSERVATION LA English DT Article DE Fragmented populations; Genetic rescue; Inbreeding depression; Loss of genetic diversity; Outbreeding depression; Species concepts ID EFFECTIVE POPULATION-SIZE; PETROGALE MARSUPIALIA; PHENOTYPIC DIVERGENCE; SIGNIFICANT-UNITS; ROCK-WALLABIES; GENE FLOW; CONSERVATION; TAXONOMY; DNA; MACROPODIDAE AB The 26 definitions of species often yield different numbers of species and disparate groupings, with financial, legal, biological and conservation implications. Using conservation genetic considerations, we demonstrate that different species concepts have a critical bearing on our ability to conserve species. Many species of animals and plants persist as small isolated populations suffering inbreeding depression, loss of genetic diversity, and elevated extinction risks. Such small populations usually can be rescued by restoring gene flow, but substantial genetic drift effects can lead them to be classified as distinct species under the diagnostic phylogenetic species concept. Minimum harm to fitness is done and maximum potential fitness and evolutionary potential benefits accrue when reproductive isolation (pre- and/or post-zygotic) is used as the criterion to define distinct species. For sympatric populations, distinct species are diagnosed by very limited gene flow. For allopatric populations, both minimal gene flow and evidence of reduced reproductive fitness in crosses (or effects predicted from adaptive differentiation among populations and/or fixed chromosomal differences) are required to satisfy conservation issues. Species delineations based upon the biological and differential fitness species concepts meet the above requirements. Conversely, if species are delineated using the diagnostic phylogenetic species concept, genetic rescue of small genetically isolated populations may require crosses between species, with consequent legal and regulatory ramifications that could preclude actions to prevent extinction. Consequently, we conclude that the diagnostic phylogenetic species concept is unsuitable for use in conservation contexts, especially for classifying allopatric populations. (C) 2012 Elsevier Ltd. All rights reserved. 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 Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Dudash, Michele R.; Fenster, Charles B.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Lacy, Robert C.] Chicago Zool Soc, Brookfield, IL 60513 USA. [Mendelson, Joseph R., III] Zoo Atlanta, Atlanta, GA 30315 USA. [Mendelson, Joseph R., III] Georgia Inst Technol, Sch Biol, Atlanta, GA 30332 USA. [Porton, Ingrid J.] St Louis Zoo, St Louis, MO 63110 USA. [Ryder, Oliver A.] San Diego Zoo Inst Conservat Res, Escondido, CA 92027 USA. RP Frankham, R (reprint author), Macquarie Univ, Dept Biol Sci, N Ryde, NSW 2109, Australia. EM richard.frankham@mq.edu.au; ballouj@si.edu; mdudash@umd.edu; mark.eldridge@austmus.gov.au; cfenster@umd.edu; rlacy@ix.netcom.com; jmendelson@zooatlanta.org; Porton@stlzoo.org; rallsk@the-grid.net; oryder@sandiegozoo.org FU Saint Louis Zoo FX RF thanks R. Lacy, J. Ballou and I. Porton for inviting him to speak on this topic at a meeting at Saint Louis Zoo in 2011 and to the Saint Louis Zoo for providing travel funds. JRM thanks C. Feldman for helpful discussion. We thank J. Avise, D. Colgan, G. Cooke, K. de Queiroz, S. Donellan, B. Hausdorf, G. Mace, S. Smith, A. Stow, P. Sunnucks, R. Waples and four anonymous reviewers for comments on the manuscript, and J. Hey for answering queries relating to his published work. NR 68 TC 69 Z9 70 U1 9 U2 209 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD SEP PY 2012 VL 153 BP 25 EP 31 DI 10.1016/j.biocon.2012.04.034 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 994GB UT WOS:000307917800004 ER PT J AU Aylward, FO Burnum, KE Scott, JJ Suen, G Tringe, SG Adams, SM Barry, KW Nicora, CD Piehowski, PD Purvine, SO Starrett, GJ Goodwin, LA Smith, RD Lipton, MS Currie, CR AF Aylward, Frank O. Burnum, Kristin E. Scott, Jarrod J. Suen, Garret Tringe, Susannah G. Adams, Sandra M. Barry, Kerrie W. Nicora, Carrie D. Piehowski, Paul D. Purvine, Samuel O. Starrett, Gabriel J. Goodwin, Lynne A. Smith, Richard D. Lipton, Mary S. Currie, Cameron R. TI Metagenomic and metaproteomic insights into bacterial communities in leaf-cutter ant fungus gardens SO ISME JOURNAL LA English DT Article DE leaf-cutter ants; symbiosis; Leucoagaricus gongylophorus; microbial consortia; Atta ID ATTA-SEXDENS-RUBROPILOSA; CUTTING ANTS; GROWING ANTS; LEUCOAGARICUS-GONGYLOPHORUS; SYMBIOTIC FUNGUS; AGRICULTURE; MICROBIOME; CELLULOSE; DATABASE; GENOMES AB Herbivores gain access to nutrients stored in plant biomass largely by harnessing the metabolic activities of microbes. Leaf-cutter ants of the genus Atta are a hallmark example; these dominant neotropical herbivores cultivate symbiotic fungus gardens on large quantities of fresh plant forage. As the external digestive system of the ants, fungus gardens facilitate the production and sustenance of millions of workers. Using metagenomic and metaproteomic techniques, we characterize the bacterial diversity and physiological potential of fungus gardens from two species of Atta. Our analysis of over 1.2 Gbp of community metagenomic sequence and three 16S pyrotag libraries reveals that in addition to harboring the dominant fungal crop, these ecosystems contain abundant populations of Enterobacteriaceae, including the genera Enterobacter, Pantoea, Klebsiella, Citrobacter and Escherichia. We show that these bacterial communities possess genes associated with lignocellulose degradation and diverse biosynthetic pathways, suggesting that they play a role in nutrient cycling by converting the nitrogen-poor forage of the ants into B-vitamins, amino acids and other cellular components. Our metaproteomic analysis confirms that bacterial glycosyl hydrolases and proteins with putative biosynthetic functions are produced in both field-collected and laboratory-reared colonies. These results are consistent with the hypothesis that fungus gardens are specialized fungus-bacteria communities that convert plant material into energy for their ant hosts. Together with recent investigations into the microbial symbionts of vertebrates, our work underscores the importance of microbial communities in the ecology and evolution of herbivorous metazoans. The ISME Journal (2012) 6, 1688-1701; doi:10.1038/ismej.2012.10; published online 1 March 2012 Subject Category: integrated genomics and post-genomics approaches in microbial ecology C1 [Aylward, Frank O.; Scott, Jarrod J.; Suen, Garret; Adams, Sandra M.; Starrett, Gabriel J.; Currie, Cameron R.] Univ Wisconsin, Dept Bacteriol, Madison, WI 53706 USA. [Aylward, Frank O.; Scott, Jarrod J.; Suen, Garret; Adams, Sandra M.; Starrett, Gabriel J.; Currie, Cameron R.] Univ Wisconsin, Great Lakes Bioenergy Res Ctr, Dept Energy, Madison, WI 53706 USA. [Burnum, Kristin E.; Nicora, Carrie D.; Piehowski, Paul D.; Purvine, Samuel O.; Smith, Richard D.; Lipton, Mary S.] Pacific NW Natl Lab, Div Biol Sci, Richland, WA 99352 USA. [Scott, Jarrod J.; Currie, Cameron R.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Tringe, Susannah G.; Barry, Kerrie W.; Goodwin, Lynne A.] Joint Genome Inst, Dept Energy, Walnut Creek, CA USA. RP Currie, CR (reprint author), Univ Wisconsin, Dept Bacteriol, 6155 Microbial Sci Bldg,1550 Linden Dr, Madison, WI 53706 USA. EM currie@bact.wisc.edu RI Smith, Richard/J-3664-2012; Piehowski, Paul/B-1108-2011; Burnum, Kristin/B-1308-2011; OI Smith, Richard/0000-0002-2381-2349; Burnum, Kristin/0000-0002-2722-4149; Suen, Garret/0000-0002-6170-711X; Tringe, Susannah/0000-0001-6479-8427; Piehowski, Paul/0000-0001-5108-2227 FU Office of Science of the US Department of Energy [DE-AC02-05CH11231]; US Department of Energy's (DOE) Office of Biological and Environmental Research (OBER) Panomics program; Battelle for the DOE [DE-AC05-76RL01830]; National Science Foundation [DEB-0747002, MCB-0702025, MCB-0731822]; DOE Great Lakes Bioenergy Research Center (DOE Office of Science) [BER DE-FC02-07ER64494] FX We thank the staff of the Joint Genome Institute, Pacific Northwest National Laboratories, and the Smithsonian Tropical Research Institute for their expertise and support in the collection and processing of all samples, in particular S Malfatti, L Seid, Y Clemons, R Urriola, M Paz and O Arosemena. We thank all members of the Currie lab for their comments on the manuscript. We also thank three anonymous reviewers for their comments on the manuscript. The US Department of Energy Joint Genome Institute effort was supported by the Office of Science of the US Department of Energy under Contract No. DE-AC02-05CH11231. Proteomic work was performed in the Environmental Molecular Sciences Laboratory, a US Department of Energy (DOE) Office of Biological and Environmental Research national scientific user facility on the Pacific Northwest National Laboratory (PNNL) campus. Portions of this research were supported by the US Department of Energy's (DOE) Office of Biological and Environmental Research (OBER) Panomics program. PNNL is a multiprogram national laboratory operated by Battelle for the DOE under Contract DE-AC05-76RL01830. This work is also supported by the National Science Foundation (grants DEB-0747002, MCB-0702025, and MCB-0731822 to CRC) and the DOE Great Lakes Bioenergy Research Center (DOE Office of Science BER DE-FC02-07ER64494). NR 47 TC 35 Z9 35 U1 10 U2 106 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 1751-7362 J9 ISME J JI ISME J. PD SEP PY 2012 VL 6 IS 9 BP 1688 EP 1701 DI 10.1038/ismej.2012.10 PG 14 WC Ecology; Microbiology SC Environmental Sciences & Ecology; Microbiology GA 997CN UT WOS:000308141900007 PM 22378535 ER PT J AU Loehr, JF Almarode, JT Tai, RH Sadler, PM AF Loehr, John F. Almarode, John T. Tai, Robert H. Sadler, Philip M. TI High school and college biology: a multi-level model of the effects of high school courses on introductory course performance SO JOURNAL OF BIOLOGICAL EDUCATION LA English DT Article DE high school; preparedness; biology; achievement; college science outcomes ID CHEMISTRY; ACHIEVEMENT; SUCCESS; STUDENTS AB In a climate where increasing numbers of students are encouraged to pursue post-secondary education, the level of preparedness students have for college-level coursework is not far from the minds of all educators, especially high school teachers. Specifically within the biological sciences, introductory biology classes often serve as the gatekeeper or a pre-requisite for subsequent coursework in those fields and pre-professional programmes (eg pre-medicine or pre-veterinarian). Thus, how helpful high school science and mathematics experiences are in preparing students for their introductory biology classes is important and relevant for teachers, science educators and policy makers alike. This quantitative study looked at the association between students' high school science and mathematics experiences with introductory college biology performance. Using a nationally representative sample of US students (n = 2667) enrolled in 33 introductory college biology courses, a multi-level statistical model was developed to analyse the association between high school educational experiences and the final course grade in introductory biology courses. Advanced high school science and mathematics coursework, an emphasis on a deep conceptual understanding of biology concepts and a prior knowledge of concepts addressed in well-structured laboratory investigations are all positively associated with students' achievement in introductory college biology. C1 [Almarode, John T.] James Madison Univ, Coll Educ, Dept Early Elementary & Reading Educ, Harrisonburg, VA 22807 USA. [Loehr, John F.] Chicago Publ Sch, Off Curriculum & Instruct Sci, Chicago, IL USA. [Tai, Robert H.] Univ Virginia, Curriculum Instruct & Special Educ, Charlottesville, VA USA. [Sadler, Philip M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Almarode, JT (reprint author), James Madison Univ, Coll Educ, Dept Early Elementary & Reading Educ, Mem Hall 3100,MSC 6909, Harrisonburg, VA 22807 USA. EM almarojt@jmu.edu NR 26 TC 0 Z9 0 U1 0 U2 8 PU ROUTLEDGE JOURNALS, TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXFORDSHIRE, ENGLAND SN 0021-9266 J9 J BIOL EDUC JI J. Biol. Educ. PD SEP PY 2012 VL 46 IS 3 BP 165 EP 172 DI 10.1080/00219266.2011.617767 PG 8 WC Biology; Education & Educational Research; Education, Scientific Disciplines SC Life Sciences & Biomedicine - Other Topics; Education & Educational Research GA 995RY UT WOS:000308031200007 ER PT J AU Eckles, MA Roubik, DW Nieh, JC AF Eckles, M. A. Roubik, D. W. Nieh, J. C. TI A stingless bee can use visual odometry to estimate both height and distance SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE distance; height; navigation; optic flow; stingless bees; visual odometry ID CELESTIAL COMPASS CUES; OPTIC FLOW; HONEYBEE NAVIGATION; CATAGLYPHIS-FORTIS; DESERT ANTS; GUARD BEES; MOLECULAR PHYLOGENY; FOOD SOURCE; APIDAE; MELIPONA AB Bees move and forage within three dimensions and rely heavily on vision for navigation. The use of vision-based odometry has been studied extensively in horizontal distance measurement, but not vertical distance measurement. The honey bee Apis mellifera and the stingless bee Melipona seminigra measure distance visually using optic flow-movement of images as they pass across the retina. The honey bees gauge height using image motion in the ventral visual field. The stingless bees forage at different tropical forest canopy levels, ranging up to 40 m at our site. Thus, estimating height would be advantageous. We provide the first evidence that the stingless bee Melipona panamica utilizes optic flow information to gauge not only distance traveled but also height above ground, by processing information primarily from the lateral visual field. After training bees to forage at a set height in a vertical tunnel lined with black and white stripes, we observed foragers that explored a new tunnel with no feeder. In a new tunnel, bees searched at the same height they were trained to. In a narrower tunnel, bees experienced more image motion and significantly lowered their search height. In a wider tunnel, bees experienced less image motion and searched at significantly greater heights. In a tunnel without optic cues, bees were disoriented and searched at random heights. A horizontal tunnel testing these variables similarly affected foraging, but bees exhibited less precision (greater variance in search positions). Accurately gauging flight height above ground may be crucial for this species and others that compete for resources located at heights ranging from ground level to the high tropical forest canopies. C1 [Eckles, M. A.; Nieh, J. C.] Univ Calif, San Diego Div Biol Sci, Sect Ecol Behav & Evolut, La Jolla, CA 92093 USA. [Roubik, D. W.] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. RP Eckles, MA (reprint author), Univ Calif, San Diego Div Biol Sci, Sect Ecol Behav & Evolut, Mail Code 0116,9500 Gilman Dr, La Jolla, CA 92093 USA. EM meckles@ucsd.edu FU Smithsonian Tropical Research Institute; Jean-Marie Messier Fellowship; Smithsonian Tropical Research Institute Short-Term Fellowship; Smithsonian Pre-Doctoral Fellowship; National Science Foundation [NSF] [IBN 0316697]; ORBS program; NSF [IBN 0545856] FX The authors wish to thank The Smithsonian Tropical Research Institute for its support of this research. Thanks also to David Holway, William Wcislo and Egbert Giles Leigh for significant intellectual contributions. Sonia Reveco, Michelle Renner, Jennifer Phillips, Katherine LeVan, Femke Maas, Marco Visser and Meg Crofoot provided field assistance and research help. Oris Acevedo and Belkys Jimenez provided extensive and invaluable project support.; This work was funded by a Jean-Marie Messier Fellowship (to M.A.E.), a Smithsonian Tropical Research Institute Short-Term Fellowship (to M.A.E.) and a Smithsonian Pre-Doctoral Fellowship (to M.A.E.). This research was also supported by the National Science Foundation [NSF grant IBN 0316697, to J.C.N.] and by the ORBS program [funded by NSF grant IBN 0545856, to J.C.N.]. NR 51 TC 10 Z9 10 U1 2 U2 24 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 SEP PY 2012 VL 215 IS 18 BP 3155 EP 3160 DI 10.1242/jeb.070540 PG 6 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 995VH UT WOS:000308041400008 PM 22915710 ER PT J AU Hopkins, PF Hernquist, L Hayward, CC Narayanan, D AF Hopkins, Philip F. Hernquist, Lars Hayward, Christopher C. Narayanan, Desika TI Why are active galactic nuclei and host galaxies misaligned? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: evolution; quasars: general; cosmology: theory ID SUPERMASSIVE BLACK-HOLES; M-BH-SIGMA; PARTICLE HYDRODYNAMICS SIMULATIONS; CENTRAL MASS CONCENTRATIONS; HUBBLE-SPACE-TELESCOPE; MERGING DISK GALAXIES; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; X-RAY; SEYFERT-GALAXIES AB It is well established observationally that the characteristic angular momentum axis on small scales around active galactic nuclei (AGN), traced by radio jets and the putative torus, is not well correlated with the large-scale angular momentum axis of the host galaxy. In this paper, we show that such misalignments arise naturally in high-resolution simulations in which we follow angular momentum transport and inflows from galaxy to sub-pc scales near AGN, triggered either during galaxy mergers or by instabilities in isolated discs. Sudden misalignments can sometimes be caused by single massive clumps falling into the centre slightly off-axis, but more generally, they arise even when the gas inflows are smooth and trace only global gravitational instabilities. When several nested, self-gravitating modes are present, the inner ones can precess and tumble in the potential of the outer modes. Resonant angular momentum exchange can flip or re-align the spin of an inner mode on a short time-scale, even without the presence of massive clumps. We therefore do not expect that AGN and their host galaxies will be preferentially aligned, nor should the relative alignment be an indicator of the AGN fuelling mechanism. We discuss implications of this conclusion for AGN feedback and black hole (BH) spin evolution. The misalignments may mean that even BHs accreting from smooth large-scale discs will not be spun up to maximal rotation and so have more modest radiative efficiencies and inefficient jet formation. Even more random orientations/lower spins are possible if there is further unresolved clumpiness in the gas, and more ordered accretion may occur if the inflow is slower and not self-gravitating. C1 [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hernquist, Lars; Hayward, Christopher C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM phopkins@astro.berkeley.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU NASA [PF1-120083]; NSF [AST-1009452] FX We thank Massimo Dotti and the anonymous referee for comments and suggestions that greatly improved this paper, in particular in the discussion of BH spin. We also thank Eliot Quataert and Robert Antonucci for helpful discussions in the development of this work. Support for PFH was provided by NASA through Einstein Postdoctoral Fellowship Award Number PF1-120083. DN acknowledges support from the NSF via grant AST-1009452. NR 149 TC 21 Z9 21 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 SEP PY 2012 VL 425 IS 2 BP 1121 EP 1128 DI 10.1111/j.1365-2966.2012.21449.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VQ UT WOS:000307888300021 ER PT J AU Bernardini, MG Margutti, R Zaninoni, E Chincarini, G AF Bernardini, M. G. Margutti, R. Zaninoni, E. Chincarini, G. TI A universal scaling for short and long gamma-ray bursts: E-X,E-iso-E-gamma,E-iso-E-pk SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanism: non-thermal; gamma-rays: general; X-rays: general ID XMM-NEWTON OBSERVATIONS; HIGH-ENERGY EMISSION; PEAK ENERGY; LUMINOSITY RELATION; TIGHT CORRELATION; FLARING ACTIVITY; PROMPT EMISSION; GRB 101225A; FLARES; SWIFT AB The comprehensive statistical analysis of Swift X-ray light curves, collecting data from six years of operation, revealed the existence of a universal scaling among the isotropic energy emitted in the rest-frame 1 - 104?keV energy band during the prompt emission (E?, iso ), the peak of the prompt emission energy spectrum (Epk) and the X-ray energy emitted in the 0.310?keV observed energy band (EX, iso). In this paper, we show that this three-parameter correlation is robust and does not depend on our definition of EX, iso. It is shared by long, short and low-energetic gamma-ray bursts (GRBs), and thus reflects the existence of some properties which are shared by the GRB class as a whole. A more intuitive way to express the three-parameter correlation is in the form of a two-parameter correlation between the GRB efficiency and Epk. We speculate that the physical origin of such a relation is connected with the outflow Lorentz factor. C1 [Bernardini, M. G.; Margutti, R.; Zaninoni, E.; Chincarini, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zaninoni, E.] Univ Padua, Phys & Astron Dept Galileo Galilei, I-35131 Padua, Italy. [Chincarini, G.] Univ Milano Bicocca, Dept Phys, I-20126 Milan, Italy. RP Bernardini, MG (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, LC, Italy. EM grazia.bernardini@brera.inaf.it FU ASI [SWIFT I/004/11/0] FX We thank the referee for his/her constructive and well-directed comments. We also thank Lorenzo Amati for sharing his data before publication. This work is supported by ASI grant SWIFT I/004/11/0. NR 63 TC 22 Z9 22 U1 0 U2 3 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 SEP PY 2012 VL 425 IS 2 BP 1199 EP 1204 DI 10.1111/j.1365-2966.2012.21487.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VQ UT WOS:000307888300026 ER PT J AU Derekas, A Szabo, GM Berdnikov, L Szabo, R Smolec, R Kiss, LL Szabados, L Chadid, M Evans, NR Kinemuchi, K Nemec, JM Seader, SE Smith, JC Tenenbaum, P AF Derekas, A. Szabo, Gy. M. Berdnikov, L. Szabo, R. Smolec, R. Kiss, L. L. Szabados, L. Chadid, M. Evans, N. R. Kinemuchi, K. Nemec, J. M. Seader, S. E. Smith, J. C. Tenenbaum, P. TI Period and light-curve fluctuations of the Kepler Cepheid V1154 Cygni SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE techniques: photometric; planets and satellites: detection; stars: individual: V1154 Cyg; stars: variables: Cepheids ID GRAVITATIONAL LENSING EXPERIMENT.; OGLE-III CATALOG; LARGE-MAGELLANIC-CLOUD; CLASSICAL CEPHEIDS; INITIAL CHARACTERISTICS; CADENCE DATA; MODELS; PULSATIONS; STARS; POLARIS AB We present a detailed period analysis of the bright Cepheid-type variable star V1154 Cygni (V1154 Cyg; V = 9.1?mag, P 4.9?d) based on almost 600?d of continuous observations by the Kepler space telescope. The data reveal significant cycle-to-cycle fluctuations in the pulsation period, indicating that classical Cepheids may not be as accurate astrophysical clocks as commonly believed: regardless of the specific points used to determine the O - C values, the cycle lengths show a scatter of 0.0150.02?d over 120 cycles covered by the observations. A very slight correlation between the individual Fourier parameters and the O - C values was found, suggesting that the O - C variations might be due to the instability of the light-curve shape. Random-fluctuation tests revealed a linear trend up to a cycle difference 15, but for long term, the period remains around the mean value. We compare the measurements with simulated light curves that were constructed to mimic V1154 Cyg as a perfect pulsator modulated only by the light travel time effect caused by low-mass companions. We show that the observed period jitter in V1154 Cyg represents a serious limitation in the search for binary companions. While the Kepler data are accurate enough to allow the detection of planetary bodies in close orbits around a Cepheid, the astrophysical noise can easily hide the signal of the light-time effect. C1 [Derekas, A.; Szabo, Gy. M.; Szabo, R.; Kiss, L. L.; Szabados, L.] Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, H-1121 Budapest, Hungary. [Derekas, A.] Eotvos Lorand Univ, Dept Astron, Budapest, Hungary. [Derekas, A.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Berdnikov, L.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Berdnikov, L.] Isaac Newton Inst Chile, Moscow Branch, Moscow 119992, Russia. [Smolec, R.] Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Chadid, M.] Univ Nice Sophia Antipolis, Observ Cote Azur, UMR 7293, F-06108 Nice 02, France. [Evans, N. R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kinemuchi, K.; Seader, S. E.; Smith, J. C.; Tenenbaum, P.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Nemec, J. M.] Camosun Coll, Dept Phys & Astron, Victoria, BC V8P 5J2, Canada. [Nemec, J. M.] Int Stat & Res Corp, Brentwood Bay, BC V8M 1R3, Canada. RP Derekas, A (reprint author), Hungarian Acad Sci, Konkoly Observ, Res Ctr Astron & Earth Sci, Konkoly Thege Miklos 15-17, H-1121 Budapest, Hungary. EM derekas@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; Szabo, Robert/0000-0002-3258-1909 FU Hungarian OTKA [K76816, K83790, MB08C 81013]; ESA PECS [C98090]; Hungarian Academy of Sciences; Magyary Zoltan Public Foundation; Hungarian Eotvos fellowship; NASA's Science Mission Directorate FX This project has been supported by the Hungarian OTKA Grants K76816, K83790 and MB08C 81013, ESA PECS C98090 and the 'Lendulet-2009' Young Researchers Program of the Hungarian Academy of Sciences. AD gratefully acknowledges financial support from the Magyary Zoltan Public Foundation. AD was supported by the Hungarian Eotvos fellowship. RS, AD and GyMSz have been supported by the Janos Bolyai Research Scholarship of the Hungarian Academy of Sciences. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. Fruitful discussions with Zoltan Kollath are gratefully acknowledged. NR 37 TC 25 Z9 25 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 SEP PY 2012 VL 425 IS 2 BP 1312 EP 1319 DI 10.1111/j.1365-2966.2012.21538.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VQ UT WOS:000307888300038 ER PT J AU Krause, GH Winter, K Matsubara, S Krause, B Jahns, P Virgo, A Aranda, J Garcia, M AF Krause, G. Heinrich Winter, Klaus Matsubara, Shizue Krause, Barbara Jahns, Peter Virgo, Aurelio Aranda, Jorge Garcia, Milton TI Photosynthesis, photoprotection, and growth of shade-tolerant tropical tree seedlings under full sunlight SO PHOTOSYNTHESIS RESEARCH LA English DT Article DE Chlorophyll fluorescence; CO2 assimilation; Photoacclimation; Photoinhibition of photosystem II; Photosynthetic pigments; Shade-tolerant tropical trees; Tocopherol ID HIGH-LIGHT STRESS; XANTHOPHYLL-CYCLE ACTIVITY; LUTEIN EPOXIDE CYCLE; CHLOROPHYLL FLUORESCENCE; PHOTOSYSTEM-II; ULTRAVIOLET-RADIATION; PHOTOOXIDATIVE STRESS; ALOCASIA-MACRORRHIZA; ENERGY-DISSIPATION; BIOMASS ALLOCATION AB High solar radiation in the tropics is known to cause transient reduction in photosystem II (PSII) efficiency and CO2 assimilation in sun-exposed leaves, but little is known how these responses affect the actual growth performance of tropical plants. The present study addresses this question. Seedlings of five woody neotropical forest species were cultivated under full sunlight and shaded conditions. In full sunlight, strong photoinhibition of PSII at midday was documented for the late-successional tree species Ormosia macrocalyx and Tetragastris panamensis and the understory/forest gap species, Piper reticulatum. In leaves of O. macrocalyx, PSII inhibition was accompanied by substantial midday depression of net CO2 assimilation. Leaves of all species had increased pools of violaxanthin-cycle pigments. Other features of photoacclimation, such as increased Chl a/b ratio and contents of lutein, beta-carotene and tocopherol varied. High light caused strong increase of tocopherol in leaves of T. panamensis and another late-successional species, Virola surinamensis. O. macrocalyx had low contents of tocopherol and UV-absorbing substances. Under full sunlight, biomass accumulation was not reduced in seedlings of T. panamensis, P. reticulatum, and V. surinamensis, but O. macrocalyx exhibited substantial growth inhibition. In the highly shade-tolerant understory species Psychotria marginata, full sunlight caused strongly reduced growth of most individuals. However, some plants showed relatively high growth rates under full sun approaching those of seedlings at 40 % ambient irradiance. It is concluded that shade-tolerant tropical tree seedlings can achieve efficient photoacclimation and high growth rates in full sunlight. C1 [Krause, G. Heinrich; Jahns, Peter] Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. [Krause, G. Heinrich; Winter, Klaus; Krause, Barbara; Virgo, Aurelio; Aranda, Jorge; Garcia, Milton] Smithsonian Trop Res Inst, Panama City, Panama. [Matsubara, Shizue] Forschungszentrum Julich, IBG Pflanzenwissensch 2, D-52425 Julich, Germany. RP Krause, GH (reprint author), Univ Dusseldorf, Inst Plant Biochem, Univ Str 1, D-40225 Dusseldorf, Germany. EM ghkrause@uni-duesseldorf.de RI Matsubara, Shizue/A-5673-2011 OI Matsubara, Shizue/0000-0002-1440-6496 FU Smithsonian Tropical Research Institute, Panama; Deutsche Forschungsgemeinschaft (DFG), Germany FX We thank Maria Graf for competent assistance in HPLC analyses. The study was supported by the Smithsonian Tropical Research Institute, Panama, and Deutsche Forschungsgemeinschaft (DFG), Germany. NR 55 TC 9 Z9 10 U1 2 U2 99 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0166-8595 J9 PHOTOSYNTH RES JI Photosynth. Res. PD SEP PY 2012 VL 113 IS 1-3 SI SI BP 273 EP 285 DI 10.1007/s11120-012-9731-z PG 13 WC Plant Sciences SC Plant Sciences GA 997TI UT WOS:000308188800020 PM 22466529 ER PT J AU Gegenbauer, C Mayer, VE Zotz, G Richter, A AF Gegenbauer, Christian Mayer, Veronika E. Zotz, Gerhard Richter, Andreas TI Uptake of ant-derived nitrogen in the myrmecophytic orchid Caularthron bilamellatum SO ANNALS OF BOTANY LA English DT Article DE Antplant interactions; mutualism; nutrient uptake; MichaelisMenten kinetics; N-15 labelling; myrmecophytes; epiphytes; Caularthron bilamellatum; Orchidaceae; BCNM ID SCHOMBURGKIA-TIBICINIS ORCHIDACEAE; EXTRAFLORAL NECTARIES; EPIPHYTIC BROMELIAD; FOOD BODIES; RAIN-FOREST; FED PLANTS; ABSORPTION; MUTUALISM; ASSOCIATION; HYMENOPTERA AB Mutualistic antplant associations are common in a variety of plant families. Some myrmecophytic plants, such as the epiphytic orchid Caularthron bilamellatum, actively form hollow structures that provide nesting space for ants (myrmecodomatia), despite a substantial loss of water-storage tissue. This study aimed at assessing the ability of the orchid to take up nitrogen from ant-inhabited domatia as possible trade-off for the sacrifice of potential water storage capacity. Nitrogen uptake capabilities and uptake kinetics of N-15-labelled compounds (NH4, urea and l -glutamine) were studied in field-grown Caularthron bilamellatum plants in a tropical moist forest in Panama. Plants were either labelled directly, by injecting substrates into the hollow pseudobulbs or indirectly, by labelling of the associated ants in situ. Caularthron bilamellatum plants were able to take up all tested inorganic and organic nitrogen forms through the inner surface of the pseudobulbs. Uptake of NH4 and glutamine followed MichaelisMenten kinetics, but urea uptake was not saturable up to 2 mm. N-15-labelled compounds were rapidly translocated and incorporated into vegetative and reproductive structures. By labelling ants with N-15 in situ, we were able to prove that ants transfer N to the plants under field conditions. Based on N-15 labelling experiments we were able to demonstrate, for the first time, that a myrmecophytic orchid is capable of actively acquiring different forms of nitrogen from its domatia and that nutrient flux from ants to plants does indeed occur under natural conditions. This suggests that beyond anti-herbivore protection host plants benefit from ants by taking up nitrogen derived from ant debris. C1 [Gegenbauer, Christian; Mayer, Veronika E.] Univ Vienna, Fac Life Sci, Dept Struct & Funct Bot, A-1010 Vienna, Austria. [Gegenbauer, Christian; Richter, Andreas] Univ Vienna, Fac Life Sci, Dept Terr Ecosyst Res, A-1010 Vienna, Austria. [Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Dept Biol & Environm Sci, Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Balboa, Panama. RP Mayer, VE (reprint author), Univ Vienna, Fac Life Sci, Dept Struct & Funct Bot, A-1010 Vienna, Austria. EM veronika.mayer@univie.ac.at; andreas.richter@univie.ac.at RI Richter, Andreas/D-8483-2012 OI Richter, Andreas/0000-0003-3282-4808 NR 51 TC 8 Z9 8 U1 4 U2 34 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0305-7364 J9 ANN BOT-LONDON JI Ann. Bot. PD SEP PY 2012 VL 110 IS 4 BP 757 EP 765 DI 10.1093/aob/mcs140 PG 9 WC Plant Sciences SC Plant Sciences GA 995NN UT WOS:000308016100001 PM 22778148 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 (vol 141, pg 179, 2011) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Chan, Tucker; Ingemyr, Mikael; Winn, Joshua N.; Sanchis-Ojeda, Roberto] MIT, Dept Phys, Cambridge, MA 02139 USA. [Chan, Tucker; Ingemyr, Mikael; Winn, Joshua N.; Sanchis-Ojeda, Roberto] 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 NR 3 TC 1 Z9 1 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2012 VL 144 IS 3 AR 90 DI 10.1088/0004-6256/144/3/90 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995JF UT WOS:000308003600020 ER PT J AU Haschke, R Grebel, EK Frebel, A Duffau, S Hansen, CJ Koch, A AF Haschke, Raoul Grebel, Eva K. Frebel, Anna Duffau, Sonia Hansen, Camilla J. Koch, Andreas TI CHEMICAL ABUNDANCES OF METAL-POOR RR LYRAE STARS IN THE MAGELLANIC CLOUDS SO ASTRONOMICAL JOURNAL LA English DT Article DE Magellanic Clouds; stars: abundances; stars: variables: RR Lyrae; techniques: spectroscopic ID DWARF SPHEROIDAL GALAXY; GRAVITATIONAL LENSING EXPERIMENT.; HORIZONTAL-BRANCH STARS; AGE-METALLICITY RELATION; III PHOTOMETRIC MAPS; RED GIANT STARS; SEGUE 1 SYSTEM; MILKY-WAY; GLOBULAR-CLUSTERS; INNER REGIONS AB We present for the first time a detailed spectroscopic study of chemical element abundances of metal-poor RR Lyrae stars in the Large and Small Magellanic Cloud (LMC and SMC). Using the MagE echelle spectrograph at the 6.5 m Magellan telescopes, we obtain medium resolution (R similar to 2000-6000) spectra of six RR Lyrae stars in the LMC and three RR Lyrae stars in the SMC. These stars were chosen because their previously determined photometric metallicities were among the lowest metallicities found for stars belonging to the old populations in theMagellanic Clouds. We find the spectroscopic metallicities of these stars to be as low as [Fe/H](spec) = -2.7 dex, the lowest metallicity yet measured for any star in the Magellanic Clouds. We confirm that for metal-poor stars, the photometric metallicities from the Fourier decomposition of the light curves are systematically too high compared to their spectroscopic counterparts. However, for even more metal-poor stars below [Fe/H](phot) < -2.8 dex this trend is reversed and the spectroscopic metallicities are systematically higher than the photometric estimates. We are able to determine abundance ratios for 10 chemical elements (Fe, Na, Mg, Al, Ca, Sc, Ti, Cr, Sr, and Ba), which extend the abundance measurements of chemical elements for RR Lyrae stars in the Clouds beyond [Fe/H] for the first time. For the overall [alpha/Fe] ratio, we obtain an overabundance of 0.36 dex, which is in very good agreement with results from metal-poor stars in the Milky Way halo as well as from the metal-poor tail in dwarf spheroidal galaxies. Comparing the abundances with those of the stars in the Milky Way halo we find that the abundance ratios of stars of both populations are consistent with another. Therefore, we conclude that from a chemical point of view early contributions from Magellanic-type galaxies to the formation of the Galactic halo as claimed in cosmological models are plausible. C1 [Haschke, Raoul; Grebel, Eva K.; Duffau, Sonia] Univ Heidelberg, Astron Rechen Inst, Zentrum Astron, D-69120 Heidelberg, Germany. [Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frebel, Anna] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hansen, Camilla J.; Koch, Andreas] Univ Heidelberg, Zentrum Astron, Landessternwarte, D-69117 Heidelberg, Germany. RP Haschke, R (reprint author), Univ Heidelberg, Astron Rechen Inst, Zentrum Astron, Monchhofstr 12-14, D-69120 Heidelberg, Germany. EM haschke@ari.uni-heidelberg.de OI Hansen, Camilla Juul/0000-0002-7277-7922; Koch, Andreas/0000-0002-9859-4956; /0000-0002-1891-3794 FU Heidelberg Graduate School for Fundamental Physics (HGSFP) [129/1]; Deutsche Forschungsgemeinschaft (DFG) [Sonderforschungbereich SFB881]; Clay Fellowship; DFG from Emmy-Noether [Ko 4161/1] FX R.H. is grateful to the Heidelberg Graduate School for Fundamental Physics (HGSFP) (grant number 129/1) for providing support for a scientific visit at Harvard University. E. K. G., S. D., and C.J.H. acknowledge support by the Sonderforschungbereich SFB881 ("The Milky Way System") of the Deutsche Forschungsgemeinschaft (DFG) in the subprojects A2, A3, and A5. A. F. is supported by a Clay Fellowship administered by the Smithsonian Astrophysical Observatory. A. K. acknowledges the DFG for funding from Emmy-Noether grant Ko 4161/1. NR 106 TC 10 Z9 10 U1 0 U2 1 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 SEP PY 2012 VL 144 IS 3 AR 88 DI 10.1088/0004-6256/144/3/88 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995JF UT WOS:000308003600018 ER PT J AU Willman, B Strader, J AF Willman, B. Strader, J. TI "GALAXY," DEFINED SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: kinematics and dynamics; galaxies: star clusters: general ID DWARF SPHEROIDAL GALAXIES; MULTIPLE STELLAR POPULATIONS; GLOBULAR-CLUSTER SYSTEMS; INITIAL MASS FUNCTION; NA-O ANTICORRELATION; MILKY-WAY SATELLITE; ULTRA-COMPACT DWARFS; DARK-MATTER HALOS; MULTIELEMENT ABUNDANCE MEASUREMENTS; DISPERSION-SUPPORTED GALAXIES AB A growing number of low luminosity and low surface brightness astronomical objects challenge traditional notions of both galaxies and star clusters. To address this challenge, we propose a definition of galaxy that does not depend on a cold dark matter model of the universe: a galaxy is a gravitationally bound collection of stars whose properties cannot be explained by a combination of baryons and Newton's laws of gravity. After exploring several possible observational diagnostics of this definition, we critically examine the classification of ultra-faint dwarfs, globular clusters, ultra-compact dwarfs, and tidal dwarfs. While kinematic studies provide an effective diagnostic of the definition in many regimes, they can be less useful for compact or very faint systems. To explore the utility of using the [Fe/H] spread as a complementary diagnostic, we use published spectroscopic [Fe/H] measurements of 16 Milky Way dwarfs and 24 globular clusters to uniformly calculate their [Fe/H] spreads and associated uncertainties. Our principal results are (1) no known, old star cluster less luminous than M-V = -10 has a significant (greater than or similar to 0.1 dex) spread in its iron abundance; (2) known ultra-faint dwarf galaxies can be unambiguously classified with a combination of kinematic and [Fe/H] observations; (3) the observed [Fe/H] spreads in massive (greater than or similar to 10(6) M-circle dot) globular clusters do not necessarily imply that they are the stripped nuclei of dwarfs, nor a need for dark matter; and (4) if ultra-compact dwarf galaxies reside in dark matter halos akin to those of ultra-faint dwarfs of the same half-light radii, then they will show no clear dynamical signature of dark matter. We suggest several measurements that may assist the future classification of massive globular clusters, ultra-compact dwarfs, and ultra-faint galaxies. Our galaxy definition is designed to be independent of the details of current observations and models, while our proposed diagnostics can be refined or replaced as our understanding of the universe evolves. C1 [Willman, B.] Haverford Coll, Dept Astron, Haverford, PA 19041 USA. [Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02144 USA. RP Willman, B (reprint author), Haverford Coll, Dept Astron, 370 Lancaster Ave, Haverford, PA 19041 USA. EM bwillman@haverford.edu; jstrader@cfa.harvard.edu FU NSF [AST-0908193] FX B.W. acknowledges support from NSF AST-0908193. B.W. also thanks NYU's Center for Cosmology and Particle Physics and Drexel University's Physics Department for hosting her during the writing of this paper. We thank Dr. Pierre-Alain Duc, the referee, for comments that helped improve the quality and clarity of this paper. We thank Michele Bellazzini, Joerg Dabringhausen, Ross Fadely, Duncan Forbes, Amanda Ford, Marla Geha, Amina Helmi, David Hogg, Evan Kirby, Pavel Kroupa, George Lake, Erik Tollerud, and Enrico Vesperini for stimulating conversations and e-mails leading up to and during the preparation of this paper. This research has made use of NASA's Astrophysics Data System Bibliographic Services. NR 154 TC 61 Z9 61 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2012 VL 144 IS 3 AR 76 DI 10.1088/0004-6256/144/3/76 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995JF UT WOS:000308003600006 ER PT J AU Mannion, PD Benson, RBJ Upchurch, P Butler, RJ Carrano, MT Barrett, PM AF Mannion, Philip D. Benson, Roger B. J. Upchurch, Paul Butler, Richard J. Carrano, Matthew T. Barrett, Paul M. TI A temperate palaeodiversity peak in Mesozoic dinosaurs and evidence for Late Cretaceous geographical partitioning SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Biogeography; birds; climatic zonation; dinosaurs; diversity; latitudinal biodiversity gradient; palaeontology; sampling; seasonality ID LATITUDINAL DIVERSITY GRADIENT; SPECIES-RICHNESS; ROCK RECORD; MASS EXTINCTIONS; SAMPLING BIASES; CLIMATE-CHANGE; FOSSIL RECORD; PATTERNS; BIODIVERSITY; EVOLUTION AB Aim Modern biodiversity peaks in the tropics and declines poleward, a pattern that is potentially driven by climate. Although this latitudinal biodiversity gradient (LBG) also characterizes the marine invertebrate fossil record, distributions of ancient terrestrial faunas are poorly understood. This study utilizes data on the dinosaur fossil record to examine spatial patterns in terrestrial biodiversity throughout the Mesozoic. Location We compiled data on fossil occurrences across the globe. Methods We compiled a comprehensive dataset of Mesozoic dinosaur genera (738), including birds. Following the utilization of sampling standardization techniques to mediate for the uneven sampling of the fossil record, we constructed latitudinal patterns of biodiversity from this dataset. Results The dominant group of Mesozoic terrestrial vertebrates did not conform to the modern LBG. Instead, dinosaur diversity was highest at temperate palaeolatitudes throughout the 160 million year span of dinosaurian evolutionary history. Latitudinal diversity correlates strongly with the distribution of land area. Late Cretaceous sauropods and ornithischians exhibit disparate LBGs. Main conclusions The continuity of the palaeotemperate peak in dinosaur diversity indicates a diminished role for climate on the Mesozoic LBG; instead, dinosaur diversity may have been driven by the amount of land area among latitudinal belts. There is no evidence that the tropics acted as a cradle for dinosaur diversity. Geographical partitioning among major clades of herbivorous dinosaurs in the Late Cretaceous may result from the advanced stages of continental fragmentation and/or differing responses to increasing latitudinal climatic zonation. Our results suggest that the modern-day LBG on land was only established 30 million years ago, following a significant post-Eocene recalibration, potentially related to increased seasonality. C1 [Mannion, Philip D.] Museum Nat Kunde, D-10115 Berlin, Germany. [Mannion, Philip D.; Upchurch, Paul] UCL, Dept Earth Sci, London WC1E 6BT, England. [Benson, Roger B. J.] Univ Cambridge, Dept Earth Sci, Cambridge CB2 3EQ, England. [Butler, Richard J.] Univ Munich, Geobio Ctr, D-80333 Munich, Germany. [Butler, Richard J.] Bayer Staatssammlung Palaontol & Geol, D-80333 Munich, Germany. [Carrano, Matthew T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Barrett, Paul M.] Nat Hist Museum, Dept Palaeontol, London SW7 5BD, England. RP Mannion, PD (reprint author), Museum Nat Kunde, Invalidenstr 43, D-10115 Berlin, Germany. EM philipdmannion@gmail.com RI Upchurch, Paul/C-1654-2008; Barrett, Paul/A-2648-2010; Butler, Richard/A-5239-2011; Carrano, Matthew/C-7601-2011; OI Barrett, Paul/0000-0003-0412-3000; Butler, Richard/0000-0003-2136-7541; Carrano, Matthew/0000-0003-2129-1612; Benson, Roger/0000-0001-8244-6177 FU NERC [NER/S/A/2006/14347]; Alexander von Humboldt Research Fellowship; Leverhulme Foundation [RPG-129] FX This study is Paleobiology Database official publication number 142. Reviews by John Alroy, Steve Brusatte, Richard Field, Shanan Peters and one anonymous referee greatly improved earlier versions of this manuscript. Kate Littler also provided helpful discussion regarding Cenozoic climate. P.D.M.'s research was supported by NERC studentship NER/S/A/2006/14347 and an Alexander von Humboldt Research Fellowship. R.J.B. is supported by an Alexander von Humboldt Research Fellowship. R.B.J.B and P. U. are supported by Leverhulme Foundation grant RPG-129. NR 70 TC 19 Z9 19 U1 0 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD SEP PY 2012 VL 21 IS 9 BP 898 EP 908 DI 10.1111/j.1466-8238.2011.00735.x PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 993YS UT WOS:000307897200003 ER PT J AU Sholts, SB Stanford, DJ Flores, LM Warmlander, SKTS AF Sholts, Sabrina B. Stanford, Dennis J. Flores, Louise M. Warmlander, Sebastian K. T. S. TI Flake scar patterns of Clovis points analyzed with a new digital morphometrics approach: evidence for direct transmission of technological knowledge across early North America SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Lithic technology; Pleistocene; Paleoindians; 3D scanning; Contour analysis; Morphology ID PROJECTILE-POINTS; BIFACE; ORIGIN; SITE; AGE AB Clovis points are the principal diagnostic artifacts of a Clovis complex that spread across North America between ca. 11,050-10,800 radiocarbon years before present. Clovis may be the best documented Paleoamerican culture in North America, but much remains to be learned about the movement and interactions of Clovis peoples. Similarities among Clovis points from geographically diverse locations have led some researchers to suggest that a uniform projectile point technology existed across North America during Clovis times. Others have rejected this idea, proposing local and independent technological adaptations to different regional environments. To investigate these ideas, we used digital morphometrics to analyze 50 Clovis points from nine different contexts. First, 3D surface models of the points were created with a portable laser scanner. Next, these models were digitally cross-sectioned through both faces, yielding two-dimensional isoheight contours of flake scar patterns that reflect the original reduction techniques used to shape the projectile points. In the final step, the contours were transformed with elliptic Fourier analysis into Fourier coefficient series, and patterns of variation and symmetry were explored with principal components analysis. When compared to modern Clovis point replicas made by an expert knapper, the flake scar contours of the ancient Clovis points showed little morphological variation and a large degree of bifacial symmetry. Our results support the existence of a widespread standardized "Clovis" knapping technique, most likely transmitted through direct interaction between knappers from different groups. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Warmlander, Sebastian K. T. S.] Univ Stockholm, Arrhenius Labs, Div Biophys, S-10691 Stockholm, Sweden. [Sholts, Sabrina B.; Flores, Louise M.; Warmlander, Sebastian K. T. S.] Univ Calif Santa Barbara, Dept Anthropol, Santa Barbara, CA 93106 USA. [Sholts, Sabrina B.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Stanford, Dennis J.] Smithsonian Inst, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Warmlander, Sebastian K. T. S.] Univ Calif Los Angeles, Cotsen Inst Archaeol, UCLA Getty Conservat Programme, Los Angeles, CA USA. RP Warmlander, SKTS (reprint author), Univ Stockholm, Arrhenius Labs, Div Biophys, S-10691 Stockholm, Sweden. EM seb@dbb.su.se NR 55 TC 20 Z9 20 U1 0 U2 15 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 SEP PY 2012 VL 39 IS 9 BP 3018 EP 3026 DI 10.1016/j.jas.2012.04.049 PG 9 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 976VS UT WOS:000306616000017 ER PT J AU Drexler, JF Seelen, A Corman, VM Tateno, AF Cottontail, V Zerbinati, RM Gloza-Rausch, F Klose, SM Adu-Sarkodie, Y Oppong, SK Kalko, EKV Osterman, A Rasche, A Adam, A Muller, MA Ulrich, RG Leroy, EM Lukashev, AN Drosten, C AF Drexler, Jan Felix Seelen, Annika Corman, Victor Max Tateno, Adriana Fumie Cottontail, Veronika Zerbinati, Rodrigo Melim Gloza-Rausch, Florian Klose, Stefan M. Adu-Sarkodie, Yaw Oppong, Samuel K. Kalko, Elisabeth K. V. Osterman, Andreas Rasche, Andrea Adam, Alexander Mueller, Marcel A. Ulrich, Rainer G. Leroy, Eric M. Lukashev, Alexander N. Drosten, Christian TI Bats Worldwide Carry Hepatitis E Virus-Related Viruses That Form a Putative Novel Genus within the Family Hepeviridae SO JOURNAL OF VIROLOGY LA English DT Article ID HUMAN-IMMUNODEFICIENCY-VIRUS; UNITED-STATES; HIGHLY PREVALENT; PREGNANT-WOMEN; BLOOD-DONORS; ORF3 PROTEIN; E VACCINE; C VIRUS; INFECTION; RNA AB Hepatitis E virus (HEV) is one of the most common causes of acute hepatitis in tropical and temperate climates. Tropical genotypes 1 and 2 are associated with food-borne and waterborne transmission. Zoonotic reservoirs (mainly pigs, wild boar, and deer) are considered for genotypes 3 and 4, which exist in temperate climates. In view of the association of several zoonotic viruses with bats, we analyzed 3,869 bat specimens from 85 different species and from five continents for hepevirus RNA. HEVs were detected in African, Central American, and European bats, forming a novel phylogenetic clade in the family Hepeviridae. Bat hepeviruses were highly diversified and comparable to human HEY in sequence variation. No evidence for the transmission of bat hepeviruses to humans was found in over 90,000 human blood donations and individual patient sera. Full-genome analysis of one representative virus confirmed formal classification within the family Hepeviridae. Sequence- and distance-based taxonomic evaluations suggested that bat hepeviruses constitute a distinct genus within the family Hepeviridae and that at least three other genera comprising human, rodent, and avian hepeviruses can be designated. This may imply that hepeviruses invaded mammalian hosts nonrecently and underwent speciation according to their host restrictions. Human HEY-related viruses in farmed and peridomestic animals might represent secondary acquisitions of human viruses, rather than animal precursors causally involved in the evolution of human HEV. C1 [Drexler, Jan Felix; Seelen, Annika; Corman, Victor Max; Tateno, Adriana Fumie; Zerbinati, Rodrigo Melim; Gloza-Rausch, Florian; Klose, Stefan M.; Mueller, Marcel A.; Drosten, Christian] Univ Bonn, Inst Virol, Med Ctr, Bonn, Germany. [Cottontail, Veronika; Klose, Stefan M.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Gloza-Rausch, Florian] Noctalis, Ctr Bat Protect & Informat, Bad Segeberg, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Adu-Sarkodie, Yaw; Oppong, Samuel K.] Kwame Nkrumah Univ Sci & Technol, Kumasi, Ghana. [Osterman, Andreas] Max von Pettenkofer Inst, Dept Virol, Munich, Germany. [Rasche, Andrea] Univ Vet Med Hannover, Hannover, Germany. [Adam, Alexander] Univ Cologne, Inst Pathol, Med Ctr, Cologne, Germany. [Ulrich, Rainer G.] Inst Novel & Emerging Infect Dis, Friedrich Loeffler Inst, Greifswald, Germany. [Leroy, Eric M.] Ctr Int Rech Med Franceville, Unite Malad Virales Emergentes, Franceville, Gabon. [Lukashev, Alexander N.] Chumakov Inst Poliomyelitis & Viral Encephalitide, Moscow, Russia. RP Drosten, C (reprint author), Univ Bonn, Inst Virol, Med Ctr, Bonn, Germany. EM drosten@virology-bonn.de RI Ulrich, Rainer/A-4411-2013; Lukashev, Alexander/G-2777-2013; Drexler, Jan Felix/C-1004-2014; LEROY, Eric/I-4347-2016; OI Lukashev, Alexander/0000-0001-7365-0352; LEROY, Eric/0000-0003-0022-0890; Mueller, Marcel/0000-0003-2242-5117; Corman, Victor Max/0000-0002-3605-0136 FU European Union [223498, 228292, 278976]; German Federal Ministry of Education and Research (BMBF) [01KIO701]; German Research Foundation (DFG) [DR 772/3-1, KA 1241/18-1]; DAAD [D/00/39390]; Australian Government Endeavor Programme FX This study was funded by the European Union FP7 projects EMPERIE (grant agreement number 223498), EVA (grant agreement number 228292), and ANTIGONE (grant agreement number 278976); the German Federal Ministry of Education and Research (BMBF) (project code 01KIO701); the German Research Foundation (DFG) (grant agreement numbers DR 772/3-1 and KA 1241/18-1); the DAAD (D/00/39390); and the Australian Government Endeavor Programme (to S.M.K.). NR 74 TC 105 Z9 107 U1 2 U2 29 PU AMER SOC MICROBIOLOGY PI WASHINGTON PA 1752 N ST NW, WASHINGTON, DC 20036-2904 USA SN 0022-538X J9 J VIROL JI J. Virol. PD SEP PY 2012 VL 86 IS 17 BP 9134 EP 9147 DI 10.1128/JVI.00800-12 PG 14 WC Virology SC Virology GA 990JW UT WOS:000307627800020 PM 22696648 ER PT J AU Glynn, PW Colley, SB Mate, JL Baums, IB Feingold, JS Cortes, J Guzman, HM Afflerbach, JC Brandtneris, VW Ault, JS AF Glynn, P. W. Colley, S. B. Mate, J. L. Baums, I. B. Feingold, J. S. Cortes, J. Guzman, H. M. Afflerbach, J. C. Brandtneris, V. W. Ault, J. S. TI Reef coral reproduction in the equatorial eastern Pacific: Costa Rica, Panama, and the Galapagos Islands (Ecuador). VII. Siderastreidae, Psammocora stellata and Psammocora profundacella SO MARINE BIOLOGY LA English DT Article ID 1997-98 EL-NINO; SCLERACTINIAN CORALS; COMMUNITY STRUCTURE; RED-SEA; POCILLOPORA-DAMICORNIS; SOUTHERN-OSCILLATION; SEXUAL REPRODUCTION; SPECIES BOUNDARIES; BREEDING SEASONS; PAVONA-GIGANTEA AB Two zooxanthellate, scleractinian species present in the equatorial eastern Pacific, Psammocora stellata and Psammocora profundacella, were examined in terms of their reproductive biology and ecology at four study sites, non-upwelling (Cao Island, Costa Rica, and Uva Island, Panama), upwelling (Gulf of Panama, Panama), and seasonally varying thermal environments (Galapagos Islands). Both species were gonochoric broadcast spawners lacking zooxanthellae in mature ova. Mature gametes and spawned gonads are present around full moon; however, no spawning was observed naturally or in outdoor aquaria. Mature gametes occurred in P. stellata at Cao Island for nearly 6 months, and year round at Uva Island, both non-upwelling sites. Reproductively active colonies occurred mostly in the warmer months in the Gulf of Panama and Galapagos Islands. In the Galapagos Islands, where collecting effort was greatest for P. profundacella, mature gametes were also most prevalent during the warm season. Annual fecundity was high in both species, 1.3-1.8 x 10(4) ova cm(-2) year(-1) in P. stellata and 1.2-2.0 x 10(4) ova cm(-2) year(-1) in P. profundacella. Compared to other eastern Pacific corals, P. stellata was relatively resistant to ENSO-related bleaching and mortality, especially populations inhabiting deep (12-20 m) coral communities. Rapid recovery and persistence of Psammocora spp. can be attributed to several factors: (a) relative resistance to bleaching, (b) deep refuge populations, (c) broadcast spawning, (d) protracted seasonal reproduction, (e) high fecundity, and (f) asexual propagation. C1 [Glynn, P. W.; Afflerbach, J. C.; Brandtneris, V. W.; Ault, J. S.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. [Colley, S. B.] Off Coastal Protect & Restorat, Louisiana Appl Coastal Engn & Sci Div, Baton Rouge, LA 70801 USA. [Mate, J. L.; Guzman, H. M.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baums, I. B.] Penn State Univ, Dept Biol, University Pk, PA 16802 USA. [Feingold, J. S.] Nova SE Univ, Oceanog Ctr, Dania, FL 33004 USA. [Cortes, J.] Univ Costa Rica, Ctr Invest Ciencias Mar & Limnol CIMAR, San Jose 110512060, Costa Rica. [Cortes, J.] Univ Costa Rica, Escuela Biol, San Jose 110512060, Costa Rica. RP Glynn, PW (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM pglynn@rsmas.miami.edu RI Baums, Iliana/G-6435-2010; Ault, Jerald/A-5241-2008 OI Baums, Iliana/0000-0001-6463-7308; Ault, Jerald/0000-0001-9657-8007 FU U. S. National Science Foundation, Biological Oceanography Program [OCE-0526361] FX We thank Adrienne M. S. Correa, Peggy Fong, Christiane Hueerkamp, Priscilla Martinez, and Fernando Rivera for help in the field, and Rebecca Ball-Bailey, Kathy Black, Kathryn Brown, Erin Kapostasy, Susan Laessig, Alison Moulding, Juan Pena, David Smith, Joy H Ting, Bonnie Tucker, and Joyce A Yager for various analytical tasks in the laboratory. Francesca Benzoni kindly assisted in the identification of Psammocora species. The following host countries, agencies, and institutions granted permission and variously assisted during the course of this study: Costa Rica, Centro de Investigaciones en Ciencias del Mar y Limnologia (CIMAR), Universidad de Costa Rica, and Sistema Nacional de Areas de Conservacion, Ministerio del Ambiente y Energia; Panama, Departamento de Biologia Acuatica (Universidad de Panama), Autoridad Nacional del Ambiente (ANAM), and Smithsonian Tropical Research Institute; Ecuador, Charles Darwin Research Station, and the Galapagos National Park Service. Research support was provided by the U. S. National Science Foundation, Biological Oceanography Program, grant OCE-0526361 and earlier awards. NR 76 TC 4 Z9 4 U1 1 U2 39 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0025-3162 J9 MAR BIOL JI Mar. Biol. PD SEP PY 2012 VL 159 IS 9 BP 1917 EP 1932 DI 10.1007/s00227-012-1979-5 PG 16 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 996EE UT WOS:000308066400005 ER PT J AU Forbes, DA Ponman, T O'Sullivan, E AF Forbes, Duncan A. Ponman, Trevor O'Sullivan, Ewan TI The baryonic haloes of elliptical galaxies: radial distribution of globular clusters and diffuse hot gas SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE globular clusters: general; galaxies: formation; galaxies: individual; galaxies: star clusters ID X-RAY; WIDE-FIELD; VIRGO CLUSTER; STELLAR HALOES; INTERSTELLAR-MEDIUM; FORNAX CLUSTER; DARK-MATTER; LARGE-SCALE; NGC 1407; SYSTEM AB For a sample of nine well-studied giant ellipticals, we compare the projected radial distribution of their red and blue globular cluster (GC) subpopulations with their host galaxy stellar and X-ray surface brightness profiles. We support previous findings that the surface density distribution of red (metal-rich) GCs follows that of the host galaxy starlight. We find good agreement between the outer slope of the blue GC surface density and that of the galaxy X-ray emission. This coincidence of projected radial profiles is likely due to the fact that both blue GCs and X-ray emitting hot gas share the same gravitational potential in equilibrium. When deprojected the X-ray emitting hot gas has a radial density dependence that is the square root of that for the GC density. We further show that the energy per unit mass for blue GCs is roughly half that of the hot gas. C1 [Forbes, Duncan A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Ponman, Trevor; O'Sullivan, Ewan] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [O'Sullivan, Ewan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forbes, DA (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM dforbes@swin.edu.au OI O'Sullivan, Ewan/0000-0002-5671-6900 FU European Community under the Marie Curie Research Training Network; National Aeronautics and Space Administration through Chandra X-ray Observatory Center [AR1-12014X]; National Aeronautics and Space Administration [NAS8-03060] FX We would like to thank A. Romanowsky, R. Crain, J. Strader, C. Frenk and G. Poole for useful discussions. We also thank V. Pota, K. Woodley, K. Rhode, L. Spitler and S. Kartha for supplying GC profile data. EOS acknowledges support from the European Community under the Marie Curie Research Training Network, and from the National Aeronautics and Space Administration through Chandra Award Number AR1-12014X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS8-03060. Some data used in this research come from the Hyperleda and NED data bases. We also thank the referees for their careful reading and useful comments. NR 56 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 SEP PY 2012 VL 425 IS 1 BP 66 EP 73 DI 10.1111/j.1365-2966.2012.21368.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300022 ER PT J AU Francis, KJ Drinkwater, MJ Chilingarian, IV Bolt, AM Firth, P AF Francis, K. J. Drinkwater, M. J. Chilingarian, Igor V. Bolt, A. M. Firth, P. TI The chemical composition of ultracompact dwarf galaxies in the Virgo and Fornax clusters SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: dwarf; galaxies: formation; galaxies: star clusters: general; galaxies: stellar content ID COMPACT STELLAR-SYSTEMS; ELEMENT ABUNDANCE RATIOS; MASSIVE STAR-CLUSTERS; ELLIPTIC GALAXIES; GLOBULAR-CLUSTERS; LUMINOSITY FUNCTION; POPULATION-MODELS; LICK INDEXES; COMA CLUSTER; DARK-MATTER AB We present spectroscopic observations of ultracompact dwarf (UCD) galaxies in the Fornax and Virgo clusters made to measure and compare their stellar populations. The spectra were obtained on the Gemini-North (Virgo) and Gemini-South (Fornax) telescopes using the respective Gemini Multi-Object Spectrographs. We estimated the ages, metallicities and abundances of the objects from measurements of Lick line-strength indices in the spectra; we also estimated the ages and metallicities independently using a direct spectral fitting technique. Both methods revealed that the UCDs are old (mean age 10.8 +/- 0.7 Gyr) and (generally) metal rich (mean [Fe/H] = -0.8 +/- 0.1). The a-element abundances of the objects measured from the Lick indices are super-solar. We used these measurements to test the hypothesis that UCDs are formed by the tidal disruption of present-day nucleated dwarf elliptical galaxies. The data are not consistent with this hypothesis because both the ages and abundances are significantly higher than those of observed dwarf galaxy nuclei (this does not exclude disruption of an earlier generation of dwarf galaxies). They are more consistent with the properties of globular star clusters, although at higher mean metallicity. The UCDs display a very wide range of metallicity (-1.7 < [Fe/H] < 0.0), spanning the full range of both globular clusters and dwarf galaxy nuclei. We confirm previous reports that most UCDs have high metalliticities for their luminosities, lying significantly above the canonical metallicitiyluminosity relation followed by early-type galaxies. In contrast to previous work, we find that there is no significant difference in either the mean ages or the mean metallicities of the Virgo and Fornax UCD populations. C1 [Francis, K. J.; Drinkwater, M. J.; Bolt, A. M.; Firth, P.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Chilingarian, Igor V.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor V.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. RP Francis, KJ (reprint author), Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. EM katy.francis@uqconnect.edu.au RI Drinkwater, Michael/A-2201-2008; Chilingarian, Igor/N-5117-2016 OI Drinkwater, Michael/0000-0003-4867-0022; Chilingarian, Igor/0000-0002-7924-3253 FU Russian Federation [MD-3288.2012.2] FX IC acknowledges the support from the grant of the president of the Russian Federation MD-3288.2012.2. NR 63 TC 15 Z9 15 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2012 VL 425 IS 1 BP 325 EP 337 DI 10.1111/j.1365-2966.2012.21465.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300046 ER PT J AU Sanchez, AG Scoccola, CG Ross, AJ Percival, W Manera, M Montesano, F Mazzalay, X Cuesta, AJ Eisenstein, DJ Kazin, E McBride, CK Mehta, K Montero-Dorta, AD Padmanabhan, N Prada, F Rubino-Martin, JA Tojeiro, R Xu, X Magana, MV Aubourg, E Bahcall, NA Bailey, S Bizyaev, D Bolton, AS Brewington, H Brinkmann, J Brownstein, JR Gott, JR Hamilton, JC Ho, S Honscheid, K Labatie, A Malanushenko, E Malanushenko, V Maraston, C Muna, D Nichol, RC Oravetz, D Pan, K Ross, NP Roe, NA Reid, BA Schlegel, DJ Shelden, A Schneider, DP Simmons, A Skibba, R Snedden, S Thomas, D Tinker, J Wake, DA Weaver, BA Weinberg, DH White, M Zehavi, I Zhao, G AF Sanchez, Ariel G. Scoccola, C. G. Ross, A. J. Percival, W. Manera, M. Montesano, F. Mazzalay, X. Cuesta, A. J. Eisenstein, D. J. Kazin, E. McBride, C. K. Mehta, K. Montero-Dorta, A. D. Padmanabhan, N. Prada, F. Rubino-Martin, J. A. Tojeiro, R. Xu, X. Magana, M. Vargas Aubourg, E. Bahcall, N. A. Bailey, S. Bizyaev, D. Bolton, A. S. Brewington, H. Brinkmann, J. Brownstein, J. R. Gott, J. Richard, III Hamilton, J. C. Ho, S. Honscheid, K. Labatie, A. Malanushenko, E. Malanushenko, V. Maraston, C. Muna, D. Nichol, R. C. Oravetz, D. Pan, K. Ross, N. P. Roe, N. A. Reid, B. A. Schlegel, D. J. Shelden, A. Schneider, D. P. Simmons, A. Skibba, R. Snedden, S. Thomas, D. Tinker, J. Wake, D. A. Weaver, B. A. Weinberg, David H. White, Martin Zehavi, I. Zhao, G. TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological implications of the large-scale two-point correlation function SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE cosmological parameters; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; PROBE WMAP OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; MICROWAVE BACKGROUND ANISOTROPIES; DARK ENERGY; ACOUSTIC-OSCILLATIONS; POWER-SPECTRUM; REDSHIFT SURVEY; DATA RELEASE AB We obtain constraints on cosmological parameters from the spherically averaged redshift-space correlation function of the CMASS Data Release 9 (DR9) sample of the Baryonic Oscillation Spectroscopic Survey (BOSS). We combine this information with additional data from recent cosmic microwave background (CMB), supernova and baryon acoustic oscillation measurements. Our results show no significant evidence of deviations from the standard flat ? cold dark matter model, whose basic parameters can be specified by Om = 0.285 +/- 0.009, 100?Ob = 4.59 +/- 0.09, ns = 0.961 +/- 0.009, H0 = 69.4 +/- 0.8?km?s-1?Mpc-1 and s8 = 0.80 +/- 0.02. The CMB+CMASS combination sets tight constraints on the curvature of the Universe, with Ok = -0.0043 +/- 0.0049, and the tensor-to-scalar amplitude ratio, for which we find r < 0.16 at the 95?per cent confidence level (CL). These data show a clear signature of a deviation from scale invariance also in the presence of tensor modes, with ns < 1 at the 99.7?per cent CL. We derive constraints on the fraction of massive neutrinos of f? < 0.049 (95?per cent CL), implying a limit of ?m? < 0.51?eV. We find no signature of a deviation from a cosmological constant from the combination of all data sets, with a constraint of wDE = -1.033 +/- 0.073 when this parameter is assumed time-independent, and no evidence of a departure from this value when it is allowed to evolve as wDE(a) = w0 + wa(1 - a). The achieved accuracy on our cosmological constraints is a clear demonstration of the constraining power of current cosmological observations. C1 [Sanchez, Ariel G.; Montesano, F.; Mazzalay, X.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Scoccola, C. G.; Rubino-Martin, J. A.] Inst Astrofis Canarias, Tenerife, Spain. [Scoccola, C. G.; Rubino-Martin, J. A.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Ross, A. J.; Percival, W.; Manera, M.; Tojeiro, R.; Maraston, C.; Nichol, R. C.; Thomas, D.; Zhao, G.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Cuesta, A. J.; Padmanabhan, N.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Eisenstein, D. J.; McBride, C. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kazin, E.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Mehta, K.; Xu, X.; Skibba, R.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Montero-Dorta, A. D.; Prada, F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Prada, F.] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, F.] Univ Autonoma Madrid, Inst Fis Teor, CSIC, E-28049 Madrid, Spain. [Magana, M. Vargas; Aubourg, E.; Hamilton, J. C.; Labatie, A.] Univ Paris Diderot, APC, CNRS, CEA,IRFU,Observ Paris,IN2P3, Sorbonne Paris Cite, France. [Bahcall, N. A.; Gott, J. Richard, III] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08540 USA. [Bailey, S.; Ho, S.; Ross, N. P.; Roe, N. A.; Reid, B. A.; Schlegel, D. J.; White, Martin] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Bizyaev, D.; Brewington, H.; Brinkmann, J.; Malanushenko, E.; Malanushenko, V.; Oravetz, D.; Pan, K.; Simmons, A.; Snedden, S.] Apache Point Observ, Sunspot, NM 88349 USA. [Bolton, A. S.; Brownstein, J. R.; Shelden, A.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Ho, S.] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Honscheid, K.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Muna, D.; Tinker, J.; Weaver, B. A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Schneider, D. P.] Penn State Univ, Dept Phys & Astron, University Pk, PA 16802 USA. [Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Wake, D. A.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Honscheid, K.; Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Zehavi, I.] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Zhao, G.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Sanchez, AG (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. EM arielsan@mpe.mpg.de RI White, Martin/I-3880-2015; OI Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470; White, Martin/0000-0001-9912-5070; Rubino-Martin, Jose Alberto/0000-0001-5289-3021 FU Spanish Ministry of Science and Innovation (MICINN) [AYA2010-21766-C03-02]; UK Science and Technology Facilities Council [ST/I001204/1]; UK Science and Technology Facilities Research Council; Leverhulme Trust; European Research Council; Spanish MICINNs Consolider grant MultiDark [CSD2009-00064]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We would like to thank Ryan Keisler for his help with the implementation of the SPT likelihood code in COSMOMC. We also thank Bradford Benson for helping us find a bug in our modifications to COSMOMC by pointing out a discrepancy between our constraints on the equation of state of dark energy using only CMB data and the reported values by the WMAP team. AGS would like to thank all users of the Pan-STARRS cluster in Garching for their patience and support. CGS and JAR acknowledge funding from project AYA2010-21766-C03-02 of the Spanish Ministry of Science and Innovation (MICINN). AJR is grateful to the UK Science and Technology Facilities Council for financial support through the grant ST/I001204/1. WP is grateful for support from the UK Science and Technology Facilities Research Council, the Leverhulme Trust and the European Research Council. FP acknowledges support from the Spanish MICINNs Consolider grant MultiDark CSD2009-00064. JAR is a Ramon y Cajal fellow of the Spanish Ministry of Science and Innovation (MICINN).; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, The Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, The Ohio State University, The Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 130 TC 100 Z9 101 U1 1 U2 9 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 SEP PY 2012 VL 425 IS 1 BP 415 EP 437 DI 10.1111/j.1365-2966.2012.21502.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300051 ER PT J AU McKernan, B Ford, KES Lyra, W Perets, HB AF McKernan, B. Ford, K. E. S. Lyra, W. Perets, H. B. TI Intermediate mass black holes in AGN discs - I. Production and growth SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion-discs; planets-disc interactions; protoplanetary discs; binaries:close; galaxies: active; galaxies:nuclei ID ACTIVE GALACTIC NUCLEI; X-RAY; PROTOPLANETARY DISKS; ORBITAL MIGRATION; STELLAR REMNANTS; PLANET FORMATION; STAR-FORMATION; ACCRETION; EVOLUTION; BINARY AB Here we propose a mechanism for efficiently growing intermediate mass black holes (IMBH) in discs around supermassive black holes. Stellar mass objects can efficiently agglomerate when facilitated by the gas disc. Stars, compact objects and binaries can migrate, accrete and merge within discs around supermassive black holes. While dynamical heating by cusp stars excites the velocity dispersion of nuclear cluster objects (NCOs) in the disc, gas in the disc damps NCO orbits. If gas damping dominates, NCOs remain in the disc with circularized orbits and large collision cross-sections. IMBH seeds can grow extremely rapidly by collisions with disc NCOs at low relative velocities, allowing for super-Eddington growth rates. Once an IMBH seed has cleared out its feeding zone of disc NCOs, growth of IMBH seeds can become dominated by gas accretion from the active galactic nucleus (AGN) disc. However, the IMBH can migrate in the disc and expand its feeding zone, permitting a super-Eddington accretion rate to continue. Growth of IMBH seeds via NCO collisions is enhanced by a pile-up of migrators. We highlight the remarkable parallel between the growth of IMBH in AGN discs with models of giant planet growth in protoplanetary discs. If an IMBH becomes massive enough it can open a gap in the AGN disc. IMBH migration in AGN discs may stall, allowing them to survive the end of the AGN phase and remain in galactic nuclei. Our proposed mechanisms should be more efficient at growing IMBH in AGN discs than the standard model of IMBH growth in stellar clusters. Dynamical heating of disc NCOs by cusp stars is transferred to the gas in an AGN disc helping to maintain the outer disc against gravitational instability. Model predictions, observational constraints and implications are discussed in a companion paper (Paper II). C1 [McKernan, B.; Ford, K. E. S.] CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. [McKernan, B.; Ford, K. E. S.; Lyra, W.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [McKernan, B.; Ford, K. E. S.] CUNY, Grad Ctr, New York, NY 10016 USA. [Lyra, W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Perets, H. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McKernan, B (reprint author), CUNY, Dept Sci, Borough Manhattan Community Coll, New York, NY 10007 USA. EM bmckernan@amnh.org RI Perets, Hagai/K-9605-2015 OI Perets, Hagai/0000-0002-5004-199X NR 61 TC 16 Z9 16 U1 2 U2 3 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 SEP PY 2012 VL 425 IS 1 BP 460 EP 469 DI 10.1111/j.1365-2966.2012.21486.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300054 ER PT J AU Lusso, E Comastri, A Simmons, BD Mignoli, M Zamorani, G Vignali, C Brusa, M Shankar, F Lutz, D Trump, JR Maiolino, R Gilli, R Bolzonella, M Puccetti, S Salvato, M Impey, CD Civano, F Elvis, M Mainieri, V Silverman, JD Koekemoer, AM Bongiorno, A Merloni, A Berta, S Le Floc'h, E Magnelli, B Pozzi, F Riguccini, L AF Lusso, E. Comastri, A. Simmons, B. D. Mignoli, M. Zamorani, G. Vignali, C. Brusa, M. Shankar, F. Lutz, D. Trump, J. R. Maiolino, R. Gilli, R. Bolzonella, M. Puccetti, S. Salvato, M. Impey, C. D. Civano, F. Elvis, M. Mainieri, V. Silverman, J. D. Koekemoer, A. M. Bongiorno, A. Merloni, A. Berta, S. Le Floc'h, E. Magnelli, B. Pozzi, F. Riguccini, L. TI Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; galaxies: active; galaxies: evolution; quasars: general ID SUPERMASSIVE BLACK-HOLES; SPECTRAL ENERGY-DISTRIBUTIONS; DIGITAL SKY SURVEY; WIDE-FIELD SURVEY; STELLAR POPULATION SYNTHESIS; STAR-FORMING GALAXIES; HOST GALAXIES; ACCRETION RATE; HELLAS2XMM SURVEY; MASS FUNCTION AB Bolometric luminosities and Eddington ratios of both X-ray selected broad-line (Type-1) and narrow-line (Type-2) active galactic nuclei (AGN) from the XMMNewton survey in the Cosmic Evolution Survey field are presented. The sample is composed of 929 AGN (382 Type-1 AGN and 547 Type-2 AGN) and it covers a wide range of redshifts, X-ray luminosities and absorbing column densities. About 65?per cent of the sources are spectroscopically identified as either Type-1 or Type-2 AGN (83 and 52?per cent, respectively), while accurate photometric redshifts are available for the rest of the sample. The study of such a large sample of X-ray selected AGN with a high-quality multiwavelength coverage from the far-infrared (now with the inclusion of Herschel data at 100 and 160 mu m) to the opticalultraviolet allows us to obtain accurate estimates of bolometric luminosities, bolometric corrections and Eddington ratios. The kbol - Lbol relations derived in this work are calibrated for the first time against a sizable AGN sample, and rely on observed redshifts, X-ray luminosities and column density distributions. We find that kbol is significantly lower at high Lbol with respect to previous estimates by Marconi et al. and Hopkins et al. Black hole (BH) masses and Eddington ratios are available for 170 Type-1 AGN, while BH masses for Type-2 AGN are computed for 481 objects using the BH massstellar mass relation and the morphological information. We confirm a trend between kbol and ?Edd, with lower hard X-ray bolometric corrections at lower Eddington ratios for both Type-1 and Type-2 AGN. We find that, on average, the Eddington ratio increases with redshift for all types of AGN at any given MBH, while no clear evolution with redshift is seen at any given Lbol. C1 [Lusso, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lusso, E.; Comastri, A.; Mignoli, M.; Zamorani, G.; Vignali, C.; Gilli, R.; Bolzonella, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Simmons, B. D.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Simmons, B. D.] Yale Univ, Yale Ctr Astron & Astrophys, Dept Phys, New Haven, CT 06511 USA. [Vignali, C.; Pozzi, F.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Brusa, M.; Lutz, D.; Salvato, M.; Merloni, A.; Berta, S.; Magnelli, B.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Shankar, F.] Univ Paris Diderot, GEPI, Observ Paris, CNRS, F-92195 Meudon, France. [Trump, J. R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Maiolino, R.; Bongiorno, A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, RM, Italy. [Maiolino, R.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Salvato, M.; Merloni, A.] Max Planck Inst Plasma Phys & Excellence Cluster, D-85748 Garching, Germany. [Impey, C. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mainieri, V.] ESO, D-85748 Garching, Germany. [Silverman, J. D.] Univ Tokyo, IPMU, Chiba 2778568, Japan. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Le Floc'h, E.; Riguccini, L.] Univ Paris Diderot, Lab AIM, CEA, DSM,CNRS,IRFU,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. RP Lusso, E (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM lusso@mpia.de RI Vignali, Cristian/J-4974-2012; Mignoli, Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Vignali, Cristian/0000-0002-8853-9611; Mignoli, Marco/0000-0002-9087-2835; Bolzonella, Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Bongiorno, Angela/0000-0002-0101-6624; Puccetti, Simonetta/0000-0002-2734-7835; Koekemoer, Anton/0000-0002-6610-2048; Zamorani, Giovanni/0000-0002-2318-301X; Simmons, Brooke/0000-0001-5882-3323; Brusa, Marcella/0000-0002-5059-6848 FU ASI-INAF [I/009/10/0, I/088/06, ASI/COFIS/WP3110 I/026/07/0]; Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt; Max Planck Society; German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize [FKZ HA1850/28-1]; Marie Curie grant FX In Italy, the XMM-COSMOS project is supported by ASI-INAF grants I/009/10/0, I/088/06 and ASI/COFIS/WP3110 I/026/07/0. In Germany, the XMM-Newton project is supported by the Bundesministerium fur Wirtshaft und Techologie/Deutsches Zentrum fur Luft und Raumfahrt and the Max Planck Society. MS acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA1850/28-1). FS acknowledges support from a Marie Curie grant. The authors acknowledge the anonymous reviewer who provided many useful suggestions for improving the paper. The entire COSMOS collaboration is gratefully acknowledged. NR 91 TC 84 Z9 84 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2012 VL 425 IS 1 BP 623 EP 640 DI 10.1111/j.1365-2966.2012.21513.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300066 ER PT J AU Shetty, R Beaumont, CN Burton, MG Kelly, BC Klessen, RS AF Shetty, Rahul Beaumont, Christopher N. Burton, Michael G. Kelly, Brandon C. Klessen, Ralf S. TI The linewidth-size relationship in the dense interstellar medium of the Central Molecular Zone SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; stars: formation; ISM: clouds; ISM: molecules; ISM: structure ID THERMAL/DYNAMICAL EQUILIBRIUM-MODEL; MULTIPHASE GALACTIC DISKS; STAR-FORMATION RATES; MILKY-WAY; MASS-SIZE; STATISTICAL PROPERTIES; STARBURST REGULATION; VELOCITY STRUCTURE; NEARBY GALAXIES; CLOUD MODELS AB The linewidthsize (sR) relationship of the interstellar medium (ISM) has been extensively measured and analysed, in both the local ISM and in nearby normal galaxies. Generally, a power law describes the relationship well with an index ranging from 0.2 to 0.6, and is now referred to as one of the Larson's Relationships. The nature of turbulence and star formation is considered to be intimately related to these relationships, so evaluating the sR correlations in various environments is important for developing a comprehensive understanding of the ISM. We measure the linewidthsize relationship in the Central Molecular Zone (CMZ) of the Galactic Centre using spectral line observations of the high-density tracers N2H+, HCN, H13CN and HCO+. We construct dendrograms, which map the hierarchical nature of the positionpositionvelocity (PPV) data, and compute the linewidths and sizes of the dendrogram-defined structures. The dispersions range from similar to 2 to 30 km s-1 in structures spanning sizes 240 pc. By performing Bayesian inference, we show that a power law with exponent 0.31.1 can reasonably describe the sR trend. We demonstrate that the derived sR relationship is independent of the locations in the PPV data set where s and R are measured. The uniformity in the sR relationship indicates that turbulence in the CMZ is driven on the large scales beyond greater than or similar to 30 pc. We compare the CMZ sR relationship to that measured in the Galactic molecular cloud Perseus. The exponents between the two systems are similar, suggestive of a connection between the turbulent properties within a cloud to its ambient medium. Yet, the velocity dispersion in the CMZ is systematically higher, resulting in a scaling coefficient that is approximately five times larger. The systematic enhancement of turbulent velocities may be due to the combined effects of increased star formation activity, larger densities and higher pressures relative to the local ISM. C1 [Shetty, Rahul; Klessen, Ralf S.] Univ Heidelberg, Zentrum Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [Beaumont, Christopher N.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Beaumont, Christopher N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burton, Michael G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Kelly, Brandon C.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. RP Shetty, R (reprint author), Univ Heidelberg, Zentrum Astron, Inst Theoret Astrophys, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. EM r.shetty@uni-heidelberg.de OI Burton, Michael/0000-0001-7289-1998 FU Deutsche Forschungsgemeinschaft (DFG) [SFB 881, SPP 1573]; Australian Research Council [DP0879202] FX We are very grateful to Paul Jones for leading the effort in producing the Mopra CMZ data sets. We also thank Erik Bertram, Paul Clark, Roland Crocker, Jonathan Foster, Simon Glover, Mark Heyer, David Jones, Nicholas Kevlahan, Lukas Konstandin, Volker Ossenkopf, Eve Ostriker and Farhad Yusef-Zadeh for informative discussions regarding the GC, turbulence and the linewidth-size relationship. This paper improved from constructive comments by an anonymous referee. We acknowledge the use of NEMO software (Teuben 1995) to carry out parts of our analysis. RS and RSK acknowledge support from the Deutsche Forschungsgemeinschaft (DFG) via the SFB 881 (B1 and B2) 'The Milky Way System', and the SPP (priority program) 1573, 'Physics of the ISM'. MGB is supported by the Australian Research Council for Discovery Project grant DP0879202. NR 50 TC 42 Z9 42 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 SEP PY 2012 VL 425 IS 1 BP 720 EP 729 DI 10.1111/j.1365-2966.2012.21588.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300072 ER PT J AU Genel, S Dekel, A Cacciato, M AF Genel, Shy Dekel, Avishai Cacciato, Marcello TI On the effect of cosmological inflow on turbulence and instability in galactic discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE methods: analytical; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: kinematics and dynamics; galaxies: star formation ID STAR-FORMING GALAXIES; SIMILAR-TO 2; ACCRETION-DRIVEN TURBULENCE; INTEGRAL FIELD SPECTROSCOPY; DARK-MATTER HALOES; HIGH-REDSHIFT; INTERSTELLAR-MEDIUM; MASSIVE GALAXIES; ANGULAR-MOMENTUM; COLD STREAMS AB We analyse the evolution of turbulence and gravitational instability of a galactic disc in a quasi-steady state governed by cosmological inflow. We focus on the possibility that the coupling between the in-streaming gas and the disc is maximal, e.g. via dense clumps, and ask whether the streams could be the driver of turbulence in an unstable disc with a Toomre parameter Q similar to 1. Our fiducial model assumes an efficiency of similar to 0.5 per dynamical time for the decay of turbulence energy, and similar to 0.02 for each of the processes that depletes the disc gas, i.e. star formation, outflow and inflow within the disc into a central bulge. In this case, the in-streaming drives a ratio of turbulent to rotation velocity s/V similar to 0.20.3, which at z similar to 2 induces an instability with Q similar to 1, both as observed. However, in conflict with observations, this model predicts that s/V remains constant with time, independent of the cosmological accretion rate, because mass and turbulence have the same external source. Such strongly coupled cosmological inflow tends to stabilize the disc at low z, with Q similar to a few, which may be consistent with observations. The instability could instead be maintained for longer, with a properly declining s/V, if it is self-regulated to oscillations about Q similar to 1 by a duty cycle for disc depletion. However, the off phases of this duty cycle become long at low z, which may be hard to reconcile with observations. Alternatively, the coupling between the in-streaming gas and the disc may weaken in time, reflecting an evolving nature of the accretion. If, instead, that coupling is weak at all times, the likely energy source for self-regulated stirring up of the turbulence is the inflow within the disc down the potential gradient (studied in a companion paper). C1 [Genel, Shy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Genel, Shy] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Dekel, Avishai; Cacciato, Marcello] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel. RP Genel, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sgenel@cfa.harvard.edu OI Genel, Shy/0000-0002-3185-1540 FU ISF [6/08]; GIF [G-1052-104.7/2009]; DIP; NSF at UCSC [AST-1010033]; Minerva fellowship (Max-Planck Gesellschaft) FX We acknowledge stimulating discussions with Nicolas Bouche, Andreas Burkert, John Forbes, Mark Krumholz, Amiel Sternberg and Romain Teyssier. This work has been supported by the ISF through grant 6/08, by GIF through grant G-1052-104.7/2009, by a DIP grant and by an NSF grant AST-1010033 at UCSC. MC has been supported at HU by a Minerva fellowship (Max-Planck Gesellschaft). NR 101 TC 24 Z9 24 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 SEP PY 2012 VL 425 IS 1 BP 788 EP 800 DI 10.1111/j.1365-2966.2012.21652.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300078 ER PT J AU Pan, T Loeb, A AF Pan, Tony Loeb, Abraham TI Identifying stars of mass > 150 M-circle dot from their eclipse by a binary companion SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: general; galaxies: star clusters: general ID BLACK-HOLES; LOSS RATES; CLUSTERS; EVOLUTION; RUNAWAY; PARAMETERS; SUPERNOVAE; EXPLOSION; NEBULA; RADII AB We examine the possibility that very massive stars greatly exceeding the commonly adopted stellar mass limit of 150 M? may be present in young star clusters in the local universe. We identify 10 candidate clusters, some of which may host stars with masses up to 600 M? formed via runaway collisions. We estimate the probabilities of these very massive stars being in eclipsing binaries to be ?30 per cent. Although most of these systems cannot be resolved at present, their transits can be detected at distances of 3 Mpc even under the contamination of the background cluster light, due to the large associated luminosities similar to 107 L? and mean transit depths of similar to 106 L?. Discovery of very massive eclipsing binaries would flag possible progenitors of pair-instability supernovae and intermediate-mass black holes. C1 [Pan, Tony; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pan, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM span@physics.harvard.edu FU Hertz Foundation; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We thank Paul Crowther, Dave Latham, Philip Myers, Guillermo Torres and Simon Portegies Zwart for helpful discussions. We thank Eran Ofek for his eclipsing binary scripts, 3 which we built upon to generate our example light curves. TP was supported by the Hertz Foundation. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 43 TC 1 Z9 1 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 SEP PY 2012 VL 425 IS 1 BP L91 EP L95 DI 10.1111/j.1745-3933.2012.01308.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993VG UT WOS:000307887300029 ER PT J AU Wilting, A Sollmann, R Meijaard, E Helgen, KM Fickel, J AF Wilting, Andreas Sollmann, Rahel Meijaard, Erik Helgen, Kristofer M. Fickel, Joerns TI Mentawai's endemic, relictual fauna: is it evidence for Pleistocene extinctions on Sumatra? SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Biogeography; extinction; immigration; mammals; palaeoclimate; Southeast Asia; Sunda Shelf; Toba volcanic eruption ID LAST GLACIAL PERIOD; SOUTHEAST-ASIA; MOLECULAR PHYLOGENY; EVOLUTIONARY HISTORY; CLIMATIC-CHANGE; SUPER-ERUPTION; RAIN-FORESTS; SUNDA SHELF; PALM CIVETS; BIOGEOGRAPHY AB Aim The four Mentawai islands, south-west of Sumatra, have long been isolated from the remainder of Sundaland, resulting in a high level of endemism. We examined the distribution of 151 species of the Mentawai Islands in Sundaland and assessed various processes that may have resulted in the various biogeographical patterns. Location Southeast Asia, particularly the Mentawai Islands and nearby large landmasses (Sumatra, Java, Borneo and Peninsular Malaysia). Methods We compared the faunal composition of the Mentawai Islands for selected taxa (43 mammals, 92 reptiles and 16 amphibians) with that of the four nearby large landmasses of Sundaland using morphological comparisons and the most recent molecular phylogenetic analyses available in the literature. These comparisons yielded sister taxa, which were used to simulate species absence data for the four Sundaland landmasses under several scenarios to investigate how patterns of species absence could have arisen. Results In contrast to our expectations, several Mentawai species did not have their closest relatives on neighbouring Sumatra, but rather on the more distant Borneo, Java or Peninsular Malaysia. For mammals, the similarity between species from Mentawai and Borneo was greater than that observed between species from Mentawai and Sumatra. We conclude that the relationships represent traces of species historically distributed throughout Sundaland that became extinct in Sumatra during the Pleistocene. For reptiles and amphibians the observed pattern of species absences generally resembled the simulated pattern expected under the scenario of absence rates increasing with landmass isolation, whereas for mammals we observed more species than expected missing from Java and Sumatra, and fewer than expected from Borneo. Main conclusions The potential extinctions on Sumatra probably had two causes: changes of climate and vegetation during the Pleistocene and environmental impacts from the Toba supervolcanic eruption. C1 [Wilting, Andreas] Leibniz Inst Zoo & Wildlife Res, Dept Evolutionary Genet, D-10315 Berlin, Germany. [Sollmann, Rahel] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Meijaard, Erik] People & Nat Consulting Int, Badung, Bali, Indonesia. [Meijaard, Erik] Australian Natl Univ, Fac Arts, Sch Archaeol & Anthropol, Canberra, ACT 0200, Australia. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Wilting, A (reprint author), Leibniz Inst Zoo & Wildlife Res, Dept Evolutionary Genet, Alfred Kowalke Str 17, D-10315 Berlin, Germany. EM a.wilting@gmx.de RI Meijaard, Erik/A-2687-2016 OI Meijaard, Erik/0000-0001-8685-3685 FU Deutsche Forschungsgemeinschaft [FI 698/5-1] FX We thank Lawrence R. Heaney, Jacob A. Esselstyn and the anonymous referee for their valuable comments and suggestions on earlier drafts of this paper. We also thank Kathleen Rollig for the design of the animal icons in Fig. 2 and Frank Tillack for providing information on the distribution of amphibians and reptiles in the Sunda Shelf. This study was supported by the Deutsche Forschungsgemeinschaft (Grant FI 698/5-1). Study of museum specimens was facilitated by staff at the National Museum of Natural History, Smithsonian Institution (Washington); the American Museum of Natural History (New York); the Museum fur Naturkunde, Humboldt University (Berlin); and the Natural History Museum (London). NR 72 TC 22 Z9 23 U1 5 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 EI 1365-2699 J9 J BIOGEOGR JI J. Biogeogr. PD SEP PY 2012 VL 39 IS 9 BP 1608 EP 1620 DI 10.1111/j.1365-2699.2012.02717.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 989LT UT WOS:000307562200006 ER PT J AU Dalling, JW Schnitzer, SA Baldeck, C Harms, KE John, R Mangan, SA Lobo, E Yavitt, JB Hubbell, SP AF Dalling, James W. Schnitzer, Stefan A. Baldeck, Claire Harms, Kyle E. John, Robert Mangan, Scott A. Lobo, Elena Yavitt, Joseph B. Hubbell, Stephen P. TI Resource-based habitat associations in a neotropical liana community SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; canopy disturbance; determinants of plant community diversity and structure; habitat association; liana community; light detection and ranging; soil resources; topography; treefall gap ID BARRO-COLORADO ISLAND; TROPICAL RAIN-FORESTS; LONG-TERM PLOTS; DROUGHT SENSITIVITY; TREE REGENERATION; LOWLAND FOREST; NATIONAL-PARK; PATTERNS; DIVERSITY; PANAMA AB 1. Lianas are a conspicuous element of many tropical forests, accounting for up to 40% of woody stem density and 20% of species richness in seasonal forests. However, lianas have seldom been surveyed at sufficiently large spatial scales to allow an assessment of the importance of habitat variables in structuring liana communities. 2. We compare the association patterns of 82 liana species and an equivalent sample of tree species on the 50 ha Forest Dynamics Project plot on Barro Colorado Island, Panama, with topographic habitat variables (high and low plateau, slope, swamp and streamside), and thirteen mapped soil chemical variables. In addition, we test for liana species associations with canopy disturbance using a canopy height map of the plot generated using light detection and ranging. 3. For all liana species combined, densities differed among topographic habitat types in the plot, with significantly higher densities on the seasonally drier lower plateau habitat (1044 individuals ha-1) than the moister slope habitat (729 individuals ha-1). Lianas were also significantly more abundant than expected in areas with low canopy height. 4. The proportion of liana species associated with one or more topographic habitat variables (44%) was significantly lower than that for trees (66%). Similarly, liana species were significantly less frequently associated with PC axes derived from soil chemical variables (21%) than trees (52%). The majority of liana species (63%) were significantly associated with areas of the plot with low canopy height reflecting an affinity for treefall gaps. 5. Synthesis. The habitat associations detected here suggest that liana density is associated primarily with canopy disturbance, and to a lesser extent with topography and soil chemistry. Relative to trees, few liana species were associated with local variation in topography and soil chemistry, suggesting that nutrient availability exerts only weak effects on liana community composition compared to trees. Results from this study support the contention that increases in forest disturbance rates are a driver of recently observed increases in liana abundance and biomass in neotropical forests. C1 [Dalling, James W.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [Dalling, James W.; Schnitzer, Stefan A.; Harms, Kyle E.; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Unit 0948, DPO AA, Miami, FL 34002 USA. [Schnitzer, Stefan A.; Mangan, Scott A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Baldeck, Claire; Lobo, Elena] Univ Illinois, Program Ecol Evolut & Conservat Biol, Urbana, IL 61801 USA. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [John, Robert] Indian Inst Sci Educ & Res Kolkata, Mohanpur 741252, W Bengal, India. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. RP Dalling, JW (reprint author), Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. EM dallingj@life.uiuc.edu OI Schnitzer, Stefan/0000-0002-2715-9455 FU Smithsonian Tropical Research Institute; National Science Foundation [DEB021104, 021115, 0212284, 0212818, DEB0939907, DEB0613666] FX We gratefully acknowledge financial and logistic support from the Smithsonian Tropical Research Institute and the National Science Foundation for grants DEB021104, 021115, 0212284 and 0212818 supporting soils mapping in the BCI plot, DEB0939907 for LiDAR data collection and DEB0613666 for the liana census. We thank Alicia Ledo for assistance with preparing Fig. 1. Additional support was provided to EL and CB from the Program in Ecology and Evolutionary Biology, University of Illinois. NR 67 TC 40 Z9 40 U1 1 U2 58 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD SEP PY 2012 VL 100 IS 5 BP 1174 EP 1182 DI 10.1111/j.1365-2745.2012.01989.x PG 9 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 989IU UT WOS:000307554300013 ER PT J AU Sedio, BE Wright, SJ Dick, CW AF Sedio, Brian E. Joseph Wright, S. Dick, Christopher W. TI Trait evolution and the coexistence of a species swarm in the tropical forest understorey SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; community assembly; determinants of plant community diversity and structure; phylogenetic community structure; phylogenetic signal; Psychotria ID BELOW-GROUND COMPETITION; RAIN-FOREST; TREE SEEDLINGS; HISTORICAL BIOGEOGRAPHY; INTERSPECIFIC VARIATION; PHYLOGENETIC SIGNAL; PLANT DIVERSITY; SEED DISPERSAL; SPATIAL SCALES; COMMUNITIES AB 1. A small number of species-rich plant genera make a substantial contribution to the a diversity of tropical forests. These species swarms (Gentry 1982) challenge a view of community assembly that maintains that niche overlap, and hence, the likelihood of competitive exclusion should increase with phylogenetic affinity. Related species may, however, occupy different microhabitats within a forest stand or, alternatively, differ ecologically in ways that allow them to coexist syntopically. 2. To explore the relationship between phylogenetic history and niche differentiation among sympatric, congeneric species, we performed phylogenetic analyses of microhabitat preferences, photosynthetic and hydraulic traits, and experimental responses to light and water availability for 20 species of Psychotria (Rubiaceae) from Barro Colorado Island (BCI), Panama. 3. The Psychotria present in small (3-m radius), circular plots were more closely related than expected by chance. Photosynthetic and hydraulic traits were both associated with species habitat distributions, but only hydraulic traits were conserved phylogenetically. Experimental responses to water availability were also conserved phylogenetically. Functional trait analyses revealed little or no evidence of niche partitioning within sites. 4. We conclude that Psychotria species responses to both light and moisture availability determine their microhabitat distributions on BCI and that evolutionarily conserved hydraulic traits lead to phylogenetic clustering of co-occurring species. 5. Synthesis. The evolutionary conservation of hydraulic traits related to soil moisture tolerance largely explains phylogenetic clustering in the local assembly of the hyperdiverse genus Psychotria. We suggest that close relatives are unlikely to exclude one another from shared habitats because resource availability is determined largely by asymmetric competition with the overstorey, rather than by competition with neighbouring understorey plants. In light of the recent biogeographic admixture in central Panama, the phylogenetic niche conservatism exhibited by Psychotria on BCI raises the possibility of an association between local microhabitats and the ancestral climatic regimes under which major Psychotria lineages evolved before arriving in sympatry. C1 [Sedio, Brian E.; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Joseph Wright, S.; Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sedio, BE (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 830 N Univ, Ann Arbor, MI 48109 USA. EM bsedio@umich.edu RI Dick, Christopher/A-8744-2008; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Andrew W. Mellon Foundation; University of Michigan Matthei Botanical Gardens Research Endowment Award; Angeline B. Whittier Fellowship in Plant Biology; NSF Graduate Research Fellowship; NSF [DEB 064039] FX We thank Milton Garcia, Mirna Samaniego and Blake Hodgin for their assistance. Funding was provided by the Andrew W. Mellon Foundation to S.J.W. and by the University of Michigan Matthei Botanical Gardens Research Endowment Award, the Angeline B. Whittier Fellowship in Plant Biology, and an NSF Graduate Research Fellowship to B. E. S. We thank Nathan Kraft for valuable discussion and Egbert Leigh, William Cornwell, Timothy Paine and two anonymous referees for comments that improved the manuscript. C. W. D. acknowledges support from NSF award DEB 064039. NR 81 TC 19 Z9 19 U1 3 U2 80 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD SEP PY 2012 VL 100 IS 5 BP 1183 EP 1193 DI 10.1111/j.1365-2745.2012.01993.x PG 11 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 989IU UT WOS:000307554300014 ER PT J AU O'Dea, A Hoyos, N Rodriguez, F Degracia, B De Gracia, C AF O'Dea, Aaron Hoyos, Natalia Rodriguez, Felix Degracia, Brigida De Gracia, Carlos TI History of upwelling in the Tropical Eastern Pacific and the paleogeography of the Isthmus of Panama SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE zs-MART; Communities; Paleoelevation; Paleoaltitude ID BOCAS-DEL-TORO; AMERICAN BIOTIC INTERCHANGE; ZOOID SIZE; SOUTH-AMERICA; THERMOHALINE CIRCULATION; CHEILOSTOME BRYOZOANS; CARIBBEAN NEOGENE; FAUNAL TURNOVER; WESTERN PANAMA; MARINE RECORD AB Today there is a tight-knit relationship between the elevation of the Central American Isthmus and the oceanographic conditions of the Tropical Eastern Pacific. Where the elevation drops below 500 m low-level wind jets pass seasonally from the Atlantic to the Pacific driving coastal upwelling in the Tropical Eastern Pacific. This paper determines if seasonal upwelling was present in five Pliocene and Pleistocene fossiliferous sites on the Pacific coast of the Burica region of the Isthmus of Panama using two independent approaches that compare bryozoan morphology and whole community composition of fossiliferous localities with material from upwelling and non-upwelling modem localities. No definitive evidence of seasonal upwelling exists in the Pliocene, implying non-analogous oceanographic conditions because of continued interoceanic connection prior to the closure of the Isthmus of Panama. Conversely, data from three mid-Pleistocene sites reveal robust evidence of strong seasonal upwelling suggesting that the elevation of the Isthmus must have been sufficiently low to permit wind-jets to form. A low-elevation Isthmus of Panama may have persisted until as recently as the mid-Pleistocene. (C) 2012 Elsevier B.V. All rights reserved. C1 [O'Dea, Aaron; Hoyos, Natalia; Rodriguez, Felix; Degracia, Brigida; De Gracia, Carlos] Smithsonian Trop Res Inst, Balboa, Panama. RP O'Dea, A (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Panama. EM aaronodea@yahoo.com RI O'Dea, Aaron/D-4114-2011; OI De Gracia, Carlos/0000-0003-0637-3302 FU National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT); National Science Foundation [EAR03-45471]; National Geographic Society FX This research was supported financially by the National System of Investigators (SNI) of the National Research of the National Secretariat for Science, Technology and Innovation of Panama (SENACYT) to AO, the National Science Foundation (EAR03-45471) and the National Geographic Society. Recursos Minerales granted collecting permits. We would like to thank Ethan Grossman, Beth Okamura, John Robbins, Paul Taylor and Andrew Ugan for their tremendous efforts collecting material in the field. Yadixa del Valle processed a lot of the material. Celideth DeLeon, Mercedes Arosemena, and Alejandro Arze gave first class logistical support to the project. Discussion over the years with Luis D'Croz, Jeremy Jackson and Anthony Coates were particularly insightful. Beth Okamura, Ethan Grossman, David Farris and Marcus Key gave thoughtful comments on the manuscript. NR 98 TC 19 Z9 20 U1 1 U2 31 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD SEP 1 PY 2012 VL 348 BP 59 EP 66 DI 10.1016/j.palaeo.2012.06.007 PG 8 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 990ER UT WOS:000307614300006 ER PT J AU Castillo, RF Ubelaker, DH Djorojevic, M AF Fernandez Castillo, Rafael Ubelaker, Douglas H. Djorojevic, Mirjana TI Age estimation through histological study of trabecular volume and cortical bone width of the iliac crest SO SCIENCE & JUSTICE LA English DT Article DE Bone histomorphometry; Age at death; Trabecular bone; Cortical width ID MICROSCOPIC DETERMINATION; DEATH; IMPACT; RIB AB There have been many methods proposed to estimate the age of human bones in forensic medicine or in forensic anthropology, including those that assess histological structures. In this study, age was evaluated through the histomorphometric study of trabecular volume and cortical width of the right iliac crest. A total of 25 samples A total of 66 samples (42 male and 24 female) were obtained from necropsies of judicial cases, with ages ranging from 13 to 58 years, who had died a sudden or violent death. The samples were obtained using Bordier's trocar for bone biopsy, in a period not exceeding 24 h after death. The samples were examined without decalcification, with 96 degrees alcohol dehydration, embedding in methyl methacrylate, and sectioned with a microtome Reichert (3 mu m). The sections were fixed on microscope slides and stained using toluidine blue, Goldner trichrome and hematoxylin-eosin methods. The samples were studied under a Leica DM LB microscope and the images were digitally captured. The digital images were processed using an image analysis program and data were analyzed using the SPSS statistical package. The results demonstrated that the combination of the trabecular volume and cortical width acted as predictors of the age in subjects which did not suffer from any deterioration of bone and/or mineral metabolism. (C) 2011 Forensic Science Society. Published by Elsevier Ireland Ltd. All rights reserved. C1 [Fernandez Castillo, Rafael] Univ Granada, Phys Anthropol Dept, Fac Med, Lab Anthropol, E-18071 Granada, Spain. [Ubelaker, Douglas H.] Natl Museum Nat Hist, Dept Anthropol, Smithsonian Inst, Washington, DC 20560 USA. RP Castillo, RF (reprint author), Univ Granada, Phys Anthropol Dept, Fac Med, Lab Anthropol, Avda Madrid S-N, E-18071 Granada, Spain. EM rafaelfernandez@ugr.es; ubelaked@si.edu; dmiriana@yahoo.com RI Castillo, Rafael/H-2178-2013 OI Castillo, Rafael/0000-0002-1814-5254 NR 21 TC 3 Z9 3 U1 1 U2 37 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 1355-0306 J9 SCI JUSTICE JI Sci. Justice PD SEP PY 2012 VL 52 IS 3 BP 177 EP 180 DI 10.1016/j.scijus.2011.09.004 PG 4 WC Medicine, Legal; Pathology SC Legal Medicine; Pathology GA 990FE UT WOS:000307615600007 PM 22841141 ER PT J AU Studds, CE McFarland, KP Aubry, Y Rimmer, CC Hobson, KA Marra, PP Wassenaar, LI AF Studds, Colin E. McFarland, Kent P. Aubry, Yves Rimmer, Christopher C. Hobson, Keith A. Marra, Peter P. Wassenaar, Leonard I. TI Stable-hydrogen isotope measures of natal dispersal reflect observed population declines in a threatened migratory songbird SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Bicknell's thrush; conservation biogeography; dispersal; movement ecology; Neotropical-Nearctic migratory bird; population declines; stable isotopes ID LONG-DISTANCE DISPERSAL; THRUSH CATHARUS-BICKNELLI; INDIVIDUAL BEHAVIOR; BREEDING DISPERSAL; MONTANE FORESTS; CLIMATE-CHANGE; NORTH-AMERICA; BIRDS; ABUNDANCE; CONNECTIVITY AB Aim Measuring dispersal is crucial for estimating demographic rates that inform conservation plans for rare and threatened species. We evaluated natal dispersal patterns in Bicknell's thrush (Catharus bicknelli) across most of the breeding range using a 10-year data set of stable-hydrogen isotope ratios in feathers (d2HF) grown on the natal area and sampled 1 year later at the first breeding site. Location North-eastern United States and south-eastern Canada. Methods We used d2HF values of adult thrushes sampled at 25 breeding sites as prior information for assigning first-time breeders to their natal site. We calculated the minimum distance birds moved from their natal to first breeding site and fit these data to three statistical distributions for characterizing the importance of long-distance dispersal: the exponential, Weibull and half-Cauchy. Finally, we assessed differences in the probability of dispersal across the breeding range and through time to understand spatio-temporal variation in demographic connectivity. Results The d2HF values of first-time breeders were lower compared with those of adults, a difference that was greater at the southern compared with northern breeding range extreme. Assignment tests accounting for age differences in d2HF suggested that most birds dispersed < 200 km from their natal area and within the centre of the breeding range, whereas comparatively few individuals dispersed up to 700 km. A Weibull distribution provided the best fit to these data. Two of three corrections for age differences in d2HF indicated that natal dispersal probability declined by 3038% from 1996 to 2005. Main conclusions Our findings suggest that estimating natal dispersal with d2HF measurements may contribute to understanding the resilience of geographically isolated Bicknell's thrush populations. Declining natal dispersal may be symptomatic of observed population declines and could compound this trend by limiting demographic exchange between habitat patches predicted to be increasingly isolated by natural and anthropogenic habitat changes. C1 [Studds, Colin E.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. [McFarland, Kent P.; Rimmer, Christopher C.] Vermont Ctr Ecostudies, Norwich, VT 05055 USA. [Aubry, Yves] Environm Canada, Quebec City, PQ G1J 0C3, Canada. [Hobson, Keith A.; Wassenaar, Leonard I.] Environm Canada, Saskatoon, SK S7N 3H5, Canada. RP Studds, CE (reprint author), Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. EM c.studds@uq.edu.au RI Wassenaar, Leonard/B-5996-2013; Studds, Colin/C-3701-2012; OI Wassenaar, Leonard/0000-0001-5532-0771 FU Conservation and Research Foundation; Davis Conservation Foundation; Frank and Brinna Sands Foundation; National Fish and Wildlife Foundation; Nature Conservancy; Nuttall Ornithological Club; Philanthropic Collaborative; Stratton Foundation; Stratton Mountain Resort; Thomas Marshall Foundation; Wallace Genetic Foundation; State Wildlife Grant through the Vermont Fish and Wildlife Department; Vermont Monitoring Cooperative; USDA Forest Service Northeastern Research Station; U.S. Fish and Wildlife Service; William P. Wharton Trust; Vermont Center for Ecostudies; Vermont Institute of Natural Science; Environment Canada FX We are grateful to the many field biologists who dedicated countless hours of fieldwork. We also thank the Stratton Mountain Resort, the Mt. Mansfield Company, the East Haven Development Company, the Essex Timber Company, the Foret Habitee du Mont Gosford and the Societe des Etablissements de Plein-Air du Quebec for valuable logistic support. Funding was provided by the Conservation and Research Foundation, the Davis Conservation Foundation, the Frank and Brinna Sands Foundation, the National Fish and Wildlife Foundation, The Nature Conservancy, the Nuttall Ornithological Club, the Philanthropic Collaborative, the Stratton Foundation, the Stratton Mountain Resort, the Thomas Marshall Foundation, the Wallace Genetic Foundation, a State Wildlife Grant through the Vermont Fish and Wildlife Department, the Vermont Monitoring Cooperative, USDA Forest Service Northeastern Research Station, U.S. Fish and Wildlife Service, the William P. Wharton Trust, friends of the Vermont Center for Ecostudies and the Vermont Institute of Natural Science, and Environment Canada. NR 70 TC 20 Z9 20 U1 0 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD SEP PY 2012 VL 18 IS 9 BP 919 EP 930 DI 10.1111/j.1472-4642.2012.00931.x PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 987AU UT WOS:000307389600007 ER PT J AU Null, KA Dimova, NT Knee, KL Esser, BK Swarzenski, PW Singleton, MJ Stacey, M Paytan, A AF Null, Kimberly A. Dimova, Natasha T. Knee, Karen L. Esser, Bradley K. Swarzenski, Peter W. Singleton, Michael J. Stacey, Mark Paytan, Adina TI Submarine Groundwater Discharge-Derived Nutrient Loads to San Francisco Bay: Implications to Future Ecosystem Changes SO ESTUARIES AND COASTS LA English DT Article DE Submarine groundwater discharge; Radium; Radon; Estuaries; Nutrient loading; San Francisco Bay ID DELAYED COINCIDENCE COUNTER; RADIUM ISOTOPES; SUBTERRANEAN ESTUARY; COASTAL ZONE; PHYTOPLANKTON BLOOMS; MIXING PROCESSES; SEDIMENT-WATER; SEA-WATER; DYNAMICS; NITROGEN AB Submarine groundwater discharge (SGD) was quantified at select sites in San Francisco Bay (SFB) from radium (Ra-223 and Ra-224) and radon (Rn-222) activities measured in groundwater and surface water using simple mass balance box models. Based on these models, discharge rates in South and Central Bays were 0.3-7.4 m(3) day(-1) m(-1). Although SGD fluxes at the two regions (Central and South Bays) of SFB were of the same order of magnitude, the dissolved inorganic nitrogen (DIN) species associated with SGD were different. In the South Bay, ammonium (NH (4) (+) ) concentrations in groundwater were three-fold higher than in open bay waters, and NH (4) (+) was the primary DIN form discharged by SGD. At the Central Bay site, the primary DIN form in groundwater and associated discharge was nitrate (NO (3) (-) ). The stable isotope signatures (delta N-15(NO3) and delta O-18(NO3)) of NO (3) (-) in the South Bay groundwater and surface waters were both consistent with NO (3) (-) derived from NH (4) (+) that was isotopically enriched in N-15 by NH (4) (+) volatilization. Based on the calculated SGD fluxes and groundwater nutrient concentrations, nutrient fluxes associated with SGD can account for up to 16 % of DIN and 22 % of DIP in South and Central Bays. The form of DIN contributed to surface waters from SGD may impact the ratio of NO (3) (-) to NH (4) (+) available to phytoplankton with implications to bay productivity, phytoplankton species distribution, and nutrient uptake rates. This assessment of nutrient delivery via groundwater discharge in SFB may provide vital information for future bay ecological wellbeing and sensitivity to future environmental stressors. C1 [Null, Kimberly A.; Dimova, Natasha T.; Paytan, Adina] Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA. [Dimova, Natasha T.] Univ Alabama, Dept Geol Sci, Tuscaloosa, AL USA. [Knee, Karen L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Esser, Bradley K.; Singleton, Michael J.] Lawrence Livermore Natl Lab, Livermore, CA USA. [Swarzenski, Peter W.] US Geol Survey, Pacific Coastal & Marine Sci Ctr, Santa Cruz, CA USA. [Stacey, Mark] Univ Calif Berkeley, Dept Civil & Environm Engn, Berkeley, CA 94720 USA. RP Null, KA (reprint author), Univ Calif Santa Cruz, Inst Marine Sci, Santa Cruz, CA 95064 USA. EM kimberly.null@gmail.com; natodi@gmail.com RI Esser, Bradley/G-4283-2010 OI Esser, Bradley/0000-0002-3219-4298 FU University of California FX We would like to thank the University of California Lab Fees Research Program for funding. We would also like to thank Ellen Gray and Zhongwu Ma for assistance with fieldwork, Rob Franks at the UCSC analytical facility for help with analytical procedures, and many thanks to others that helped collect samples in the field. We extend special thanks to the park rangers and staff at Angel Island State Park for their hospitality and logistical support. PWS is grateful to the USGS Coastal and Marine Geology Program for continued support. NR 83 TC 11 Z9 11 U1 0 U2 46 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD SEP PY 2012 VL 35 IS 5 BP 1299 EP 1315 DI 10.1007/s12237-012-9526-7 PG 17 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 986HJ UT WOS:000307332400013 ER PT J AU Tulbure, MG Ghioca-Robrecht, DM Johnston, CA Whigham, DF AF Tulbure, Mirela G. Ghioca-Robrecht, Dana M. Johnston, Carol A. Whigham, Dennis F. TI Inventory and Ventilation Efficiency of Nonnative and Native Phragmites australis (Common Reed) in Tidal Wetlands of the Chesapeake Bay SO ESTUARIES AND COASTS LA English DT Article DE Patch inventory; Intragenic physiological differences; Intrapatch biomass allocation; Pressurized ventilation; Ventilation efficiency; Invasive wetland plants; Phragmites; Chesapeake Bay ID SALT-MARSH; SPARTINA-ALTERNIFLORA; CRYPTIC INVASION; NORTH-AMERICA; FRESH-WATER; NEW-JERSEY; EXPANSION; SALINITY; DYNAMICS; POACEAE AB Nonnative Phragmites is among the most invasive plants in the U.S. Atlantic coast tidal wetlands, whereas the native Phragmites has declined. Native and nonnative patches growing side by side provided an ideal setting for studying mechanisms that enable nonnative Phragmites to be a successful invader. We conducted an inventory followed by genetic analysis and compared differences in growth patterns and ventilation efficiency between adjacent native and nonnative Phragmites stands. Genetic analysis of 212 patches revealed that only 14 were native suggesting that very few native Phragmites populations existed in the study area. Shoot density decreased towards the periphery of native patches, but not in nonnative patches. Ventilation efficiency was 300 % higher per unit area for nonnative than native Phragmites, likely resulting in increased oxidation of the rhizosphere and invasive behavior of nonnative Phragmites. Management of nonnative Phragmites stands should include mechanisms that inhibit pressurized ventilation of shoots. C1 [Tulbure, Mirela G.] Univ New S Wales, Australian Wetlands Rivers & Landscapes Ctr, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. [Tulbure, Mirela G.; Ghioca-Robrecht, Dana M.; Johnston, Carol A.] S Dakota State Univ, Dept Biol & Microbiol, Brookings, SD 57007 USA. [Whigham, Dennis F.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Tulbure, MG (reprint author), Univ New S Wales, Australian Wetlands Rivers & Landscapes Ctr, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. EM Mirela.Tulbure@unsw.edu.au RI Tulbure, Mirela/B-3030-2012; OI Tulbure, Mirela/0000-0003-1456-183X; Johnston, Carol/0000-0002-9663-5048; Whigham, Dennis/0000-0003-1488-820X FU Joseph F. Nelson scholarship FX We thank Dr. Doug Samson from The Nature Conservancy for providing information about the King's Creek Preserve, Drs. Joydeep Bhattacharjee and Neil Reese for help with choosing the instruments, Jay O'Neill for lab assistance, Dr. Kristin Saltonstall and Robert Meadows for suggestions regarding native stand locations in Maryland, Elaine Friebele for permission to sample Jug Bay wetlands, and Ned Gerber for allowing us to use his farm during the field season. Funding came through the Joseph F. Nelson scholarship to MGT. We thank the editors and two anonymous reviewers for helpful comments on an earlier draft. NR 54 TC 12 Z9 12 U1 1 U2 34 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD SEP PY 2012 VL 35 IS 5 BP 1353 EP 1359 DI 10.1007/s12237-012-9529-4 PG 7 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 986HJ UT WOS:000307332400018 ER PT J AU Puerta-Pinero, C Espelta, JM Sanchez-Humanes, B Rodrigo, A Coll, L Brotons, L AF Puerta-Pinero, Carolina Espelta, Josep M. Sanchez-Humanes, Belen Rodrigo, Anselm Coll, Lluis Brotons, Lluis TI History matters: Previous land use changes determine post-fire vegetation recovery in forested Mediterranean landscapes SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Global change; Mediterranean forest; Quercus; Pinus; Passive restoration ID EASTERN IBERIAN PENINSULA; QUERCUS-ILEX; REGENERATION PATTERNS; NORTHEASTERN SPAIN; PLANT-COMMUNITIES; PINE PLANTATIONS; SEED DISPERSAL; LARGE WILDFIRE; NE SPAIN; FIRE AB Land use changes and shifts in disturbance regimes (e.g. wildfires) are recognized worldwide as two of the major drivers of the current global change in terrestrial ecosystems. We expect that, in areas with large-scale land use changes, legacies from previous land uses persist and affect current ecosystem responses to climate-associated disturbances like fire. This study analyses whether post-fire vegetation dynamics may differ according to specific historical land use histories in a Mediterranean forest landscape of about 60,000 ha that was burnt by extensive fires. For that, we assessed land use history of the whole area through the second half of the XXth century, and evaluated the post-fire regeneration success in terms of: (i) forest cover and (ii) tree species composition (biotic-dispersed, resprouter species, Quercus spp. vs. wind-dispersed species with or without fire-resistant seed bank. Pinus spp.). Results showed that stable forest areas exhibited a higher post-fire recovery than younger forests. Furthermore. the longer since crop abandonment translates into a faster post-fire recovery. Results highlight that to anticipate the impacts of disturbances on ecosystems, historical land trajectories should be taken into account. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Puerta-Pinero, Carolina; Coll, Lluis; Brotons, Lluis] Forest Sci Ctr Catalonia CTFC, E-25280 Solsona, Spain. [Espelta, Josep M.; Sanchez-Humanes, Belen; Rodrigo, Anselm; Coll, Lluis; Brotons, Lluis] CREAF, Cerdanyola Del Valles 08193, Catalonia, Spain. [Rodrigo, Anselm] Univ Autonoma Barcelona, Fac Biociencies, Unitat Ecol, Cerdanyola Del Valles 08193, Spain. RP Puerta-Pinero, C (reprint author), Smithsonian Trop Res Inst, CTFS, Unit 0948, DPO, AA 34002 USA. EM puertac@si.edu; Josep.Espelta@uab.es; belen.sanchez@creaf.uab.es; anselm.rodrigo@uab.es; lluis.coll@ctfc.es; lluis.brotons@ctfc.es RI Puerta Pinero, Carolina/B-3186-2012; Coll, Lluis/E-8724-2015; Espelta, Josep Maria/I-3891-2016; Brotons, Lluis/D-1570-2009; OI Puerta Pinero, Carolina/0000-0002-0584-7548; Coll, Lluis/0000-0002-8035-5949; Espelta, Josep Maria/0000-0002-0242-4988; Brotons, Lluis/0000-0002-4826-4457; Rodrigo, Anselm/0000-0001-6341-0363 FU Spanish Ministry of Science and Innovation [CSD2008-00040]; Spanish Ministry of Education [EX2009-0703] FX Collaborative work was facilitated by the Consolider-Ingenio Montes CSD2008-00040 project by Spanish Ministry of Science and Innovation. Postdoctoral and predoctoral fellowships to CPP (EX2009-0703) and BSH (FPU) were provides by Spanish Ministry of Education. Laura Juarez kindly helped us with NDVI computations and maps building. NR 53 TC 17 Z9 17 U1 2 U2 43 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 SEP 1 PY 2012 VL 279 BP 121 EP 127 DI 10.1016/j.foreco.2012.05.020 PG 7 WC Forestry SC Forestry GA 983CD UT WOS:000307092900013 ER PT J AU Henry, TJ AF Henry, Thomas J. TI Dr. J. E. McPherson, Educator and Researcher Extraordinaire: Biographical Sketch and List of Publications SO GREAT LAKES ENTOMOLOGIST LA English DT Article C1 ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Henry, TJ (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, MRC 168, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov NR 171 TC 0 Z9 0 U1 0 U2 0 PU MICH ENTOMOL SOC PI E LANSING PA MICH STATE UNIV DEPT ENTOMOL, E LANSING, MI 48823 USA SN 0090-0222 J9 GREAT LAKES ENTOMOL JI Gt. Lakes Entomol. PD FAL-WIN PY 2012 VL 45 IS 3-4 BP 111 EP 123 PG 13 WC Entomology SC Entomology GA V36TJ UT WOS:000209233200001 ER PT J AU Li, S McShea, WJ Wang, DJ Huang, JZ Shao, LK AF Li, Sheng McShea, William J. Wang, Dajun Huang, Junzhong Shao, Liangkun TI A Direct Comparison of Camera-Trapping and Sign Transects for Monitoring Wildlife in the Wanglang National Nature Reserve, China SO WILDLIFE SOCIETY BULLETIN LA English DT Article DE large mammal; monitoring index; protected area management; species richness; temperate forest; wildlife monitoring AB Wildlife monitoring plays a critical role in evaluating the management and conservation of biodiversity. During monitoring activities in Chinese nature reserves dedicated to giant panda conservation, indirect sign surveys along fixed transects are the standard methodology used to monitor large-mammal populations. Camera-trapping has been recently introduced to these reserves as an additional monitoring tool. We present a case study of comparing current sign-transect monitoring with camera-trapping in Wanglang National Nature Reserve, China, from September 2004 through October 2005, and we assess the effectiveness of both methods in detecting terrestrial fauna. Camera-trapping detected 21 mammal species, while sign transects detected 16 species. We found no significant difference in the animal community detected by each method; however, sign transects were weighted toward detecting large-sized animals. Each survey technique had different strengths; therefore, a combined sampling of camera-trapping (800 camera-days) and sign transects (80 km) was sufficient to detect 95% of detectable large, terrestrial mammal species within this 323-km(2) reserve. Our estimate of species richness based on camera-trapping (39.0 +/- 13.6 species) and sign transects (20.0 +/- 4.4 species) suggests that camera-trapping can detect more species when extensive sampling effort is employed by both methods. Camera-trapping also has the potential for more robust estimates of population parameters than are possible with sign transects. We propose that the giant panda reserves in China can increase their efficiency and range of species monitored by using a system that integrates camera-trapping with sign transects. (C) 2012 The Wildlife Society. C1 [Li, Sheng; McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Li, Sheng; Wang, Dajun] Peking Univ, Sch Life Sci, Ctr Nat & Soc, Beijing 100871, Peoples R China. [Huang, Junzhong] Xuebaoding Natl Nat Reserve, Pingwu Cty 622550, Sichuan Provinc, Peoples R China. [Shao, Liangkun] Wanglang Natl Nat Reserve, Pingwu Cty 622550, Sichuan Provinc, Peoples R China. RP Li, S (reprint author), Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI 53706 USA. EM lis@si.edu FU Smithsonian National Zoological Park, Friends of the National Zoo, and Peking University FX The Smithsonian National Zoological Park, Friends of the National Zoo, and Peking University supported this study financially. We appreciate Peking University, Sichuan Forestry Department and Pingwu Forestry Bureau for permission and logistical support. We thank C. Youping, J. Shiwei, Z. Lianjun, Y. Luogui, L. Jian, L. Bin, Z. Yinzhu, Z. Jianhua, L. Gaoshan and all the other field staff who contributed to field work, data collection, and logistic support. We also thank I. C. Bruce for reviewing our manuscript and providing valuable comments. NR 59 TC 4 Z9 7 U1 4 U2 18 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1938-5463 J9 WILDLIFE SOC B JI Wildl. Soc. Bull. PD SEP PY 2012 VL 36 IS 3 BP 538 EP 545 DI 10.1002/wsb.161 PG 8 WC Biodiversity Conservation SC Biodiversity & Conservation GA V38GZ UT WOS:000209333200020 ER PT J AU Dutta, T Sharma, S Maldonado, JE Wood, TC Seidensticker, J AF Dutta, Trishna Sharma, Sandeep Maldonado, Jesus E. Wood, Thomas C. Seidensticker, John TI A reliable method for individual identification and gender determination of wild leopards (Panthera pardus fusca) using non-invasive samples SO CONSERVATION GENETICS RESOURCES LA English DT Article DE Noninvasive DNA sampling; Panthera pardus fusca; Individual identification; Microsatellite; Sex assignment ID NATURAL-POPULATIONS; MICROSATELLITES; SOFTWARE; TIGRIS; PCR AB We describe a highly polymorphic microsatellite panel for identifying individual leopards using DNA from scat. After successfully screening 16 published microsatellites, we optimized a panel of 7 microsatellites that yields a Probability of Identity between siblings value of 5.24E-04. We used this panel to identify 217 individuals from 287 leopard scats collected from five tiger-reserves in Central India. We identified 101 males and 92 females by amplifying a fragment of the Amelogenin protein gene. This panel will be helpful to study genetic structure, gene flow, relatedness and sex ratio of leopards. C1 [Dutta, Trishna; Sharma, Sandeep; Maldonado, Jesus E.; Seidensticker, John] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. [Dutta, Trishna; Sharma, Sandeep; Maldonado, Jesus E.; Wood, Thomas C.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Dutta, T (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. EM trishnad@gmail.com FU Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo; George Mason University FX Funding was provided by Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo, and George Mason University. We thank H. S. Panwar, the Principal Chief Conservator of Forests (PCCF) Wildlife, Madhya Pradesh and Maharashtra and field directors and staff of all five tiger reserves (Kanha, Satpura, Melghat, Pench MP and Mh) for providing research permissions and logistical help. We thank Robert Fleischer, Center for Conservation and Evolutionary Genetics, SCBI and Yogesh S. Shouche, National Center for Cell Sciences (NCCS), Pune, Maharashtra, India for providing laboratory space and facilitating lab work; Nancy Rotzel, Libby Dougan and Hitendra Munot for logistical support, and Susan Lumpkin for editorial comments. NR 19 TC 11 Z9 11 U1 3 U2 33 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1877-7252 J9 CONSERV GENET RESOUR JI Conserv. Genet. Resour. PD SEP PY 2012 VL 4 IS 3 BP 665 EP 667 DI 10.1007/s12686-012-9618-5 PG 3 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 976LS UT WOS:000306586800030 ER PT J AU Bermudez, SE Castro, A Esser, H Liefting, Y Garcia, G Miranda, RJ AF Bermudez C, Sergio E. Castro, Angelica Esser, Helen Liefting, Yorick Garcia, Gleydis Miranda, Roberto J. TI Ticks (Ixodida) on humans from central Panama, Panama (2010-2011) SO EXPERIMENTAL AND APPLIED ACAROLOGY LA English DT Article DE Ticks; Environments; Human; Panama ID MOUNTAIN-SPOTTED-FEVER; SOUTH-AMERICA; ACARI AB From January 2010 to December 2011, a total of 138 cases of ticks feeding on humans were reported from 11 locations in central Panama. Five of these locations were situated in forest environments, three in rural landscapes and three in urban areas. The ticks were submitted to the Gorgas Memorial Institute, where nine species were identified among 65 specimens: Amblyomma cajennense s.l., A. dissimile, A. naponense, A. oblongoguttatum, A. ovale, A. sabanerae, A. tapirellum, Haemaphysalis juxtakochi and Rhipicephalus sanguineus s.l. The remaining 73 specimens consisted of unidentified immature ticks, all belonging to the genus of Amblyomma. Rhipicephalus sanguineus s.l. was the species most frequently associated with humans, particularly in urban environments. In rural landscapes, tick bites were most often caused by A. cajennense s.l., whereas A. tapirellum was the species most often found parasitizing humans in forest environments. These data provide information on the tick species most commonly associated with humans in forested environments, rural areas and cities around the Panama Canal. C1 [Bermudez C, Sergio E.; Castro, Angelica; Garcia, Gleydis; Miranda, Roberto J.] Inst Conmemorativo Gorgas Estudios Salud, Dept Med Entomol, Panama City, Panama. [Esser, Helen; Liefting, Yorick] Smithsonian Trop Res Inst, Panama City, Panama. RP Bermudez, SE (reprint author), Inst Conmemorativo Gorgas Estudios Salud, Dept Med Entomol, Ave Justo Arosemena,Apo Postal 0816-02593, Panama City, Panama. EM bermudezsec@gmail.com OI Bermudez, Sergio/0000-0003-1830-3133 NR 35 TC 7 Z9 8 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0168-8162 J9 EXP APPL ACAROL JI Exp. Appl. Acarol. PD SEP PY 2012 VL 58 IS 1 BP 81 EP 88 DI 10.1007/s10493-012-9564-7 PG 8 WC Entomology SC Entomology GA 975XH UT WOS:000306544500008 PM 22544074 ER PT J AU Anker, A Baeza, JA AF Anker, Arthur Antonio Baeza, J. TI Molecular and morphological phylogeny of hooded shrimps, genera Betaeus and Betaeopsis (Decapoda, Alpheidae): Testing the center of origin biogeographic model and evolution of life history traits SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cladistics; Sociobiology; Character mapping; Biogeography; Symbiosis; Center of origin ID SOCIAL MONOGAMY; SNAPPING SHRIMP; CRUSTACEA; GENUS; CONSEQUENCES; EUSOCIALITY; ENVIRONMENT; HYPOTHESIS; SYNALPHEUS; INFERENCE AB The phylogenetic relationships of the alpheid shrimp genera Betaeus (Dana, 1852) (15 species) and Betaeopsis (Yaldwyn, 1971) (three species), collectively known as hooded shrimps, are analyzed with morphological, molecular (16S and H3) and combined "total evidence" (morphology + DNA) datasets. The tree topology resulting from morphological and combined analyses places Betaeus jucundus as sister to all the remaining species of Betaeus and Betaeopsis, rendering Betaeus paraphyletic. On the other hand, Betaeopsis is recovered as monophyletic. Betaeus australis is positioned as sister to the remaining species of Betaeus s. str. (excluding B. jucundus), which is composed of three well-supported and resolved clades. Mapping of biogeographic traits on the combined tree suggests at least two possible historic scenarios. In the first scenario, the North-East Pacific harboring the highest diversity of hooded shrimps (seven species of Betaeus), acted as the "center of origin", where species appeared, matured and eventually migrated toward peripheral regions. In the second scenario, Betaeus + Betaeopsis originated in the southern Indo-West Pacific and subsequently colonized the North-East Pacific, where a major radiation involving dispersal/vicariance events took place. The mapping of life history traits (symbiosis vs. free living and gregariousness vs. single/pair living) in the combined tree suggests (1) that different types of symbioses with dissimilar host organisms (sea urchins, abalones, other decapods, spoon worms) evolved independently more than once in the group (in B. jucundus and in various lineages of Betaeus s. str.), and (2) that gregariousness was ancestral in the Betaeus s. str. - Betaeopsis clade and later shifted toward single/pair living in several lineages. Published by Elsevier Inc. C1 [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Anker, Arthur] Univ Fed Ceara, Inst Ciencias Mar Labomar, Fortaleza, Ceara, Brazil. [Antonio Baeza, J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23435 USA. [Antonio Baeza, J.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM arthuranker7@yahoo.com; baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773 FU SMSFP; CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) of the Brazilian Government; National Geographic research grant FX J.A.B. was supported by a postdoctoral fellowship from SMSFP. A.A. was supported by a postdoctoral fellowship from CAPES (Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior) of the Brazilian Government. This study was partially funded by a National Geographic research grant to J.A.B. Some specimens used in this study were provided by our colleagues: Constance Gramlich (San Diego State University), Gregory Jensen (University of Washington), Richard Taylor (Leigh Marine Laboratory, New Zealand), Charles Griffiths (University of Cape Town, Republic of South Africa), Ernesto Campos (Universidad Autonoma de Baja California, Mexico), Gustav Paulay (FLMNH, USA), Sammy De Grave (OUMNH, United Kingdom), Luis Ignacio Vilchis and William A. Newman (Scripps Institution of Oceanography, University of California at San Diego, USA), Jimmy O'Donnell (University of California at Santa Cruz, USA), Ivan N. Mann (AN. Severtzov Institute of Ecology and Evolution, RAS, Moscow, Russia), Ivan Hinojosa (UCN, Chile), and Tomas Luppi, Nahuel Farias, Eduardo Spivak, and Marcelo Scelzo (UNdMP, Argentina). Special thanks to Martin Thiel (UCN, Chile) for inviting both of us to co-instruct (together with Raymond T. Bauer) a short course on biology of caridean shrimps in Coquimbo in 2007. Jeff Hunt and Lee Weigt (Laboratory of Analytical Biology, USNM) provided logistical support for the molecular analysis. Additional color photographs used in Fig. 2 were provided by Richard Taylor, Gustav Paulay, Kevin Lee (www.diverkevin.com, USA), Larry Jon Friesen (www.sbnature.net, USA), and Madoka Itoh (Japan). The comments by three anonymous referees improved considerably the present manuscript. This is Smithsonian Marine Station at Fort Pierce contribution number 882. NR 70 TC 9 Z9 10 U1 0 U2 23 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 SEP PY 2012 VL 64 IS 3 BP 401 EP 415 DI 10.1016/j.ympev.2012.04.015 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 976XT UT WOS:000306621400003 PM 22579811 ER PT J AU Sessa, EB Zimmer, EA Givnish, TJ AF Sessa, Emily B. Zimmer, Elizabeth A. Givnish, Thomas J. TI Reticulate evolution on a global scale: A nuclear phylogeny for New World Dryopteris (Dryopteridaceae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ferns; Divergence time estimates; Hybridization; Neotropics; Phylogeny; Polyploidy ID LENGTH DIFFERENCE TEST; FERN GENUS DRYOPTERIS; PHLOROGLUCINOL DERIVATIVES; DIVERGENCE TIMES; HISTORICAL BIOGEOGRAPHY; MAXIMUM-LIKELIHOOD; SPINULOSA COMPLEX; CHLOROPLAST DNA; CANARY ISLANDS; MIXED MODELS AB Reticulate, or non-bifurcating, evolution is now recognized as an important phenomenon shaping the histories of many organisms. It appears to be particularly common in plants, especially in ferns, which have relatively few barriers to intra- and interspecific hybridization. Reticulate evolutionary patterns have been recognized in many fern groups, though very few have been studied rigorously using modern molecular phylogenetic techniques in order to determine the causes of the reticulate patterns. In the current study, we examine patterns of branching and reticulate evolution in the genus Dryopteris, the woodferns. The North American members of this group have long been recognized as a classic example of reticulate evolution in plants, and we extend analysis of the genus to all 30 species in the New World, as well as numerous taxa from other regions. We employ sequence data from the plastid and nuclear genomes and use maximum parsimony (MP), maximum likelihood (ML), Bayesian inference (BI), and divergence time analyses to explore the relationships of New World Dryopteris to other regions and to reconstruct the timing and events which may have led to taxa displaying reticulate rather than strictly branching histories. We find evidence for reticulation among both the North and Central/South American groups of species, and our data support a classic hypothesis for reticulate evolution via allopolyploid speciation in the North America taxa, including an extinct diploid progenitor in this group. In the Central and South American species, we find evidence of extensive reticulation involving unknown ancestors from Asia, and we reject deep coalescent processes such as incomplete lineage sorting in favor of more recent intercontinental hybridization and chloroplast capture as an explanation for the origin of the Latin American reticulate taxa. (C) 2012 Elsevier Inc. All rights reserved. C1 [Sessa, Emily B.; Givnish, Thomas J.] Univ Wisconsin, Dept Bot, Madison, WI 53706 USA. [Zimmer, Elizabeth A.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Sessa, EB (reprint author), Univ Wisconsin, Dept Bot, 430 Lincoln Dr, Madison, WI 53706 USA. EM esessa@wisc.edu FU National Science Foundation (DDIG Award) [DEB-1110335]; Huron Mountain Wildlife Foundation; Botanical Society of America; American Society of Plant Taxonomists; Torrey Botanical Society; Smithsonian Graduate Research Fellowship FX The authors thank E. Alverson, S. Bornell, B. Gilman, T. Grabs, A. Jandl, C. Line, S. Lorbeer, B. and A. Manierre, T. Meyer, A. Reznicek, C. Taylor, B. Vesterby, S. Wechsler, D. Werier, F.R. Wesley, K. Woods, and especially T. Goforth for help in the field; J. Geiger, S. Hennequin, C. Rothfels, and J.E. Watkins for providing material; D. Giblin, M. McNamara, R. Moran, R. Olmstead, A. Smith, M. Sundue, and S. Vance for help with arranging herbarium visits; herbaria BH, NY, MO, UC, US, WTU for letting us view specimens; and the Finger Lakes Land Trust, Huron Mountain Club, Fernwood Botanical Gardens, and University of Wisconsin - Madison Arboretum for allowing us to visit and collect Dryopteris in the field. Profound thanks to M. Ames, B. Berger, A. Gardner, P. Gonsiska, B. Grady, J. Hunt, R. Jabaily, D. Stein, K. Sytsma, J. Wen, and especially C. Ane for advice and discussion. We gratefully acknowledge financial support for this research from: the National Science Foundation (DDIG Award to E.B.S., T.J.G.; Grant DEB-1110335); the Huron Mountain Wildlife Foundation (E.B.S., T.J.G.); graduate research awards from the Botanical Society of America, American Society of Plant Taxonomists, and Torrey Botanical Society (EBS), and a Smithsonian Graduate Research Fellowship (E.B.S.). Funding sources had no involvement in study design, data collection, analysis, interpretation, or article preparation or submission. NR 100 TC 21 Z9 23 U1 0 U2 38 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 SEP PY 2012 VL 64 IS 3 BP 563 EP 581 DI 10.1016/j.ympev.2012.05.009 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 976XT UT WOS:000306621400015 PM 22634937 ER PT J AU Miller, JJ Delwiche, CF Coats, DW AF Miller, John J. Delwiche, Charles F. Coats, D. Wayne TI Ultrastructure of Amoebophrya sp and its Changes during the Course of Infection SO PROTIST LA English DT Article DE Apicomplexa; Amoebophrya; dinoflagellate; parasitism; Syndiniales; ultrastructure ID TOXOPLASMA-GONDII; FINE-STRUCTURE; PARASITOPHOROUS VACUOLE; GENETIC DIVERSITY; CHESAPEAKE BAY; LIFE-CYCLE; DINOFLAGELLATE CHROMOSOMES; INTRACELLULAR PARASITE; ELECTRON-MICROSCOPY; ALEXANDRIUM-AFFINE AB Amoebophrya is a syndinian parasite that kills harmful bloom forming algae. Previously uncharacterized ultrastructural aspects of infection and development were elucidated. The biflagellate dinospore has two mitochondria, electron-dense bodies, striated strips, trichocysts, and a nucleus with peripherally condensed chromatin. After finding an Akashiwo sanguinea host and adhering to its surface, the parasite penetrates the host surface, apparently using a microfilament based motility and electron-dense bodies within a microtubular basket in the process of parasitophorous vacuole membrane formation. After entering the host nucleus, possibly by a similar mechanism used to enter the host cell, the parasite cytosol expanded substantially prior to mitosis. From 12-36 hours mitochondria were inconspicuous but present. Chromatin condensation was variable. By 36 hours post-infection, parasites had multiple nuclei, a microtubule-supported cytopharynx, and were beginning to form a fully internal mastigocoel. By 48 hours, the characteristic "beehive" appearance was apparent with flagella projecting into a fully developed mastigocoel. The cytoplasm contained trichocysts, elongated mitochondria, and nuclei with peripherally condensed chromatin. Although Amoebophrya lacks an apical complex, its electron-dense bodies show functional similarities to apicomplexan rhoptries. Its lack of permanently condensed chromosomes, but compact dinospore chromatin, supports the idea that dinoflagellate permanently condensed chromosomes may be a remnant of a parasitic ancestor with a compact dispersal stage. (C) 2011 Elsevier GmbH. All rights reserved. C1 [Miller, John J.; Delwiche, Charles F.] Univ Maryland, Dept Cell Biol & Mol Genet, College Pk, MD 20742 USA. [Delwiche, Charles F.] MAES, Edgewater, MD 21037 USA. [Coats, D. Wayne] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Miller, JJ (reprint author), Univ Maryland, Dept Cell Biol & Mol Genet, 2108 Biosci Res Bldg, College Pk, MD 20742 USA. EM jjmiller@umd.edu RI Delwiche, Charles/C-6549-2008 OI Delwiche, Charles/0000-0001-7854-8584 FU NSF [MCB0629624] FX Thanks to Tim Maugel and Jan Endlich in the Laboratory for Biological Ultrastructure at the University of Maryland, College Park for their advice regarding the ultrastructural work. We would also like to acknowledge Letitia Cosbert for her help maintaining Akashiwo sanguinea and Amoebophrya sp. cultures and Liam McTurk for his help photocopying articles. Thanks also to Dr. Juan Saldarriaga for his valuable suggestions about the possible importance of parasitism in the evolution of the dinokaryon and to Dr. Norman R. Pace for the use of his microscope. Two anonymous reviewers provided thoughtful suggestions, which improved this manuscript substantially. This work was supported in part by NSF grant MCB0629624. NR 87 TC 14 Z9 16 U1 2 U2 24 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 1434-4610 J9 PROTIST JI Protist PD SEP PY 2012 VL 163 IS 5 BP 720 EP 745 DI 10.1016/j.protis.2011.11.007 PG 26 WC Microbiology SC Microbiology GA 970EI UT WOS:000306110500004 PM 22209083 ER PT J AU Whitfeld, TJS Kress, WJ Erickson, DL Weiblen, GD AF Whitfeld, T. J. S. Kress, W. J. Erickson, D. L. Weiblen, G. D. TI Change in community phylogenetic structure during tropical forest succession: evidence from New Guinea SO ECOGRAPHY LA English DT Article ID BORNEAN RAIN-FOREST; NULL MODEL ANALYSIS; PLANT-COMMUNITIES; TREE COMMUNITY; ECOLOGICAL COMMUNITIES; FUNCTIONAL TRAITS; DIVERSITY; EVOLUTION; DENSITY; ASSOCIATIONS AB Ecologists have recently interpreted patterns of phylogenetic distance among coexisting species as indicative of processes affecting community assembly during forest succession. We investigated plant community phylogenetic structure along a successional gradient in New Guinean lowland rain forest. We surveyed all trees with diameter at breast height = 5 cm in nineteen 0.25 ha plots representing younger secondary, older secondary, and primary forest. We estimated plant community phylogeny from rbcL gene sequences to quantify change in phylogenetic structure during succession. Mean phylogenetic distance among co-occurring trees increased with total basal area per plot, a proxy for forest age. Significant phylogenetic clustering was detected in secondary forest whereas primary forest was significantly over-dispersed relative to null expectations. We examined the sensitivity of these patterns to various methods of branch length estimation and phylogenetic uncertainty. Power to detect community phylogenetic patterns when equal branch lengths were assumed was weak in comparison to direct molecular and time-calibrated measures of divergence. Inferred change during forest succession was also robust to phylogenetic uncertainty so long as temporal information was incorporated in estimates of divergence. The observed patterns are consistent with processes of environmental filtering during tropical forest succession giving way to other processes in primary forests including density-dependence. C1 [Whitfeld, T. J. S.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Kress, W. J.; Erickson, D. L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166, Washington, DC 20013 USA. [Weiblen, G. D.] Univ Minnesota, Bell Museum Nat Hist, St Paul, MN 55108 USA. [Weiblen, G. D.] 250 Biol Sci Ctr, Dept Plant Biol, St Paul, MN 55108 USA. RP Whitfeld, TJS (reprint author), Univ Minnesota, Dept Forest Resources, 115 Green Hall,1530 Cleveland Ave N, St Paul, MN 55108 USA. EM whitf015@umn.edu FU US National Science Foundation [DEB-0515678]; Consortium for the Barcode of Life; Arnold Arboretum; Society of Systematic Biologists; Systematics Association; Univ. of Minnesota (Dept of Plant Biology, Dept of Ecology, Evolution, and Behavior, Office of International Programs, Graduate School) FX We thank Jeannine Cavender-Bares and Rebecca Montgomery for comments and guidance. Steve Kembel, Jessica Savage, Cam Webb, Jonathan Eastman, Nathan Swenson, and Eric Lind for advice and assistance with analyses. Annika Moe for comments that improved the manuscript. Vojtech Novotny and staff at the New Guinea Binatang Research Center particularly Gibson Sosanika and Kenneth Molem. For assistance with data management and specimen curation we thank Ross Bernard, Rosanne Healy, and Erin Treiber. Billy Bau and Kipiro Damas (PNG Forest Research Inst.) for help with specimen identifications and fieldwork. Wanang village assistants for help with fieldwork. This work was supported by a US National Science Foundation grant (DEB-0515678), the Consortium for the Barcode of Life, the Arnold Arboretum (Deland Award for student research), the Society of Systematic Biologists (award for Graduate Student Research), the Systematics Association (Systematics Research Fund), and Univ. of Minnesota (Dept of Plant Biology, Dept of Ecology, Evolution, and Behavior, Office of International Programs, Graduate School). NR 63 TC 38 Z9 39 U1 6 U2 82 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0906-7590 J9 ECOGRAPHY JI Ecography PD SEP PY 2012 VL 35 IS 9 BP 821 EP 830 DI 10.1111/j.1600-0587.2011.07181.x PG 10 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 967XP UT WOS:000305941800006 ER PT J AU Zeder, MA AF Zeder, Melinda A. TI The Broad Spectrum Revolution at 40: Resource diversity, intensification, and an alternative to optimal foraging explanations SO JOURNAL OF ANTHROPOLOGICAL ARCHAEOLOGY LA English DT Review DE Broad Spectrum Revolution; Optimal foraging theory; Niche construction theory; Resource diversification; Resource intensification ID EASTERN NORTH-AMERICA; HUMAN BEHAVIORAL ECOLOGY; DIVISION-OF-LABOR; NICHE CONSTRUCTION; DIET BREADTH; FOOD-PRODUCTION; AGRICULTURAL ORIGINS; SUBSISTENCE CHANGE; SOUTHERN LEVANT; PREY CHOICE AB More than 40 years ago Kent Flannery coined the term Broad Spectrum Revolution (BSR) in reference to a broadening of the subsistence base of Late Pleistocene hunter-gatherers in the Near East that preceded and helped pave the way for the domestication and plants and animals and the emergence of agriculture. Set within a demographic density model that projected differential rates of population growth and emigration in different resource zones of the Near East, Flannery's BSR quickly became a global construct linking resource diversification and intensification to imbalances between population and environmental carrying capacity. In recent years the BSR has proven especially attractive to researchers working within an optimal foraging theory (OFT) framework in which diversification and intensification of subsistence only occurs within the context of resource depression, caused by either demographic pressure or environmental deterioration. This OFT perspective, that situates human societies in a one-way adaptive framework as they are forced to adapt to declining availability of optimal resources, however, is increasingly being called into question. Numerous examples of diversification and intensification are being documented in contexts of resource abundance shaped, in part, by deliberate human efforts at ecosystem engineering intended to promote resource productivity. An alternative approach, framed within a newer paradigm from evolutionary biology, niche construction theory (NCT), provides a more powerful explanatory framework for the BSR wherever it occurred. Published by Elsevier Inc. C1 Smithsonian Inst, Natl Museum Amer Hist, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. RP Zeder, MA (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Program Human Ecol & Archaeobiol, POB 37012,MRC 112, Washington, DC 20013 USA. EM zederm@si.edu NR 241 TC 65 Z9 68 U1 7 U2 76 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0278-4165 J9 J ANTHROPOL ARCHAEOL JI J. Anthropol. Archaeol. PD SEP PY 2012 VL 31 IS 3 BP 241 EP 264 DI 10.1016/j.jaa.2012.03.003 PG 24 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 951RL UT WOS:000304737600001 ER PT J AU Rogers, J AF Rogers, J. Daniel TI Inner Asian States and Empires: Theories and Synthesis SO JOURNAL OF ARCHAEOLOGICAL RESEARCH LA English DT Article DE Empires; States; Inner Asia; Pastoralism ID COMPLEX SOCIETIES; HISTORY; ARCHAEOLOGY; MONGOLIA; NOMADS; CHINA; AGE AB By 200 B.C. a series of expansive polities emerged in Inner Asia that would dominate the history of this region and, at times, a very large portion of Eurasia for the next 2,000 years. The pastoralist polities originating in the steppes have typically been described in world history as ephemeral or derivative of the earlier sedentary agricultural states of China. These polities, however, emerged from local traditions of mobility, multiresource pastoralism, and distributed forms of hierarchy and administrative control that represent important alternative pathways in the comparative study of early states and empires. The review of evidence from 15 polities illustrates long traditions of political and administrative organization that derive from the steppe, with Bronze Age origins well before 200 B.C. Pastoralist economies from the steppe innovated new forms of political organization and were as capable as those based on agricultural production of supporting the development of complex societies. C1 Smithsonian Inst, Natl Museum Nat Hist, NHB 112, Dept Anthropol, Washington, DC 20013 USA. RP Rogers, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, NHB 112, Dept Anthropol, POB 37012, Washington, DC 20013 USA. EM rogersd@si.edu NR 304 TC 8 Z9 8 U1 1 U2 17 PU SPRINGER/PLENUM PUBLISHERS PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1059-0161 EI 1573-7756 J9 J ARCHAEOL RES JI J. Archaeol. Res. PD SEP PY 2012 VL 20 IS 3 BP 205 EP 256 DI 10.1007/s10814-011-9053-2 PG 52 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 940IQ UT WOS:000303883600001 ER PT J AU Tornabene, L Van Tassell, JL Robertson, DR AF Tornabene, Luke Van Tassell, James L. Ross Robertson, D. TI Microgobius urraca (Teleostei: Gobiidae), a new species of goby from the tropical eastern Pacific SO ZOOTAXA LA English DT Article DE Gobiosomatini; Microgobius group; Gobiiformes; Panama; American seven-spined gobies ID GENUS; GOBIOSOMATINI; PHYLOGENY AB A new species of goby in the genus Microgobius (Teleostei: Gobiidae: Gobiosomatini) is described from the Pacific coast of Panama. It is morphologically similar to M. erectus, but differs from that species in possessing fewer lateral scale rows, lacking a patch of ctenoid scales under the pectoral fin, having unpigmented epaxial myosepta, having a distinct oval-shaped dark blotch on the first dorsal fin, and possessing three blue-white stripes on a dark caudal fin. Differences in both the number and type of scales, dorsal and anal fin ray counts, the poor development of a fleshy dorsal crest, and overall color patterns further distinguish this species from the remaining eastern Pacific congeners. Photographs of all Pacific species of Microgobius and a dichotomous key to the Pacific members of the genus are provided. C1 [Tornabene, Luke] Texas A&M Univ, Corpus Christi, TX 78418 USA. [Van Tassell, James L.] Amer Museum Nat Hist, Dept Ichthyol, New York, NY 11024 USA. [Ross Robertson, D.] Smithsonian Trop Res Inst, Balboa, Panam, Panama. RP Tornabene, L (reprint author), Texas A&M Univ, 6300 Ocean Dr, Corpus Christi, TX 78418 USA. EM Luke.Tornabene@tamucc.edu; jvantassell@gobiidae.com; drr@stri.org FU Smithsonian Tropical Research Institute FX We thank J. Earle and the crew of the R/V Urraca for their assistance in the field. Funding for field work was provided by Smithsonian Tropical Research Institute to DRR. R. Arrindell, B. Brown and R. Schelly at AMNH; and J. Williams, C. Baldwin and D. Pitassy at USNM provided assistance with digital radiographs and museum material. Special thanks to S. Large for his assistance with the map and F. Pezold for his review of an earlier version of this paper. NR 23 TC 2 Z9 2 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD AUG 31 PY 2012 IS 3447 BP 41 EP 55 PG 15 WC Zoology SC Zoology GA 003HW UT WOS:000308602100003 ER PT J AU Lucas, SG Harris, SK Spielmann, JA Berman, DS Henrici, AC Krainer, K Rinehart, LF Dimichele, WA Chaney, DS Kerp, H AF Lucas, Spencer G. Harris, Susan K. Spielmann, Justin A. Berman, David S. Henrici, Amy C. Krainer, Karl Rinehart, Larry F. Dimichele, William A. Chaney, Dan S. Kerp, Hans TI LITHOSTRATIGRAPHY, PALEONTOLOGY, BIOSTRATIGRAPHY, AND AGE OF THE UPPER PALEOZOIC ABO FORMATION NEAR JEMEZ SPRINGS, NORTHERN NEW MEXICO, USA SO ANNALS OF CARNEGIE MUSEUM LA English DT Article DE Coyotean; Early Permian; paleoflora; vertebrate fossils; Wolfcampian ID STRATIGRAPHY; COUNTY; DEPOSITS; ENGLAND; FACIES; FILLS AB In the Jemez Springs area of Sandoval County, northern New Mexico, siliciclastic red beds of the upper Paleozoic Abo Formation are well exposed and yield fossil plants and vertebrates. The local Abo Formation section is more than 190 m thick and rests disconformably on the Upper Pennsylvanian Guadalupe Box Formation and is conformably overlain by the Lower Permian DeChelly Sandstone (Yeso Group). Abo sandstone sheets are low sinuosity river deposits, and intercalated sandstone beds and lenses represent sheet splays and minor channel fills that formed during overbank flooding. The dominant Abo lithofacies is mudstone, which represents floodplain deposits, many with calcareous paleosols. Fossils are present in three stratigraphic intervals of the lower to middle Abo Formation. All three intervals yield eupelycosaur-dominated vertebrate fossil assemblages of Coyotean age (Coyotean = late Virgilian-Wolfcampian on the North American provincial marine timescale: Lucas 2006). The lowest interval also yields the Spanish Queen Mine paleoflora of pteridosperms and conifers. Strata of the Guadalupe Box Formation disconformably below the Abo Formation contain late Virgilian fusulinids. We correlate the Abo Formation fossil assemblages in the Jemez Springs area to the Coyotean-age fossil assemblages in the upper part of the El Cobre Canyon Formation in the Arroyo del Agua area and in the Canon del Cobre in the Chama basin of northern New Mexico. This suggests a middle Wolfcampian age for the Jemez Springs area fossil assemblages, an age very close to the Pennsylvanian-Permian boundary. C1 [Lucas, Spencer G.; Harris, Susan K.; Spielmann, Justin A.; Rinehart, Larry F.] New Mexico Museum Nat Hist & Sci, Collect & Res Dept, Albuquerque, NM 87104 USA. [Berman, David S.; Henrici, Amy C.] Camegie Museum Nat Hist, Sect Vertebrate Paleontol, Pittsburgh, PA 15213 USA. [Krainer, Karl] Univ Innsbruck, Inst Geol & Paleontol, A-6020 Innsbruck, Austria. [Dimichele, William A.; Chaney, Dan S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Kerp, Hans] Univ Munster, Inst Geol & Palaontol, Forschungsstelle Paldobot, D-48143 Munster, Germany. RP Lucas, SG (reprint author), New Mexico Museum Nat Hist & Sci, Collect & Res Dept, 1801 Mt Rd NW, Albuquerque, NM 87104 USA. EM spencer.lucas@state.nm.us; harris_susank@hotmail.com; justin.spielmann1@state.nm.us; bermand@camegiemnh.org; henricia@camegiemnh.org; karl.krainer@uibk.ac.at; larry.rinehart@state.nm.us; dimichel@si.edu; chaneyd@si.edu; kerp@uni-muenster.de RI DiMichele, William/K-4301-2012 NR 70 TC 3 Z9 3 U1 2 U2 10 PU CARNEGIE MUSEUM NATURAL HISTORY PI PITTSBURGH PA 4400 FORBES AVE, PITTSBURGH, PA 15213 USA SN 0097-4463 J9 ANN CARNEGIE MUS JI Ann. Carnegie Mus. PD AUG 31 PY 2012 VL 80 IS 4 BP 323 EP 350 PG 28 WC Paleontology; Zoology SC Paleontology; Zoology GA 014NG UT WOS:000309382000003 ER PT J AU Kanzaki, N Giblin-Davis, RM Scheffrahn, RH Taki, H Esquivel, A Davies, KA Herre, EA AF Kanzaki, Natsumi Giblin-Davis, Robin M. Scheffrahn, Rudolf H. Taki, Hisatomo Esquivel, Alejandro Davies, Kerrie A. Allen Herre, E. TI Reverse Taxonomy for Elucidating Diversity of Insect-Associated Nematodes: A Case Study with Termites SO PLOS ONE LA English DT Article ID N. SP; ENVIRONMENTAL DNA; RAIN-FOREST; APHELENCHOIDIDAE; SEQUENCES; DIPLOGASTRIDAE; BIODIVERSITY; TYLENCHINA; MORPHOLOGY; PHYLOGENY AB Background: The molecular operational taxonomic unit (MOTU) has recently been applied to microbial and microscopic animal biodiversity surveys. However, in many cases, some of the MOTUs cannot be definitively tied to any of the taxonomic groups in current databases. To surmount these limitations, the concept of "reverse taxonomy" has been proposed, i.e. to primarily list the MOTUs with morphological information, and then identify and/ordescribe them at genus/species level using subsamples or by re-isolating the target organisms. Nevertheless, the application of "reverse taxonomy" has not been sufficiently evaluated. Therefore, the practical applicability of "reverse taxonomy" is tested using termite-associated nematodes as a model system for phoretic/parasitic organisms which have high habitat specificity and a potential handle (their termite host species) for re-isolation attempts. Methodology: Forty-eight species (from 298 colonies) of termites collected from the American tropics and subtropics were examined for their nematode associates using the reverse taxonomy method and culturing attempts (morphological identification and further sequencing efforts). The survey yielded 51 sequence types (= MOTUs) belonging to 19 tentatively identified genera. Within these, four were identified based on molecular data with preliminary morphological observation, and an additional seven were identified or characterized from successful culturing, leaving eight genera unidentified. Conclusions: That 1/3 of the genera were not successfully identified suggests deficiencies in the depth of available sequences in the database and biological characters, i.e. usually isolated as phoretic/parasitic stages which are not available for morphological identification, and too many undiscovered lineages of nematodes. Although there still is the issue of culturability of nematodes, culturing attempts could help to make reverse taxonomy methods more effective. However, expansion of the database, i.e., production of more DNA barcodes tied to biological information by finding and characterizing additional new and known lineages, is necessary for analyzing functional diversity. C1 [Kanzaki, Natsumi; Giblin-Davis, Robin M.; Scheffrahn, Rudolf H.] Univ Florida IFAS, Ft Lauderdale Res & Educ Ctr, Davie, FL USA. [Kanzaki, Natsumi; Taki, Hisatomo] Forestry & Forest Prod Res Inst, Tsukuba, Ibaraki 305, Japan. [Esquivel, Alejandro] Univ Nacl, Escuela Ciencias Agr, Lab Nematol, Heredia, Costa Rica. [Davies, Kerrie A.] Univ Adelaide, Sch Agr Food & Wine, Ctr Evolutionary Biol & Biodivers, Glen Osmond, SA, Australia. [Allen Herre, E.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Kanzaki, N (reprint author), Univ Florida IFAS, Ft Lauderdale Res & Educ Ctr, Davie, FL USA. EM nkanzaki@affrc.go.jp FU National Science Foundation [DEB-0450537]; Ministry of Education, Culture, Sports, Science and Technology, Japan [21770094] FX This work was partially supported by the National Science Foundation (DEB-0450537) - Biodiversity Surveys and Inventories, and a Grant-in-Aid for Young Scientists (B) (#21770094) from The Ministry of Education, Culture, Sports, Science and Technology, Japan. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 49 TC 13 Z9 13 U1 2 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 AUG 28 PY 2012 VL 7 IS 8 AR e43865 DI 10.1371/journal.pone.0043865 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 998CA UT WOS:000308213600052 PM 22952792 ER PT J AU Rogers, JD Nichols, T Emmerich, T Latek, M Cioffi-Revilla, C AF Rogers, J. Daniel Nichols, Teresa Emmerich, Theresa Latek, Maciej Cioffi-Revilla, Claudio TI Modeling scale and variability in human-environmental interactions in Inner Asia SO ECOLOGICAL MODELLING LA English DT Article DE Complexity; Pastoralism; Inner Asia; Weather; Agent-based modeling; Simulations ID REGIME SHIFTS; MONGOLIA; RESILIENCE; SYSTEMS; DISCONTINUITIES; BIODIVERSITY; EQUILIBRIUM; DEGRADATION; ECOSYSTEMS; MANAGEMENT AB Pastoralism represents a complex adaptive system that has existed in Inner Asia for thousands of years. The challenges of environmental change have highlighted the need to assess the potential for long-term sustainability while also considering the characteristics of systems that have the potential to maintain resilience. Here we assess the interaction between slow and fast processes and how interpretations of adaptive capacity and system resilience are affected by the scale at which observations are made. Agent-based modeling is used to identify the social and demographic interactions between landscape and weather variability for pastoralists in Inner Asia at a variety of social scales and from temporal scales of societal change ranging from a few days to 1000 years. Results indicate that the scale of abrupt changes may not be proportional to the severity or duration of the weather event, but is highly impacted by internal social factors. At the scale of individual families, highly interconnected social systems with less mobility and restricted decision making are less effective. When viewed from the vantage point of larger social units, highly interconnected kinship systems and restrictions in access to land may serve purposes that are counterproductive for individual families. Published by Elsevier B.V. C1 [Rogers, J. Daniel] Smithsonian Inst, Washington, DC 20560 USA. [Nichols, Teresa] Indiana Univ, Bloomington, IN 47405 USA. [Emmerich, Theresa] Univ Exeter, Exeter EX4 4QJ, Devon, England. [Latek, Maciej; Cioffi-Revilla, Claudio] George Mason Univ, Fairfax, VA 22030 USA. RP Rogers, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. EM rogersd@si.edu NR 81 TC 8 Z9 8 U1 4 U2 22 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 J9 ECOL MODEL JI Ecol. Model. PD AUG 24 PY 2012 VL 241 SI SI BP 5 EP 14 DI 10.1016/j.ecolmode1.2011.11.025 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 983OZ UT WOS:000307129900003 ER PT J AU Li, DQ Oh, J Kralj-Fiser, S Kuntner, M AF Li, Daiqin Oh, Joelyn Kralj-Fiser, Simona Kuntner, Matjaz TI Remote copulation: male adaptation to female cannibalism SO BIOLOGY LETTERS LA English DT Article DE sexual conflict; sexual cannibalism; coevolution; genital emasculation ID ORB-WEB SPIDER; MALE SACRIFICE; GENITAL MUTILATION; SEXUAL CANNIBALISM; SPERM COMPETITION; NEPHILID SPIDERS; ARANEAE; BEHAVIOR; CONFLICT; DURATION AB Sexual cannibalism by females and associated male behaviours may be driven by sexual conflict. One such male behaviour is the eunuch phenomenon in spiders, caused by total genital emasculation, which is a seemingly maladaptive behaviour. Here, we provide the first empirical testing of an adaptive hypothesis to explain this behaviour, the remote copulation, in a highly sexually cannibalistic orb-web spider Nephilengys malabarensis. We demonstrate that sperm transfer continues from the severed male organ into female genitals after the male has been detached from copula. Remote copulation increases the total amount of sperm transferred, and thus probably enhances paternity. We conclude that the mechanism may have evolved in response to sexual cannibalism and female-controlled short copulation duration. C1 [Li, Daiqin; Oh, Joelyn] Natl Univ Singapore, Dept Biol Sci, Singapore 117543, Singapore. [Li, Daiqin; Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. [Kralj-Fiser, Simona; Kuntner, Matjaz] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Li, DQ (reprint author), Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore. EM dbslidq@nus.edu.sg RI Li, Daiqin/D-6922-2013 OI Li, Daiqin/0000-0001-8269-7734 FU Ministry of Education Academic Research Fund (AcRF) [R-154-000-435-112]; Slovenian Research Agency (ARRS) [J1-2063, 1000-10-720023]; Humboldt's grant; Singapore NParks [NP/RP10-036] FX The study was supported by the Ministry of Education Academic Research Fund (AcRF) grant to D.L. (R-154-000-435-112), in part by the Slovenian Research Agency (ARRS) grants to M. K. (J1-2063 and 1000-10-720023) and Humboldt's grant to S.K.F. We thank Poh Moi Goh and Chun Hong Cheung for providing fruitflies and house flies. Spiders were collected under research permit (NP/RP10-036) granted by Singapore NParks. NR 26 TC 15 Z9 15 U1 6 U2 66 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 EI 1744-957X J9 BIOL LETTERS JI Biol. Lett. PD AUG 23 PY 2012 VL 8 IS 4 BP 512 EP 515 DI 10.1098/rsbl.2011.1202 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 973LN UT WOS:000306361700010 PM 22298805 ER PT J AU Craddock, RA Howard, AD Irwin, RP Tooth, S Williams, RME Chu, PS AF Craddock, Robert A. Howard, Alan D. Irwin, Rossman P., III Tooth, Stephen Williams, Rebecca M. E. Chu, Pao-Shin TI Drainage network development in the Keanakako'i tephra, Kilauea Volcano, Hawai'i: Implications for fluvial erosion and valley network formation on early Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID MARTIAN OUTFLOW CHANNELS; CARBON-DIOXIDE CLOUDS; GRAVEL-BED RIVERS; GUSEV CRATER; EXPLOSIVE ERUPTIONS; SEDIMENT TRANSPORT; ORBITER CAMERA; WATER FLOWS; ASH MEMBER; SURFACE AB A number of studies have attempted to characterize Martian valley and channel networks. To date, however, little attention has been paid to the role of lithology, which could influence the rate of incision, morphology, and hydrology as well as the characteristics of transported materials. Here, we present an analysis of the physical and hydrologic characteristics of drainage networks (gullies and channels) that have incised the Keanakako'i tephra, a basaltic pyroclastic deposit that occurs mainly in the summit area of Kilauea Volcano and in the adjoining Ka'u Desert, Hawai'i. The Keanakako'i tephra is up to similar to 10 m meters thick and largely devoid of vegetation, making it a good analog for the Martian surface. Although the scales are different, the Keanakako'i drainage networks suggest that several typical morphologic characteristics of Martian valley networks may be controlled by lithology in combination with ephemeral flood characteristics. Many gully headwalls and knickpoints within the drainage networks are amphitheater shaped, which results from strong-over-weak stratigraphy. Beds of fine ash, commonly bearing accretionary lapilli (pisolites), are more resistant to erosion than the interbedded, coarser weakly consolidated and friable tephra layers. Because the banks of the gullies and channels are easily eroded widths vary downslope, similar to Martian valley networks that have been characterized as "degraded." The floors of the gullies and channels tend to be low-relief with few prominent bed forms, reflecting the large proportion of sediment transported as bed load in high-energy but short-lived flood events. We calculate that the average flow velocities within the drainage networks are typically <10 cm/s, occurring during floods that probably last less than an hour. Analyses of sediment deposits that have overlain lava flows of known ages suggest that these ephemeral flood events are associated with large cold core winter cyclones, known locally as 'kona storms', that are capable of generating precipitation at rates >1 m/24 h. Given some recent modeling of the early Martian climate, our observations imply that rainfall on early Mars could also be associated with large intense events and that Martian valley network formation may be related to similar cyclonic storms. C1 [Craddock, Robert A.; Irwin, Rossman P., III] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Howard, Alan D.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. [Tooth, Stephen] Aberystwyth Univ, Inst Geog & Earth Sci, Aberystwyth, Dyfed, Wales. [Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ USA. [Chu, Pao-Shin] Univ Hawaii Manoa, Dept Meteorol, Honolulu, HI 96822 USA. RP Craddock, RA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315, Washington, DC 20560 USA. EM craddockb@si.edu RI Craddock, Robert/B-3884-2013; Tooth, Stephen/B-6105-2013 OI Tooth, Stephen/0000-0001-5714-2606 FU NASA [NNX08AN64G]; Smithsonian Institution FX This research is supported by a grant from the NASA Mars Fundamental Research Program (NNX08AN64G). An award from the Smithsonian Institution's George F. Becker Endowment Fund supported preliminary fieldwork. The authors thank Corey Fortezzo, Brent Garry, Ruslan Kuzmin, Cathy Quantin-Nataf, Sharon Wilson Purdy, Don Swanson, and Jim Zimbelman for their support in the field. Don Swanson provided many useful comments on earlier versions of this manuscript. We also appreciate the constructive reviews received from Dave Crown and Nicolas Warner. NR 123 TC 10 Z9 10 U1 1 U2 24 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 AUG 22 PY 2012 VL 117 AR E08009 DI 10.1029/2012JE004074 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 995LM UT WOS:000308009600004 ER PT J AU Cooper, MJ Martin, RV van Donkelaar, A Lamsal, L Brauer, M Brook, JR AF Cooper, Matthew J. Martin, Randall V. van Donkelaar, Aaron Lamsal, Lok Brauer, Michael Brook, Jeffrey R. TI A Satellite-Based Multi-Pollutant Index of Global Air Quality SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Editorial Material C1 [Cooper, Matthew J.; Martin, Randall V.; van Donkelaar, Aaron] Dalhousie Univ, Halifax, NS B3H 3J5, Canada. [Martin, Randall V.; Brook, Jeffrey R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lamsal, Lok] Univ Space Res Assoc, Columbia, MD 21044 USA. [Lamsal, Lok] NASA, Atmospher Chem & Dynam Lab, Div Earth Sci, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Brauer, Michael] Univ British Columbia, Vancouver, BC V6T 1Z3, Canada. [Martin, Randall V.; Brook, Jeffrey R.] Environm Canada, Air Qual Proc Res Sect, Toronto, ON M6B 2S7, Canada. RP Cooper, MJ (reprint author), Dalhousie Univ, Halifax, NS B3H 3J5, Canada. EM cooperm2@dal.ca RI Lamsal, Lok/G-4781-2012; Martin, Randall/C-1205-2014; OI Martin, Randall/0000-0003-2632-8402; Brauer, Michael/0000-0002-9103-9343 NR 5 TC 9 Z9 9 U1 1 U2 26 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD AUG 21 PY 2012 VL 46 IS 16 BP 8523 EP 8524 DI 10.1021/es302672p PG 2 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 991JQ UT WOS:000307697700001 PM 22853810 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bottcher, M Bouvier, A Bugaev, V Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Dumm, J Errando, M Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Hui, CM Imran, A Jameil, O Kaaret, P Karlsson, N Kertzman, M Kerr, J Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Lee, K Madhavan, AS Majumdar, P McArthur, S McCann, A Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Park, N Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reynolds, PT Roache, E Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Smith, AW Staszak, D Stroh, M Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Varlotta, A Vassiliev, VV Vivier, M Wakely, SP Ward, JE Weinstein, A Welsing, R Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boettcher, M. Bouvier, A. Bugaev, V. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Dumm, J. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Hui, C. M. Imran, A. Jameil, O. Kaaret, P. Karlsson, N. Kertzman, M. Kerr, J. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Madhavan, A. S. Majumdar, P. McArthur, S. McCann, A. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Park, N. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reynolds, P. T. Roache, E. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Sentuerk, G. D. Smith, A. W. Staszak, D. Stroh, M. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Varlotta, A. Vassiliev, V. V. Vivier, M. Wakely, S. P. Ward, J. E. Weinstein, A. Welsing, R. Williams, D. A. Zitzer, B. TI MULTIWAVELENGTH OBSERVATIONS OF THE AGN 1ES 0414+009 WITH VERITAS, FERMI-LAT, SWIFT-XRT, AND MDM SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: individual (1ES 0414+009, ERJ0416+011); gamma rays: galaxies ID BL LACERTAE OBJECT; GAMMA-RAY ASTRONOMY; TELESCOPE; EMISSION; SEARCH; DISCOVERY; BLAZARS; SAMPLE; STARS AB We present observations of the BL Lac object 1ES 0414+009 in the >200 GeV gamma-ray band by the VERITAS array of Cherenkov telescopes. 1ES 0414+009 was observed by VERITAS between 2008 January and 2011 February, resulting in 56.2 hr of good quality pointed observations. These observations resulted in a detection of 822 events from the source corresponding to a statistical significance of 6.4 standard deviations (6.4 sigma) above the background. The source flux, showing no evidence for variability, is measured as (5.2 +/- 1.1(stat) +/- 2.6(sys)) x 10(-12) photons cm(-2) s(-1) above 200 GeV, equivalent to approximately 2% of the Crab Nebula flux above this energy. The differential photon spectrum from 230 GeV to 850 GeV is well fit by a power law with a photon index of Gamma = 3.4 +/- 0.5(stat) +/- 0.3(sys) and a flux normalization of (1.6 +/- 0.3(stat) +/- 0.8(sys)) x 10(-11) photons cm(-2) s(-1) at 300 GeV. We also present multiwavelength results taken in the optical (MDM), x-ray (Swift-XRT), and GeV (Fermi-LAT) bands and use these results to construct a broadband spectral energy distribution (SED). Modeling of this SED indicates that homogenous one-zone leptonic scenarios are not adequate to describe emission from the system, with a lepto-hadronic model providing a better fit to the data. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; McArthur, S.; Thibadeau, S.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Boettcher, M.; Jameil, O.; Kerr, J.] Ohio Univ, Inst Astrophys, Dept Phys & Astron, Athens, OH 45701 USA. [Cannon, A.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Pohl, M.; Ruppel, J.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; Smith, A. W.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Stroh, M.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Huan, H.; Park, N.; Wakely, S. P.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Dublin, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Pichel, A.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [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. [Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM aw.smith@utah.edu RI Khassen, Yerbol/I-3806-2015; OI Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Lang, Mark/0000-0003-4641-4201; Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the U.K. FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748), and by STFC in the U.K. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. This work also made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. NR 35 TC 14 Z9 14 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 AUG 20 PY 2012 VL 755 IS 2 AR 118 DI 10.1088/0004-637X/755/2/118 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400035 ER PT J AU Brassington, NJ Fabbiano, G Zezas, A Kundu, A Kim, DW Fragos, T King, AR Pellegrini, S Trinchieri, G Zepf, S Wright, NJ AF Brassington, N. J. Fabbiano, G. Zezas, A. Kundu, A. Kim, D. -W. Fragos, T. King, A. R. Pellegrini, S. Trinchieri, G. Zepf, S. Wright, N. J. TI THE SPECTRAL AND TEMPORAL PROPERTIES OF TRANSIENT SOURCES IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 3379, NGC 4278, NGC 4697); X-rays: binaries; X-rays: galaxies ID X-RAY SOURCES; CHANDRA MONITORING OBSERVATIONS; ACCRETING NEUTRON-STARS; MASS BLACK-HOLE; GLOBULAR-CLUSTER; ELLIPTIC GALAXIES; STELLAR POPULATIONS; XMM-NEWTON; DEEP CHANDRA; WHITE-DWARF AB We report the spectral and temporal variability properties of 18 candidate transient (TC) and potential transient (PTC) sources detected in deep multi-epoch Chandra observation of the nearby elliptical galaxies, NGC 3379, NGC 4278, and NGC 4697. Only one source can be identified with a background counterpart, leaving 17 TCs + PTCs in the galaxies. Of these, 14 are in the galaxy field, supporting the theoretical picture that the majority of field X-ray binaries (XRBs) will exhibit transient accretion for >75% of their lifetime. Three sources are coincident with globular clusters, including two high-luminosity candidate black hole (BH) XRBs, with L-X = 5.4x10(38) erg s(-1) and L-X = 2.8x10(39) erg s(-1), respectively. The spectra, luminosities, and temporal behavior of these 17 sources suggest that the transient population is heterogeneous, including neutron star (NS) and BH XRBs in both normal and high-rate accretion modes, and super soft sources containing white dwarf binaries. Our TC and PTC detections are noticeably fewer than the number expected from the population synthesis (PS) models of Fragos et al., tailored to our new Chandra pointings of NGC 4278. We attribute this discrepancy to the PS assumption that the transient population is composed of NS XRBs, as well as differences between the statistical analysis and error estimates used in the model and our observations. C1 [Brassington, N. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Brassington, N. J.; Fabbiano, G.; Zezas, A.; Kim, D. -W.; Fragos, T.; Wright, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Zezas, A.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Kundu, A.] Eureka Sci Inc, Oakland, CA 94602 USA. [King, A. R.] Univ Leicester, Theoret Astrophys Grp, Leicester LE1 7RH, Leics, England. [Pellegrini, S.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Trinchieri, G.] INAF Osservatorio Astron Brera, I-20121 Milan, Italy. [Zepf, S.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP Brassington, NJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM n.brassington@herts.ac.uk RI Zezas, Andreas/C-7543-2011; Fragos, Tassos/A-3581-2016 OI Zezas, Andreas/0000-0001-8952-676X; Trinchieri, Ginevra/0000-0002-0227-502X; Fragos, Tassos/0000-0003-1474-1523 FU Chandra G0 grants [G06-7079A, GO0-11102X]; NASA [NAS8-39073]; NASA through Chandra awards [GO-11111, AR-12009]; NASA LTSA grant [NAG5-13056]; Italian Space Agency ASI (Agenzia Spaziale Italiana) [ASI-INAFI/009/10/0]; NASA ADAP grants [NNX08AJ60G, NNX11AG12G] FX We thank the CXC DS and SDS teams for their efforts in reducing the data and developing the software used for the reduction (SDP) and analysis (CIAO). We also thank the anonymous referee whose detailed and careful report has helped to improve this paper. This work was supported by Chandra G0 grants G06-7079A and GO0-11102X (PI: Fabbiano). We acknowledge partial support from NASA contract NAS8-39073 (CXC). A. Kundu acknowledges support for this work by NASA through Chandra awards GO-11111 and AR-12009. A. Zezas acknowledges support from NASA LTSA grant NAG5-13056. S. Pellegrini and G. Trinchieri acknowledge partial financial support from the Italian Space Agency ASI (Agenzia Spaziale Italiana) through grant ASI-INAFI/009/10/0. S. Zepf acknowledges support from NASA ADAP grants NNX08AJ60G and NNX11AG12G. G. Fabbiano is grateful to the Aspen Center for Physics for their hospitality. NR 97 TC 14 Z9 14 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2012 VL 755 IS 2 AR 162 DI 10.1088/0004-637X/755/2/162 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400079 ER PT J AU Chandra, P Chevalier, RA Chugai, N Fransson, C Irwin, CM Soderberg, AM Chakraborti, S Immler, S AF Chandra, Poonam Chevalier, Roger A. Chugai, Nikolai Fransson, Claes Irwin, Christopher M. Soderberg, Alicia M. Chakraborti, Sayan Immler, Stefan TI RADIO AND X-RAY OBSERVATIONS OF SN 2006jd: ANOTHER STRONGLY INTERACTING TYPE IIn SUPERNOVA SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; hydrodynamics; radio continuum: general; stars: mass-loss; supernovae: general; supernovae: individual (SN 2006jd) ID PARTICLE-ACCELERATION; GALAXY NGC-891; EMISSION; SN-1988Z; STAR; INSTABILITIES; ABSORPTION; EVOLUTION; REMNANTS; SPECTRA AB We report four years of radio and X-ray monitoring of the Type IIn supernova SN 2006jd at radio wavelengths with the Very Large Array, Giant Metrewave Radio Telescope, and Expanded Very Large Array; at X-ray wavelengths with Chandra, XMM-Newton, and Swift-XRT. We assume that the radio and X-ray emitting particles are produced by shock interaction with a dense circumstellar medium. The radio emission shows an initial rise that can be attributed to free-free absorption by cool gas mixed into the nonthermal emitting region; external free-free absorption is disfavored because of the shape of the rising light curves and the low gas column density inferred along the line of sight to the emission region. The X-ray luminosity implies a preshock circumstellar density similar to 10(6) cm(-3) at a radius r similar to 2 x 10(16) cm, but the column density inferred from the photoabsorption of X-rays along the line of sight suggests a significantly lower density. The implication may be an asymmetry in the interaction. The X-ray spectrum shows Fe line emission at 6.9 keV that is stronger than is expected for the conditions in the X-ray emitting gas. We suggest that cool gas mixed into the hot gas plays a role in the line emission. Our radio and X-ray data both suggest the density profile is flatter than r(-2) because of the slow evolution of the unabsorbed emission. C1 [Chandra, Poonam] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [Chevalier, Roger A.; Irwin, Christopher M.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Chugai, Nikolai] Russian Acad Sci, Inst Astron, Moscow 109017, Russia. [Fransson, Claes] Stockholm Univ, Dept Astron, AlbaNova, SE-10691 Stockholm, Sweden. [Soderberg, Alicia M.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chakraborti, Sayan] Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Immler, Stefan] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Immler, Stefan] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Chandra, P (reprint author), Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. EM Poonam.Chandra@rmc.ca FU NSERC; NASA [NNX09AH58G, GO9-0079X]; NSF [AST-0807727] FX P.C. and R. C. are grateful to Craig Sarazin for discussions on X-ray emission and analysis. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. P. C. is supported by her NSERC Discovery grants. R. C. and C. I. acknowledge support from NASA grants NNX09AH58G (XMM) and GO9-0079X (Chandra), and NSF grant AST-0807727. NR 43 TC 27 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 AUG 20 PY 2012 VL 755 IS 2 AR 110 DI 10.1088/0004-637X/755/2/110 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400027 ER PT J AU Conroy, C Kratter, KM AF Conroy, Charlie Kratter, Kaitlin M. TI RUNAWAY STARS AND THE ESCAPE OF IONIZING RADIATION FROM HIGH-REDSHIFT GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; galaxies: formation; galaxies: high-redshift ID LYMAN-CONTINUUM EMISSION; REGION LUMINOSITY FUNCTION; M-CIRCLE-DOT; STELLAR POPULATIONS; FORMING GALAXIES; OB ASSOCIATIONS; STARBURST GALAXIES; DWARF GALAXIES; YOUNG GALAXIES; MASSIVE STARS AB Approximately 30% of all massive stars in the Galaxy are runaways with velocities exceeding 30 km s(-1). Their high speeds allow them to travel similar to 0.1-1 kpc away from their birthplace before they explode at the end of their several Myr lifetimes. At high redshift, when galaxies were much smaller than in the local universe, runaways could venture far from the dense inner regions of their host galaxies. From these large radii, and therefore low column densities, much of their ionizing radiation is able to escape into the intergalactic medium. Runaways may therefore significantly enhance the overall escape fraction of ionizing radiation, f(esc), from small galaxies at high redshift. We present simple models of the high-redshift runaway population and its impact on f(esc) as a function of halo mass, size, and redshift. We find that the inclusion of runaways enhances f(esc) by factors of approximate to 1.1-8, depending on halo mass, galaxy geometry, and the mechanism of runaway production, implying that runaways may contribute 50%-90% of the total ionizing radiation escaping from high-redshift galaxies. Runaways may therefore play an important role in reionizing the universe. C1 [Conroy, Charlie; Kratter, Kaitlin M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Conroy, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 86 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 AUG 20 PY 2012 VL 755 IS 2 AR 123 DI 10.1088/0004-637X/755/2/123 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400040 ER PT J AU D'Abrusco, R Fabbiano, G Djorgovski, G Donalek, C Laurino, O Longo, G AF D'Abrusco, R. Fabbiano, G. Djorgovski, G. Donalek, C. Laurino, O. Longo, G. TI CLaSPS: A NEW METHODOLOGY FOR KNOWLEDGE EXTRACTION FROM COMPLEX ASTRONOMICAL DATA SETS SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; methods: statistical; surveys ID ARTIFICIAL NEURAL-NETWORKS; SELF-ORGANIZING MAP; X-RAY-EMISSION; PHOTOMETRIC REDSHIFTS; SOURCE CATALOG; STATISTICAL-ANALYSIS; DATA RELEASE; SKY; SELECTION; GALAXIES AB In this paper, we present the Clustering-Labels-Score Patterns Spotter (CLaSPS), a new methodology for the determination of correlations among astronomical observables in complex data sets, based on the application of distinct unsupervised clustering techniques. The novelty in CLaSPS is the criterion used for the selection of the optimal clusterings, based on a quantitative measure of the degree of correlation between the cluster memberships and the distribution of a set of observables, the labels, not employed for the clustering. CLaSPS has been primarily developed as a tool to tackle the challenging complexity of the multi-wavelength complex and massive astronomical data sets produced by the federation of the data from modern automated astronomical facilities. In this paper, we discuss the applications of CLaSPS to two simple astronomical data sets, both composed of extragalactic sources with photometric observations at different wavelengths from large area surveys. The first data set, CSC+, is composed of optical quasars spectroscopically selected in the Sloan Digital Sky Survey data, observed in the x-rays by Chandra and with multi-wavelength observations in the near-infrared, optical, and ultraviolet spectral intervals. One of the results of the application of CLaSPS to the CSC+ is the re-identification of a well-known correlation between the alpha(OX) parameter and the near-ultraviolet color, in a subset of CSC+ sources with relatively small values of the near-ultraviolet colors. The other data set consists of a sample of blazars for which photometric observations in the optical, mid-, and near-infrared are available, complemented for a subset of the sources, by Fermi gamma-ray data. The main results of the application of CLaSPS to such data sets have been the discovery of a strong correlation between the multi-wavelength color distribution of blazars and their optical spectral classification in BL Lac objects and flat-spectrum radio quasars, and a peculiar pattern followed by blazars in the WISE mid-infrared colors space. This pattern and its physical interpretation have been discussed in detail in other papers by one of the authors. C1 [D'Abrusco, R.; Fabbiano, G.; Laurino, O.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Djorgovski, G.; Donalek, C.; Longo, G.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Longo, G.] Univ Naples Federico II, Dipartimento Sci Fis, I-80126 Naples, Italy. RP D'Abrusco, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI D'Abrusco, Raffaele/L-2767-2016 OI D'Abrusco, Raffaele/0000-0003-3073-0605 FU US Virtual Astronomical Observatory; National Science Foundation; National Aeronautics and Space Administration; NASA [NAS-39073] FX R. D'Abrusco acknowledges the financial support of the US Virtual Astronomical Observatory, which is sponsored by the National Science Foundation and the National Aeronautics and Space Administration. We acknowledge partial support by NASA Contract NAS-39073 (CXC). The CLaSPS method is implemented in R (R Development Core Team 2012), an open-source free statistical environment developed under the GNU GPL (http://www.r-project.org/). TOPCAT and STILTS (http://www.star.bris.ac.uk/similar to mbt/topcat/) (Taylor 2005) were extensively used for the preparation and manipulation of the tabular data in this work. NR 57 TC 3 Z9 3 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 AUG 20 PY 2012 VL 755 IS 2 AR 92 DI 10.1088/0004-637X/755/2/92 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400009 ER PT J AU Dunham, MM Arce, HG Bourke, TL Chen, XP van Kempen, TA Green, JD AF Dunham, Michael M. Arce, Hector G. Bourke, Tyler L. Chen, Xuepeng van Kempen, Tim A. Green, Joel D. TI REVEALING THE MILLIMETER ENVIRONMENT OF THE NEW FU ORIONIS CANDIDATE HBC722 WITH THE SUBMILLIMETER ARRAY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (HBC722); ISM: jets and outflows; stars: flare; stars: formation; stars: low-mass; stars: protostars; stars: variables: T Tauri, Herbig Ae/Be ID 1ST HYDROSTATIC CORE; SPITZER-SPACE-TELESCOPE; C2D SMALL CLOUDS; STAR-FORMATION; MOLECULAR OUTFLOW; NORTH-AMERICAN; TAURUS-AURIGA; DARK CLOUD; ACCRETION; PROTOSTARS AB We present 230 GHz Submillimeter Array continuum and molecular line observations of the newly discovered FU Orionis candidate HBC722. We report the detection of seven 1.3 mm continuum sources in the vicinity of HBC722, none of which corresponds to HBC722 itself. We compile infrared and submillimeter continuum photometry of each source from previous studies and conclude that three are Class 0 embedded protostars, one is a Class I embedded protostar, one is a Class I/II transition object, and two are either starless cores or very young, very low luminosity protostars or first hydrostatic cores. We detect a northwest-southeast outflow, consistent with the previous detection of such an outflow in low-resolution, single-dish observations, and note that its axis may be precessing. We show that this outflow is centered on and driven by one of the nearby Class 0 sources rather than HBC722, and find no conclusive evidence that HBC722 itself is driving an outflow. The non-detection of HBC722 in the 1.3 mm continuum observations suggests an upper limit of 0.02 M-circle dot for the mass of the circumstellar disk. This limit is consistent with typical T Tauri disks and with a disk that provides sufficient mass to power the burst. C1 [Dunham, Michael M.; Arce, Hector G.; Chen, Xuepeng] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Kempen, Tim A.] Joint ALMA Off, Santiago, Chile. [van Kempen, Tim A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Green, Joel D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Dunham, MM (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM michael.dunham@yale.edu FU Smithsonian Institution; Academia Sinica; NSF [AST-0845619] FX The authors express their gratitude to L. Rebull and S. Guieu for providing their Spitzer images of HBC722. We thank Neal Evans for reading a draft in advance of publication and providing helpful comments. This work is based primarily on observations obtained with the Submillimeter Array, a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and funded by the Smithsonian Institution and the Academia Sinica. This research has made use of NASA's Astrophysics Data System (ADS) Abstract Service, the IDL Astronomy Library hosted by the NASA Goddard Space Flight Center, and the SIMBAD database operated at CDS, Strasbourg, France. Support for this work was provided by the NSF through grant AST-0845619 to H.G.A. T.v.K is grateful for the Joint ALMA Observatory for providing the facilities for his scientific research. NR 61 TC 9 Z9 9 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 AUG 20 PY 2012 VL 755 IS 2 AR 157 DI 10.1088/0004-637X/755/2/157 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400074 ER PT J AU Giacintucci, S O'Sullivan, E Clarke, TE Murgia, M Vrtilek, JM Venturi, T David, LP Raychaudhury, S Athreya, RM AF Giacintucci, Simona O'Sullivan, Ewan Clarke, Tracy E. Murgia, Matteo Vrtilek, Jan M. Venturi, Tiziana David, Laurence P. Raychaudhury, Somak Athreya, Ramana M. TI RECURRENT RADIO OUTBURSTS AT THE CENTER OF THE NGC 1407 GALAXY GROUP SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (NGC 1407); intergalactic medium; radio continuum: galaxies; X-rays: galaxies: clusters ID GALACTIC NUCLEUS FEEDBACK; X-RAY CAVITIES; SYNCHROTRON SPECTRUM; INTERGALACTIC MEDIUM; SHOCK ACCELERATION; LOCAL UNIVERSE; HOT GAS; CLUSTERS; BUBBLES; CHANDRA AB We present deep Giant Metrewave Radio Telescope (GMRT) radio observations at 240, 330, and 610 MHz of the complex radio source at the center of the NGC 1407 galaxy group. Previous GMRT observations at 240 MHz revealed faint, diffuse emission enclosing the central twin-jet radio galaxy. This has been interpreted as an indication of two possible radio outbursts occurring at different times. Both the inner double and diffuse components are detected in the new GMRT images at high levels of significance. Combining the GMRT observations with archival Very Large Array data at 1.4 and 4.9 GHz, we derive the total spectrum of both components. The inner double has a spectral index alpha = 0.7, typical for active, extended radio galaxies, whereas the spectrum of the large-scale emission is very steep, with alpha = 1.8 between 240 MHz and 1.4 GHz. The radiative age of the large-scale component is very long, similar to 300 Myr, compared to similar to 30 Myr estimated for the central double, confirming that the diffuse component was generated during a former cycle of activity of the central galaxy. The current activity have so far released an energy which is nearly one order of magnitude lower than that associated with the former outburst. The group x-ray emission in the Chandra and XMM-Newton images and extended radio emission show a similar swept-back morphology. We speculate that the two structures are both affected by the motion of the group core, perhaps due to the core sloshing in response to a recent encounter with the nearby elliptical galaxy NGC 1400. C1 [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [O'Sullivan, Ewan; Vrtilek, Jan M.; David, Laurence P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clarke, Tracy E.] USN, Res Lab, Washington, DC 20375 USA. [Murgia, Matteo] INAF, Osservatorio Astronom Cagliari, I-09012 Capoterra, CA, Italy. [Venturi, Tiziana] INAF, Ist Radioastron, I-40129 Bologna, Italy. [Raychaudhury, Somak] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Athreya, Ramana M.] Indian Inst Sci Educ & Res, Pune 411021, Maharashtra, India. RP Giacintucci, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM simona@astro.umd.edu OI Murgia, Matteo/0000-0002-4800-0806; O'Sullivan, Ewan/0000-0002-5671-6900; Venturi, Tiziana/0000-0002-8476-6307 FU NASA through Einstein Postdoctoral Fellowship [PF0-110071]; European Community under the Marie Curie Research Training Network; 6.1 Base funding; Smithsonian Institution; CXC; Chandra X-Ray Center (CXC) 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. 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 the Smithsonian Astrophysical Observatory (SAO). E.O.S. acknowledges the support of the European Community under the Marie Curie Research Training Network. Basic research in astronomy at the Naval Research Laboratory is funded by 6.1 Base funding. J.M.V., L. P. D., and E.O.S. acknowledge the support of the Smithsonian Institution and CXC. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 64 TC 7 Z9 7 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2012 VL 755 IS 2 AR 172 DI 10.1088/0004-637X/755/2/172 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400089 ER PT J AU Godfrey, LEH Bicknell, GV Lovell, JEJ Jauncey, DL Gelbord, J Schwartz, DA Perlman, ES Marshall, HL Birkinshaw, M Worrall, DM Georganopoulos, M Murphy, DW AF Godfrey, L. E. H. Bicknell, G. V. Lovell, J. E. J. Jauncey, D. L. Gelbord, J. Schwartz, D. A. Perlman, E. S. Marshall, H. L. Birkinshaw, M. Worrall, D. M. Georganopoulos, M. Murphy, D. W. TI A MULTI-WAVELENGTH STUDY OF THE JET, LOBES, AND CORE OF THE QUASAR PKS 2101-490 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (PKS 2101-490) ID X-RAY-EMISSION; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; LARGE-SCALE JETS; II RADIO-SOURCES; MAGNETIC-FIELD STRENGTHS; INVERSE-COMPTON MODEL; HOT-SPOTS; CHANDRA OBSERVATIONS; IMAGING SURVEY AB We present a detailed study of the x-ray, optical, and radio emission from the jet, lobes, and core of the quasar PKS 2101-490 as revealed by new Chandra, Hubble Space Telescope (HST), and ATCA images. We extract the radio to x-ray spectral energy distributions from seven regions of the 13 '' jet, and model the jet x-ray emission in terms of Doppler beamed inverse Compton scattering of the cosmic microwave background (IC/CMB) for a jet in a state of equipartition between particle and magnetic field energy densities. This model implies that the jet remains highly relativistic hundreds of kiloparsecs from the nucleus, with a bulk Lorentz factor Gamma similar to 6 and magnetic field of the order of 30 mu G. We detect an apparent radiative cooling break in the synchrotron spectrum of one of the jet knots, and are able to interpret this in terms of a standard one-zone continuous injection model, based on jet parameters derived from the IC/CMB model. However, we note apparent substructure in the bright optical knot in one of the HST bands. We confront the IC/CMB model with independent estimates of the jet power, and find that the IC/CMB model jet power is consistent with the independent estimates, provided that the minimum electron Lorentz factor gamma(min) greater than or similar to 50, and the knots are significantly longer than the jet width, as implied by de-projection of the observed knot lengths. C1 [Godfrey, L. E. H.] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA 6102, Australia. [Godfrey, L. E. H.; Bicknell, G. V.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Lovell, J. E. J.; Jauncey, D. L.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. [Lovell, J. E. J.] CSIRO, Ind Phys, Lindfield, NSW 2070, Australia. [Lovell, J. E. J.] Univ Tasmania, Dept Phys, Hobart, Tas 7001, Australia. [Gelbord, J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Schwartz, D. A.; Birkinshaw, M.; Worrall, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Marshall, H. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Georganopoulos, M.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. [Murphy, D. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Godfrey, LEH (reprint author), Curtin Univ Technol, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6102, Australia. EM L.Godfrey@curtin.edu.au RI Godfrey, Leith/B-5283-2013 FU Grote Reber Foundation; HST [GO-10352]; NASA [NAS8-03060]; CXC [GO9-0121B]; Commonwealth of Australia FX L.E.H.G thanks the Grote Reber Foundation for financial support during part of this work. H. L. M., E. S. P., and J.G. acknowledge the support of HST grant GO-10352. D. A. S. is supported by NASA contract NAS8-03060 and CXC grant GO9-0121B. The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We gratefully acknowledge the anonymous referee for their comments which helped to improve and clarify the manuscript. NR 66 TC 3 Z9 3 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 AUG 20 PY 2012 VL 755 IS 2 AR 174 DI 10.1088/0004-637X/755/2/174 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400091 ER PT J AU Humphrey, PJ Buote, DA O'Sullivan, E Ponman, TJ AF Humphrey, Philip J. Buote, David A. O'Sullivan, Ewan Ponman, Trevor J. TI THE ElIXr GALAXY SURVEY. II. BARYONS AND DARK MATTER IN AN ISOLATED ELLIPTICAL GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: fundamental parameters; galaxies: individual (NGC 1521); galaxies: ISM; X-rays: galaxies ID X-RAY-EMISSION; SUPERMASSIVE BLACK-HOLE; XMM-NEWTON OBSERVATION; INITIAL MASS FUNCTION; HOT GAS; COSMOLOGICAL SIMULATIONS; INTERGALACTIC MEDIUM; EMITTING GAS; MILKY-WAY; CHANDRA OBSERVATIONS AB The Elliptical Isolated X-ray (ElIXr) Galaxy Survey is a volume-limited (< 110 Mpc) study of optically selected, isolated, L* elliptical galaxies to provide an X-ray census of galaxy-scale (virial mass, M-vir less than or similar to 10(13) M-circle dot) objects and identify candidates for detailed hydrostatic mass modeling. In this paper, we present a Chandra and XMM study of one such candidate, NGC1521, and constrain its distribution of dark and baryonic matter. We find a morphologically relaxed hot gas halo, extending almost to R-500, that is well described by hydrostatic models similar to the benchmark, baryonically closed, Milky Way mass elliptical galaxy NGC720. We obtain good constraints on the enclosed gravitating mass (M-500 = [3.8 +/- 1.0] x 10(12) M-circle dot, slightly higher than NGC720) and baryon fraction (f(b,500) = 0.13 +/- 0.03). We confirm at 8.2 sigma the presence of a dark matter (DM) halo consistent with Lambda CDM. Assuming a Navarro-Frenk-White DM profile, our self-consistent, physical model enables meaningful constraints beyond R500, revealing that most of the baryons are in the hot gas. Within the virial radius, f(b) is consistent with the cosmic mean, suggesting that the predicted massive, quasi-hydrostatic gas halos may be more common than previously thought. We confirm that the DM and stars conspire to produce an approximately power-law total mass profile (rho(tot) proportional to r(-alpha)) that follows the recently discovered scaling relation between alpha and optical effective radius. Our conclusions are insensitive to modest, observationally motivated, deviations from hydrostatic equilibrium. Finally, after correcting for the enclosed gas fraction, the entropy profile is close to the self-similar prediction of gravitational structure formation simulations, as observed in massive galaxy clusters. C1 [Humphrey, Philip J.; Buote, David A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [O'Sullivan, Ewan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [O'Sullivan, Ewan; Ponman, Trevor J.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RP Humphrey, PJ (reprint author), Univ Calif Irvine, Dept Phys & Astron, 4129 Frederick Reines Hall, Irvine, CA 92697 USA. OI O'Sullivan, Ewan/0000-0002-5671-6900 FU Chandra award [G09-0092X]; NASA under XMM [NNX08AX74G, NNX10AD07G] FX We thank Aaron Barth and Luis Ho for kindly providing their optical data, taken as part of the Carnegie-Irvine Galaxy Survey (http://cgs.obs.carnegiescience.edu/CGS/Home.html). We also thank Fabio Gastaldello for discussions and support with the XMM analysis. We thank Christina Topchyan for suggesting the acronym ElIXr. This research made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA, and the HyperLEDA database (http://leda.univ-lyon1.fr.) We are grateful to the WIND-SWE team for making their data publicly available. P.J.H. and D. A. B. gratefully acknowledge support from Chandra award G09-0092X, issued by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. Partial support for this work was also provided by NASA under XMM grant NNX08AX74G and grant NNX10AD07G, issued through the office of Space Science Astrophysics Data Program. NR 132 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2012 VL 755 IS 2 AR 166 DI 10.1088/0004-637X/755/2/166 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400083 ER PT J AU Kasliwal, MM Kulkarni, SR Gal-Yam, A Nugent, PE Sullivan, M Bildsten, L Yaron, O Perets, HB Arcavi, I Ben-Ami, S Bhalerao, VB Bloom, JS Cenko, SB Filippenko, AV Frail, DA Ganeshalingam, M Horesh, A Howell, DA Law, NM Leonard, DC Li, WD Ofek, EO Polishook, D Poznanski, D Quimby, RM Silverman, JM Sternberg, A Xu, D AF Kasliwal, Mansi M. Kulkarni, S. R. Gal-Yam, Avishay Nugent, Peter E. Sullivan, Mark Bildsten, Lars Yaron, Ofer Perets, Hagai B. Arcavi, Iair Ben-Ami, Sagi Bhalerao, Varun B. Bloom, Joshua S. Cenko, S. Bradley Filippenko, Alexei V. Frail, Dale A. Ganeshalingam, Mohan Horesh, Assaf Howell, D. Andrew Law, Nicholas M. Leonard, Douglas C. Li, Weidong Ofek, Eran O. Polishook, David Poznanski, Dovi Quimby, Robert M. Silverman, Jeffrey M. Sternberg, Assaf Xu, Dong TI CALCIUM-RICH GAP TRANSIENTS IN THE REMOTE OUTSKIRTS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; Galaxy: halo; novae, cataclysmic variables; supernovae: individual (SN2005E, SN2007ke, PTF09dav, PTF10iuv, PTF11bij); surveys; white dwarfs ID OBSERVATORY SUPERNOVA SEARCH; CORE-COLLAPSE SUPERNOVAE; CHANDRASEKHAR MASS MODELS; HELIUM SHELL DETONATIONS; IA SUPERNOVAE; LOW-LUMINOSITY; WHITE-DWARF; HOST GALAXY; LIGHT-CURVE; BLACK-HOLE AB From the first two seasons of the Palomar Transient Factory, we identify three peculiar transients (PTF 09dav, PTF 10iuv, and PTF 11bij) with five distinguishing characteristics: peak luminosity in the gap between novae and supernovae (M-R approximate to -15.5 to -16.5 mag), rapid photometric evolution (t(rise) approximate to 12-15 days), large photospheric velocities (approximate to 6000-11,000 km s(-1)), early spectroscopic evolution into nebular phase (approximate to 1-3 months), and peculiar nebular spectra dominated by calcium. We also culled the extensive decade-long Lick Observatory Supernova Search database and identified an additional member of this group, SN 2007ke. Our choice of photometric and spectroscopic properties was motivated by SN 2005E (Perets et al.). To our surprise, as in the case of SN 2005E, all four members of this group are also clearly offset from the bulk of their host galaxy. Given the well-sampled early-and late-time light curves, we derive ejecta masses in the range of 0.4-0.7 M-circle dot. Spectroscopically, we find that there may be a diversity in the photospheric phase, but the commonality is in the unusual nebular spectra. Our extensive follow-up observations rule out standard thermonuclear and standard core-collapse explosions for this class of "calcium-rich gap" transients. If the progenitor is a white dwarf, we are likely seeing a detonation of the white dwarf core and perhaps even shock-front interaction with a previously ejected nova shell. If the progenitor is a massive star, a nonstandard channel specific to a low-metallicity environment needs to be invoked (e. g., ejecta fallback leading to black hole formation). Detection (or the lack thereof) of a faint underlying host (dwarf galaxy and cluster) will provide a crucial and decisive diagnostic to choose between these alternatives. C1 [Kasliwal, Mansi M.; Kulkarni, S. R.; Bhalerao, Varun B.; Horesh, Assaf; Quimby, Robert M.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Gal-Yam, Avishay; Yaron, Ofer; Arcavi, Iair; Ben-Ami, Sagi; Ofek, Eran O.; Polishook, David; Sternberg, Assaf; Xu, Dong] Weizmann Inst Sci, Fac Phys, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA. [Nugent, Peter E.; Bloom, Joshua S.; Cenko, S. Bradley; Filippenko, Alexei V.; Ganeshalingam, Mohan; Li, Weidong; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Sullivan, Mark] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Bildsten, Lars] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bildsten, Lars; Howell, D. Andrew] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Perets, Hagai B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02338 USA. [Frail, Dale A.] Natl Radio Astron Observ, Array Operat Ctr, Socorro, NM 87801 USA. [Howell, D. Andrew] Las Cumbres Observ Global Telescope Network Inc, Santa Barbara, CA 93117 USA. [Law, Nicholas M.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Quimby, Robert M.] Univ Tokyo, IPMU, Kashiwa, Chiba, Japan. RP Kasliwal, MM (reprint author), CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. RI Perets, Hagai/K-9605-2015; Horesh, Assaf/O-9873-2016; OI Perets, Hagai/0000-0002-5004-199X; Horesh, Assaf/0000-0002-5936-1156; Bhalerao, Varun/0000-0002-6112-7609; Sullivan, Mark/0000-0001-9053-4820 FU Hubble Fellowship; Carnegie-Princeton Fellowship; Einstein Fellowship; Israel Science Foundation; US-Israel Binational Science Foundation; Minerva/ARCHES Prize; Richard and Rhoda Goldman Fund; TABASGO Foundation; National Science Foundation (NSF) [AST-0908886]; Sun Microsystems, Inc.; Hewlett-Packard Company; Hewlett-Packard Company, AutoScope Corporation; Lick Observatory; NSF; University of California; Sylvia and Jim Katzman Foundation; U.S, DOE [DE-AC02-05CH11231, DE-FG02-06ER06-04]; NSF-CDI [0941742]; Royal Society; NSF [PHY-11-25915, AST-11-09174, AST-1009571]; W. M. Keck Foundation FX M.M.K. acknowledges support from the Hubble Fellowship and Carnegie-Princeton Fellowship. E.O.O. is supported by an Einstein Fellowship. H. B. P. is a CfA and Bikura prize fellow. The Weizmann Institute's participation in PTF is supported by grants to AGY from the Israel Science Foundation, the US-Israel Binational Science Foundation and the Minerva/ARCHES Prize. A. V. F. and his group at UC Berkeley acknowledge generous financial assistance from Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, and National Science Foundation (NSF) grant AST-0908886. KAIT was constructed and supported by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. Computational resources and data storage were contributed by NERSC, supported by U.S, DOE contract DE-AC02-05CH11231. P.E.N. acknowledges support from the U.S. DOE contract DE-FG02-06ER06-04. J.S.B. acknowledges support of an NSF-CDI grant 0941742, "Real-time Classification of Massive Time-series Data Streams." M. S. acknowledges support from the Royal Society. L. B. acknowledges NSF grants PHY-11-25915 and AST-11-09174. D. C. L. acknowledges NSF grant AST-1009571.; Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration; it was made possible by the generous financial support of the W. M. Keck Foundation. The Expanded Very Large Array is operated by the National Radio Astronomy Observatory, a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. 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. All spectra are available in digital form at WISEREP (Yaron & Gal-Yam 2012; http:www.weizmann.ac.il/astrophysics/wiserep/). NR 66 TC 47 Z9 47 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 AUG 20 PY 2012 VL 755 IS 2 AR 161 DI 10.1088/0004-637X/755/2/161 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400078 ER PT J AU Lau, ET Nagai, D Kravtsov, AV Vikhlinin, A Zentner, AR AF Lau, Erwin T. Nagai, Daisuke Kravtsov, Andrey V. Vikhlinin, Alexey Zentner, Andrew R. TI CONSTRAINING CLUSTER PHYSICS WITH THE SHAPE OF X-RAY CLUSTERS: COMPARISON OF LOCAL X-RAY CLUSTERS VERSUS Lambda CDM CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; X-rays: galaxies: clusters ID DARK-MATTER HALOES; GALAXY CLUSTERS; INTRACLUSTER MEDIUM; ANGULAR-MOMENTUM; LENSING ANALYSIS; SIMULATIONS; UNIVERSE; GAS; ALIGNMENTS; COSMOLOGY AB Recent simulations of cluster formation have demonstrated that condensation of baryons into central galaxies during cluster formation can drive the shape of the gas distribution in galaxy clusters significantly rounder out to their virial radius. These simulations generally predict stellar fractions within cluster virial radii that are similar to 2-3 times larger than the stellar masses deduced from observations. In this paper, we compare ellipticity profiles of simulated clusters performed with varying input physics (radiative cooling, star formation, and supernova feedback) to the cluster ellipticity profiles derived from Chandra and ROSAT observations, in an effort to constrain the fraction of gas that cools and condenses into the central galaxies within clusters. We find that local relaxed clusters have an average ellipticity of epsilon = 0.18 +/- 0.05 in the radial range of 0.04 <= r/r(500) <= 1. At larger radii r > 0.1r(500), the observed ellipticity profiles agree well with the predictions of non-radiative simulations. In contrast, the ellipticity profiles of simulated clusters that include dissipative gas physics deviate significantly from the observed ellipticity profiles at all radii. The dissipative simulations overpredict (underpredict) ellipticity in the inner (outer) regions of galaxy clusters. By comparing simulations with and without dissipative gas physics, we show that gas cooling causes the gas distribution to be more oblate in the central regions, but makes the outer gas distribution more spherical. We find that late-time gas cooling and star formation are responsible for the significantly oblate gas distributions in cluster cores, but the gas shapes outside of cluster cores are set primarily by baryon dissipation at high redshift (z >= 2). Our results indicate that the shapes of X-ray emitting gas in galaxy clusters, especially at large radii, can be used to place constraints on cluster gas physics, making it potential probes of the history of baryonic cooling in galaxy clusters. C1 [Lau, Erwin T.; Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Lau, Erwin T.; Nagai, Daisuke] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Kravtsov, Andrey V.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Kravtsov, Andrey V.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vikhlinin, Alexey] Space Res Inst, Moscow 117997, Russia. [Zentner, Andrew R.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Zentner, Andrew R.] Univ Pittsburgh, Pittsburgh Particle Phys Astrophys & Cosmol Ctr P, Pittsburgh, PA 15260 USA. RP Lau, ET (reprint author), Yale Univ, Dept Phys, New Haven, CT 06520 USA. EM erwin.lau@yale.edu FU NSF [AST-1009811, AST-0507596, AST-0807444, AST-0806367, AST-1108802]; NASA ATP [NNX11AE07G]; Yale University; NASA [NAG5-13274]; Kavli Institute for Cosmological Physics at the University of Chicago [NSF PHY-0551142, PHY-1125897]; Pittsburgh Particle physics, Astrophysics, and Cosmology Center (PITT PACC) FX The cosmological simulations used in this study were performed on the IBM RS/6000 SP4 system (copper) at the National Center for Supercomputing Applications (NCSA). This work was supported in part by the facilities and staff of the Yale University Faculty of Arts and Sciences High Performance Computing Center. E. L. and D.N. acknowledge the support from the NSF grant AST-1009811, by NASA ATP grant NNX11AE07G, and by Yale University. A. K. was supported by NSF grants AST-0507596 and AST-0807444, NASA grant NAG5-13274, and by the Kavli Institute for Cosmological Physics at the University of Chicago through grants NSF PHY-0551142 and PHY-1125897. A.R.Z. was supported by the Pittsburgh Particle physics, Astrophysics, and Cosmology Center (PITT PACC) and by the NSF through grants AST-0806367 and AST-1108802. NR 58 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2012 VL 755 IS 2 AR 116 DI 10.1088/0004-637X/755/2/116 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400033 ER PT J AU Masters, D Capak, P Salvato, M Civano, F Mobasher, B Siana, B Hasinger, G Impey, CD Nagao, T Trump, JR Ikeda, H Elvis, M Scoville, N AF Masters, D. Capak, P. Salvato, M. Civano, F. Mobasher, B. Siana, B. Hasinger, G. Impey, C. D. Nagao, T. Trump, J. R. Ikeda, H. Elvis, M. Scoville, N. TI EVOLUTION OF THE QUASAR LUMINOSITY FUNCTION OVER 3 < z < 5 IN THE COSMOS SURVEY FIELD SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: luminosity function, mass function; Galaxy: evolution; quasars: general ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; SIMILAR-TO 4; HIGH-REDSHIFT; RADIATIVE-TRANSFER; FAINT END; PHOTOMETRIC REDSHIFT AB We investigate the high-redshift quasar luminosity function (QLF) down to an apparent magnitude of I-AB = 25 in the Cosmic Evolution Survey (COSMOS). Careful analysis of the extensive COSMOS photometry and imaging data allows us to identify and remove stellar and low-redshift contaminants, enabling a selection that is nearly complete for type-1 quasars at the redshifts of interest. We find 155 likely quasars at z > 3.1, 39 of which have prior spectroscopic confirmation. We present our sample in detail and use these confirmed and likely quasars to compute the rest-frame UV QLF in the redshift bins 3.1 < z < 3.5 and 3.5 < z < 5. The space density of faint quasars decreases by roughly a factor of four from z similar to 3.2 to z similar to 4, with faint-end slopes of beta similar to -1.7 at both redshifts. The decline in space density of faint optical quasars at z > 3 is similar to what has been found for more luminous optical and X-ray quasars. We compare the rest-frame UV luminosity functions found here with the X-ray luminosity function at z > 3, and find that they evolve similarly between z similar to 3.2 and z similar to 4; however, the different normalizations imply that roughly 75% of X-ray bright active galactic nuclei (AGNs) at z similar to 3-4 are optically obscured. This fraction is higher than found at lower redshift and may imply that the obscured, type-2 fraction continues to increase with redshift at least to z similar to 4. Finally, the implications of the results derived here for the contribution of quasars to cosmic reionization are discussed. C1 [Masters, D.; Mobasher, B.; Siana, B.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Masters, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Capak, P.; Scoville, N.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Capak, P.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Salvato, M.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Civano, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Impey, C. D.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Impey, C. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Nagao, T.; Ikeda, H.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Trump, J. R.; Elvis, M.] Univ Calif Santa Cruz, Lick Observ, Univ Calif Observ, Santa Cruz, CA 95064 USA. [Trump, J. R.; Elvis, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Masters, D (reprint author), Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. FU German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize [FKZ HA 1850/28-1]; Infrared Processing and Analysis Center (IPAC) Visiting Graduate Fellowship program; Carnegie Visiting Graduate Fellowship program FX We gratefully acknowledge the contributions of the entire COSMOS collaboration. More information about the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. We acknowledge the anonymous referee for suggestions that significantly improved this work. We thank Dr. Eilat Glikman for helpful discussions. M. S. and G. H. acknowledge support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). D. M. gratefully acknowledges the support of the Infrared Processing and Analysis Center (IPAC) Visiting Graduate Fellowship program, as well as the Carnegie Visiting Graduate Fellowship program. NR 58 TC 41 Z9 41 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 AUG 20 PY 2012 VL 755 IS 2 AR 169 DI 10.1088/0004-637X/755/2/169 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400086 ER PT J AU Neill, JL Muckle, MT Zaleski, DP Steber, AL Pate, BH Lattanzi, V Spezzano, S McCarthy, MC Remijan, AJ AF Neill, Justin L. Muckle, Matt T. Zaleski, Daniel P. Steber, Amanda L. Pate, Brooks H. Lattanzi, Valerio Spezzano, Silvia McCarthy, Michael C. Remijan, Anthony J. TI LABORATORY AND TENTATIVE INTERSTELLAR DETECTION OF TRANS-METHYL FORMATE USING THE PUBLICLY AVAILABLE GREEN BANK TELESCOPE PRIMOS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: clouds; ISM: individual objects (Sagittarius B2(N)); ISM: molecules ID DOUBLE-RESONANCE SPECTROSCOPY; HOT MOLECULAR CORES; GAS-PHASE; SAGITTARIUS B2; DISSOCIATIVE RECOMBINATION; MICROWAVE SPECTROMETER; GALACTIC-CENTER; STAR-FORMATION; FORMIC-ACID; ORGANIC-MOLECULES AB The rotational spectrum of the higher-energy trans-conformational isomer of methyl formate has been assigned for the first time using several pulsed-jet Fourier transform microwave spectrometers in the 6-60 GHz frequency range. This species has also been sought toward the Sagittarius B2(N) molecular cloud using the publicly available PRIMOS survey from the Green Bank Telescope. We detect seven absorption features in the survey that coincide with laboratory transitions of trans-methyl formate, from which we derive a column density of 3.1 (+2.6, -1.2) x 10(13) cm(-2) and a rotational temperature of 7.6 +/- 1.5 K. This excitation temperature is significantly lower than that of the more stable cis conformer in the same source but is consistent with that of other complex molecular species recently detected in Sgr B2(N). The difference in the rotational temperatures of the two conformers suggests that they have different spatial distributions in this source. As the abundance of trans-methyl formate is far higher than would be expected if the cis and trans conformers are in thermodynamic equilibrium, processes that could preferentially form trans-methyl formate in this region are discussed. We also discuss measurements that could be performed to make this detection more certain. This manuscript demonstrates how publicly available broadband radio astronomical surveys of chemically rich molecular clouds can be used in conjunction with laboratory rotational spectroscopy to search for new molecules in the interstellar medium. C1 [Neill, Justin L.; Muckle, Matt T.; Zaleski, Daniel P.; Steber, Amanda L.; Pate, Brooks H.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Neill, Justin L.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lattanzi, Valerio; Spezzano, Silvia; McCarthy, Michael C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lattanzi, Valerio; Spezzano, Silvia; McCarthy, Michael C.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Remijan, Anthony J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. RP Neill, JL (reprint author), Univ Virginia, Dept Chem, McCormick Rd,POB 400319, Charlottesville, VA 22904 USA. EM jneill@umich.edu; brookspate@virginia.edu; aremijan@nrao.edu OI Steber, Amanda/0000-0002-8203-2174; McCarthy, Michael/0000-0001-9142-0008; Zaleski, Daniel/0000-0003-0153-9158 FU NSF Centers for Chemical Innovation [CHE-0847919] FX The authors acknowledge support from the NSF Centers for Chemical Innovation (CHE-0847919). We also thank Eric Herbst and Susanna Widicus Weaver for fruitful discussions, and the anonymous referee for helpful comments to improve the manuscript. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 71 TC 25 Z9 25 U1 2 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 AUG 20 PY 2012 VL 755 IS 2 AR 153 DI 10.1088/0004-637X/755/2/153 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400070 ER PT J AU Reynolds, CS Brenneman, LW Lohfink, AM Trippe, ML Miller, JM Fabian, AC Nowak, MA AF Reynolds, Christopher S. Brenneman, Laura W. Lohfink, Anne M. Trippe, Margaret L. Miller, Jon M. Fabian, Andrew C. Nowak, Michael A. TI A MONTE CARLO MARKOV CHAIN BASED INVESTIGATION OF BLACK HOLE SPIN IN THE ACTIVE GALAXY NGC 3783 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: individual (NGC 3783); galaxies: nuclei; galaxies: Seyfert; X-rays: galaxies ID GALACTIC NUCLEI; RADIATIVE LEVITATION; SEYFERT-1 GALAXIES; EDDINGTON RATIO; EMISSION-LINES; IONIZED-GAS; IRON LINES; SYSTEMS; SPECTROSCOPY; VARIABILITY AB The analysis of relativistically broadened X-ray spectral features from the inner accretion disk provides a powerful tool for measuring the spin of supermassive black holes in active galactic nuclei (AGNs). However, AGN spectra are often complex and careful analysis employing appropriate and self-consistent models is required if one has to obtain robust results. In this paper, we revisit the deep 2009 July Suzaku observation of the Seyfert galaxy NGC 3783 in order to study in a rigorous manner the robustness of the inferred black hole spin parameter. Using Monte Carlo Markov chain techniques, we identify a (partial) modeling degeneracy between the iron abundance of the disk and the black hole spin parameter. We show that the data for NGC 3783 strongly require both supersolar iron abundance (Z(Fe) = 2-4Z(circle dot)) and a rapidly spinning black hole (a > 0.89). We discuss various astrophysical considerations that can affect the measured abundance. We note that, while the abundance enhancement inferred in NGC 3783 is modest, the X-ray analysis of some other objects has found extreme iron abundances. We introduce the hypothesis that the radiative levitation of iron ions in the innermost regions of radiation-dominated AGN disks can enhance the photospheric abundance of iron. We show that radiative levitation is a plausible mechanism in the very inner regions of high accretion rate AGN disks. C1 [Reynolds, Christopher S.; Lohfink, Anne M.; Trippe, Margaret L.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reynolds, Christopher S.; Lohfink, Anne M.; Trippe, Margaret L.] Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Brenneman, Laura W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Fabian, Andrew C.] Inst Astron, Cambridge CB3 OHA, England. [Nowak, Michael A.] MIT Kavli Inst Astrophys, Cambridge, MA USA. RP Reynolds, CS (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM chris@astro.umd.edu; alohfink@astro.umd.edu RI XRAY, SUZAKU/A-1808-2009 FU NASA Suzaku Guest Observer Program [NNX10AR31G]; NASA Long Term Space Astrophysics grant [NAG513065] FX We thank Cole Miller, James Reeves, and Adam Patrick for useful discussions during the course of this work. We also thank the anonymous referee for their positive and insightful comments, which significantly improved the paper. 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. C.S.R. and A.M.L. thank support from the NASA Suzaku Guest Observer Program under grant NNX10AR31G. M.L.T. thanks support from NASA Long Term Space Astrophysics grant NAG513065. NR 38 TC 27 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 AUG 20 PY 2012 VL 755 IS 2 AR 88 DI 10.1088/0004-637X/755/2/88 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400005 ER PT J AU Rosenfield, P Johnson, LC Girardi, L Dalcanton, JJ Bressan, A Lang, D Williams, BF Guhathakurta, P Howley, KM Lauer, TR Bell, EF Bianchi, L Caldwell, N Dolphin, A Dorman, CE Gilbert, KM Kalirai, J Larsen, SS Olsen, KAG Rix, HW Seth, AC Skillman, ED Weisz, DR AF Rosenfield, Philip Johnson, L. Clifton Girardi, Leo Dalcanton, Julianne J. Bressan, Alessandro Lang, Dustin Williams, Benjamin F. Guhathakurta, Puragra Howley, Kirsten M. Lauer, Tod R. Bell, Eric F. Bianchi, Luciana Caldwell, Nelson Dolphin, Andrew Dorman, Claire E. Gilbert, Karoline M. Kalirai, Jason Larsen, Soren S. Olsen, Knut A. G. Rix, Hans-Walter Seth, Anil C. Skillman, Evan D. Weisz, Daniel R. TI THE PANCHROMATIC HUBBLE ANDROMEDA TREASURY. I. BRIGHT UV STARS IN THE BULGE OF M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (M31); galaxies: stellar content; stars: evolution; stars: horizontal-branch ID EARLY-TYPE GALAXIES; GALACTIC GLOBULAR-CLUSTERS; HORIZONTAL-BRANCH STARS; SUBDWARF-B-STARS; ELLIPTIC GALAXIES; STELLAR POPULATIONS; FAR-ULTRAVIOLET; GIANT BRANCH; SURFACE PHOTOMETRY; LINE-STRENGTHS AB As part of the Panchromatic Hubble Andromeda Treasury multi-cycle program, we observed a 12' x 6.'5 area of the bulge of M31 with theWFC3/UVIS filters F275W and F336W. From these data we have assembled a sample of similar to 4000 UV-bright, old stars, vastly larger than previously available. We use updated Padova stellar evolutionary tracks to classify these hot stars into three classes: Post-AGB stars (P-AGB), Post-Early AGB (PE-AGB) stars, and AGB-manque stars. P-AGB stars are the end result of the asymptotic giant branch (AGB) phase and are expected in a wide range of stellar populations, whereas PE-AGB and AGB-manque (together referred to as the hot post-horizontal branch; HP-HB) stars are the result of insufficient envelope masses to allow a full AGB phase, and are expected to be particularly prominent at high helium or alpha abundances when the mass loss on the red giant branch is high. Our data support previous claims that most UV-bright sources in the bulge are likely hot (extreme) horizontal branch (EHB) stars and their progeny. We construct the first radial profiles of these stellar populations and show that they are highly centrally concentrated, even more so than the integrated UV or optical light. However, we find that this UV-bright population does not dominate the total UV luminosity at any radius, as we are detecting only the progeny of the EHB stars that are the likely source of the UV excess. We calculate that only a few percent of main-sequence stars in the central bulge can have gone through the HP-HB phase and that this percentage decreases strongly with distance from the center. We also find that the surface density of hot UV-bright stars has the same radial variation as that of low-mass X-ray binaries. We discuss age, metallicity, and abundance variations as possible explanations for the observed radial variation in the UV-bright population. C1 [Rosenfield, Philip; Johnson, L. Clifton; Dalcanton, Julianne J.; Williams, Benjamin F.; Gilbert, Karoline M.; Weisz, Daniel R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Girardi, Leo] Osservatorio Astron Padova INAF, I-35122 Padua, Italy. [Bressan, Alessandro] SISSA, I-34136 Trieste, Italy. [Lang, Dustin] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Guhathakurta, Puragra; Dorman, Claire E.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Guhathakurta, Puragra; Dorman, Claire E.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Howley, Kirsten M.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Lauer, Tod R.; Olsen, Knut A. G.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bianchi, Luciana] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dolphin, Andrew] Raytheon Co, Tucson, AZ 85756 USA. [Kalirai, Jason] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Larsen, Soren S.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. [Rix, Hans-Walter] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Seth, Anil C.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Skillman, Evan D.] Univ Minnesota, Minnesota Inst Astrophys, Minneapolis, MN 55455 USA. RP Rosenfield, P (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. OI Rosenfield, Philip/0000-0001-9306-6049; Johnson, Lent/0000-0001-6421-0953; Bell, Eric/0000-0002-5564-9873 FU NASA [NAS 5-26555, NAS5-26555]; Space Telescope Science Institute [GO-12055]; [ASI-INAF I/009/10/0] FX Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.; This work was supported by the Space Telescope Science Institute through GO-12055. P. R. wishes to express his gratitude to L. G., A. B., and Paola Marigo for invaluable guidance and for graciously hosting him in Padova. We thank Brent Groves and the M31 Herschel imaging collaboration for allowing us to examine early Herschel observations of the bulge. We are grateful to Pauline Barmby for providing us the Spitzer IRAC images. We thank Roberto Saglia for providing us with metallicity values of the M31 bulge. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by JPL/Caltech, under contract with NASA. The FOC data have been 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. L. G. and A. B. acknowledge support from contract ASI-INAF I/009/10/0. NR 72 TC 15 Z9 15 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 AUG 20 PY 2012 VL 755 IS 2 AR 131 DI 10.1088/0004-637X/755/2/131 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400048 ER PT J AU Schnee, S Sadavoy, S Di Francesco, J Johnstone, D Wei, L AF Schnee, Scott Sadavoy, Sarah Di Francesco, James Johnstone, Doug Wei, Lisa TI AN OBSERVED LACK OF SUBSTRUCTURE IN STARLESS CORES. II. SUPER-JEANS CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: jets and outflows; stars: formation; stars: protostars ID MAGNETIZED MOLECULAR CLOUDS; 1ST HYDROSTATIC CORE; GOULD BELT CLOUDS; DENSE CORES; PROTOSTELLAR CORES; SUBMILLIMETER ARRAY; INITIAL CONDITIONS; GAS TEMPERATURE; PRESTELLAR CORE; PERSEUS AB We present SMA and CARMA continuum and spectral line observations of five dense cores located in the Perseus and Ophiuchus molecular clouds whose masses exceed their thermal Jeans masses. Three of these cores have previously been identified as being starless and two have been classified as being possibly protostellar. We find that one core is certainly protostellar. The other four cores, however, are starless and undetected in both (CO)-O-18 and 1.3 mm continuum emission. These four starless cores have flat density profiles out to at least similar to 0.006 pc, which is typical for starless cores in general. Density profiles predicted by some collapse models, especially in the early stages of infall, are consistent with our observations. Archival data reveal that these starless cores have significant non-thermal support against collapse, although they may still be unstable. C1 [Schnee, Scott] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Sadavoy, Sarah; Di Francesco, James; Johnstone, Doug] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Sadavoy, Sarah; Di Francesco, James; Johnstone, Doug] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Wei, Lisa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wei, Lisa] Atmospher & Environm Res, Lexington, MA 02421 USA. RP Schnee, S (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM sschnee@nrao.edu OI Johnstone, Doug/0000-0002-6773-459X FU National Research Council of Canada; Natural Sciences and Engineering Council of Canada; Natural Sciences and Engineering Research Council of Canada (NSERC); 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; state of California; state of Illinois; state of Maryland; National Science Foundation FX We thank Robert Gutermuth for helpful discussion on the nature of Per-8. We thank our anonymous referee for suggestions that improved this paper. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. J.D.F. acknowledges support by the National Research Council of Canada and the Natural Sciences and Engineering Council of Canada (via a Discovery Grant). D.J. is supported by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant. 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 41 TC 10 Z9 10 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 AUG 20 PY 2012 VL 755 IS 2 AR 178 DI 10.1088/0004-637X/755/2/178 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400095 ER PT J AU Shcherbakov, RV Penna, RF McKinney, JC AF Shcherbakov, Roman V. Penna, Robert F. McKinney, Jonathan C. TI SAGITTARIUS A* ACCRETION FLOW AND BLACK HOLE PARAMETERS FROM GENERAL RELATIVISTIC DYNAMICAL AND POLARIZED RADIATIVE MODELING SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; Galaxy: center; polarization; radiative transfer; relativistic processes ID ADVECTION-DOMINATED ACCRETION; MAGNETIC-FIELD GEOMETRY; NEAR-INFRARED FLARES; GALACTIC-CENTER; SYNCHROTRON-RADIATION; CIRCULAR-POLARIZATION; X-RAY; LINEAR-POLARIZATION; MILLIMETER-VLBI; 86 GHZ AB We obtain estimates of Sgr A* accretion flow and black hole parameters by fitting polarized submillimeter observations with spectra computed using three-dimensional general relativistic (GR) magnetohydrodynamical (MHD) (GRMHD) simulations. Observations are compiled from averages over many epochs from reports in 29 papers for estimating the mean fluxes F-nu, linear polarization (LP) fractions, circular polarization (CP) fractions, and electric vector position angles. GRMHD simulations are computed with dimensionless spins a(*) = 0, 0.5, 0.7, 0.9, 0.98 over a 20,000 M time interval. We perform fully self-consistent GR polarized radiative transfer using our new code to explore the effects of spin a*, inclination angle theta, position angle (P. A.), accretion rate (M) over dot, and electron temperature T-e (T-e is reported for radius 6M). By fitting the mean submillimeter fluxes and LP/CP fractions, we obtain estimates for these model parameters and determine the physical effects that could produce polarization signatures. Our best-bet model has a(*) = 0.5, theta = 75 degrees, P.A. = 115 degrees, (M) over dot = 4.6 x 10(-8) M-circle dot yr(-1), and T-e = 3.1x10(10) K at 6M. The submillimeter CP is mainly produced by Faraday conversion as modified by Faraday rotation, and the emission region size at 230 GHz is consistent with the very long baseline interferometry size of 37 mu as. Across all spins, model parameters are in the ranges theta = 42 degrees-75 degrees, (M) over dot = (1.4-7.0) x 10(-8) M-circle dot yr(-1), and T-e = (3-4) x 10(10) K. Polarization is found both to help differentiate models and to introduce new observational constraints on the effects of the magnetic field that might not be fit by accretion models so far considered. C1 [Shcherbakov, Roman V.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Penna, Robert F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [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 Shcherbakov, RV (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM roman@astro.umd.edu; rpenna@cfa.harvard.edu; jmckinne@stanford.edu FU NSF [TG-AST080025N, TG-AST080026N]; NASA [NNX08AX04H, NNX08AH32G, NNX11AE16G, HST-HF-51298.01, PF7-80048] FX The authors are grateful to Lei Huang for checking various emissivity prescriptions; to Ramesh Narayan for extensive discussions and comments; to Avi Loeb, Avery Broderick, James Moran, Alexander Tchekhovskoy, Cole Miller, Julian Krolik, Steven Cranmer for insightful comments; and to Jim Stone for encouragement with self-consistent radiative transfer. We thank the anonymous referees for their extensive feedback, which helped to improve the manuscript. The numerical simulations and the radiative transfer calculations in this paper were partially run on the Odyssey cluster supported by the FAS Sciences Division Research Computing Group at Harvard, Deepthought cluster at the University of Maryland, and were partially supported by NSF through TeraGrid resources provided by NCSA (Abe), LONI (QueenBee), and NICS (Kraken) under grant numbers TG-AST080025N and TG-AST080026N. The paper is partially supported by NASA grants NNX08AX04H (R.V.S. and Ramesh Narayan), NNX08AH32G and NNX11AE16G (Ramesh Narayan), NASA Hubble Fellowship grant HST-HF-51298.01 (R.V.S.), NSF Graduate Research Fellowship (R. F. P.), and NASA Chandra Fellowship PF7-80048 (J.C.M.). NR 107 TC 46 Z9 45 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 AUG 20 PY 2012 VL 755 IS 2 AR 133 DI 10.1088/0004-637X/755/2/133 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 992PL UT WOS:000307791400050 ER PT J AU Berger, E Chornock, R Lunnan, R Foley, R Czekala, I Rest, A Leibler, C Soderberg, AM Roth, K Narayan, G Huber, ME Milisavljevic, D Sanders, NE Drout, M Margutti, R Kirshner, RP Marion, GH Challis, PJ Riess, AG Smartt, SJ Burgett, WS Hodapp, KW Heasley, JN Kaiser, N Kudritzki, RP Magnier, EA McCrum, M Price, PA Smith, K Tonry, JL Wainscoat, RJ AF Berger, E. Chornock, R. Lunnan, R. Foley, R. Czekala, I. Rest, A. Leibler, C. Soderberg, A. M. Roth, K. Narayan, G. Huber, M. E. Milisavljevic, D. Sanders, N. E. Drout, M. Margutti, R. Kirshner, R. P. Marion, G. H. Challis, P. J. Riess, A. G. Smartt, S. J. Burgett, W. S. Hodapp, K. W. Heasley, J. N. Kaiser, N. Kudritzki, R. -P. Magnier, E. A. McCrum, M. Price, P. A. Smith, K. Tonry, J. L. Wainscoat, R. J. TI ULTRALUMINOUS SUPERNOVAE AS A NEW PROBE OF THE INTERSTELLAR MEDIUM IN DISTANT GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: ISM; supernovae: individual (PS1-11bam) ID GAMMA-RAY BURST; MASS-METALLICITY RELATION; HUBBLE-SPACE-TELESCOPE; LY-ALPHA SYSTEMS; DEEP DEEP SURVEY; STAR-FORMATION; HOST GALAXIES; REDSHIFT; AFTERGLOWS; ABSORPTION AB We present the Pan-STARRS1 discovery and light curves, and follow-up MMT and Gemini spectroscopy of an ultraluminous supernova (ULSN; dubbed PS1-11bam) at a redshift of z = 1.566 with a peak brightness of M-UV approximate to -22.3 mag. PS1-11bam is one of the highest redshift spectroscopically confirmed SNe known to date. The spectrum exhibits broad absorption features typical of previous ULSNe (e.g., C II, Si III), and strong and narrow Mg II and Fe II absorption lines from the interstellar medium (ISM) of the host galaxy, confirmed by an [O II]lambda 3727 emission line at the same redshift. The equivalent widths of the Fe II lambda 2600 and Mg II lambda 2803 lines are in the top quartile of the quasar intervening absorption system distribution, but are weaker than those of gamma-ray burst intrinsic absorbers (i.e., GRB host galaxies). We also detect the host galaxy in pre-explosion Pan-STARRS1 data and find that its UV spectral energy distribution is best fit with a young stellar population age of tau(*) approximate to 15-45 Myr and a stellar mass of M-* approximate to (1.1-2.6) x 10(9) M-circle dot (for Z = 0.05-1 Z(circle dot)). The star formation rate inferred from the UV continuum and [O II]lambda 3727 emission line is approximate to 10 M-circle dot yr(-1), higher than in previous ULSN hosts. PS1-11bam provides the first direct demonstration that ULSNe can serve as probes of the ISM in distant galaxies. The depth and red sensitivity of PS1 are uniquely suited to finding such events at cosmologically interesting redshifts (z similar to 1-2); the future combination of LSST and 30 m class telescopes promises to extend this technique to z similar to 4. C1 [Berger, E.; Chornock, R.; Lunnan, R.; Foley, R.; Czekala, I.; Leibler, C.; Soderberg, A. M.; Narayan, G.; Milisavljevic, D.; Sanders, N. E.; Drout, M.; Margutti, R.; Kirshner, R. P.; Marion, G. H.; Challis, P. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rest, A.; Riess, A. G.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Roth, K.] Gemini Observ, Hilo, HI 96720 USA. [Huber, M. E.; Burgett, W. S.; Hodapp, K. W.; Heasley, J. N.; Kaiser, N.; Kudritzki, R. -P.; Magnier, E. A.; Tonry, J. L.; Wainscoat, R. J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Riess, A. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Smartt, S. J.; McCrum, M.; Smith, K.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Berger, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Lunnan, Ragnhild/0000-0001-9454-4639; Narayan, Gautham/0000-0001-6022-0484; Czekala, Ian/0000-0002-1483-8811 FU National Aeronautics and Space Administration [NNX08AR22G]; FAS Science Division Research Computing Group at Harvard University FX PS1 has been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS1 Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen'sUniversity Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network, Incorporated, the National Central University of Taiwan, and the National Aeronautics and Space Administration under grant NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. This work is based in part on observations obtained at the Gemini Observatory (Program GN-2011B-Q-3; PI: Berger), 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, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Observations were also obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 30 TC 30 Z9 30 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 AUG 20 PY 2012 VL 755 IS 2 AR L29 DI 10.1088/2041-8205/755/2/L29 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 989VM UT WOS:000307588900007 ER PT J AU McDonald, M Wei, LH Veilleux, S AF McDonald, Michael Wei, Lisa H. Veilleux, Sylvain TI COLD MOLECULAR GAS ALONG THE COOLING X-RAY FILAMENT IN A1795 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: clusters: individual (Abell 1795); galaxies: clusters: intracluster medium; galaxies: elliptical and lenticular, cD; ISM: jets and outflows; submillimeter: ISM ID BRIGHTEST CLUSTER GALAXIES; H-ALPHA FILAMENTS; FLOW CLUSTERS; HERSCHEL OBSERVATIONS; HYDROGEN EMISSION; LUMINOUS CLUSTERS; SPACE-TELESCOPE; NGC 1275; SPECTROSCOPY; CORES AB We present the results of interferometric observations of the cool core of A1795 at CO(1-0) using the Combined Array for Research in Millimeter-wave Astronomy. In agreement with previous work, we detect a significant amount of cold molecular gas (3.9 +/- 0.4 x 10(9) M-circle dot) in the central similar to 10 kpc. We report the discovery of a substantial clump of cold molecular gas at clustercentric radius of 30 kpc (2.9 +/- 0.4 x 10(9) M-circle dot), coincident in both position and velocity with the warm, ionized filaments. We also place an upper limit on the H-2 mass at the outer edge of the star-forming filament, corresponding to a distance of 60 kpc (<0.9 x 10(9) M-circle dot). We measure a strong gradient in the H alpha/H-2 ratio as a function of radius, suggesting different ionization mechanisms in the nucleus and filaments of A1795. The total mass of cold molecular gas (similar to 7 x 10(9) M-circle dot) is roughly 30% of the classical cooling estimate at the same position, assuming a cooling time of 10(9) yr. Combining the cold molecular gas mass with the UV-derived star formation rate and the warm, ionized gas mass, the spectroscopically derived X-ray cooling rate is fully accounted for and in good agreement with the cooling byproducts over timescales of similar to 10(9) yr. The overall agreement between the cooling rate of the hot intracluster medium and the mass of the cool gas reservoir suggests that, at least in this system, the cooling flow problem stems from a lack of observable cooling in the more diffuse regions at large radii. C1 [McDonald, Michael] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Wei, Lisa H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wei, Lisa H.] Atmospher & Environm Res, Lexington, MA 02421 USA. [Veilleux, Sylvain] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mcdonald@space.mit.edu; lisa.wei@cfa.harvard.edu; veilleux@astro.umd.edu FU NASA [2834-MIT-SAO-4018]; CXO [NAS8-03060]; NSF [AST-0606932, 100958]; Senior NPP Award FX M.M. was supported by NASA through contract 2834-MIT-SAO-4018, issued by CXO under contract NAS8-03060. S.V. acknowledges support from NSF through contracts AST-0606932, 100958, and from a Senior NPP Award held at the NASA GSFC. CARMA development and operations are supported by NSF and partner universities. We thank R. Mushotzky and L. Mundy for helpful discussions. Finally, we thank the anonymous referee for a careful review, which has greatly improved the final manuscript. NR 39 TC 9 Z9 10 U1 0 U2 2 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 AUG 20 PY 2012 VL 755 IS 2 AR L24 DI 10.1088/2041-8205/755/2/L24 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 989VM UT WOS:000307588900002 ER PT J AU Nidever, DL Zasowski, G Majewski, SR Bird, J Robin, AC Martinez-Valpuesta, I Beaton, RL Schonrich, R Schultheis, M Wilson, JC Skrutskie, MF O'Connell, RW Shetrone, M Schiavon, RP Johnson, JA Weiner, B Gerhard, O Schneider, DP Prieto, CA Sellgren, K Bizyaev, D Brewington, H Brinkmann, J Eisenstein, DJ Frinchaboy, PM Perez, AEG Holtzman, J Hearty, FR Malanushenko, E Malanushenko, V Muna, D Oravetz, D Pan, K Simmons, A Snedden, S Weaver, BA AF Nidever, David L. Zasowski, Gail Majewski, Steven R. Bird, Jonathan Robin, Annie C. Martinez-Valpuesta, Inma Beaton, Rachael L. Schoenrich, Ralph Schultheis, Mathias Wilson, John C. Skrutskie, Michael F. O'Connell, Robert W. Shetrone, Matthew Schiavon, Ricardo P. Johnson, Jennifer A. Weiner, Benjamin Gerhard, Ortwin Schneider, Donald P. Prieto, Carlos Allende Sellgren, Kris Bizyaev, Dmitry Brewington, Howard Brinkmann, Jon Eisenstein, Daniel J. Frinchaboy, Peter M. Perez, Ana Elia Garcia Holtzman, Jon Hearty, Fred R. Malanushenko, Elena Malanushenko, Viktor Muna, Demitri Oravetz, Daniel Pan, Kaike Simmons, Audrey Snedden, Stephanie Weaver, Benjamin A. TI THE APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT: FIRST DETECTION OF HIGH-VELOCITY MILKY WAY BAR STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: bulge; Galaxy: kinematics and dynamics; Galaxy: structure; surveys ID ON SPIRAL GALAXIES; STELLAR BARS; DATA RELEASE; SKY SURVEY; LONG BAR; BULGE; DIAGNOSTICS; KINEMATICS; SYSTEMS; SAMPLE AB Commissioning observations with the Apache Point Observatory Galactic Evolution Experiment (APOGEE), part of the Sloan Digital Sky Survey III, have produced radial velocities (RVs) for similar to 4700 K/M-giant stars in the Milky Way (MW) bulge. These high-resolution (R similar to 22,500), high-S/N (>100 per resolution element), near-infrared (NIR; 1.51-1.70 mu m) spectra provide accurate RVs (epsilon(V) similar to 0.2 km s(-1)) for the sample of stars in 18 Galactic bulge fields spanning -1 degrees < l < 20 degrees, vertical bar b vertical bar < 20 degrees, and delta > -32 degrees. This represents the largest NIR high-resolution spectroscopic sample of giant stars ever assembled in this region of the Galaxy. A cold (sigma(V) similar to 30 km s(-1)), high-velocity peak (V-GSR approximate to + 200 km s(-1)) is found to comprise a significant fraction (similar to 10%) of stars in many of these fields. These high RVs have not been detected in previous MW surveys and are not expected for a simple, circularly rotating disk. Preliminary distance estimates rule out an origin from the background Sagittarius tidal stream or a new stream in the MW disk. Comparison to various Galactic models suggests that these high RVs are best explained by stars in orbits of the Galactic bar potential, although some observational features remain unexplained. C1 [Nidever, David L.; Zasowski, Gail; Majewski, Steven R.; Beaton, Rachael L.; Wilson, John C.; Skrutskie, Michael F.; O'Connell, Robert W.; Perez, Ana Elia Garcia; Hearty, Fred R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Bird, Jonathan; Schoenrich, Ralph; Johnson, Jennifer A.; Sellgren, Kris] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Bird, Jonathan; Schoenrich, Ralph; Johnson, Jennifer A.; Sellgren, Kris] Ohio State Univ, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Robin, Annie C.; Schultheis, Mathias] Univ Franche Comte, OSU THETA, CNRS UMR 6213, Inst Utinam, F-25000 Besancon, France. [Martinez-Valpuesta, Inma; Gerhard, Ortwin] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Shetrone, Matthew] Univ Texas Austin, McDonald Observ, Ft Davis, TX 79734 USA. [Schiavon, Ricardo P.] Gemini Observ, Hilo, HI 96720 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Tucson, AZ 85721 USA. [Prieto, Carlos Allende] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Bizyaev, Dmitry; Brewington, Howard; Brinkmann, Jon; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Frinchaboy, Peter M.] Texas Christian Univ, Dept Phys & Astron, Ft Worth, TX 76129 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Muna, Demitri; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Weiner, Benjamin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Nidever, DL (reprint author), Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. EM dln5q@virginia.edu OI Weiner, Benjamin/0000-0001-6065-7483; Beaton, Rachael/0000-0002-1691-8217 FU SDSS-III/APOGEE; NSF [AST-0807945]; NASA Earth & Space Science Fellowship; French Agence Nationale de la Recherche [ANR-2010-BLAN-0508-01OTP]; Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy Office of Science.; National Aeronautics and Space Administration FX We thank Stelios Kazantzidis for giving us permission to use his N-body model. Support for D.L.N. was provided by SDSS-III/APOGEE and NSF grant AST-0807945. G.Z. was supported by a NASA Earth & Space Science Fellowship. A.C.R. acknowledges support from the French Agence Nationale de la Recherche under contract ANR-2010-BLAN-0508-01OTP. We thank the anonymous referee for useful comments that improved the manuscript.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 42 TC 35 Z9 35 U1 1 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 AUG 20 PY 2012 VL 755 IS 2 AR L25 DI 10.1088/2041-8205/755/2/L25 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 989VM UT WOS:000307588900003 ER PT J AU Chance, K AF Chance, Kelly TI Continuous pollution monitoring from space: The molecular physics, the spectroscopy, and the measurements SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 244th National Fall Meeting of the American-Chemical-Society (ACS) CY AUG 19-23, 2012 CL Philadelphia, PA SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc C1 [Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM kchance@cfa.harvard.edu NR 0 TC 0 Z9 0 U1 0 U2 0 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 AUG 19 PY 2012 VL 244 MA 45-PHYS PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 220XX UT WOS:000324621807209 ER PT J AU Peterson, KM Heaney, PJ Post, JE AF Peterson, Kristina M. Heaney, Peter J. Post, Jeffrey E. TI Time-resolved XRD study of the in situ formation of monoclinic hydrohematite SO ABSTRACTS OF PAPERS OF THE AMERICAN CHEMICAL SOCIETY LA English DT Meeting Abstract CT 244th National Fall Meeting of the American-Chemical-Society (ACS) CY AUG 19-23, 2012 CL Philadelphia, PA SP Amer Chem Soc, Div Hist Chem, Amer Chem Soc C1 [Peterson, Kristina M.; Heaney, Peter J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM kmp286@psu.edu NR 0 TC 0 Z9 0 U1 0 U2 1 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 AUG 19 PY 2012 VL 244 MA 105-ENVR PG 1 WC Chemistry, Multidisciplinary SC Chemistry GA 220XX UT WOS:000324621804330 ER PT J AU McDonald, M Bayliss, M Benson, BA Foley, RJ Ruel, J Sullivan, P Veilleux, S Aird, KA Ashby, MLN Bautz, M Bazin, G Bleem, LE Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT Dehaan, T Desai, S Dobbs, MA Dudley, JP Egami, E Forman, WR Garmire, GP George, EM Gladders, MD Gonzalez, AH Halverson, NW Harrington, NL High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McMahon, JJ Mehl, J Meyer, SS Miller, ED Mocanu, L Mohr, JJ Montroy, TE Murray, SS Natoli, T Padin, S Plagge, T Pryke, C Rawle, TD Reichardt, CL Rest, A Rex, M Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shaw, L Shirokoff, E Simcoe, R Song, J Spieler, HG Stalder, B Staniszewski, Z Stark, AA Story, K Stubbs, CW Suhada, R van Engelen, A Vanderlinde, K Vieira, JD Vikhlinin, A Williamson, R Zahn, O Zenteno, A AF McDonald, M. Bayliss, M. Benson, B. A. Foley, R. J. Ruel, J. Sullivan, P. Veilleux, S. Aird, K. A. Ashby, M. L. N. Bautz, M. Bazin, G. Bleem, L. E. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. Dehaan, T. Desai, S. Dobbs, M. A. Dudley, J. P. Egami, E. Forman, W. R. Garmire, G. P. George, E. M. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. Harrington, N. L. 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. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Miller, E. D. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Natoli, T. Padin, S. Plagge, T. Pryke, C. Rawle, T. D. Reichardt, C. L. Rest, A. Rex, M. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shaw, L. Shirokoff, E. Simcoe, R. Song, J. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Story, K. Stubbs, C. W. Suhada, R. van Engelen, A. Vanderlinde, K. Vieira, J. D. Vikhlinin, A. Williamson, R. Zahn, O. Zenteno, A. TI A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies SO NATURE LA English DT Article ID ACTIVE GALACTIC NUCLEI; SOUTH-POLE TELESCOPE; H-ALPHA FILAMENTS; X-RAY SOURCES; GAS; SPECTROSCOPY; EMISSION AB In the cores of some clusters of galaxies the hot intracluster plasma is dense enough that it should cool radiatively in the cluster's lifetime(1-3), leading to continuous 'cooling flows' of gas sinking towards the cluster centre, yet no such cooling flow has been observed. The low observed star-formation rates(4,5) and cool gas masses(6) for these 'cool-core' clusters suggest that much of the cooling must be offset by feedback to prevent the formation of a runaway cooling flow(7-10). Here we report X-ray, optical and infrared observations of the galaxy cluster SPT-CLJ2344-4243 (ref. 11) at redshift z = 0.596. These observations reveal an exceptionally luminous (8.2 x 10(45) erg s(-1)) galaxy cluster that hosts an extremely strong cooling flow (around 3,820 solar masses a year). Further, the central galaxy in this cluster appears to be experiencing a massive starburst (formation of around 740 solar masses a year), which suggests that the feedback source responsible for preventing runaway cooling in nearby cool-core clusters may not yet be fully established in SPT-CLJ2344-4243. This large starformation rate implies that a significant fraction of the stars in the central galaxy of this cluster may form through accretion of the intracluster medium, rather than (as is currently thought) assembling entirely via mergers. C1 [McDonald, M.; Sullivan, P.; Bautz, M.; Miller, E. D.; Simcoe, R.] MIT, MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Bayliss, M.; Ruel, J.; Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 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.; Mantz, A.; McMahon, J. J.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Natoli, T.; Padin, S.; Plagge, T.; 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.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Foley, R. J.; Ashby, M. L. N.; Forman, W. R.; Jones, C.; Murray, S. S.; Stalder, B.; Stark, A. A.; Stubbs, C. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Veilleux, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Veilleux, S.] NASA, Astroparticle Phys Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bazin, G.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Zenteno, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Natoli, T.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica, Dept Astron & Astrofis, Santiago, Chile. [Dehaan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Egami, E.; Marrone, D. P.; Rawle, T. D.; Rex, M.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Garmire, G. P.; Lueker, M.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [George, E. M.; Harrington, N. L.; Holzapfel, W. L.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] 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 Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Phys Div, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [McMahon, J. 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, Ctr Educ & Res Cosmol & Astrophys, Phys Dept, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Phys Dept, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Inst Chicago, Sch Art, Liberal Arts Dept, Chicago, IL 60603 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. RP McDonald, M (reprint author), MIT, MIT Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mcdonald@space.mit.edu RI Holzapfel, William/I-4836-2015; Stubbs, Christopher/C-2829-2012; Williamson, Ross/H-1734-2015; OI Stubbs, Christopher/0000-0003-0347-1724; Williamson, Ross/0000-0002-6945-2975; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU MIT by NASA; National Science Foundation; Kavli Foundation; Moore Foundation; NSERC; CRC programme; CIfAR; Harvard University by the NSF; NASA Hubble Fellowship; KICP Fellowship; Alfred P. Sloan Research Fellowship; BCCP fellowship FX M.McD. was supported at MIT by NASA through the Chandra X-ray Observatory. The South Pole Telescope is supported by the National Science Foundation, with partial support provided by the Kavli Foundation, and the Moore Foundation. Support for X-ray analysis was provided by NASA. Work at McGill University is supported by NSERC, the CRC programme, and CIfAR, and at Harvard University by the NSF. S. V. acknowledges a Senior NPP Award held at the NASA Goddard Space Flight Center. R. K. acknowledges a NASA Hubble Fellowship, B. A. B. acknowledges a KICP Fellowship, M. A. D. acknowledges an Alfred P. Sloan Research Fellowship, and O.Z. acknowledges a BCCP fellowship. NR 30 TC 65 Z9 66 U1 2 U2 11 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 AUG 16 PY 2012 VL 488 IS 7411 BP 349 EP 352 DI 10.1038/nature11379 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 988OS UT WOS:000307501000035 PM 22895340 ER PT J AU Cheng, T Rivard, B Sanchez-Azofeifa, AG Feret, JB Jacquemoud, S Ustin, SL AF Cheng, Tao Rivard, Benoit Sanchez-Azofeifa, Arturo G. Feret, Jean-Baptiste Jacquemoud, Stephane Ustin, Susan L. TI Predicting leaf gravimetric water content from foliar reflectance across a range of plant species using continuous wavelet analysis SO JOURNAL OF PLANT PHYSIOLOGY LA English DT Article DE Leaf water content; PROSPECT model; Remote sensing; Spectral reflectance; Wavelet analysis ID FUEL MOISTURE-CONTENT; OPTICAL-PROPERTIES MODEL; SPECTROSCOPIC DETERMINATION; ABSORPTION FEATURES; HYPERSPECTRAL DATA; PROSPECT; CANOPY; LEAVES; DECOMPOSITION; VEGETATION AB Leaf water content is an important variable for understanding plant physiological properties. This study evaluates a spectral analysis approach, continuous wavelet analysis (CWA), for the spectroscopic estimation of leaf gravimetric water content (GWC, %) and determines robust spectral indicators of GWC across a wide range of plant species from different ecosystems. CWA is both applied to the Leaf Optical Properties Experiment (LOPEX) data set and a synthetic data set consisting of leaf reflectance spectra simulated using the leaf optical properties spectra (PROSPECT) model. The results for the two data sets, including wavelet feature selection and GWC prediction derived using those features, are compared to the results obtained from a previous study for leaf samples collected in the Republic of Panama (PANAMA), to assess the predictive capabilities and robustness of CWA across species. Furthermore, predictive models of GWC using wavelet features derived from PROSPECT simulations are examined to assess their applicability to measured data. The two measured data sets (LOPEX and PANAMA) reveal five common wavelet feature regions that correlate well with leaf GWC. All three data sets display common wavelet features in three wavelength regions that span 1732-1736 nm at scale 4, 1874-1878 nm at scale 6, and 1338-1341 nm at scale 7 and produce accurate estimates of leaf GWC. This confirms the applicability of the wavelet-based methodology for estimating leaf GWC for leaves representative of various ecosystems. The PROSPECT-derived predictive models perform well on the LOPEX data set but are less successful on the PANAMA data set. The selection of high-scale and low-scale features emphasizes significant changes in both overall amplitude over broad spectral regions and local spectral shape over narrower regions in response to changes in leaf GWC. The wavelet-based spectral analysis tool adds a new dimension to the modeling of plant physiological properties with spectroscopy data. (c) 2012 Elsevier GmbH. All rights reserved. C1 [Cheng, Tao; Ustin, Susan L.] Univ Calif Davis, Ctr Spatial Technol & Remote Sensing, Dept Land Air & Water Resources, Davis, CA 95616 USA. [Cheng, Tao; Rivard, Benoit; Sanchez-Azofeifa, Arturo G.] Univ Alberta, Earth Observat Syst Lab, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Sanchez-Azofeifa, Arturo G.] Smithsonian Trop Res Inst, Panama City, Panama. [Feret, Jean-Baptiste] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Jacquemoud, Stephane] Univ Paris Diderot, Inst Phys Globe Paris, CNRS, UMR 7154, F-75013 Paris, France. RP Cheng, T (reprint author), Univ Calif Davis, Ctr Spatial Technol & Remote Sensing, Dept Land Air & Water Resources, Davis, CA 95616 USA. EM qtcheng@ucdavis.edu RI Jacquemoud, Stephane/F-8842-2010; Cheng, Tao/B-4807-2010; Feret, Jean-Baptiste/A-8351-2013 OI Cheng, Tao/0000-0002-4184-0730; Feret, Jean-Baptiste/0000-0002-0151-1334 FU Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant; NASA Terrestrial Hydrology Program [NNX09AN51G]; Inter-American Institute for Global Change Research (IAI), Collaborative Research Network program Tropi-Dry (National Science Foundation) [CRN2-021, Geo 0452325]; French Space Agency (CNES) in the frame of the program "Terre Ocean Surfaces Continentales Atmosphere" FX This study was funded by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant to B.R. and partly funded by the NASA Terrestrial Hydrology Program (Grant # NNX09AN51G). This work was also supported by the Inter-American Institute for Global Change Research (IAI), Collaborative Research Network program CRN2-021 Tropi-Dry (National Science Foundation Grant No. Geo 0452325). The development of PROSPECT-5 was funded by the French Space Agency (CNES) in the frame of the program "Terre Ocean Surfaces Continentales Atmosphere". The contribution of author S.J. to this work is IPGP contribution no. 3289. NR 39 TC 16 Z9 21 U1 3 U2 37 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0176-1617 J9 J PLANT PHYSIOL JI J. Plant Physiol. PD AUG 15 PY 2012 VL 169 IS 12 BP 1134 EP 1142 DI 10.1016/j.jplph.2012.04.006 PG 9 WC Plant Sciences SC Plant Sciences GA 027ZP UT WOS:000310392900002 PM 22608180 ER PT J AU Fayolle, A Engelbrecht, B Freycon, V Mortier, F Swaine, M Rejou-Mechain, M Doucet, JL Fauvet, N Cornu, G Gourlet-Fleury, S AF Fayolle, Adeline Engelbrecht, Bettina Freycon, Vincent Mortier, Frederic Swaine, Michael Rejou-Mechain, Maxime Doucet, Jean-Louis Fauvet, Nicolas Cornu, Guillaume Gourlet-Fleury, Sylvie TI Geological Substrates Shape Tree Species and Trait Distributions in African Moist Forests SO PLOS ONE LA English DT Article ID TROPICAL RAIN-FOREST; HABITAT ASSOCIATIONS; FUNCTIONAL TRAITS; AMAZONIAN FORESTS; CLIMATIC GRADIENT; SOIL FERTILITY; PATTERNS; SEEDLINGS; SPECIALIZATION; CONVERGENCE AB Background: Understanding the factors that shape the distribution of tropical tree species at large scales is a central issue in ecology, conservation and forest management. The aims of this study were to (i) assess the importance of environmental factors relative to historical factors for tree species distributions in the semi-evergreen forests of the northern Congo basin; and to (ii) identify potential mechanisms explaining distribution patterns through a trait-based approach. Methodology/Principal Findings: We analyzed the distribution patterns of 31 common tree species in an area of more than 700,000 km(2) spanning the borders of Cameroon, the Central African Republic, and the Republic of Congo using forest inventory data from 56,445 0.5-ha plots. Spatial variation of environmental (climate, topography and geology) and historical factors (human disturbance) were quantified from maps and satellite records. Four key functional traits (leaf phenology, shade tolerance, wood density, and maximum growth rate) were extracted from the literature. The geological substrate was of major importance for the distribution of the focal species, while climate and past human disturbances had a significant but lesser impact. Species distribution patterns were significantly related to functional traits. Species associated with sandy soils typical of sandstone and alluvium were characterized by slow growth rates, shade tolerance, evergreen leaves, and high wood density, traits allowing persistence on resource-poor soils. In contrast, fast-growing pioneer species rarely occurred on sandy soils, except for Lophira alata. Conclusions/Significance: The results indicate strong environmental filtering due to differential soil resource availability across geological substrates. Additionally, long-term human disturbances in resource-rich areas may have accentuated the observed patterns of species and trait distributions. Trait differences across geological substrates imply pronounced differences in population and ecosystem processes, and call for different conservation and management strategies. C1 [Fayolle, Adeline; Freycon, Vincent; Mortier, Frederic; Fauvet, Nicolas; Cornu, Guillaume; Gourlet-Fleury, Sylvie] Ctr Cooperat Int Rech Agron Dev CIRAD, UPR Biens & Serv Ecosyst Forestiers Tropicaux BSE, Montpellier, France. [Fayolle, Adeline; Doucet, Jean-Louis] Univ Liege ULg, Gembloux Agrobio Tech GxABT, Unite Gest Ressources Forestieres & Milieux Nat G, Lab Foresterie Reg Trop & Subtrop FORTHOP, Gembloux, Belgium. [Engelbrecht, Bettina] Univ Bayreuth, Dept Plant Ecol, Bayreuth Ctr Ecol & Environm Res BayCEER, Bayreuth, Germany. [Engelbrecht, Bettina] Smithsonian Trop Res Inst STRI, Balboa, Ancon, Panama. [Swaine, Michael] Univ Aberdeen, Sch Biol Sci, Aberdeen, Scotland. [Rejou-Mechain, Maxime] Univ Toulouse 3, CNRS, Lab Evolut & Divers Biol, F-31062 Toulouse, France. RP Fayolle, A (reprint author), Ctr Cooperat Int Rech Agron Dev CIRAD, UPR Biens & Serv Ecosyst Forestiers Tropicaux BSE, Montpellier, France. EM adeline.fayolle@ulg.ac.be RI Cornu, Guillaume/C-1607-2014 OI Cornu, Guillaume/0000-0002-7523-5176 FU National Research Agency (ANR); Natural Environment Research Council (NERC) FX This study is part of the ErA Net BiodivERsA CoForChange project, funded by the National Research Agency (ANR) and the Natural Environment Research Council (NERC), involving 16 European, African and international partners and a number of timber companies (see list on the website, http://www.coforchange.eu). AF was supported by ANR funding. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 65 TC 28 Z9 28 U1 5 U2 58 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 AUG 15 PY 2012 VL 7 IS 8 AR e42381 DI 10.1371/journal.pone.0042381 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 993AG UT WOS:000307823600012 PM 22905127 ER PT J AU Laughinghouse, HD Pra, D Silva-Stenico, ME Rieger, A Frescura, VDS Fiore, MF Tedesco, SB AF Laughinghouse, Haywood Dail Pra, Daniel Silva-Stenico, Maria Estela Rieger, Alexandre Frescura, Viviane Dal-Souto Fiore, Marli Fatima Tedesco, Solange Bosio TI Biomonitoring genotoxicity and cytotoxicity of Microcystis aeruginosa (Chroococcales, Cyanobacteria) using the Allium cepa test SO SCIENCE OF THE TOTAL ENVIRONMENT LA English DT Article DE Genotoxicity; Cytotoxicity; Cyanotoxins; Microcystis aeruginosa; Allium cepa test ID DNA-DAMAGE; LR; EXTRACTS; CELLS; HEPATOCYTES; INHIBITION; NODULARIN; TOXINS; ASSAY; L. AB Water pollution caused by toxic cyanobacteria is a problem worldwide, increasing with eutrophication. Due to its biological significance, genotoxicity should be a focus for biomonitoring pollution owing to the increasing complexity of the toxicological environment in which organisms are exposed. Cyanobacteria produce a large number of bioactive compounds, most of which lack toxicological data. Microcystins comprise a class of potent cyclic heptapeptide toxins produced mainly by Microcystis aeruginosa. Other natural products can also be synthesized by cyanobacteria, such as the protease inhibitor, aeruginosin. The hepatotoxicity of microcystins has been well documented, but information on the genotoxic effects of aeruginosins is relatively scarce. In this study, the genotoxicity and ecotoxicity of methanolic extracts from two strains of M. aeruginosa NPLJ-4, containing high levels of microcystin, and M. aeruginosa NPCD-1, with high levels of aeruginosin, were evaluated. Four endpoints, using plant assays in Allium cepa were applied: rootlet growth inhibition, chromosomal aberrations, mitotic divisions, and micronucleus assays. The microcystin content of M. aeruginosa NPLJ-4 was confirmed through ELISA, while M. aeruginosa NPCD-1 did not produce microcystins. The extracts of M. aeruginosa NPLJ-4 were diluted at 0.01, 0.1, 1 and 10 ppb of microcystins: the same procedure was used to dilute M. aeruginosa NPCD-1 used as a parameter for comparison, and water was used as the control. The results demonstrated that both strains inhibited root growth and induced rootlet abnormalities. The strain rich in aeruginosin was more genotoxic, altering the cell cycle, while microcystins were more mitogenic. These findings indicate the need for future research on non-microcystin producing cyanobacterial strains. Understanding the genotoxicity of M. aeruginosa extracts can help determine a possible link between contamination by aquatic cyanobacteria and high risk of primary liver cancer found in some areas as well as establish water level limits for compounds not yet studied. (C) 2012 Elsevier B.V. All rights reserved. C1 [Laughinghouse, Haywood Dail; Pra, Daniel; Rieger, Alexandre] Univ Santa Cruz do Sul, Dept Biol & Pharm, Lab Biotechnol & Genet, Santa Cruz Do Sul, RS, Brazil. [Pra, Daniel] Univ Catolica Pelotas, Ctr Life & Hlth Sci, Lab Genet & Neurosci, Pelotas, RS, Brazil. [Silva-Stenico, Maria Estela; Fiore, Marli Fatima] Univ Sao Paulo, Ctr Nucl Energy Agr, Lab Mol Ecol Cyanobacteria, Piracicaba, SP, Brazil. [Frescura, Viviane Dal-Souto; Tedesco, Solange Bosio] Univ Fed Santa Maria, Agrobiol Grad Program, Santa Maria, RS, Brazil. [Tedesco, Solange Bosio] Univ Fed Santa Maria, Dept Biol, Lab Plant Cytogenet & Genotox, Santa Maria, RS, Brazil. [Pra, Daniel] Univ Santa Cruz do Sul, Grad Course Hlth Promot, Santa Cruz Do Sul, RS, Brazil. RP Laughinghouse, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC 166,POB 37012, Washington, DC 20013 USA. EM hdliv@hotmail.com RI Pra, D/D-2849-2009; Rieger, Alexandre/C-1809-2015; Fiore, Marli/C-1436-2012; Laughinghouse, Haywood/M-5836-2016; Stenico, Maria Estela/B-8110-2012 OI Pra, D/0000-0003-2818-0173; Rieger, Alexandre/0000-0001-7523-7211; Fiore, Marli/0000-0003-2555-7967; Laughinghouse, Haywood/0000-0003-1018-6948; Stenico, Maria Estela/0000-0001-9542-863X FU State of Sao Paulo Research Foundation [FAPESP 2009/05474-5]; CNPq [308299/2009-4, 151931/2010-0]; FAPESP [2010/09867-9] FX This study was supported by grants from The State of Sao Paulo Research Foundation (FAPESP 2009/05474-5). M.F. Fiore would like to thank CNPq for a research fellowship (308299/2009-4). M.E. Silva-Stenico was the recipient og a postdoctoral fellowship from FAPESP (2010/09867-9) and CNPq (151931/2010-0). We thank Prof. Valdemar Tornisielo for LC-MS analysis support in the Laboratory of Ecotoxicology, CENA-USP, Brazil. We are also indebted to three anonymous reviewers that revised an earlier version of this manuscript. NR 45 TC 12 Z9 12 U1 0 U2 26 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0048-9697 EI 1879-1026 J9 SCI TOTAL ENVIRON JI Sci. Total Environ. PD AUG 15 PY 2012 VL 432 BP 180 EP 188 DI 10.1016/j.scitotenv.2012.05.093 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA 998WI UT WOS:000308270700020 PM 22728963 ER PT J AU Olson, SL AF Olson, Storrs L. TI A new species of small owl of the genus Aegolius (Aves: Strigidae) from Quaternary deposits on Bermuda SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Aegolius acadicus; Colaptes; fossil birds; Holocene; Northern Saw-whet Owl; Picidae; Pleistocene; woodpeckers ID QUEEN-CHARLOTTE-ISLANDS; SAW-WHET OWLS; BRITISH-COLUMBIA; LATE PLEISTOCENE; EVOLUTION; POECILOZONITES; GEOCHRONOLOGY; FOSSIL AB Fossil remains of a small owl found in eight separate localities on Bermuda ranging in age from the end of the last interglacial period (Marine Isotope Stage 5a, ca. 80,000 years ago) and up into the Holocene are described here as a new species, Aegolius gradyi, the only representative of its genus known from a remote oceanic island. This differed from its probable North American ancestor, A. acadicus, in its more robust hindlimb elements, smaller head, and a possible tendency for smaller wing elements. Its colonization was probably made possible by the unique conditions of suitable habitat for hunting, roosting, and nesting afforded by Bermuda, including the presence of woodpeckers (Picidae) that would have excavated nest sites suitable for the owls in the endemic palm trees (Sabal bermudana). From accounts dating to the early 1600s, the species appears likely to have persisted into the historic period. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds NHB MRC 116, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds NHB MRC 116, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 28 TC 2 Z9 2 U1 3 U2 7 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 AUG 14 PY 2012 VL 125 IS 2 BP 97 EP 105 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 993NS UT WOS:000307867000001 ER PT J AU Lewis, C Migita, M Hashimoto, H Collins, AG AF Lewis, Cheryl Migita, Masao Hashimoto, Hiroshi Collins, Allen G. TI On the occurrence of freshwater jellyfish in Japan 1928-2011: eighty-three years of records of mamizu kurage (Limnomedusae, Olindiidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Astrohydra japonica; Cnidaria; Craspedacusta sowerbii; Craspedacusta iseana; distribution; Limnomedusae; polyps; taxonomy ID CRASPEDACUSTA-SOWERBII LANKESTER; ASTROHYDRA-JAPONICA; CNIDARIA HYDROZOA; MEDUSAE AB In Japan three freshwater Limnomedusae have been reported: Craspedacusta sowerbii, C. iseana, and Astrohydra japonica. The latter two species, though known only from Japan, have not been reported in ninety and thirty years, respectively. The type material for C. iseana is lost, and the only known specimens of A. japonica have recently been deposited in the National Museum of Natural History, Smithsonian Institution, Washington, D.C. Craspedacusta sowerbii, on the other hand, is a cosmopolitan species found throughout the archipelago of Japan. Reports of C. sowerbii in China, Europe, and North America are commonplace in international publications, but particulars about the occurrence of this freshwater jellyfish, known as mamizu kurage in Japan, were previously not well understood by the international scientific community due to a lack of related English-language publications. The aim of this paper is to provide naturalists and citizen scientists in Japan with a means to both locate and identify mamizu kurage in all nine geographical regions of Japan. Here we provide an extensive history of the occurrence of mamizu kurage in Japan from the time of its first sighting in 1928 until 2011, while also providing personal observations on populations of C. sowerhii in Okinawa, Shiga, and Shizuoka Prefectures. The distribution list and map herein represent the most extensive compilation of data on the 217 reports of mamizu kurage in Japan, and should serve as the basis for future molecular genetics studies on its phylogeography to determine if all accounts correspond to a single species called C. sowerbii. C1 [Lewis, Cheryl; Collins, Allen G.] Smithsonian Inst, NOAA, Natl Systemat Lab, Fisheries Serv,Natl Museum Nat Hist, Washington, DC 20013 USA. [Lewis, Cheryl] Univ Maryland, Biol Sci Grad Program, College Pk, MD 20742 USA. [Migita, Masao] Shiga Univ Med Sci, Fac Educ, Otsu, Shiga 5200862, Japan. RP Lewis, C (reprint author), Smithsonian Inst, NOAA, Natl Systemat Lab, Fisheries Serv,Natl Museum Nat Hist, MRC 153,POB 37012, Washington, DC 20013 USA. EM amesc@si.edu FU Japanese Government Monbukagakusho Scholarship FX We thank Profs. K. Tachihara and M. Yamaguchi (University of the Ryukyus) for facilitating the acquisition of the live jellyfish used in this study. We are indebted to Dr. R. Wilson and Dr. B. Bentlage for their extensive advice on an earlier version of the manuscript. We would also like to acknowledge G. Sasaki, K. Tateishi, M. Kobayashi, and Ms Ozawa (Hekinan Seaside Aquarium), Dr. T. Moriyama (Shinshu University), and Prof. K. Furuhashi (Shiga University) for their assistance. We are grateful to two anonymous reviewers that provided valuable advice on the manuscript. Finally, this paper would not have come together without the help of the library staff at the Smithsonian National Museum of Natural History in finding rare articles on this freshwater jellyfish. Part of this research was made possible by funding through a Japanese Government Monbukagakusho Scholarship. NR 46 TC 2 Z9 2 U1 3 U2 11 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 AUG 14 PY 2012 VL 125 IS 2 BP 165 EP 179 PG 15 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 993NS UT WOS:000307867000006 ER PT J AU Cairns, SD AF Cairns, Stephen D. TI New primnoid genus and species (Alcyonacea: Primnoidae) from the southwestern Atlantic SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Alcyonacea; Argentina; new genus; new species; Octocorallia; Primnoidae; Subantarctic ID OCTOCORALLIA PRIMNOIDAE; ANTARCTIC WATERS; SOUTHERN-OCEAN; ANTHOZOA AB A new genus and species of primnoid octocoral, Heptaprimnoa patagonica, is described from deep water from the cold temperate/Subantarctic region off Argentina and Burdwood Bank. It is distinguished from other primnoid genera by having only seven rows of body wall scales. C1 Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. EM cairnss@si.edu NR 14 TC 1 Z9 1 U1 0 U2 2 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 AUG 14 PY 2012 VL 125 IS 2 BP 180 EP 188 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 993NS UT WOS:000307867000007 ER PT J AU Jameson, SC Cairns, SD AF Jameson, Stephen C. Cairns, Stephen D. TI Neotypes for Porites porites (Pallas, 1766) and Porites divaricata Le Sueur, 1820 and remarks on other western Atlantic species of Porites (Anthozoa: Scleractinia) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE coral taxonomy; neotypes; Porites divaricata; Porites ponies; Porites verrillii; western Atlantic ID CORAL; COLONENSIS; JAMAICA AB To stabilize the taxonomy of the genus Porites in the western Atlantic and provide a foundation from which to launch future taxonomic research, neotypes for the coral species Porites porites and P. divaricata are chosen and Porites verrillii is proposed as a junior synonym of P. astreoides. Colony photographs and stereo scanning electron micrographs are provided of corallites of: 1) neotypes of P. porites (i.e., the P. clavaria holotype) and P. divaricata, 2) the holotypes of P. furcata, P. branneri, P. colonensis, and P. verrillii, and 3) a common P. astreoides. A brief taxonomic history of the genus is also provided. C1 [Jameson, Stephen C.; Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Jameson, SC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, POB 37012, Washington, DC 20013 USA. EM sjameson@coralseas.com; cairnss@si.edu NR 37 TC 4 Z9 4 U1 0 U2 3 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 AUG 14 PY 2012 VL 125 IS 2 BP 189 EP 207 PG 19 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 993NS UT WOS:000307867000008 ER PT J AU Zalamea, PC Heuret, P Sarmiento, C Rodriguez, M Berthouly, A Guitet, S Nicolini, E Delnatte, C Barthelemy, D Stevenson, PR AF Zalamea, Paul-Camilo Heuret, Patrick Sarmiento, Carolina Rodriguez, Manuel Berthouly, Anne Guitet, Stephane Nicolini, Eric Delnatte, Cesar Barthelemy, Daniel Stevenson, Pablo R. TI The Genus Cecropia: A Biological Clock to Estimate the Age of Recently Disturbed Areas in the Neotropics SO PLOS ONE LA English DT Article ID RAIN-FOREST TREES; SECONDARY FORESTS; AMAZONIA; PATTERNS; RATES AB Forest successional processes following disturbance take decades to play out, even in tropical forests. Nonetheless, records of vegetation change in this ecosystem are scarce, increasing the importance of the chronosequence approach to study forest recovery. However, this approach requires accurate dating of secondary forests, which until now was a difficult and/or expensive task. Cecropia is a widespread and abundant pioneer tree genus of the Neotropics. Here we propose and validate a rapid and straightforward method to estimate the age of secondary forest patches based on morphological observations of Cecropia trees. We found that Cecropia-inferred ages were highly correlated with known ages of the forest. We also demonstrate that Cecropia can be used to accurately date disturbances and propose twenty-one species distributed all over the geographical range of the genus as potential secondary forest chronometer species. Our method is limited in applicability by the maximal longevity of Cecropia individuals. Although the oldest chronosequence used in this study was 20 years old, we argue that at least for the first four decades after disturbance, the method described in this study provides very accurate estimations of secondary forest ages. The age of pioneer trees provides not only information needed to calculate the recovery of carbon stocks that would help to improve forest management, but also provides information needed to characterize the initial floristic composition and the rates of species remigration into secondary forest. Our contribution shows how successional studies can be reliably and inexpensively extended without the need to obtain forest ages based on expensive or potentially inaccurate data across the Neotropics. C1 [Zalamea, Paul-Camilo] IRD, UMR AMAP Bot & Bioinformat Architecture Plantes, Montpellier, France. [Zalamea, Paul-Camilo; Sarmiento, Carolina; Rodriguez, Manuel; Stevenson, Pablo R.] Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia. [Heuret, Patrick; Berthouly, Anne] INRA, UMR ECOFOG Ecol Forets Guyane, Kourou, French Guiana. [Heuret, Patrick; Delnatte, Cesar] Museum Hist Nat, Aix En Provence, France. [Sarmiento, Carolina; Nicolini, Eric] CIRAD, UMR AMAP Bot & Bioinformat Architecture Plantes, Montpellier, France. [Guitet, Stephane] DTRD, Off Natl Forets, Cayenne, French Guiana. [Guitet, Stephane; Barthelemy, Daniel] INRA, UMR AMAP Bot & Bioinformat Architecture Plantes, F-34060 Montpellier, France. [Barthelemy, Daniel] CIRAD, BIOS Direct, Montpellier, France. RP Zalamea, PC (reprint author), Smithsonian Trop Res Inst, Ancon, Panama. EM camilozalamea@gmail.com RI guitet, stephane/F-5616-2016; OI guitet, stephane/0000-0003-2374-4240; Sarmiento, Carolina/0000-0002-8575-7170 FU Ecos-Nord-Colciencias and Paris 13 University grant [C08A01]; Institut de Recherche pour le Developpement (France) FX This research was supported by an Ecos-Nord-Colciencias and Paris 13 University grant (C08A01), and the Institut de Recherche pour le Developpement (France) doctoral grant to PCZ. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 27 TC 6 Z9 6 U1 0 U2 20 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 AUG 10 PY 2012 VL 7 IS 8 AR e42643 DI 10.1371/journal.pone.0042643 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 986XO UT WOS:000307380900053 PM 22916144 ER PT J AU Deck, KM Holman, MJ Agol, E Carter, JA Lissauer, JJ Ragozzine, D Winn, JN AF Deck, Katherine M. Holman, Matthew J. Agol, Eric Carter, Joshua A. Lissauer, Jack J. Ragozzine, Darin Winn, Joshua N. TI RAPID DYNAMICAL CHAOS IN AN EXOPLANETARY SYSTEM SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE celestial mechanics; planets and satellites: dynamical evolution and stability ID OUTER ASTEROID BELT; N-BODY PROBLEM; SYMPLECTIC MAPS; 3-BODY PROBLEM; SOLAR-SYSTEM; SUPER-EARTHS; STABILITY; PROMETHEUS; BEHAVIOR; PANDORA AB We report on the long-term dynamical evolution of the two-planet Kepler-36 system, which consists of a super-Earth and a sub-Neptune in a tightly packed orbital configuration. The orbits of the planets, which we studied through numerical integrations of initial conditions that are consistent with observations of the system, are chaotic with a Lyapunov time of only similar to 10 years. The chaos is a consequence of a particular set of orbital resonances, with the inner planet orbiting 34 times for every 29 orbits of the outer planet. The rapidity of the chaos is due to the interaction of the 29: 34 resonance with the nearby first-order 6: 7 resonance, in contrast to the usual case in which secular terms in the Hamiltonian play a dominant role. Only one contiguous region of phase space, accounting for similar to 4.5% of the sample of initial conditions studied, corresponds to planetary orbits that do not show large-scale orbital instabilities on the timescale of our integrations (similar to 200 million years). Restricting the orbits to this long-lived region allows a refinement of estimates of the masses and radii of the planets. We find that the long-lived region consists of the initial conditions that satisfy the Hill stability criterion by the largest margin. Any successful theory for the formation of this system will need to account for why its current state is so close to unstable regions of phase space. C1 [Deck, Katherine M.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Holman, Matthew J.; Carter, Joshua A.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Deck, KM (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. RI Carter, Joshua/A-8280-2013; Agol, Eric/B-8775-2013; Ragozzine, Darin/C-4926-2013; OI Agol, Eric/0000-0002-0802-9145; Carter, Joshua/0000-0001-8152-2561 FU NSF [AST-0645416] FX We thank J. Wisdom for sharing with us his code that calculates coefficients in the disturbing function, as well as other members of the Kepler TTV team and our anonymous reviewer for helpful comments on the text. E. A. acknowledges support for this work which was provided by NSF Career grant AST-0645416. NR 29 TC 21 Z9 21 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 AUG 10 PY 2012 VL 755 IS 1 AR L21 DI 10.1088/2041-8205/755/1/L21 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980YS UT WOS:000306930700021 ER PT J AU Kinman, TD Aoki, W Beers, TC Brown, WR AF Kinman, T. D. Aoki, Wako Beers, Timothy C. Brown, Warren R. TI A NEW CEMP-s RR LYRAE STAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: structure; stars: abundances; stars: horizontal-branch ID METAL-POOR STARS; DIGITAL SKY SURVEY; HORIZONTAL-BRANCH STARS; HAMBURG/ESO SURVEY; VARIABILITY SURVEY; MILKY-WAY; CH-STARS; NGC 6441; CARBON; VARIABLES AB We show that SDSS J170733.93+585059.7 (hereafter SDSS J1707+58), previously identified by Aoki and collaborators as a carbon-enhanced metal-poor star (with s-process-element enhancements, CEMP-s), on the assumption that it is a main-sequence turnoff star, is the RR Lyrae star VIII-14 identified by the Lick Astrograph Survey. Revised abundances for SDSS J1707+58 are [Fe/H] = -2.92, [C/Fe] = +2.79, and [Ba/Fe] = +2.83. It is thus one of the most metal-poor RR Lyrae stars known, and has more extreme [C/Fe] and [Ba/Fe] than the only other RR Lyrae star known to have a CEMP-s spectrum (TY Gru). Both stars are Oosterhoff II stars with prograde kinematics, in contrast to stars with [C/Fe] < +0.7, such as KP Cyg and UY CrB, which are disk stars. Twelve other RR Lyrae stars with [C/Fe] >= +0.7 are presented as CEMP candidates for further study. C1 [Kinman, T. D.; Beers, Timothy C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Aoki, Wako] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Aoki, Wako] Grad Univ Adv Studies SOKENDAI, Dept Astron Sci, Sch Phys Sci, Mitaka, Tokyo 1818588, Japan. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kinman, TD (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. FU Alfred P. Sloan Foundation; NSF; US D.O.E.; U.S. National Science Foundation [PHY 02-16783, PHY 08-22648] FX Abundance measurements are based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. We used the VizieR catalog access tool, CDC, Strasbourg, France. We acknowledge using data from the SDSS-III, funded by the Alfred P. Sloan Foundation, the Participating Institutions, the NSF and the US D.O.E. The SDSS-III Web site is http://www.sdss3.org/. Use was also made of MAST (Multimission Archive at the STSci which is operated for NASA by AURA), the SIM-BAD database (operated at the CDS, Strasbourg, France), ADS (the NASA Astrophysics Data System), and the arXiv e-print server.; T.C.B. acknowledges partial funding of this work from grants PHY 02-16783 and PHY 08-22648, Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the U.S. National Science Foundation. NOAO is operated by AURA, Inc., under cooperative agreement with the National Science Foundation. NR 47 TC 5 Z9 5 U1 0 U2 1 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 AUG 10 PY 2012 VL 755 IS 1 AR L18 DI 10.1088/2041-8205/755/1/L18 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980YS UT WOS:000306930700018 ER PT J AU Miller-Jones, JCA Wrobel, JM Sivakoff, GR Heinke, CO Miller, RE Plotkin, RM Di Stefano, R Greene, JE Ho, LC Joseph, TD Kong, AKH Maccarone, TJ AF Miller-Jones, J. C. A. Wrobel, J. M. Sivakoff, G. R. Heinke, C. O. Miller, R. E. Plotkin, R. M. Di Stefano, R. Greene, J. E. Ho, L. C. Joseph, T. D. Kong, A. K. H. Maccarone, T. J. TI THE ABSENCE OF RADIO EMISSION FROM THE GLOBULAR CLUSTER G1 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE accretion, accretion disks; globular clusters: individual (Mayall-II=G1); X-rays: binaries ID MASS BLACK-HOLE; FUNDAMENTAL PLANE; STAR-CLUSTERS; MAYALL II=G1; XMM-NEWTON; X-RAYS; TELESCOPE; EVOLUTION; GALAXY; M31 AB The detections of both X-ray and radio emission from the cluster G1 in M31 have provided strong support for existing dynamical evidence for an intermediate-mass black hole (IMBH) of mass (1.8 +/- 0.5) x 10(4) M-circle dot at the cluster center. However, given the relatively low significance and astrometric accuracy of the radio detection, and the non-simultaneity of the X-ray and radio measurements, this identification required further confirmation. Here we present deep, high angular resolution, strictly simultaneous X-ray and radio observations of G1. While the X-ray emission (L-X = 1.74(-0.44)(+0.53) x 10(36) (d/750 kpc)(2) erg s(-1) in the 0.5-10 keV band) remained fully consistent with previous observations, we detected no radio emission from the cluster center down to a 3 sigma upper limit of 4.7 mu Jy beam(-1). Our favored explanation for the previous radio detection is flaring activity from a black hole low-mass X-ray binary (LMXB). We performed a new regression of the "Fundamental Plane" of black hole activity, valid for determining black hole mass from radio and X-ray observations of sub-Eddington black holes, finding log M-BH = (1.638 +/- 0.070) log L-R - (1.136 +/- 0.077) log L-X - (6.863 +/- 0.790), with an empirically determined uncertainty of 0.44 dex. This constrains the mass of the X-ray source in G1, if a black hole, to be <9.7 x 10(3) M-circle dot at 95% confidence, suggesting that it is a persistent LMXB. This annuls what was previously the most convincing evidence from radiation for an IMBH in the Local Group, though the evidence for an IMBH in G1 from velocity dispersion measurements remains unaffected by these results. C1 [Miller-Jones, J. C. A.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Wrobel, J. M.] NRAO Domenici Sci Operat Ctr, Socorro, NM 87801 USA. [Sivakoff, G. R.; Heinke, C. O.; Miller, R. E.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2G7, Canada. [Plotkin, R. M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Di Stefano, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Greene, J. E.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Ho, L. C.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Joseph, T. D.; Maccarone, T. J.] Univ Southampton, Sch Phys & Astron, Highfield SO17 1BJ, England. [Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. RP Miller-Jones, JCA (reprint author), Curtin Univ, Int Ctr Radio Astron Res, GPO Box U1987, Perth, WA 6845, Australia. EM james.miller-jones@curtin.edu.au RI Miller-Jones, James/B-2411-2013; Sivakoff, Gregory/G-9602-2011; OI Miller-Jones, James/0000-0003-3124-2814; Sivakoff, Gregory/0000-0001-6682-916X; Heinke, Craig/0000-0003-3944-6109 FU NSERC; Ingenuity New Faculty Award; NWO Vidi Fellowship FX The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. G. R. S. and C.O.H. are supported by NSERC, and C.O.H. also by an Ingenuity New Faculty Award. R. M. P. acknowledges support from an NWO Vidi Fellowship. This research has made use of NASA's Astrophysics Data System. NR 44 TC 20 Z9 21 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 AUG 10 PY 2012 VL 755 IS 1 AR L1 DI 10.1088/2041-8205/755/1/L1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980YS UT WOS:000306930700001 ER PT J AU Bogdan, A Forman, WR Kraft, RP Jones, C Blom, C Randall, SW Zhang, ZL Zhuravleva, I Churazov, E Li, ZY Nulsen, PEJ Vikhlinin, A Schindler, S AF Bogdan, Akos Forman, William R. Kraft, Ralph P. Jones, Christine Blom, Christina Randall, Scott W. Zhang, Zhongli Zhuravleva, Irina Churazov, Eugene Li, Zhiyuan Nulsen, Paul E. J. Vikhlinin, Alexey Schindler, Sabine TI CHANDRA OBSERVATIONS OF NGC 4342, AN OPTICALLY FAINT, X-RAY GAS-RICH EARLY-TYPE GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 4342); galaxies: stellar content; intergalactic medium; X-rays: galaxies; X-rays: ISM ID GLOBULAR-CLUSTER SYSTEMS; ACS-VIRGO CLUSTER; BLACK-HOLE; DARK-MATTER; HOT GAS; MASS; EMISSION; BINARIES; BULGE; CATALOG AB Chandra x-ray observations of NGC 4342, a low-stellar mass (M-K = -22.79 mag) early-type galaxy, show luminous, diffuse x-ray emission originating from hot gas with temperature of kT similar to 0.6 keV. The observed 0.5-2 keV band luminosity of the diffuse x-ray emission within the D-25 ellipse is L0.5-2 (keV) = 2.7 x 10(39) erg s(-1). The hot gas has a significantly broader distribution than the stellar light, and shows strong hydrodynamic disturbances with a sharp surface brightness edge to the northeast and a trailing tail. We identify the edge as a cold front and conclude that the distorted morphology of the hot gas is produced by ram pressure as NGC 4342 moves through external gas. From the thermal pressure ratios inside and outside the cold front, we estimate the velocity of NGC 4342 and find that it moves supersonically (M similar to 2.6) toward the northeast. Outside the optical extent of the galaxy, we detect similar to 17 bright (L0.5-8 (keV) greater than or similar to 3 x 10(37) erg s(-1)) excess x-ray point sources. The excess sources are presumably LMXBs located in metal-poor globular clusters (GCs) in the extended dark matter halo of NGC 4342. Based on the number of excess sources and the average frequency of bright LMXBs in GCs, we estimate that NGC 4342 may host roughly 850-1700 GCs. In good agreement with this, optical observations hint that NGC 4342 may harbor 1200 +/- 500 GCs. This number corresponds to a GC specific frequency of S-N = 19.9 +/- 8.3, which is among the largest values observed in full-size galaxies. C1 [Bogdan, Akos; Forman, William R.; Kraft, Ralph P.; Jones, Christine; Randall, Scott W.; Li, Zhiyuan; Nulsen, Paul E. J.; Vikhlinin, Alexey] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Blom, Christina] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Zhang, Zhongli; Zhuravleva, Irina; Churazov, Eugene] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Schindler, Sabine] Leopold Franzens Univ Innsbruck, Inst Astrophys, A-6020 Innsbruck, Austria. RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; OI Randall, Scott/0000-0002-3984-4337; Nulsen, Paul/0000-0003-0297-4493 FU National Aeronautics and Space Administration [NAS8-03060]; National Science Foundation; Smithsonian Institution; NASA through Chandra X-ray Center [PF1-120081] FX We thank the anonymous referee for useful and constructive comments. This research has made use of Chandra data provided by the Chandra X-ray Center. The publication makes use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. In this work, the Digitized Sky Survey (DSS) and the NASA/IPAC Extragalactic Database (NED) have been used. A.B. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant No. PF1-120081 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. W. F. and C.J. acknowledge support from the Smithsonian Institution. NR 39 TC 8 Z9 8 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 AUG 10 PY 2012 VL 755 IS 1 AR 25 DI 10.1088/0004-637X/755/1/25 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500025 ER PT J AU Goulding, AD Alexander, DM Bauer, FE Forman, WR Hickox, RC Jones, C Mullaney, JR Trichas, M AF Goulding, A. D. Alexander, D. M. Bauer, F. E. Forman, W. R. Hickox, R. C. Jones, C. Mullaney, J. R. Trichas, M. TI DEEP SILICATE ABSORPTION FEATURES IN COMPTON-THICK ACTIVE GALACTIC NUCLEI PREDOMINANTLY ARISE DUE TO DUST IN THE HOST GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: Seyfert; infrared: galaxies; X-rays: galaxies ID SEYFERT 2 GALAXY; ULTRALUMINOUS INFRARED GALAXIES; X-RAY-ABSORPTION; LOW-LUMINOSITY AGN; BEPPOSAX OBSERVATION; BLACK-HOLES; MIDINFRARED PROPERTIES; INTERSTELLAR DUST; MASSIVE GALAXIES; NEARBY GALAXIES AB We explore the origin of mid-infrared (mid-IR) dust extinction in all 20 nearby (z < 0.05) bona fide Compton-thick (N-H > 1.5x10(24) cm(-2)) active galactic nuclei (AGNs) with hard energy (E > 10 keV) X-ray spectral measurements. We accurately measure the silicate absorption features at lambda similar to 9.7 mu m in archival low-resolution (R similar to 57-127) Spitzer Infrared Spectrograph spectroscopy, and show that only a minority (approximate to 45%) of nearby Compton-thick AGNs have strong Si-absorption features (S-9.7 = ln(f(int)/f(obs)) greater than or similar to 0.5) which would indicate significant dust attenuation. The majority (approximate to 60%) are star formation dominated (AGN: SB < 0.5) at mid-IR wavelengths and lack the spectral signatures of AGN activity at optical wavelengths, most likely because the AGN emission lines are optically extinguished. Those Compton-thick AGNs hosted in low-inclination-angle galaxies exhibit a narrow range in Si-absorption (S-9.7 similar to 0-0.3), which is consistent with that predicted by clumpy-torus models. However, on the basis of the IR spectra and additional lines of evidence, we conclude that the dominant contribution to the observed mid-IR dust extinction is dust located in the host galaxy (i.e., due to disturbed morphologies, dust lanes, galaxy inclination angles) and not necessarily a compact obscuring torus surrounding the central engine. C1 [Goulding, A. D.; Forman, W. R.; Jones, C.; Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Alexander, D. M.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bauer, F. E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Mullaney, J. R.] Univ Paris Diderot, Laboratoire AIM, CEA DSM CNRS, Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. RP Goulding, AD (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM agoulding@cfa.harvard.edu OI Alexander, David/0000-0002-5896-6313 FU NASA [13637399, AR8-9017X]; Science and Technologies Funding Council; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, ALMA-CONICYT 31100004] FX The authors thank the anonymous referee for their timely and considered report which has allowed us to clarify and improve several aspects of the manuscript. We are also grateful to G. Risaliti for helpful discussions. This work was partially supported by NASA grants 13637399 and AR8-9017X. D. M. A. acknowledges funding from the Science and Technologies Funding Council. F. E. B. acknowledges support from Basal-CATA (PFB-06/2007) and CONICYT-Chile (FONDECYT 1101024 and ALMA-CONICYT 31100004). This work is based on observations made with the Spitzer Space Telescope and has made use of the NASA/IPAC Infrared Science Archive which are operated by the Jet Propulsion Laboratories, Californian Institute of Technology under contract with NASA. NR 94 TC 64 Z9 64 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2012 VL 755 IS 1 AR 5 DI 10.1088/0004-637X/755/1/5 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500005 ER PT J AU Kendrew, S Simpson, R Bressert, E Povich, MS Sherman, R Lintott, CJ Robitaille, TP Schawinski, K Wolf-Chase, G AF Kendrew, S. Simpson, R. Bressert, E. Povich, M. S. Sherman, R. Lintott, C. J. Robitaille, T. P. Schawinski, K. Wolf-Chase, G. TI THE MILKY WAY PROJECT: A STATISTICAL STUDY OF MASSIVE STAR FORMATION ASSOCIATED WITH INFRARED BUBBLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; infrared: ISM; ISM: bubbles; stars: formation; stars: massive ID H-II REGIONS; BRIGHT-RIMMED CLOUDS; GALACTIC PLANE; INTERSTELLAR BUBBLES; CLUSTER FORMATION; EXPANDING SHELLS; RMS SURVEY; MU-M; GALAXIES; FRAGMENTATION AB The Milky Way Project citizen science initiative recently increased the number of known infrared bubbles in the inner Galactic plane by an order of magnitude compared to previous studies. We present a detailed statistical analysis of this data set with the Red MSX Source (RMS) catalog of massive young stellar sources to investigate the association of these bubbles with massive star formation. We particularly address the question of massive triggered star formation near infrared bubbles. We find a strong positional correlation of massive young stellar objects (MYSOs) and H II regions with Milky Way Project bubbles at separations of <2 bubble radii. As bubble sizes increase, a statistically significant overdensity of massive young sources emerges in the region of the bubble rims, possibly indicating the occurrence of triggered star formation. Based on numbers of bubble-associated RMS sources, we find that 67% +/- 3% of MYSOs and (ultra-)compact H II regions appear to be associated with a bubble. We estimate that approximately 22% +/- 2% of massive young stars may have formed as a result of feedback from expanding H II regions. Using MYSO-bubble correlations, we serendipitously recovered the location of the recently discovered massive cluster Mercer 81, suggesting the potential of such analyses for discovery of heavily extincted distant clusters. C1 [Kendrew, S.; Robitaille, T. P.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Simpson, R.; Lintott, C. J.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Bressert, E.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Povich, M. S.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Sherman, R.; Wolf-Chase, G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Schawinski, K.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Lintott, C. J.; Wolf-Chase, G.] Adler Planetarium, Dept Astron, Chicago, IL 60605 USA. [Bressert, E.] ESO, D-87548 Garching, Germany. [Bressert, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kendrew, S (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM kendrew@mpia.de OI Bressert, Eli/0000-0002-6564-6182; Schawinski, Kevin/0000-0001-5464-0888; Robitaille, Thomas/0000-0002-8642-1329; Kendrew, Sarah/0000-0002-7612-0469 FU Leverhulme Trust; National Science Foundation [AST-0901646]; NASA [PF9-00069, NAS8-03060]; Chandra X-ray Observatory Center; Brinson Foundation FX The Milky Way Project and R.J.S. were supported by The Leverhulme Trust. M. S. P. was supported by a National Science Foundation Astronomy & Astrophysics Postdoctoral Fellowship under award AST-0901646. Support for the work of K. S. was provided by NASA through Einstein Postdoctoral Fellowship grant number PF9-00069 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. G.W.-C. gratefully acknowledges support from the Brinson Foundation Grant-in-Aid of astrophysics research at the Adler Planetarium. NR 62 TC 36 Z9 36 U1 0 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 AUG 10 PY 2012 VL 755 IS 1 AR 71 DI 10.1088/0004-637X/755/1/71 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500071 ER PT J AU Mao, SA McClure-Griffiths, NM Gaensler, BM Brown, JC van Eck, CL Haverkorn, M Kronberg, PP Stil, JM Shukurov, A Taylor, AR AF Mao, S. A. McClure-Griffiths, N. M. Gaensler, B. M. Brown, J. C. van Eck, C. L. Haverkorn, M. Kronberg, P. P. Stil, J. M. Shukurov, A. Taylor, A. R. TI NEW CONSTRAINTS ON THE GALACTIC HALO MAGNETIC FIELD USING ROTATION MEASURES OF EXTRAGALACTIC SOURCES TOWARD THE OUTER GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; ISM: magnetic fields; polarization ID FARADAY-ROTATION; MILKY-WAY; HYDROSTATIC EQUILIBRIUM; PLANE SURVEY; MEASURE SKY; H-ALPHA; POLARIZATION; RADIO; DISK; ARMS AB We present a study of the Milky Way disk and halo magnetic field, determined from observations of Faraday rotation measure (RM) toward 641 polarized extragalactic radio sources in the Galactic longitude range 100 degrees-117 degrees, within 30 degrees of the Galactic plane. For vertical bar b vertical bar < 15 degrees, we observe a symmetric RM distribution about the Galactic plane. This is consistent with a disk field in the Perseus arm of even parity across the Galactic mid-plane. In the range 15 degrees < vertical bar b vertical bar < 30 degrees, we find median RMs of -15 +/- 4 rad m(-2) and -62 +/- 5 rad m(-2) in the northern and southern Galactic hemispheres, respectively. If the RM distribution is a signature of the large-scale field parallel to the Galactic plane, then this suggests that the halo magnetic field toward the outer Galaxy does not reverse direction across the mid-plane. The variation of RMas a function of Galactic latitude in this longitude range is such that RMs become more negative at larger vertical bar b vertical bar. This is consistent with an azimuthal magnetic field of strength 2 mu G (7 mu G) at a height 0.8-2 kpc above (below) the Galactic plane between the local and the Perseus spiral arm. We propose that the Milky Way could possess spiral-like halo magnetic fields similar to those observed in M51. C1 [Mao, S. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mao, S. A.; McClure-Griffiths, N. M.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Mao, S. A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Mao, S. A.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Gaensler, B. M.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Brown, J. C.; van Eck, C. L.; Stil, J. M.; Taylor, A. R.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Brown, J. C.; van Eck, C. L.; Stil, J. M.; Taylor, A. R.] Univ Calgary, Inst Space Imaging Sci, Calgary, AB T2N 1N4, Canada. [Haverkorn, M.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Kronberg, P. P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kronberg, P. P.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. [Shukurov, A.] Newcastle Univ, Sch Math & Stat, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. RP Mao, SA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mao@astro.wisc.edu RI Gaensler, Bryan/F-8655-2010; OI Shukurov, Anvar/0000-0001-6200-4304; McClure-Griffiths, Naomi/0000-0003-2730-957X; Gaensler, Bryan/0000-0002-3382-9558 FU Natural Sciences and Engineering Research Council (NSERC); National Science Foundation; Australian Research Council Federation Fellowship [FF0561298]; European Union [239490]; Netherlands Organisation for Scientific Research (NWO) [639.042.915]; NSERC of Canada FX We thank Bob Sault for useful discussions on conducting polarization calibration of VLA data in MIRIAD. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The Canadian Galactic Plane Survey is a Canadian project with international partners and is supported by the Natural Sciences and Engineering Research Council (NSERC). The Wisconsin H-Alpha Mapper is funded by the National Science Foundation. The Southern H-Alpha Sky Survey Atlas (SHASSA) is supported by the National Science Foundation.; B.M.G. acknowledges the support in part by an Australian Research Council Federation Fellowship (FF0561298). M. H. acknowledges funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 239490 and research program 639.042.915, which is (partly) financed by the Netherlands Organisation for Scientific Research (NWO). P. P. K acknowledges support from NSERC of Canada. NR 66 TC 19 Z9 19 U1 2 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 AUG 10 PY 2012 VL 755 IS 1 AR 21 DI 10.1088/0004-637X/755/1/21 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500021 ER PT J AU Motta, V Mediavilla, E Falco, E Munoz, JA AF Motta, V. Mediavilla, E. Falco, E. Munoz, J. A. TI MEASURING MICROLENSING USING SPECTRA OF MULTIPLY LENSED QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; gravitational lensing: micro; gravitational lensing: strong; quasars: individual (HS0818+1227, Q0957+561, SDSS1004+4112, SDSS1029+2623, HE1104-1805) ID DARK-MATTER SUBSTRUCTURE; BROAD EMISSION-LINES; ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; QSO 0957+561 A,B; GRAVITATIONAL LENS; SDSS J1004+4112; CHANDRA OBSERVATIONS; ACCRETION DISK; TIME-DELAY AB We report on a program of spectroscopic observations of gravitationally lensed QSOs with multiple images. We seek to establish whether microlensing is occurring in each QSO image using only single-epoch observations. We calculate flux ratios for the cores of emission lines in image pairs to set a baseline for no microlensing. The offset of the continuum flux ratios relative to this baseline yields the microlensing magnification free from extinction, as extinction affects the continuum and the lines equally. When we find chromatic microlensing, we attempt to constrain the size of the QSO accretion disk. SDSSJ1004+4112 and HE1104-1805 show chromatic microlensing with amplitudes 0.2 < |Delta m| < 0.6 and 0.2 < |Delta m| < 0.4 mag, respectively. Modeling the accretion disk with a Gaussian source (I alpha exp(-R-2/2r(s)(2))) of size r(s) alpha lambda(p) and using magnification maps to simulate microlensing, we find r(s) (lambda 3363) = 7 +/- 3 lt-day(18.1 +/- 7.8x10(15) cm) and p = 1.1 +/- 0.4 for SDSS1004+4112, and r(s) (lambda 3363) = 6 +/- 2 lt-day(15.5 +/- 5.2x10(15) cm) and p = 0.7 +/- 0.1 for HE1104-1805. For SDSSJ1029+2623, we find strong chromaticity of similar to 0.4 mag in the continuum flux ratio, which probably arises from microlensing, although not all the available data fit within this explanation. For Q0957+561, we measure B-A magnitude differences of 0.4 mag, much greater than the similar to 0.05 mag amplitude usually inferred from light-curve variability. It may substantially modify the current interpretations of microlensing in this system, likely favoring the hypothesis of smaller sources and/or larger microdeflectors. For HS0818+1227, our data yield possible evidence of microlensing. C1 [Motta, V.] Univ Valparaiso, Dept Fis & Astron, Valparaiso 2360102, Chile. [Mediavilla, E.] Inst Astrofis Canarias, Tenerife 38200, Spain. [Mediavilla, E.] Univ La Laguna, Dept Astrofis, Tenerife 38205, Spain. [Falco, E.] Smithsonian Inst, Whipple Observ, Amado, AZ 85645 USA. [Munoz, J. A.] Univ Valencia, Dept Astron & Astrofis, E-46100 Valencia, Spain. RP Motta, V (reprint author), Univ Valparaiso, Dept Fis & Astron, Avda Gran Bretana 1111, Valparaiso 2360102, Chile. EM vmotta@dfa.uv.cl; emg@iac.es; falco@cfa.harvard.edu; jmunoz@uv.es FU FONDECYT [1090673, 1120741]; Spanish Ministerio de Educacion y Ciencias [AYA2007-67342-C03-01/03, AYA2010-21741-C03/02]; Generalitat Valenciana [PROMETEO/2009/64] FX We thank the anonymous referee for thoughtful suggestions. We thank G. T. Richards for kindly providing us the Keck spectra of SDSS1004+4112, and N. Inada for kindly confirming us the infrared measurements for SDSS1029+2623. V. M. gratefully acknowledges support from FONDECYT through grants 1090673 and 1120741. E. M. and J.A.M are supported by the Spanish Ministerio de Educacion y Ciencias through the grants AYA2007-67342-C03-01/03 and AYA2010-21741-C03/02. J.A.M. is also supported by the Generalitat Valenciana with the grant PROMETEO/2009/64. This research has made use of NASA's Astrophysics Data System. NR 99 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 EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2012 VL 755 IS 1 AR 82 DI 10.1088/0004-637X/755/1/82 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500082 ER PT J AU Reichardt, CL Shaw, L Zahn, O Aird, KA Benson, BA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J George, EM Halverson, NW Holder, GP Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Natoli, T Padin, S Plagge, T Pryke, C Ruhl, JE Schaffer, KK Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, K van Engelen, A Vanderlinde, K Vieira, JD Williamson, R AF Reichardt, C. L. Shaw, L. Zahn, O. Aird, K. A. Benson, B. A. Bleem, L. E. Carlstrom, J. E. Chang, C. L. Cho, H. M. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. George, E. M. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, J. D. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Natoli, T. Padin, S. Plagge, T. Pryke, C. Ruhl, J. E. Schaffer, K. K. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. TI A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmological parameters; cosmology: observations; diffuse radiation; large-scale structure of universe ID ATACAMA COSMOLOGY TELESCOPE; ZELDOVICH POWER SPECTRUM; STAR-FORMING GALAXIES; EXTRAGALACTIC SOURCES; CLUSTERS; PARAMETERS; PROBE; SKY; CONSTRAINTS; CATALOG AB We present the first three-frequency South Pole Telescope (SPT) cosmic microwave background (CMB) power spectra. The band powers presented here cover angular scales 2000 < l < 9400 in frequency bands centered at 95, 150, and 220 GHz. At these frequencies and angular scales, a combination of the primary CMB anisotropy, thermal and kinetic Sunyaev-Zel'dovich (SZ) effects, radio galaxies, and cosmic infrared background (CIB) contributes to the signal. We combine Planck/HFI and SPT data at 220 GHz to constrain the amplitude and shape of the CIB power spectrum and find strong evidence for nonlinear clustering. We explore the SZ results using a variety of cosmological models for the CMB and CIB anisotropies and find them to be robust with one exception: allowing for spatial correlations between the thermal SZ effect and CIB significantly degrades the SZ constraints. Neglecting this potential correlation, we find the thermal SZ power at 150 GHz and l = 3000 to be 3.65 +/- 0.69 mu K-2, and set an upper limit on the kinetic SZ power to be less than 2.8 mu K-2 at 95% confidence. When a correlation between the thermal SZ and CIB is allowed, we constrain a linear combination of thermal and kinetic SZ power: D-3000(tSZ) + 0.5(3000)(DkSZ) = 4.60 +/- 0.63 mu K-2, consistent with earlier measurements. We use the measured thermal SZ power and an analytic, thermal SZ model calibrated with simulations to determine sigma(8) = 0.807 +/- 0.016. Modeling uncertainties involving the astrophysics of the intracluster medium rather than the statistical uncertainty in the measured band powers are the dominant source of uncertainty on sigma(8). We also place an upper limit on the kinetic SZ power produced by patchy reionization; a companion paper uses these limits to constrain the reionization history of the universe. C1 [Reichardt, C. L.; Shaw, L.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Shaw, L.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Zahn, O.] Univ Calif Berkeley, Berkeley Ctr Cosmol Phys, Dept Phys, Berkeley, CA 94720 USA. [Zahn, O.] Lawrence Berkeley Natl Labs, Berkeley, CA 94720 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Natoli, T.; Padin, S.; Plagge, T.; Pryke, C.; Schaffer, K. K.; Story, K.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Natoli, T.; Pryke, C.; Story, K.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Pryke, C.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J.; Holder, G. P.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Joy, M.] NASA, Dept Space Sci, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Reichardt, CL (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM cr@bolo.berkeley.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996 FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics Frontier Center [PHY-0114422]; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA [HF-51275.01]; KICP; Alfred P. Sloan Research Fellowship; Yale University; NSF [AST-1009811, 0709498]; Office of Science of the U.S. Department of Energy [DE-AC02-05CH11231]; NASA Office of Space Science; Kavli Foundation; Gordon and Betty Moore Foundation FX We thank Cien Shang, Guilaine Lagache, Olivier Dore, and Marco Viero for useful discussions and assistance with the CIB modeling. The South Pole Telescope is supported by the National Science Foundation through grants ANT-0638937 and ANT-0130612. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. R. K. acknowledges support from NASA Hubble Fellowship grant HF-51275.01. B. A. B. is supported by a KICP Fellowship. M. D. acknowledges support from an Alfred P. Sloan Research Fellowship. L. S. acknowledges the support of Yale University and NSF grant AST-1009811. M. M. and L. K. acknowledge the support of NSF grant 0709498. This research used resources of the National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231. Some of the results in this paper have been derived using the HEALPix (Gorski et al. 2005) package. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 69 TC 185 Z9 185 U1 2 U2 10 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 AUG 10 PY 2012 VL 755 IS 1 AR 70 DI 10.1088/0004-637X/755/1/70 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500070 ER PT J AU Rice, TS Wolk, SJ Aspin, C AF Rice, Thomas S. Wolk, Scott J. Aspin, Colin TI NEAR-INFRARED VARIABILITY IN YOUNG STARS IN CYGNUS OB7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared: stars; stars: formation; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be ID T-TAURI STARS; ORION NEBULA CLUSTER; MAIN-SEQUENCE STARS; WIDE-FIELD CAMERA; MOLECULAR CLOUD; FORMATION REGION; CIRCUMSTELLAR DISKS; STELLAR OBJECTS; PHOTOMETRIC VARIABILITY; LOW-MASS AB We present the first results from a 124 night J, H, K near-infrared monitoring campaign of the dark cloud L 1003 in Cygnus OB7, an active star-forming region. Using three seasons of UKIRT observations spanning 1.5 years, we obtained high-quality photometry on 9200 stars down to J = 17 mag, with photometric uncertainty better than 0.04 mag. On the basis of near-infrared excesses from disks, we identify 30 pre-main-sequence stars, including 24 which are newly discovered. We analyze those stars and find that the NIR excesses are significantly variable. All 9200 stars were monitored for photometric variability; among the field star population, similar to 160 exhibited near-infrared variability (1.7% of the sample). Of the 30 young stellar objects (YSOs), 28 of them (93%) are variable at a significant level. Of the 30 YSOs, twenty-five have near-infrared excess consistent with simple disk-plus-star classical T Taurimodels. Nine of these (36%) drift in color space over the course of these observations and/or since Two Micron All Sky Survey observations such that they cross the boundary defining the NIR excess criteria; effectively, they have a transient near-infrared excess. Thus, time-series JHK observations can be used to obtain a more complete sample of disk-bearing stars than single-epoch JHK observations. About half of the YSOs have color-space variations parallel to either the classical T Tauri star locus or a hybrid track which includes the dust reddening trajectory. This indicates that the NIR variability in YSOs that possess accretion disks arises from a combination of variable extinction and changes in the inner accretion disk: either in accretion rate, central hole size, and/or the inclination of the inner disk. While some variability may be due to stellar rotation, the level of variability on the individual stars can exceed a magnitude. This is a strong empirical suggestion that protoplanetary disks are quite dynamic and exhibit more complex activity on short timescales than is attributable to rotation alone or captured in static disk models. C1 [Rice, Thomas S.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Wolk, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aspin, Colin] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. RP Rice, TS (reprint author), Harvard Univ, Dept Astron, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 FU NASA [NAS8-03060]; Spitzer Science Center [1348190]; NSF REU [0757887] FX S.J.W. is supported by NASA contract NAS8-03060 (Chandra). T. S. R. was supported by grant 1348190 from the Spitzer Science Center. Thanks also to the NSF REU program for funding part of this research via NSF REU site grant 0757887. 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. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the U.K. We thank A. Nord, L. Rizzi, and T. Carroll for assistance in obtaining these observations. We also thank the University of Hawaii Time Allocation Committee for allocating the nights during which these observations were made. 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 sacred mountain. NR 60 TC 21 Z9 21 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 AUG 10 PY 2012 VL 755 IS 1 AR 65 DI 10.1088/0004-637X/755/1/65 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500065 ER PT J AU Richardson, J Zheng, Z Chatterjee, S Nagai, D Shen, Y AF Richardson, Jonathan Zheng, Zheng Chatterjee, Suchetana Nagai, Daisuke Shen, Yue TI THE HALO OCCUPATION DISTRIBUTION OF SDSS QUASARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: nuclei; large-scale structure of universe; quasars: general ID SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; DARK-MATTER HALOES; ACTIVE GALACTIC NUCLEI; QSO REDSHIFT SURVEY; PHOTOMETRICALLY CLASSIFIED QUASARS; 2-POINT CORRELATION-FUNCTION; LUMINOUS RED GALAXIES; 5TH DATA RELEASE; X-RAY AB We present an estimate of the projected two-point correlation function (2PCF) of quasars in the Sloan Digital Sky Survey (SDSS) over the full range of one-and two-halo scales, 0.02 h(-1) Mpc < r(p) < 120 h(-1) Mpc. This was achieved by combining data from SDSS DR7 on large scales and Hennawi et al. (with appropriate statistical corrections) on small scales. Our combined clustering sample is the largest spectroscopic quasar clustering sample to date, containing similar to 48,000 quasars in the redshift range 0.4 less than or similar to z less than or similar to 2.5 with median redshift 1.4. We interpret these precise 2PCF measurements within the halo occupation distribution (HOD) framework and constrain the occupation functions of central and satellite quasars in dark matter halos. In order to explain the small-scale clustering, the HOD modeling requires that a small fraction of z similar to 1.4 quasars, f(sat) = (7.4 +/- 1.4) x 10(-4), be satellites in dark matter halos. At z similar to 1.4, the median masses of the host halos of central and satellite quasars are constrained to be M-cen = 4.1(-0.4)(+0.3) x 10(12) h(-1) M-circle dot and M-sat = 3.6(-1.0)(+0.8) x 10(14) h(-1) M-circle dot , respectively. To investigate the redshift evolution of the quasar-halo relationship, we also perform HOD modeling of the projected 2PCF measured by Shen et al. for SDSS quasars with median redshift 3.2. We find tentative evidence for an increase in the mass scale of quasar host halos-the inferred median mass of halos hosting central quasars at z similar to 3.2 is M-cen = 14.1(-6.9)(+5.8) x 10(12) h(-1) M-circle dot. The cutoff profiles of the mean occupation functions of central quasars reveal that quasar luminosity is more tightly correlated with halo mass at higher redshifts. The average quasar duty cycle around the median host halo mass is inferred to be f(q) = 7.3(-1.5)(+0.6) x 10(-4) at z similar to 1.4 and f(q) = 8.6(-7.2)(+20.4) x 10(-2) at z similar to 3.2. We discuss the implications of our results for quasar evolution and quasar-galaxy co-evolution. C1 [Richardson, Jonathan; Chatterjee, Suchetana; Nagai, Daisuke] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Richardson, Jonathan; Zheng, Zheng; Nagai, Daisuke] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Zheng, Zheng] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Chatterjee, Suchetana] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Richardson, J (reprint author), Yale Univ, Dept Astron, New Haven, CT 06520 USA. FU Yale College Dean's Science Research Fellowship; Yale Center for Astronomy and Astrophysics through YCAA fellowship; NSF [AST-0806732, AST-1009811]; NASA ATP grant [NNX11AE07G]; Yale University; Smithsonian Astrophysical Observatory (SAO) through Clay Postdoctoral Fellowship FX We thank Frank van den Bosch, Andrey Kravtsov, Adam Myers, Nikhil Padmanabhan, David Weinberg, and Martin White for useful discussions and comments. We thank Joe Hennawi for providing his data and for helpful comments. We also thank the anonymous referee for useful suggestions that improved our paper. J.R. acknowledges support from a Yale College Dean's Science Research Fellowship through an early period of the project. Z.Z. gratefully acknowledges support from the Yale Center for Astronomy and Astrophysics through a YCAA fellowship at an early stage of this work. S. C. was partially supported by NSF grant AST-0806732 during the course of this work. D.N. was supported in part by NSF grant AST-1009811, NASA ATP grant NNX11AE07G, and by Yale University. Y.S. acknowledges support from the Smithsonian Astrophysical Observatory (SAO) through a Clay Postdoctoral Fellowship. NR 129 TC 30 Z9 30 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 AUG 10 PY 2012 VL 755 IS 1 AR 30 DI 10.1088/0004-637X/755/1/30 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500030 ER PT J AU Schaefer, L Lodders, K Fegley, B AF Schaefer, Laura Lodders, Katharina Fegley, Bruce, Jr. TI VAPORIZATION OF THE EARTH: APPLICATION TO EXOPLANET ATMOSPHERES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; atmospheric effects; planets and satellites: general ID METAL-RICH ATMOSPHERE; GJ 1214B; TRANSMISSION SPECTRUM; SUPER-EARTHS; SOLAR-SYSTEM; LOW-MASS; PLANETS; CHEMISTRY; EVOLUTION; CONDENSATION AB Currently, there are about three dozen known super-Earths (M < 10 M-circle plus), of which eight are transiting planets suitable for atmospheric follow-up observations. Some of the planets are exposed to extreme temperatures as they orbit close to their host stars, e. g., CoRot-7b, and all of these planets have equilibrium temperatures significantly hotter than the Earth. Such planets can develop atmospheres through (partial) vaporization of their crustal and/or mantle silicates. We investigated the chemical equilibrium composition of such heated systems from 500 to 4000 K and total pressures from 10(-6) to 10(+2) bars. The major gases are H2O and CO2 over broad temperature and pressure ranges, and Na, K, O-2, SiO, and O at high temperatures and low pressures. We discuss the differences in atmospheric composition arising from vaporization of SiO2-rich (i.e., felsic) silicates (like Earth's continental crust) and MgO-, FeO-rich (i.e., mafic) silicates (like the bulk silicate Earth). The computational results will be useful in planning spectroscopic studies of the atmospheres of Earth-like exoplanets. C1 Washington Univ, Dept Earth & Planetary Sci, Planetary Chem Lab, St Louis, MO 63130 USA. Washington Univ, McDonnell Ctr Space Sci, St Louis, MO 63130 USA. RP Schaefer, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM laura_s@wustl.edu; lodders@wustl.edu; bfegley@wustl.edu OI Schaefer, Laura/0000-0003-2915-5025 FU NSF Astronomy Program [AST-0707377]; NASA [NNX09AG69A]; NASA Ames Research Center FX This work was supported by the NSF Astronomy Program AST-0707377 and by NASA Cooperative Agreement NNX09AG69A with the NASA Ames Research Center. NR 65 TC 19 Z9 19 U1 3 U2 26 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2012 VL 755 IS 1 AR 41 DI 10.1088/0004-637X/755/1/41 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500041 ER PT J AU Williams, CL Hewitt, JN Levine, AM de Oliveira-Costa, A Bowman, JD Briggs, FH Gaensler, BM Hernquist, LL Mitchell, DA Morales, MF Sethi, SK Subrahmanyan, R Sadler, EM Arcus, W Barnes, DG Bernardi, G Bunton, JD Cappallo, RC Crosse, BW Corey, BE Deshpande, A deSouza, L Emrich, D Goeke, RF Greenhill, LJ Hazelton, BJ Herne, D Kaplan, DL Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Morgan, EH Oberoi, D Ord, SM Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, DA Salah, JE Sault, RJ Shankar, NU Srivani, KS Stevens, JB Tingay, SJ Wayth, RB Waterson, M Webster, RL Whitney, AR Williams, AJ Wyithe, SB AF Williams, Christopher L. Hewitt, Jacqueline N. Levine, Alan M. de Oliveira-Costa, Angelica Bowman, Judd D. Briggs, Frank H. Gaensler, B. M. Hernquist, Lars L. Mitchell, Daniel A. Morales, Miguel F. Sethi, Shiv K. Subrahmanyan, Ravi Sadler, Elaine M. Arcus, Wayne Barnes, David G. Bernardi, Gianni Bunton, John D. Cappallo, Roger C. Crosse, Brian W. Corey, Brian E. Deshpande, Avinash deSouza, Ludi Emrich, David Goeke, Robert F. Greenhill, Lincoln J. Hazelton, Bryna J. Herne, David Kaplan, David L. Kasper, Justin C. Kincaid, Barton B. Koenig, Ronald Kratzenberg, Eric Lonsdale, Colin J. Lynch, Mervyn J. McWhirter, S. Russell Morgan, Edward H. Oberoi, Divya Ord, Stephen M. Pathikulangara, Joseph Prabu, Thiagaraj Remillard, Ronald A. Rogers, Alan E. E. Roshi, D. Anish Salah, Joseph E. Sault, Robert J. Shankar, N. Udaya Srivani, K. S. Stevens, Jamie B. Tingay, Steven J. Wayth, Randall B. Waterson, Mark Webster, Rachel L. Whitney, Alan R. Williams, Andrew J. Wyithe, Stuart B. TI LOW-FREQUENCY IMAGING OF FIELDS AT HIGH GALACTIC LATITUDE WITH THE MURCHISON WIDEFIELD ARRAY 32 ELEMENT PROTOTYPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; instrumentation: interferometers; methods: data analysis; surveys ID NRAO PMN SURVEYS; SPECTRUM RADIO-SOURCES; 21 CENTIMETER TOMOGRAPHY; HIGH-REDSHIFT UNIVERSE; VLA SKY SURVEY; 6C SURVEY; SOURCE CATALOG; REIONIZATION EPOCH; ZONE 30-DEGREES-LESS-THAN-DELTA-LESS-THAN-51-DEGREES; INTERGALACTIC MEDIUM AB The Murchison Widefield Array (MWA) is a new low-frequency, wide-field-of-view radio interferometer under development at the Murchison Radio-astronomy Observatory in Western Australia. We have used a 32 element MWA prototype interferometer (MWA-32T) to observe two 50 degrees diameter fields in the southern sky, covering a total of similar to 2700 deg(2), in order to evaluate the performance of the MWA-32T, to develop techniques for epoch of reionization experiments, and to make measurements of astronomical foregrounds. We developed a calibration and imaging pipeline for the MWA-32T, and used it to produce similar to 15' angular resolution maps of the two fields in the 110-200 MHz band. We perform a blind source extraction using these confusion-limited images, and detect 655 sources at high significance with an additional 871 lower significance source candidates. We compare these sources with existing low-frequency radio surveys in order to assess the MWA-32T system performance, wide-field analysis algorithms, and catalog quality. Our source catalog is found to agree well with existing low-frequency surveys in these regions of the sky and with statistical distributions of point sources derived from Northern Hemisphere surveys; it represents one of the deepest surveys to date of this sky field in the 110-200 MHz band. C1 [Williams, Christopher L.; Hewitt, Jacqueline N.; Levine, Alan M.; Goeke, Robert F.; Morgan, Edward H.; Remillard, Ronald A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [de Oliveira-Costa, Angelica; Hernquist, Lars L.; Bernardi, Gianni; Greenhill, Lincoln J.; Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowman, Judd D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Briggs, Frank H.; Waterson, Mark] Australian Natl Univ, Res Sch Astron & Astrophys, Canberra, ACT, Australia. [Briggs, Frank H.; Gaensler, B. M.; Mitchell, Daniel A.; Subrahmanyan, Ravi; Sadler, Elaine M.; Tingay, Steven J.; Wayth, Randall B.; Webster, Rachel L.; Wyithe, Stuart B.] Univ Sydney, ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW 2006, Australia. [Gaensler, B. M.; Sadler, Elaine M.; deSouza, Ludi] Univ Sydney, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Mitchell, Daniel A.; Sault, Robert J.; Webster, Rachel L.; Wyithe, Stuart B.] Univ Melbourne, Sch Phys, Melbourne, Vic, Australia. [Morales, Miguel F.; Hazelton, Bryna J.] Univ Washington, Dept Phys, Seattle, WA 98195 USA. [Sethi, Shiv K.; Subrahmanyan, Ravi; Deshpande, Avinash; Prabu, Thiagaraj; Shankar, N. Udaya; Srivani, K. S.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Arcus, Wayne; Crosse, Brian W.; Emrich, David; Herne, David; Lynch, Mervyn J.; Ord, Stephen M.; Tingay, Steven J.; Wayth, Randall B.; Waterson, Mark] Curtin Univ Technol, Int Ctr Radio Astron Res, Perth, WA, Australia. [Barnes, David G.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Melbourne, Vic, Australia. [Bunton, John D.; deSouza, Ludi; Koenig, Ronald; Pathikulangara, Joseph; Stevens, Jamie B.] CSIRO Astron & Space Sci, Epping, NSW, Australia. [Cappallo, Roger C.; Corey, Brian E.; Kincaid, Barton B.; Kratzenberg, Eric; Lonsdale, Colin J.; McWhirter, S. Russell; Oberoi, Divya; Rogers, Alan E. E.; Salah, Joseph E.; Whitney, Alan R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Kaplan, David L.] Univ Wisconsin Milwaukee, Dept Phys, Milwaukee, WI USA. [Roshi, D. Anish] NRAO, Charlottesville, VA USA. [Stevens, Jamie B.] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Williams, Andrew J.] Perth Observ, Perth, WA, Australia. RP Williams, CL (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM clmw@mit.edu RI M, Manjunath/N-4000-2014; Bunton, John/A-4944-2008; Deshpande, Avinash/D-4868-2012; Sethi, Shiv/D-4893-2012; Subrahmanyan, Ravi/D-4889-2012; Wayth, Randall/B-2444-2013; Tingay, Steven/B-5271-2013; Emrich, David/B-7002-2013; Waterson, Mark/B-7352-2013; Ord, Stephen/C-6138-2013; Kasper, Justin/D-1152-2010; Gaensler, Bryan/F-8655-2010; Williams, Andrew/K-2931-2013; Udayashankar , N/D-4901-2012 OI Wyithe, Stuart/0000-0001-7956-9758; Sadler, Elaine/0000-0002-1136-2555; Gaensler, Bryan/0000-0002-3382-9558; M, Manjunath/0000-0001-8710-0730; Wayth, Randall/0000-0002-6995-4131; Emrich, David/0000-0002-4058-1837; Waterson, Mark/0000-0002-0192-2686; Kasper, Justin/0000-0002-7077-930X; Williams, Andrew/0000-0001-9080-0105; FU Australian Research Council [LE0775621, LE0882938]; National Science Foundation [AST-0457585, AST-0821321, AST-0908884, AST-1008353, PHY-0835713]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Australian National Collaborative Research Infrastructure Strategy; Australia India Strategic Research Fund; Smithsonian Astrophysical Observatory; MIT School of Science; MIT's Marble Astrophysics Fund; Raman Research Institute; Australian National University; iVEC Petabyte Data Store; NVIDIA; International Centre for Radio Astronomy Research; Joint Venture of Curtin University of Technology; University of Western Australia; Western Australian State government; [CE11E0001020] FX This scientific work uses data obtained from the Murchison Radio-astronomy Observatory. We acknowledge the Wajarri Yamatji people as the traditional owners of the observatory site. Support for this work comes from the Australian Research Council (grant Nos. LE0775621 and LE0882938), the National Science Foundation (grant Nos. AST-0457585, AST-0821321, AST-0908884, AST-1008353, and PHY-0835713), the U.S. Air Force Office of Scientific Research (grant No. FA9550-0510247), the Australian National Collaborative Research Infrastructure Strategy, Australia India Strategic Research Fund, the Smithsonian Astrophysical Observatory, the MIT School of Science, MIT's Marble Astrophysics Fund, the Raman Research Institute, the Australian National University, the iVEC Petabyte Data Store, the NVIDIA sponsored CUDA Center for Excellence at Harvard University, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University of Technology and the University of Western Australia, funded by the Western Australian State government. The Centre for All-sky Astrophysics is an Australian Research Council Centre of Excellence, funded by grant CE11E0001020. The MRO is managed by the CSIRO, who also provide operational support to the MWA. This research work has used the TIFR GMRT Sky Survey (http://tgss.ncra.tifr.res.in) data products. C.L.W. thanks Adrian Liu, and Leo Stein for helpful discussions and comments, as well as the Halleen family for their hospitality at Boolardy Station while working at the MRO. NR 82 TC 23 Z9 23 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2012 VL 755 IS 1 AR 47 DI 10.1088/0004-637X/755/1/47 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500047 ER PT J AU Youdin, AN Kratter, KM Kenyon, SJ AF Youdin, Andrew N. Kratter, Kaitlin M. Kenyon, Scott J. TI CIRCUMBINARY CHAOS: USING PLUTO'S NEWEST MOON TO CONSTRAIN THE MASSES OF NIX AND HYDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; Kuiper Belt objects: individual (Pluto, Charon); planets and satellites: dynamical evolution and stability; planets and satellites: formation; space vehicles ID GIANT IMPACT ORIGIN; DISK TURBULENCE DRIVEN; KUIPER-BELT; PLANET SYSTEMS; BINARY-SYSTEMS; GRAVITATIONAL-INSTABILITY; STREAMING INSTABILITY; RESONANCE OVERLAP; CHARON SYSTEM; SATELLITES AB The Pluto system provides a unique local laboratory for the study of binaries with multiple low-mass companions. In this paper, we study the orbital stability of P4, the most recently discovered moon in the Pluto system. This newfound companion orbits near the plane of the Pluto-Charon (PC) binary, roughly halfway between the two minor moons Nix and Hydra. We use a suite of few body integrations to constrain the masses of Nix and Hydra, and the orbital parameters of P4. For the system to remain stable over the age of the solar system, the masses of Nix and Hydra likely do not exceed 5 x 10(16) kg and 9 x 10(16) kg, respectively. These upper limits assume a fixed mass ratio between Nix and Hydra at the value implied by their median optical brightness. Our study finds that stability is more sensitive to their total mass and that a downward revision of Charon's eccentricity (from our adopted value of 0.0035) is unlikely to significantly affect our conclusions. Our upper limits are an order of magnitude below existing astrometric limits on the masses of Nix and Hydra. For a density at least that of ice, the albedos of Nix and Hydra would exceed 0.3. This constraint implies they are icy, as predicted by giant impact models. Even with these low masses, P4 only remains stable if its eccentricity e less than or similar to 0.02. The 5: 1 commensurability with Charon is particularly unstable, combining stability constraints with the observed mean motion places the preferred orbit for P4 just exterior to the 5: 1 resonance. These predictions will be tested when the New Horizons satellite visits Pluto. Based on the results for the PC system, we expect that circumbinary, multi-planet systems will be more widely spaced than their singleton counterparts. Further, circumbinary exoplanets close to the three-body stability boundary, such as those found by Kepler, are less likely to have other companions nearby. C1 [Youdin, Andrew N.; Kratter, Kaitlin M.; Kenyon, Scott J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Youdin, AN (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Youdin, Andrew/C-1596-2013; OI Youdin, Andrew/0000-0002-3644-8726; Kenyon, Scott/0000-0003-0214-609X FU NASA [NNX10AF35G, NNX11AM37G] FX We thank Matt Holman, Alex Parker, Dan Fabrycky, and Josh Carter for helpful discussions. A.N.Y. and K. M. K. thank Tom Aldcroft, Tom Robitaille, Brian Refsdal, and Gus Muench for http://python4astronomers.github.com. Portions of this project were supported by the NASA Astrophysics Theory Program and Origins of Solar Systems Program through grant NNX10AF35G and the Outer Planets Program through grant NNX11AM37G. The computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 60 TC 23 Z9 23 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 AUG 10 PY 2012 VL 755 IS 1 AR 17 DI 10.1088/0004-637X/755/1/17 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 980RA UT WOS:000306909500017 ER PT J AU Passmore, HA Bruna, EM Heredia, SM Vasconcelos, HL AF Passmore, Heather A. Bruna, Emilio M. Heredia, Sylvia M. Vasconcelos, Heraldo L. TI Resilient Networks of Ant-Plant Mutualists in Amazonian Forest Fragments SO PLOS ONE LA English DT Article ID FOOD WEBS; POLLINATOR INTERACTIONS; ECOLOGICAL NETWORKS; GLOBAL CHANGE; RAIN-FORESTS; SPECIES LOSS; HABITAT; SPECIALIZATION; DIVERSITY; BIODIVERSITY AB Background: The organization of networks of interacting species, such as plants and animals engaged in mutualisms, strongly influences the ecology and evolution of partner communities. Habitat fragmentation is a globally pervasive form of spatial heterogeneity that could profoundly impact the structure of mutualist networks. This is particularly true for biodiversity-rich tropical ecosystems, where the majority of plant species depend on mutualisms with animals and it is thought that changes in the structure of mutualist networks could lead to cascades of extinctions. Methodology/Principal Findings: We evaluated effects of fragmentation on mutualistic networks by calculating metrics of network structure for ant-plant networks in continuous Amazonian forests with those in forest fragments. We hypothesized that networks in fragments would have fewer species and higher connectance, but equal nestedness and resilience compared to forest networks. Only one of the nine metrics we compared differed between continuous forest and forest fragments, indicating that networks were resistant to the biotic and abiotic changes that accompany fragmentation. This is partially the result of the loss of only specialist species with one connection that were lost in forest fragments. Conclusions/Significance: We found that the networks of ant-plant mutualists in twenty-five year old fragments are similar to those in continuous forest, suggesting these interactions are resistant to the detrimental changes associated with habitat fragmentation, at least in landscapes that are a mosaic of fragments, regenerating forests, and pastures. However, ant-plant mutualistic networks may have several properties that may promote their persistence in fragmented landscapes. Proactive identification of key mutualist partners may be necessary to focus conservation efforts on the interactions that insure the integrity of network structure and the ecosystems services networks provide. C1 [Passmore, Heather A.; Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32610 USA. [Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL USA. [Heredia, Sylvia M.] Univ Calif Riverside, Dept Bot & Plant Sci, Riverside, CA 92521 USA. [Vasconcelos, Heraldo L.] Univ Fed Uberlandia, Inst Biol, BR-38400 Uberlandia, MG, Brazil. [Bruna, Emilio M.; Heredia, Sylvia M.; Vasconcelos, Heraldo L.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, Manaus, Amazonas, Brazil. [Bruna, Emilio M.; Heredia, Sylvia M.; Vasconcelos, Heraldo L.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil. RP Passmore, HA (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32610 USA. EM embruna@ufl.edu RI Bruna, Emilio/H-2769-2012; Vasconcelos, Heraldo/C-3353-2013 OI Bruna, Emilio/0000-0003-3381-8477; Vasconcelos, Heraldo/0000-0001-6969-7131 FU United States National Science Foundation [DEB-0453631, DEB-0309819] FX This research was supported by grants DEB-0453631 and DEB-0309819 from the United States National Science Foundation (http://nsf.gov). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 59 TC 11 Z9 11 U1 6 U2 65 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 AUG 9 PY 2012 VL 7 IS 8 AR e40803 DI 10.1371/journal.pone.0040803 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 986WZ UT WOS:000307378500003 PM 22912666 ER PT J AU Smith, DR AF Smith, David R. TI The South American genus Lagideus Konow (Hymenoptera: Pergidae: Syzygoniinae), a Supplement SO ZOOTAXA LA English DT Article DE sawflies; new species; Central America; South America AB Six new species of the Neotropical pergid genus Lagideus are described and illustrated: Lagideus boyaca, L. magdalena, L. schmidti, and L. flavus from Colombia and L. tapanti, and L. isidro from Costa Rica. Lagideus romius Smith is newly recorded from Colombia and the female lancet is illustrated. Females are described for the first time for Lagideus longicus Smith from Costa Rica and L. albitarsis Malaise from southeastern Brazil, Uruguay, and Argentina. C1 ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM sawfly2@aol.com FU National Science Foundation [DEB9972024, DEB0205982] FX The specimens from Colombia were acquired through the Colombian Arthropod Survey, National Science Foundation Grants DEB9972024 and DEB0205982 to Michael J. Sharkey, University of Kentucky, Lexington. I appreciate the loan of specimens from P. Hanson (UCR), A. Taeger and S. M. Blank (SDEI), and J. Wiley (FSCA). Michele Touchet, Systematic Entomology Laboratory, USDA, Washington, DC, helped with the images. I appreciate the comments of the following reviewers: S. M. McKamey and T J. Henry, Systematic Entomology Laboratory, USDA, Washington, D. C. USDA is an equal opportunity provider and employer. NR 7 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 AUG 7 PY 2012 IS 3413 BP 1 EP 18 PG 18 WC Zoology SC Zoology GA 985BH UT WOS:000307237800001 ER PT J AU Erb, PL McShea, WJ Guralnick, RP AF Erb, Peter L. McShea, William J. Guralnick, Robert P. TI Anthropogenic Influences on Macro-Level Mammal Occupancy in the Appalachian Trail Corridor SO PLOS ONE LA English DT Article ID FOXES VULPES-VULPES; WHITE-TAILED DEER; WILDLIFE RESPONSES; MESOPREDATOR RELEASE; SPECIES DISTRIBUTION; CITIZEN SCIENCE; HABITAT; BIODIVERSITY; RECREATION; MODELS AB Anthropogenic effects on wildlife are typically assessed at the local level, but it is often difficult to extrapolate to larger spatial extents. Macro-level occupancy studies are one way to assess impacts of multiple disturbance factors that might vary over different geographic extents. Here we assess anthropogenic effects on occupancy and distribution for several mammal species within the Appalachian Trail (AT), a forest corridor that extends across a broad section of the eastern United States. Utilizing camera traps and a large volunteer network of citizen scientists, we were able to sample 447 sites along a 1024 km section of the AT to assess the effects of available habitat, hunting, recreation, and roads on eight mammal species. Occupancy modeling revealed the importance of available forest to all species except opossums (Didelphis virginiana) and coyotes (Canis latrans). Hunting on adjoining lands was the second strongest predictor of occupancy for three mammal species, negatively influencing black bears (Ursus americanus) and bobcats (Lynx rufus), while positively influencing raccoons (Procyon lotor). Modeling also indicated an avoidance of high trail use areas by bears and proclivity towards high use areas by red fox (Vulpes vulpes). Roads had the lowest predictive power on species occupancy within the corridor and were only significant for deer. The occupancy models stress the importance of compounding direct and indirect anthropogenic influences operating at the regional level. Scientists and managers should consider these human impacts and their potential combined influence on wildlife persistence when assessing optimal habitat or considering management actions. C1 [Erb, Peter L.; Guralnick, Robert P.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Erb, Peter L.; McShea, William J.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Guralnick, Robert P.] Univ Colorado, Museum Nat Hist, Boulder, CO 80309 USA. RP Erb, PL (reprint author), Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. EM Peter.Erb@colorado.edu FU Smithsonian Institution; University of Colorado Museum of Natural History; Department of Ecology and Evolutionary Biology at CU-Boulder; Appalachian Trail Conservancy FX Funding was provided by the Smithsonian Institution (www.si.edu), the University of Colorado Museum of Natural History (cumuseum.colorado.edu), the Department of Ecology and Evolutionary Biology at CU-Boulder (ebio.colorado.edu) and the Appalachian Trail Conservancy (www.appalachiantrail.org). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 61 TC 15 Z9 16 U1 11 U2 119 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 AUG 6 PY 2012 VL 7 IS 8 AR e42574 DI 10.1371/journal.pone.0042574 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 992WD UT WOS:000307810000047 PM 22880038 ER PT J AU Mathy, CJM Huse, DA Hulet, RG AF Mathy, Charles J. M. Huse, David A. Hulet, Randall G. TI Enlarging and cooling the Neel state in an optical lattice SO PHYSICAL REVIEW A LA English DT Article ID MOTT INSULATOR; ATOMS AB We propose an experimental scheme to favor both the realization and the detection of the Neel state in a two-component gas of ultracold fermions in a three-dimensional simple-cubic optical lattice. By adding three compensating Gaussian laser beams to the standard three pairs of retroreflected lattice beams, and adjusting the relative waists and intensities of the beams, one can significantly enhance the size of the Neel state in the trap, thus increasing the signal of optical Bragg scattering. Furthermore, the additional beams provide for adjustment of the local chemical potential and the possibility to evaporatively cool the gas while in the lattice. Our proposals are also relevant to efforts to realize other many-body quantum phases in optical lattices. C1 [Mathy, Charles J. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Mathy, Charles J. M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Huse, David A.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Hulet, Randall G.] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. RP Mathy, CJM (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. FU NSF through ITAMP at Harvard University; Smithsonian Astrophysical Observatory; ARO Award from the DARPA OLE Program [W911NF-07-1-0464]; NSF; ONR; Welch Foundation [C-1133] FX We would like to thank Pedro Duarte and Russell Hart for useful discussions. C.J.M.M. acknowledges support from the NSF through ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. This work was supported in part by ARO Award W911NF-07-1-0464 with funds from the DARPA OLE Program. The work at Rice is also supported by the NSF, ONR, and the Welch Foundation (C-1133). NR 20 TC 22 Z9 22 U1 1 U2 9 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD AUG 6 PY 2012 VL 86 IS 2 AR 023606 DI 10.1103/PhysRevA.86.023606 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 985LJ UT WOS:000307267600006 ER PT J AU Balunas, MJ Grosso, MF Villa, FA Engene, N McPhail, KL Tidgewell, K Pineda, LM Gerwick, L Spadafora, C Kyle, DE Gerwick, WH AF Balunas, Marcy J. Grosso, Manuel F. Villa, Francisco A. Engene, Niclas McPhail, Kerry L. Tidgewell, Kevin Pineda, Laura M. Gerwick, Lena Spadafora, Carmenza Kyle, Dennis E. Gerwick, William H. TI Coibacins A-D, Antileishmanial Marine Cyanobacterial Polyketides with Intriguing Biosynthetic Origins SO ORGANIC LETTERS LA English DT Article ID LYNGBYA-MAJUSCULA; NATURAL-PRODUCTS AB Four unsaturated polyketide lactone derivatives, coibacins A-D, were isolated from a Panamanian marine cyanobacterium, cf. Oscillatorla sp. The two different types of termini observed in these co-occurring metabolites, either a methyl cyclopropyl ring as seen in curacin A or a methyl vinyl chloride similar to that observed in the jamaicamides, suggest an intriguing flexibility in the "beta branch" forming biosynthetic process. The coibacins possess selective antileishmanial activity as well as potent anti-inflammatory activity. C1 [Balunas, Marcy J.; Villa, Francisco A.; Engene, Niclas; Tidgewell, Kevin; Gerwick, Lena; Gerwick, William H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. [Balunas, Marcy J.; Villa, Francisco A.; Engene, Niclas; Tidgewell, Kevin; Gerwick, Lena; Gerwick, William H.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. [Balunas, Marcy J.; Gerwick, William H.] Smithsonian Trop Res Inst, Panama City, Panama. [Balunas, Marcy J.; Grosso, Manuel F.; Pineda, Laura M.; Spadafora, Carmenza] Inst Invest Cient & Serv Alta Technol, Panama City, Panama. [McPhail, Kerry L.] Oregon State Univ, Coll Pharm, Corvallis, OR 97331 USA. [Kyle, Dennis E.] Univ S Florida, Coll Publ Hlth, Dept Global Hlth, Tampa, FL 33612 USA. RP Gerwick, WH (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. EM wgerwick@ucsd.edu OI Spadafora, Carmenza/0000-0002-3002-9467; Tidgewell , Kevin/0000-0002-0501-2604 FU Fogarty International Center (FIC) International Cooperative Biodiversity Group (ICBG) [U01 TW006634]; FIC [K01 TW008002]; Panamanian Ministry of Science (SENACYT) [EST07-030B] FX We thank A. Pereira Badilla (CD spectra, UCSD), T. Byrum (NCI-H460 bioassay data, UCSD) and A. Srivastava and B. Vesely (amastigote assays, USF), and acknowledge funding from the Fogarty International Center (FIC) International Cooperative Biodiversity Group (ICBG) (Grant No. U01 TW006634), an FIC International Research Scientist Development Award (IRSDA) to M.J.B. (K01 TW008002), and a Panamanian Ministry of Science (SENACYT) Estimulos grant to M.J.B. (EST07-030B). NR 10 TC 21 Z9 21 U1 1 U2 35 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1523-7060 J9 ORG LETT JI Org. Lett. PD AUG 3 PY 2012 VL 14 IS 15 BP 3878 EP 3881 DI 10.1021/ol301607q PG 4 WC Chemistry, Organic SC Chemistry GA 982KI UT WOS:000307041600017 PM 22794317 ER PT J AU Carter, JA Agol, E Chaplin, WJ Basu, S Bedding, TR Buchhave, LA Christensen-Dalsgaard, J Deck, KM Elsworth, Y Fabrycky, DC Ford, EB Fortney, JJ Hale, SJ Handberg, R Hekker, S Holman, MJ Huber, D Karoff, C Kawaler, SD Kjeldsen, H Lissauer, JJ Lopez, ED Lund, MN Lundkvist, M Metcalfe, TS Miglio, A Rogers, LA Stello, D Borucki, WJ Bryson, S Christiansen, JL Cochran, WD Geary, JC Gilliland, RL Haas, MR Hall, J Howard, AW Jenkins, JM Klaus, T Koch, DG Latham, DW MacQueen, PJ Sasselov, D Steffen, JH Twicken, JD Winn, JN AF Carter, Joshua A. Agol, Eric Chaplin, William J. Basu, Sarbani Bedding, Timothy R. Buchhave, Lars A. Christensen-Dalsgaard, Jorgen Deck, Katherine M. Elsworth, Yvonne Fabrycky, Daniel C. Ford, Eric B. Fortney, Jonathan J. Hale, Steven J. Handberg, Rasmus Hekker, Saskia Holman, Matthew J. Huber, Daniel Karoff, Christopher Kawaler, Steven D. Kjeldsen, Hans Lissauer, Jack J. Lopez, Eric D. Lund, Mikkel N. Lundkvist, Mia Metcalfe, Travis S. Miglio, Andrea Rogers, Leslie A. Stello, Dennis Borucki, William J. Bryson, Steve Christiansen, Jessie L. Cochran, William D. Geary, John C. Gilliland, Ronald L. Haas, Michael R. Hall, Jennifer Howard, Andrew W. Jenkins, Jon M. Klaus, Todd Koch, David G. Latham, David W. MacQueen, Phillip J. Sasselov, Dimitar Steffen, Jason H. Twicken, Joseph D. Winn, Joshua N. TI Kepler-36: A Pair of Planets with Neighboring Orbits and Dissimilar Densities SO SCIENCE LA English DT Article ID TRANSIT TIMING VARIATIONS; LOW-MASS; STAR; MISSION; SYSTEMS; PERFORMANCE; STABILITY; COMPANION; SCIENCE; CURVES AB In the solar system, the planets' compositions vary with orbital distance, with rocky planets in close orbits and lower-density gas giants in wider orbits. The detection of close-in giant planets around other stars was the first clue that this pattern is not universal and that planets' orbits can change substantially after their formation. Here, we report another violation of the orbit-composition pattern: two planets orbiting the same star with orbital distances differing by only 10% and densities differing by a factor of 8. One planet is likely a rocky "super-Earth," whereas the other is more akin to Neptune. These planets are 20 times more closely spaced and have a larger density contrast than any adjacent pair of planets in the solar system. C1 [Carter, Joshua A.; Holman, Matthew J.; Geary, John C.; Latham, David W.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Chaplin, William J.; Elsworth, Yvonne; Hale, Steven J.; Miglio, Andrea] Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, England. [Basu, Sarbani] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bedding, Timothy R.; Stello, Dennis] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bedding, Timothy R.; Stello, Dennis] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Christensen-Dalsgaard, Jorgen; Handberg, Rasmus; Karoff, Christopher; Kjeldsen, Hans; Lund, Mikkel N.; Lundkvist, Mia] Aarhus Univ, Stellar Astrophys Ctr, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Deck, Katherine M.; Rogers, Leslie A.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.; Rogers, Leslie A.; Winn, Joshua N.] Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.; Lopez, Eric D.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ford, Eric B.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Hekker, Saskia] Univ Amsterdam, Astron Inst Anton Pannekoek, Netherlands Sch Phys, Amsterdam, Netherlands. [Christiansen, Jessie L.; Jenkins, Jon M.; Twicken, Joseph D.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Kawaler, Steven D.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Metcalfe, Travis S.] White Dwarf Res Corp, Boulder, CO 80301 USA. [Cochran, William D.; MacQueen, Phillip J.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Hall, Jennifer; Klaus, Todd] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howard, Andrew W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. RP Carter, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jacarter@cfa.harvard.edu; agol@astro.washington.edu RI Steffen, Jason/A-4320-2013; Carter, Joshua/A-8280-2013; Agol, Eric/B-8775-2013; Basu, Sarbani/B-8015-2014; Hale, Steven/E-3472-2015; OI Buchhave, Lars A./0000-0003-1605-5666; Bedding, Timothy/0000-0001-5943-1460; Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661; Kawaler, Steven/0000-0002-6536-6367; Agol, Eric/0000-0002-0802-9145; Basu, Sarbani/0000-0002-6163-3472; Hale, Steven/0000-0002-6402-8382; Fortney, Jonathan/0000-0002-9843-4354; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [HF-51267.01-A, HF-51272.01-A, NAS 5-26555]; Space Telescope Science Institute; NSF [AST-0645416]; Center for Astrophysics; UK Science and Technology Facilities Council (STFC); Danish National Research Foundation; ASTERISK project (ASTERoseismic Investigations with SONG and Kepler); European Research Council [267864]; Netherlands Organization for Scientific Research (NWO); NASA Kepler Participating Scientist program [NNX12AC76G] FX NASA's Science Mission Directorate provided funding for the Kepler Discovery mission. J.A.C. and D. C. F. acknowledge support by NASA through Hubble Fellowship grants HF-51267.01-A and HF-51272.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, for NASA, under contract NAS 5-26555. E. A. acknowledges NSF Career grant AST-0645416 and thanks the Center for Astrophysics, where this work began. W.J.C., A. M., and Y.E. acknowledge the financial support of the UK Science and Technology Facilities Council (STFC). Funding for the Stellar Astrophysics Centre (SAC) is provided by the Danish National Research Foundation. The research is supported by the ASTERISK project (ASTERoseismic Investigations with SONG and Kepler) funded by the European Research Council (grant agreement no. 267864). S. H. acknowledges financial support from the Netherlands Organization for Scientific Research (NWO). Computational time on Kraken at the National Institute of Computational Sciences was provided through NSF TeraGrid allocation TG-AST090107. J.N.W. was supported by the NASA Kepler Participating Scientist program through grant NNX12AC76G. Refer to the supplementary materials for access information to data used in this work. NR 26 TC 148 Z9 149 U1 8 U2 18 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 AUG 3 PY 2012 VL 337 IS 6094 BP 556 EP 559 DI 10.1126/science.1223269 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 982PU UT WOS:000307058700038 PM 22722249 ER PT J AU Ballantine, DL Ruiz, H AF Ballantine, David L. Ruiz, Hector TI Peyssonnelia stratosa sp nov (Peyssonneliaceae, Rhodophyta), a new shallow-water species from Puerto Rico, Caribbean Sea SO CRYPTOGAMIE ALGOLOGIE LA English DT Article DE Caribbean; Peyssonnelia; Peyssonneliaceae; Puerto Rico; Rhodophyta; western Atlantic ID MARINE-ALGAE; GIGARTINALES AB A new Peyssonnelia species from shallow water habitats in southwest Puerto Rico is described. Peyssonnelia stratosa is yellowish beige or reddish in color and is composed of small overlapping blades 2-3 cm in diameter and forms extensive colonies. Peyssonnelia stratosa exhibits small cells at mid level in the perithallus, both immediate distal and proximal cells being much longer, giving the appearance of stratification within the perithallus. Tetrasporangia, cut off laterally from an enlarged proximal nemathecial cell, reach 190 mu m in length. C1 [Ballantine, David L.; Ruiz, Hector] Univ Puerto Rico, Dept Marine Sci, Mayaguez, PR 00681 USA. [Ballantine, David L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. RP Ballantine, DL (reprint author), Univ Puerto Rico, Dept Marine Sci, POB 9013, Mayaguez, PR 00681 USA. EM david.ballantine@upr.edu NR 27 TC 2 Z9 2 U1 0 U2 1 PU ADAC-CRYPTOGAMIE PI PARIS PA 12 RUE DE BUFFON, 75005 PARIS, FRANCE SN 0181-1568 J9 CRYPTOGAMIE ALGOL JI Cryptogam. Algol. PD AUG PY 2012 VL 33 IS 3 BP 235 EP 244 PG 10 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 023LT UT WOS:000310036500001 ER PT J AU Parker, JD Salminen, JP Agrawal, AA AF Parker, J. D. Salminen, J. -P. Agrawal, Anurag A. TI Evolutionary Potential of Root Chemical Defense: Genetic Correlations with Shoot Chemistry and Plant Growth SO JOURNAL OF CHEMICAL ECOLOGY LA English DT Article DE Allocation; Below-ground; Chemical defense; Growth; Phenolics; Roots; Trade-off ID PRIMROSE OENOTHERA-BIENNIS; HERBIVORY; RESISTANCE; ECOLOGY; TRAITS AB Root herbivores can affect plant fitness, and roots often contain the same secondary metabolites that act as defenses in shoots, but the ecology and evolution of root chemical defense have been little investigated. Here, we investigated genetic variance, heritability, and correlations among defensive phenolic compounds in shoot vs. root tissues of common evening primrose, Oenothera biennis. Across 20 genotypes, there were roughly similar concentrations of total phenolics in shoots vs. roots, but the allocation of particular phenolics to shoots vs. roots varied along a continuum of genotype growth rate. Slow-growing genotypes allocated 2-fold more of the potential pro-oxidant oenothein B to shoots than roots, whereas fast-growing genotypes had roughly equivalent above and belowground concentrations. Phenolic concentrations in both roots and shoots were strongly heritable, with mostly positive patterns of genetic covariation. Nonetheless, there was genotype-specific variation in the presence/absence of two major ellagitannins (oenothein A and its precursor oenothein B), indicating two different chemotypes based on alterations in this chemical pathway. Overall, the presence of strong genetic variation in root defenses suggests ample scope for the evolution of these compounds as defenses against root herbivores. C1 [Parker, J. D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Salminen, J. -P.] Univ Turku, Dept Chem, Lab Organ Chem & Chem Biol, Turku 20014, Finland. [Agrawal, Anurag A.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. RP Parker, JD (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM parkerj@si.edu RI Parker, John/F-9761-2010 OI Parker, John/0000-0002-3632-7625 FU NSF-DEB [1118783] FX We thank Alex Smith, Marc Johnson, Mike Stastny, Kailen Mooney, Scott McArt, Susan Cook-Patton, Alexis Erwin, Jennifer Thaler, Piia Koskinen, and Marc Lajeunesse for discussions or assisting with field and laboratory work. This work was supported by NSF-DEB 1118783 (A.A.A.). NR 10 TC 6 Z9 6 U1 2 U2 41 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0098-0331 J9 J CHEM ECOL JI J. Chem. Ecol. PD AUG PY 2012 VL 38 IS 8 BP 992 EP 995 DI 10.1007/s10886-012-0163-1 PG 4 WC Biochemistry & Molecular Biology; Ecology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology GA 015WU UT WOS:000309477900006 PM 22790783 ER PT J AU Arnold, LA Watson, DM Kim, KH Manoj, P Remming, I Sheehan, P Adame, L Forrest, WJ Furlan, E Mamajek, E McClure, M Espaillat, C Ausfeld, K Rapson, VA AF Arnold, L. A. Watson, Dan M. Kim, K. H. Manoj, P. Remming, I. Sheehan, P. Adame, L. Forrest, W. J. Furlan, E. Mamajek, E. McClure, M. Espaillat, C. Ausfeld, K. Rapson, V. A. TI A SPITZER IRS SURVEY OF NGC 1333: INSIGHTS INTO DISK EVOLUTION FROM A VERY YOUNG CLUSTER SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; dust, extinction; infrared: stars; open clusters and associations: individual (NGC 1333, Taurus-Auriga, Ophiuchus, Chamaeleon I); protoplanetary disks; stars: formation ID T-TAURI STARS; INFRARED SPECTROGRAPH SURVEY; MAIN-SEQUENCE STARS; LOW-MASS STARS; EVOLVED PROTOPLANETARY DISKS; DARK CLOUD COMPLEXES; CLASS-I PROTOSTARS; STELLAR OBJECTS; GRAIN-GROWTH; SPACE-TELESCOPE AB We report on the lambda = 5-36 mu m Spitzer Infrared Spectrograph (IRS) spectra of 79 young stellar objects in the very young nearby cluster NGC 1333. NGC 1333's youth enables the study of early protoplanetary disk properties, such as the degree of settling and the formation of gaps and clearings. We construct spectral energy distributions (SEDs) using our IRS data as well as published photometry and classify our sample into SED classes. Using "extinction-free" spectral indices, we determine whether the disk, envelope, or photosphere dominates the spectrum. We analyze the dereddened spectra of objects that show disk-dominated emission using spectral indices and properties of silicate features in order to study the vertical and radial structure of protoplanetary disks in NGC 1333. At least nine objects in our sample of NGC 1333 show signs of large (several AU) radial gaps or clearings in their inner disk. Disks with radial gaps in NGC 1333 show more nearly pristine silicate dust than their radially continuous counterparts. We compare properties of disks in NGC 1333 to those in three other well-studied regions, Taurus-Auriga, Ophiuchus, and Chamaeleon I, and find no difference in their degree of sedimentation and dust processing. C1 [Arnold, L. A.; Watson, Dan M.; Kim, K. H.; Manoj, P.; Remming, I.; Sheehan, P.; Forrest, W. J.; Mamajek, E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Adame, L.; McClure, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Furlan, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ausfeld, K.; Rapson, V. A.] Rochester Inst Technol, Ctr Imaging Sci, Rochester, NY 14623 USA. RP Arnold, LA (reprint author), Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. EM laa@pas.rochester.edu; dmw@pas.rochester.edu OI McClure, Melissa/0000-0003-1878-327X; Adame, Lucia/0000-0002-6328-6099; Furlan, Elise/0000-0001-9800-6248 FU National Aeronautics and Space Administration (NASA) [1407, 1257184]; National Science Foundation; JPL/Caltech; JPL [960803]; Cornell [31419-5714] 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 the National Aeronautics and Space Administration (NASA) contract 1407. In this work we make 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 also utilizes the Vizier and SIMBAD databases, operated at CDS, Strasbourg, France, NASA's Astrophysics Data System Abstract Service. Support for this work was provided by NASA through contract number 1257184 issued by JPL/Caltech, JPL contract 960803 to Cornell University, and Cornell subcontracts 31419-5714 to the University of Rochester. NR 125 TC 5 Z9 5 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 AUG PY 2012 VL 201 IS 2 AR 12 DI 10.1088/0067-0049/201/2/12 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016YN UT WOS:000309555900005 ER PT J AU Civano, F Elvis, M Brusa, M Comastri, A Salvato, M Zamorani, G Aldcroft, T Bongiorno, A Capak, P Cappelluti, N Cisternas, M Fiore, F Fruscione, A Hao, H Kartaltepe, J Koekemoer, A Gilli, R Impey, CD Lanzuisi, G Lusso, E Mainieri, V Miyaji, T Lilly, S Masters, D Puccetti, S Schawinski, K Scoville, NZ Silverman, J Trump, J Urry, M Vignali, C Wright, NJ AF Civano, F. Elvis, M. Brusa, M. Comastri, A. Salvato, M. Zamorani, G. Aldcroft, T. Bongiorno, A. Capak, P. Cappelluti, N. Cisternas, M. Fiore, F. Fruscione, A. Hao, H. Kartaltepe, J. Koekemoer, A. Gilli, R. Impey, C. D. Lanzuisi, G. Lusso, E. Mainieri, V. Miyaji, T. Lilly, S. Masters, D. Puccetti, S. Schawinski, K. Scoville, N. Z. Silverman, J. Trump, J. Urry, M. Vignali, C. Wright, N. J. TI THE CHANDRA COSMOS SURVEY. III. OPTICAL AND INFRARED IDENTIFICATION OF X-RAY POINT SOURCES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: active; surveys; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; SUPERMASSIVE BLACK-HOLES; GALAXY LIGHT CONCENTRATION; HUBBLE-SPACE-TELESCOPE; SPECTRAL ENERGY-DISTRIBUTIONS; MEDIUM-SENSITIVITY SURVEY; EVOLUTION SURVEY COSMOS; MS SOURCE CATALOGS; DIGITAL SKY SURVEY AB The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra program that has imaged the central 0.9 deg(2) of the COSMOS field down to limiting depths of 1.9 x 10(-16) erg cm(-2) s(-1) in the soft (0.5-2 keV) band, 7.3 x 10(-16) erg cm(-2) s(-1) in the hard (2-10 keV) band, and 5.7 x 10(-16) erg cm(-2) s(-1) in the full (0.5-10 keV) band. In this paper we report the i, K, and 3.6 mu m identifications of the 1761 X-ray point sources. We use the likelihood ratio technique to derive the association of optical/infrared counterparts for 97% of the X-ray sources. For most of the remaining 3%, the presence of multiple counterparts or the faintness of the possible counterpart prevented a unique association. For only 10 X-ray sources we were not able to associate a counterpart, mostly due to the presence of a very bright field source close by. Only two sources are truly empty fields. The full catalog, including spectroscopic and photometric redshifts and classification described here in detail, is available online. Making use of the large number of X-ray sources, we update the "classic locus" of active galactic nuclei (AGNs) defined 20 years ago in soft X-ray surveys and define a new locus containing 90% of the AGNs in the survey with full-band luminosity >10(42) erg s(-1). We present the linear fit between the total i-band magnitude and the X-ray flux in the soft and hard bands, drawn over two orders of magnitude in X-ray flux, obtained using the combined C-COSMOS and XMM-COSMOS samples. We focus on the X-ray to optical flux ratio (X/O) and we test its known correlation with redshift and luminosity, and a recently introduced anti-correlation with the concentration index (C). We find a strong anti-correlation (though the dispersion is of the order of 0.5 dex) between X/O computed in the hard band and C and that 90% of the obscured AGNs in the sample with morphological information live in galaxies with regular morphology (bulgy and disky/spiral), suggesting that secular processes govern a significant fraction of the black hole growth at X-ray luminosities of 10(43)-10(44.5) erg s(-1). We also investigate the degree of obscuration of the sample using the hardness ratio, and we compare the X-ray color with the near-infrared to optical color. C1 [Civano, F.; Elvis, M.; Aldcroft, T.; Fruscione, A.; Hao, H.; Lanzuisi, G.; Wright, N. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brusa, M.; Salvato, M.; Bongiorno, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Comastri, A.; Zamorani, G.; Cappelluti, N.; Gilli, R.; Lusso, E.; Vignali, C.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Salvato, M.] Excellence Cluster, D-85748 Garching, Germany. [Bongiorno, A.; Fiore, F.; Lanzuisi, G.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Capak, P.; Scoville, N. Z.] CALTECH, Pasadena, CA 91125 USA. [Cisternas, M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kartaltepe, J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Koekemoer, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Koekemoer, A.] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Impey, C. D.; Trump, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mainieri, V.] ESO, D-85748 Garching, Germany. [Miyaji, T.] Univ Nacl Autonoma Mexico Ensenada, Ensenada 22860, Baja California, Mexico. [Lilly, S.] Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Masters, D.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Schawinski, K.; Urry, M.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Silverman, J.] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Civano, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Vignali, Cristian/J-4974-2012; Lanzuisi, Giorgio/K-4378-2013; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Cappelluti, Nico/0000-0002-1697-186X; Puccetti, Simonetta/0000-0002-2734-7835; Schawinski, Kevin/0000-0001-5464-0888; Koekemoer, Anton/0000-0002-6610-2048; Zamorani, Giovanni/0000-0002-2318-301X; Vignali, Cristian/0000-0002-8853-9611; Lanzuisi, Giorgio/0000-0001-9094-0984; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Bongiorno, Angela/0000-0002-0101-6624; Urry, Meg/0000-0002-0745-9792; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157 FU NASA [GO7-8136A]; Blancheflor Boncompagni Ludovisi foundation; Smithsonian Scholarly Studies; ASI/INAF [I/009/10/0, I/088/06]; PRIN INAF; German Deutsche Forschungsgemeinschaft, DFG [FKZ HA 1850/28-1]; CONACyT [83564]; UNAM/DGAPA PAPIIT [IN110209] FX The authors thank the referee for the useful suggestions which helped to improve the paper. F. C. thanks R. D'Abrusco, A. Goulding, M. Mignoli, and M. Povic for inspiring discussions and useful comments. This work was supported in part by NASA Chandra grant number GO7-8136A (M. E., F. C., H. H.), the Blancheflor Boncompagni Ludovisi foundation (F. C.), and the Smithsonian Scholarly Studies (F. C.). In Italy this work is supported by ASI/INAF contracts I/009/10/0 and I/088/06 and by PRIN INAF 2010 "From the dawn of galaxy formation to the peak of the mass assembly." M. S. acknowledges support by the German Deutsche Forschungsgemeinschaft, DFG Leibniz Prize (FKZ HA 1850/28-1). In Mexico, this work has been supported by CONACyT Grant 83564 and UNAM/DGAPA PAPIIT Grant IN110209. This work is also based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under program ID 175.A-0839. NR 136 TC 97 Z9 97 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2012 VL 201 IS 2 AR 30 DI 10.1088/0067-0049/201/2/30 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016YN UT WOS:000309555900023 ER PT J AU Di Stefano, R AF Di Stefano, Rosanne TI SHORT-DURATION LENSING EVENTS. II. EXPECTATIONS AND PROTOCOLS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Galaxy: general; gravitational lensing: micro; planets and satellites: detection; surveys ID GRAVITATIONAL MICROLENSING EVENT; PLANETARY SYSTEMS; FIELD; MASS; MACHO-LMC-5; STAR; DISCOVERY; CHANNEL; OBJECTS; KEPLER AB Ongoing microlensing observations by OGLE and MOA regularly identify lensing events with Einstein diameter crossing time, tau(E), of 16 or fewer days. Events with estimated values of tau(E) of one to two days have been detected. Short-duration events tend to be generated by low-mass lenses or by lenses with high transverse velocities. We compute the expected rates, demonstrate the expected ranges of parameters for lenses of different mass, and develop a protocol for observing and modeling short-duration events. Relatively minor additions to the procedures presently used will increase the rate of planet discovery, and also discover or place limits on the population of high-speed dim stars and stellar remnants in the vicinity of the Sun. 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]; Smithsonian endowment FX This work benefited from discussions with Charles Alcock, Erin Arai, Mary Davies, Nitya Kallivayalil, M. J. Lehner, Christopher Night, Brandon Patel, Frank Primini, Pavlos Protopapas, Rohini Shivamoggi, Kailash Sahu, and Takahiro Sumi. Sam McCandlish provided the statistics of short-duration events in the OGLE and MOA data. I would also like to thank the anonymous referee for useful comments. The research was conducted under the aegis of NSF grants AST-0708924 and AST-0908878, and a grant from the Smithsonian endowment. I thank the Aspen Center for Physics for its hospitality during the early phases of this work. NR 31 TC 3 Z9 3 U1 0 U2 2 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 AUG PY 2012 VL 201 IS 2 AR 21 DI 10.1088/0067-0049/201/2/21 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016YN UT WOS:000309555900014 ER PT J AU Di Stefano, R AF Di Stefano, Rosanne TI SHORT-DURATION LENSING EVENTS. I. WIDE-ORBIT PLANETS? FREE-FLOATING LOW-MASS OBJECTS? OR HIGH-VELOCITY STARS? SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE Galaxy: general; gravitational lensing: micro; planets and satellites: detection; surveys ID GRAVITATIONAL MICROLENSING EVENTS; HYPERVELOCITY STARS; BROWN DWARFS; MILKY-WAY; SYSTEMS; MACHO-LMC-5; ASTROMETRY; CHANNEL; ORIGIN; LIGHT AB Short-duration lensing events tend to be generated by low-mass lenses or by lenses with high transverse velocities. Furthermore, for any given lens mass and speed, events of short duration are preferentially caused by nearby lenses (mesolenses) that can be studied in detail, or else by lenses so close to the source star that finite-source-size effects may be detected, yielding information about both the Einstein ring radius and the surface of the lensed star. Planets causing short-duration events may be in orbits with any orientation, and may have semimajor axes smaller than 1 AU, or they may reach the outer limits of their planetary systems, in the region corresponding to the solar system's Oort Cloud. They can have masses larger than Jupiter's or smaller than Pluto's. Lensing therefore has a unique potential to expand our understanding of planetary systems. A particular advantage of lensing is that it can provide precision measurements of system parameters, including the masses of and projected separation between star and planet. We demonstrate how the parameters can be extracted and show that a great deal can be learned. For example, it is remarkable that the gravitational mass of nearby free-floating planet-mass lenses can be measured by complementing observations of a photometric event with deep images that detect the planet itself. A fraction of short events may be caused by high-velocity stars located within a kiloparsec. Many high-velocity lenses are likely to be neutron stars that received large natal kicks. Other high-speed stars may be members of the halo population. Still others may be hypervelocity stars that have been ejected from the Galactic center, or runaway stars escaped from close binaries, possibly including the progenitor binaries of Type Ia supernovae. 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]; Smithsonian endowment FX This work benefited from discussions with Charles Alcock, Erin Arai, Mary Davies, Nitya Kallivayalil, M. J. Lehner, Christopher Night, Brandon Patel, Frank Primini, Pavlos Protopapas, Rohini Shivamoggi, Kailash Sahu, and Takahiro Sumi. The research was conducted under the aegis of NSF grants AST-0708924 and AST-0908878, and a grant from the Smithsonian endowment. I thank the Aspen Center for Physics for its hospitality during the early phases of this work. NR 51 TC 5 Z9 5 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 AUG PY 2012 VL 201 IS 2 AR 20 DI 10.1088/0067-0049/201/2/20 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016YN UT WOS:000309555900013 ER PT J AU Dupuy, TJ Liu, MC AF Dupuy, Trent J. Liu, Michael C. TI THE HAWAII INFRARED PARALLAX PROGRAM. I. ULTRACOOL BINARIES AND THE L/T TRANSITION SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE astrometry; brown dwarfs; infrared: stars; parallaxes; proper motions; stars: low-mass ID HUBBLE-SPACE-TELESCOPE; DIGITAL SKY SURVEY; STAR ADAPTIVE OPTICS; LOW-MASS STARS; BROWN DWARF COMPANION; HIGH PROPER MOTION; FINDING CAMPAIGN DISCOVERY; SURVEY COMMISSIONING DATA; TW-HYDRAE-ASSOCIATION; PLANETARY CAMERA 2 AB We present the first results from our high-precision infrared (IR) astrometry program at the Canada-France-Hawaii Telescope. We measure parallaxes for 83 ultracool dwarfs (spectral types M6-T9) in 49 systems, with a median uncertainty of 1.1 mas (2.3%) and as good as 0.7 mas (0.8%). We provide the first parallaxes for 48 objects in 29 systems, and for another 27 objects in 17 systems, we significantly improve upon published results, with a median (best) improvement of 1.7 times (5 times). Three systems show astrometric perturbations indicative of orbital motion; two are known binaries (2MASS J0518-2828AB and 2MASS J1404-3159AB) and one is spectrally peculiar (SDSS J0805+4812). In addition, we present here a large set of Keck adaptive optics imaging that more than triples the number of binaries with L6-T5 components that have both multi-band photometry and distances. Our data enable an unprecedented look at the photometric properties of brown dwarfs as they cool through the L/T transition. Going from approximate to L8 to approximate to T4.5, flux in the Y and J bands increases by approximate to 0.7 mag and approximate to 0.5 mag, respectively (the Y- and J-band "bumps"), while flux in the H, K, and L' bands declines monotonically. This wavelength dependence is consistent with cloud clearing over a narrow range of temperature, since condensate opacity is expected to dominate at 1.0-1.3 mu m. Interestingly, despite more than doubling the near-IR census of L/T transition objects, we find a conspicuous paucity of objects on the color-magnitude diagram just blueward of the late-L/early-T sequence. This "L/T gap" occurs at (J - H)(MKO) = 0.1-0.3 mag, (J - K)(MKO) = 0.0-0.4 mag, and implies that the last phases of cloud evolution occur rapidly. Finally, we provide a comprehensive update to the absolute magnitudes of ultracool dwarfs as a function of spectral type using a combined sample of 314 objects. C1 [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dupuy, Trent J.; 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; National Aeronautics and Space Administration [NAS 5-26555]; NSF [AST-0507833, AST-0909222]; Alfred P. Sloan Research Fellowship; Hubble Fellowship [HST-HF-51271.01-A]; Space Telescope Science Institute FX Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation.; We are deeply indebted to the CFHT staff for their constant observing support and dedication to delivering the highest quality data products, and in particular to Loic Albert. We also thank Brendan P. Bowler, Kimberly Aller, and Mark Pitts for assistance in conducting our IRTF/SpeX observations. We are grateful to S. K. Leggett and Michael J. Ireland for suggestions that significantly improved our analysis. We have benefited from discussions with Jan Kleyna, Gene Magnier, Dave Monet, John Thorstenen, Chris Tinney, John Tonry, and Fred Vrba about astrometry and parallaxes. We are grateful to Celine Reyle for customized Besancon Galaxy models. It is a pleasure to thank Joel Aycock, Randy Campbell, Al Conrad, Heather Hershley, Jim Lyke, Jason McIlroy, Gary Punawai, Julie Riviera, Hien Tran, Cynthia Wilburn, and the Keck Observatory staff for assistance with the Keck observations. Our research has employed the 2MASS data products; NASA's Astrophysical Data System; the SIMBAD database operated at CDS, Strasbourg, France; and the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication has made use of a contour plotting code written by James R. A. Davenport. T. J. D. and M. C. L. acknowledge support for this work from NSF grants AST-0507833 and AST-0909222. M. C. L. acknowledges support from an Alfred P. Sloan Research Fellowship. 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 306 TC 189 Z9 190 U1 0 U2 6 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 AUG PY 2012 VL 201 IS 2 AR 19 DI 10.1088/0067-0049/201/2/19 PG 84 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016YN UT WOS:000309555900012 ER PT J AU Howard, AW Marcy, GW Bryson, ST Jenkins, JM Rowe, JF Batalha, NM Borucki, WJ Koch, DG Dunham, EW Gautier, TN Van Cleve, J Cochran, WD Latham, DW Lissauer, JJ Torres, G Brown, TM Gilliland, RL Buchhave, LA Caldwell, DA Christensen-Dalsgaard, J Ciardi, D Fressin, F Haas, MR Howell, SB Kjeldsen, H Seager, S Rogers, L Sasselov, DD Steffen, JH Basri, GS Charbonneau, D Christiansen, J Clarke, B Dupree, A Fabrycky, DC Fischer, DA Ford, EB Fortney, JJ Tarter, J Girouard, FR Holman, MJ Johnson, JA Klaus, TC Machalek, P Moorhead, AV Morehead, RC Ragozzine, D Tenenbaum, P Twicken, JD Quinn, SN Isaacson, H Shporer, A Lucas, PW Walkowicz, LM Welsh, WF Boss, A Devore, E Gould, A Smith, JC Morris, RL Prsa, A Morton, TD Still, M Thompson, SE Mullally, F Endl, M MacQueen, PJ AF Howard, Andrew W. Marcy, Geoffrey W. Bryson, Stephen T. Jenkins, Jon M. Rowe, Jason F. Batalha, Natalie M. Borucki, William J. Koch, David G. Dunham, Edward W. Gautier, Thomas N., III Van Cleve, Jeffrey Cochran, William D. Latham, David W. Lissauer, Jack J. Torres, Guillermo Brown, Timothy M. Gilliland, Ronald L. Buchhave, Lars A. Caldwell, Douglas A. Christensen-Dalsgaard, Jorgen Ciardi, David Fressin, Francois Haas, Michael R. Howell, Steve B. Kjeldsen, Hans Seager, Sara Rogers, Leslie Sasselov, Dimitar D. Steffen, Jason H. Basri, Gibor S. Charbonneau, David Christiansen, Jessie Clarke, Bruce Dupree, Andrea Fabrycky, Daniel C. Fischer, Debra A. Ford, Eric B. Fortney, Jonathan J. Tarter, Jill Girouard, Forrest R. Holman, Matthew J. Johnson, John Asher Klaus, Todd C. Machalek, Pavel Moorhead, Althea V. Morehead, Robert C. Ragozzine, Darin Tenenbaum, Peter Twicken, Joseph D. Quinn, Samuel N. Isaacson, Howard Shporer, Avi Lucas, Philip W. Walkowicz, Lucianne M. Welsh, William F. Boss, Alan Devore, Edna Gould, Alan Smith, Jeffrey C. Morris, Robert L. Prsa, Andrej Morton, Timothy D. Still, Martin Thompson, Susan E. Mullally, Fergal Endl, Michael MacQueen, Phillip J. TI PLANET OCCURRENCE WITHIN 0.25 AU OF SOLAR-TYPE STARS FROM KEPLER SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE planetary systems; stars: statistics; techniques: photometric ID NEPTUNE-MASS PLANET; SUPER-EARTH; EXTRASOLAR PLANETS; HOT JUPITERS; DETERMINISTIC MODEL; TRANSITING PLANET; LOW-DENSITY; RADIUS RELATIONSHIPS; TERRESTRIAL PLANETS; SOLID EXOPLANETS AB We report the distribution of planets as a function of planet radius, orbital period, and stellar effective temperature for orbital periods less than 50 days around solar-type (GK) stars. These results are based on the 1235 planets (formally "planet candidates") from the Kepler mission that include a nearly complete set of detected planets as small as 2 R-circle plus. For each of the 156,000 target stars, we assess the detectability of planets as a function of planet radius, R-p, and orbital period, P, using a measure of the detection efficiency for each star. We also correct for the geometric probability of transit, R-star/a. We consider first Kepler target stars within the "solar subset" having T-eff = 4100-6100 K, log g = 4.0-4.9, and Kepler magnitude Kp < 15 mag, i.e., bright, main-sequence GK stars. We include only those stars having photometric noise low enough to permit detection of planets down to 2 R-circle plus. We count planets in small domains of R-p and P and divide by the included target stars to calculate planet occurrence in each domain. The resulting occurrence of planets varies by more than three orders of magnitude in the radius-orbital period plane and increases substantially down to the smallest radius (2 R-circle plus) and out to the longest orbital period (50 days, similar to 0.25 AU) in our study. For P < 50 days, the distribution of planet radii is given by a power law, df/d log R = k(R)R(alpha) with k(R) = 2.9(-0.4)(+0.5), alpha = -1.92 +/- 0.11, and R equivalent to R-p/R-circle plus. This rapid increase in planet occurrence with decreasing planet size agrees with the prediction of core-accretion formation but disagrees with population synthesis models that predict a desert at super-Earth and Neptune sizes for close-in orbits. Planets with orbital periods shorter than 2 days are extremely rare; for R-p > 2 R-circle plus we measure an occurrence of less than 0.001 planets per star. For all planets with orbital periods less than 50 days, we measure occurrence of 0.130 +/- 0.008, 0.023 +/- 0.003, and 0.013 +/- 0.002 planets per star for planets with radii 2-4, 4-8, and 8-32 R-circle plus, in agreement with Doppler surveys. We fit occurrence as a function of P to a power-law model with an exponential cutoff below a critical period P-0. For smaller planets, P-0 has larger values, suggesting that the "parking distance" for migrating planets moves outward with decreasing planet size. We also measured planet occurrence over a broader stellar T-eff range of 3600-7100 K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R-circle plus planets in the Kepler field increases with decreasing T-eff, with these small planets being seven times more abundant around cool stars (3600-4100 K) than the hottest stars in our sample (6600-7100 K). C1 [Howard, Andrew W.; Marcy, Geoffrey W.; Basri, Gibor S.; Isaacson, Howard; Walkowicz, Lucianne M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Jenkins, Jon M.; Van Cleve, Jeffrey; Caldwell, Douglas A.; Tarter, Jill; Machalek, Pavel; Tenenbaum, Peter; Twicken, Joseph D.; Devore, Edna; Smith, Jeffrey C.; Morris, Robert L.; Thompson, Susan E.; Mullally, Fergal] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Cochran, William D.; Endl, Michael; MacQueen, Phillip J.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Latham, David W.; Torres, Guillermo; Fressin, Francois; Sasselov, Dimitar D.; Charbonneau, David; Dupree, Andrea; Holman, Matthew J.; Ragozzine, Darin; Quinn, Samuel N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Timothy M.; Shporer, Avi] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-1168 Copenhagen, Denmark. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Christensen-Dalsgaard, Jorgen] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Ciardi, David] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Seager, Sara; Rogers, Leslie] MIT, Dept Earth Atmospher & Planetary Sci, Dept Phys, Cambridge, MA 02139 USA. [Steffen, Jason H.] Fermilab Ctr Particle Astrophys, Batavia, IL 60510 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06510 USA. [Ford, Eric B.; Moorhead, Althea V.; Morehead, Robert C.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Girouard, Forrest R.; Klaus, Todd C.; Morton, Timothy D.] NASA, Orbital Sci Corp, Ames Res Ctr, Moffett Field, CA 94035 USA. [Johnson, John Asher] CALTECH, Dept Astrophys, Pasadena, CA 91109 USA. [Shporer, Avi] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Lucas, Philip W.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Boss, Alan] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC 20015 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Prsa, Andrej] Villanova Univ, Dept Astron & Astrophys, Villanova, PA 19085 USA. [Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. RP Howard, AW (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM howard@astro.berkeley.edu RI Ragozzine, Darin/C-4926-2013; Caldwell, Douglas/L-7911-2014; Howard, Andrew/D-4148-2015; OI Caldwell, Douglas/0000-0003-1963-9616; Howard, Andrew/0000-0001-8638-0320; Fortney, Jonathan/0000-0002-9843-4354; Buchhave, Lars A./0000-0003-1605-5666; Ciardi, David/0000-0002-5741-3047; /0000-0001-6545-639X; Fischer, Debra/0000-0003-2221-0861; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA [NNX06AH52G]; National Center for Atmospheric Research; National Science Foundation; NASA's Science Mission Directorate FX We thank E. Chiang and H. Knutson for helpful conversations. We gratefully acknowledge D. Monet and many other members of the Kepler team. We thank the W. M. Keck Observatory, and both NASA and the University of California for the use of the Keck telescope. We are grateful to the Keck technical staff, especially S. Dahm, H. Tran, and G. Hill for the support of Keck instrumentation, and R. Kibrick, G. Wirth, R. Goodrich for the support of remote observing. We extend special thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. G. M. acknowledges NASA grant NNX06AH52G. J.C.-D. acknowledges support from the National Center for Atmospheric Research, which is sponsored by the National Science Foundation. Funding for the Kepler Discovery mission is provided by NASA's Science Mission Directorate. NR 107 TC 362 Z9 363 U1 5 U2 32 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 AUG PY 2012 VL 201 IS 2 AR 15 DI 10.1088/0067-0049/201/2/15 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 016YN UT WOS:000309555900008 ER PT J AU Isler, ML Cuervo, AM Bravo, GA Brumfield, RT AF Isler, Morton L. Cuervo, Andres M. Bravo, Gustavo A. Brumfield, Robb T. TI AN INTEGRATIVE APPROACH TO SPECIES-LEVEL SYSTEMATICS REVEALS THE DEPTH OF DIVERSIFICATION IN AN ANDEAN THAMNOPHILID, THE LONG-TAILED ANTBIRD SO CONDOR LA English DT Article DE Andes; Drymophila caudata; museum specimens; niche divergence; species delimitation; phylogeography; suboscines; vocalizations ID GEOGRAPHIC-VARIATION; CYTOCHROME-B; MIXED MODELS; AVES; CONSERVATISM; DELIMITATION; BIOLOGY; LIMITS; BIRDS; DIFFERENTIATION AB The geographic range of the Long-tailed Antbird (Drymophila caudata) extends from the Paria Mountains of Venezuela south through the Andes to northern Bolivia, a geographic and elevational distribution unique in the antbirds (Thamnophilidae). Plumage variation among most populations is not obvious, and although eight subspecies have been described, half have been synonymized. We took a multidimensional approach to reexamining the taxonomy of the complex. We identified lineages by evaluating divergence in mtDNA, and defined study groups within them to take into account previously described plumage differences. We then assessed the taxonomic status of principal lineages and study groups by comparing vocal differences among them to established taxonomic "yardsticks" for thamnophilid antbirds. Finally, we related taxa to the ecology of the regions in which they occur. The outcomes revealed substantial diversification, sufficient for recognition of four species, three restricted to the north and one widespread along the main body of the Andes extending from northwestern Colombia south to Bolivia. Speciation in Andean Drymophila antbirds is partially associated with elevational and environmental divergence. The results provide valuable inputs to mapping and understanding avian evolution in the Andes and demonstrate the value of a multifaceted approach in solving taxonomic problems. C1 [Isler, Morton L.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Cuervo, Andres M.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Cuervo, Andres M.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. RP Isler, ML (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC-116,POB 37012, Washington, DC 20013 USA. EM antbird@cox.net OI Brumfield, Robb/0000-0003-2307-0688 FU Louisiana State University's Museum of Natural Science (LSUMZ); Lewis and Clark Exploration Fund; Society of Systematic Biologists; Society of Integrative and Comparative Biology; F. M. Chapman Memorial Fund; American Ornithologists' Union; Wilson Ornithological Society; Idea Wild; National Science Foundation DDIG [DEB-0910285, DEB-1011435] FX We thank the following individuals who provided access to their skin and tissue collections or photographs of specimens: N. Rice (Academy of Natural Sciences of Philadelphia; ANSP), C. D. Cadena (Museo de Historia Natural, Universidad de los Andes; ANDES-BT), J. Perez-Eman and J. Miranda (Coleccion Ornitologica Phelps; COP), J. Bates and D. Willard (Field Museum of Natural History; FMNH), F. G. Stiles and J. P. Lopez (Instituto de Ciencias Naturales, Universidad Nacional de Colombia; ICN), C. A. Medina, S. Sierra, and D. Lopez (Instituto Alexander von Humboldt; IAvH), G. Lenglet (Institut Royal des Sciences Naturelles de Belgique; IRNS), M. Robbins (University of Kansas Natural History Museum; KU), J. Trimble and S. V. Edwards (Museum of Comparative Zoology, Harvard University; MZC), and H. van Grouw (Natural History Museum at Tring; BMNH). The support of J. V. Remsen and D. Dittmann at Louisiana State University's Museum of Natural Science (LSUMZ) was essential. We thank the recordists credited in the Appendix 2 (online) and collectors of specimens for providing essential material for this study. For providing archival recordings and distributional data, we appreciate the efforts of V. Caro and P. Caycedo (Banco de Sonidos Animales), G. F. Budney and M. D. Medler (Macaulay Library), J. J. Calderon and R. Fernandez (Universidad de Narino), and R. Planque and W.-P. Vellinga (Xeno-Canto). Two anonymous reviewers and editors M. A. Patten and P. Unitt provided a number of suggestions that greatly improved the manuscript. We are indebted to P. Isler for preparing the spectrograms, M. Lentino for locating literature, and F. G. Stiles for assisting with the characterization of plumage variation in Colombian specimens. S. Herzog helped with translation of the original description of D. c. klagesi. For field and laboratory support we thank J. E. Avendano, J. P. Lopez, O. Marin, J. Botero, and, especially, N. Aristizabal, N. Gutierrez-Pinto, M. Alvarez-Rebolledo, and J. Miranda. This study was partially funded by the Lewis and Clark Exploration Fund, Society of Systematic Biologists, Society of Integrative and Comparative Biology, F. M. Chapman Memorial Fund, American Ornithologists' Union, Wilson Ornithological Society, Idea Wild, and by National Science Foundation DDIG grants DEB-0910285 and DEB-1011435. We are grateful to the national authorities for supporting our research. NR 54 TC 11 Z9 13 U1 0 U2 14 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 AUG PY 2012 VL 114 IS 3 BP 571 EP 583 DI 10.1525/cond.2012.120012 PG 13 WC Ornithology SC Zoology GA 998ZN UT WOS:000308279000015 ER PT J AU Cleal, CJ Uhl, D Cascales-Minana, B Thomas, BA Bashforth, AR King, SC Zodrow, EL AF Cleal, C. J. Uhl, D. Cascales-Minana, B. Thomas, B. A. Bashforth, A. R. King, S. C. Zodrow, E. L. TI Plant biodiversity changes in Carboniferous tropical wetlands SO EARTH-SCIENCE REVIEWS LA English DT Article DE Pennsylvanian; Palaeotropical; Vegetation; Palaeoecology; Palaeoclimates ID PHANEROZOIC TAXONOMIC DIVERSITY; UPPER SILESIAN BASIN; SEA-LEVEL CHANGES; FOSSIL RECORD; NOVA-SCOTIA; SOUTH-WALES; VARISCAN EURAMERICA; SPECIES RICHNESS; WESTPHALIAN-D; MASS EXTINCTIONS AB Using a combination of species richness, polycohort and constrained cluster analyses, the plant biodiversity of Pennsylvanian (late Carboniferous) tropical wetlands ("coal swamps") has been investigated in five areas in Western Europe and eastern North America: South Wales, Pennines, Ruhr, Saarland and Sydney coal basins. In all cases, species richness expansion followed an essentially logistic curve typical of that associated with ecologically closed habitats, with niche saturation being achieved in about three million years. The resulting steady-state ("climax") coal swamp vegetation had a local-scale (within an area of c. 0.1 ha) species diversity in South Wales of 16 +/- 7 and Simpson Diversity Indices of 4.53 +/- 2.55, which are very similar to values obtained from studies on North American coal swamp vegetation. landscape diversity (within an area 10(5) km(2)) varied between 50 and 100 species in the lower to middle Westphalian Stage, falling to about 40-50 species in the upper Westphalian Stage. Regional-scale diversity (within an area > 10(5) km(2)) is difficult to estimate but was at least 120 species. Species turn-over was typically very low, at about 4 species per million years, but there were a number of intervals of more rapid species turn-over in the early Langsettian, late Duckmantian, early Bolsovian and middle Asturian times, which are recognised today as biozonal boundaries. The swamps were mostly subject to ecological stasis during early and middle Westphalian times, although they contracted locally in response to drying of substrates. Later in Westphalian times, however, the swamps were subject to regional-scale changes in composition and aerial extent, probably in response to climate change. The coal swamps had a much lower species diversity compared to modern-day tropical rain forests. (C) 2012 Elsevier B.V. All rights reserved. C1 [Cleal, C. J.] Natl Museum Wales, Dept Biodivers & Systemat Biol, Cardiff CF10 3NP, S Glam, Wales. [Uhl, D.] Senckenberg Forschungsinst, D-60325 Frankfurt, Germany. [Uhl, D.] Nat Museum Frankfurt, D-60325 Frankfurt, Germany. [Cascales-Minana, B.] Univ Zaragoza, Dept Earth Sci, E-50009 Zaragoza, Spain. [Thomas, B. A.] Aberystwyth Uni, Inst Biol Environm & Rural Sci, Aberystwyth SY23 1NL, Dyfed, Wales. [Bashforth, A. R.] Univ Copenhagen, Nat Hist Museum Denmark, Geol Museum, DK-1350 Copenhagen K, Denmark. [Bashforth, A. R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [King, S. C.] Univ Birmingham, Sch Geog Earth & Environm Sci, Birmingham B15 2TT, W Midlands, England. [Zodrow, E. L.] Cape Breton Univ, Palaeobotan Lab, Sydney, NS B1P 612, Canada. RP Cleal, CJ (reprint author), Natl Museum Wales, Dept Biodivers & Systemat Biol, Cathays Pk, Cardiff CF10 3NP, S Glam, Wales. EM chris.cleal@museumwales.ac.uk; Dieter.Uhl@senckenberg.de; borja.cascales@unizar.es; bat@aber.ac.uk; bashfortha@si.edu; s.c.king@bham.ac.uk; erwin_zodrow@cbu.ca RI Bashforth, Arden/H-6057-2013; OI Bashforth, Arden/0000-0003-3050-7032; Cleal, Christopher/0000-0002-8750-6228 FU UNESCO; IUGS; Izaak Walton Killam Predoctoral Scholarship; NSERC; European Union [DK-TAF-1207] FX The results summarised in this paper are partly the outcome of IGCP 469 Variscan terrestrial biotas and palaeoenvironments and IGCP 575 Pennsylvanian terrestrial habitats and biotas of southeastern Euramerica, and the support of UNESCO and IUGS for this project is acknowledged. The authors also recognise the support and helpful discussions with other members of the project, notably Stanislav Oplustil (Charles University, Prague), Joseph Psenicka (West Bohemian Museum, Pilsen) and Yanaki Tenchov (Geological Institute, Sofia). Some of the data from the Sydney Coalfield, Nova Scotia was the result of collaboration between three of the authors (ARB, ELZ and CJC) who are grateful for support from an Izaak Walton Killam Predoctoral Scholarship, an NSERC Discovery Grant to Martin Gibling (Dalhousie University, Halifax), and a European Union-funded SYNTHESYS Grant (DK-TAF-1207, Geological Museum, Copenhagen). NR 300 TC 17 Z9 17 U1 2 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-8252 J9 EARTH-SCI REV JI Earth-Sci. Rev. PD AUG PY 2012 VL 114 IS 1-2 BP 124 EP 155 DI 10.1016/j.earscirev.2012.05.004 PG 32 WC Geosciences, Multidisciplinary SC Geology GA 998YR UT WOS:000308276800007 ER PT J AU Boyle, SA Zartman, CE Spironello, WR Smith, AT AF Boyle, Sarah A. Zartman, Charles E. Spironello, Wilson R. Smith, Andrew T. TI Implications of habitat fragmentation on the diet of bearded saki monkeys in central Amazonian forest SO JOURNAL OF MAMMALOGY LA English DT Article DE Brazil; Chiropotes; forest fragment; frugivore; primate; seed predator ID TROPICAL RAIN-FOREST; CHIROPOTES-SATANAS-CHIROPOTES; EASTERN BRAZILIAN AMAZONIA; FEEDING ECOLOGY; NEOTROPICAL PRIMATES; ALOUATTA-SENICULUS; ATELES-GEOFFROYI; NATIONAL-PARK; LOS-TUXTLAS; CONSERVATION AB Forest fragmentation demonstrably alters plant species composition, distribution, and diversity, and, in turn, may affect the availability of food resources for primary consumers. We investigated to what extent fragmentation affected the diets of 6 groups of bearded saki monkeys (Chiropotes chiropotes) living in two 10-ha fragments, two 100-ha "fragments" that were no longer fully isolated, and 2 areas of continuous forest in central Amazonia. When changes occurred we tested whether differences in diet were due to plant species availability by comparing the prevalence of consumed items against their relative abundance at the 6 sites. En total, the monkeys consumed fruits, seeds, flowers, and leaves of 244 plant species, of which less than 2% were shared among all 6 groups. Although there was a positive correlation between relative abundance of diet species and consumption frequency, monkeys did not eat all available potential resources, and groups inhabiting the 10-ha fragments consumed items that were ignored in larger forested areas. Our findings suggest that bearded sakis living in small forest fragments are limited in their dietary choices as a consequence of the reduced number of plant species present, and therefore consume species that monkeys inhabiting continuous forests typically can ignore. We conclude that the ability to consume a diverse diet that includes seeds and unripe fruit helps this species survive in forest fragments, but it appears that these conditions are unviable unless connectivity increases among the forest fragments and continuous forest in the landscape. C1 [Boyle, Sarah A.] Rhodes Coll, Dept Biol, Memphis, TN 38112 USA. [Boyle, Sarah A.] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Boyle, Sarah A.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Boyle, Sarah A.; Smith, Andrew T.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Zartman, Charles E.] Natl Inst Amazonian Res INPA, Dept Bot, BR-69011970 Manaus, Amazonas, Brazil. RP Boyle, SA (reprint author), Rhodes Coll, Dept Biol, 2000 N Pkwy, Memphis, TN 38112 USA. EM sarahannboyle@gmail.com FU Conselho Nacional de Desenvolvimento Cientifico e Technologic; Instituto Nacional de Pesquisas da Amazonia; Biological Dynamics of Forest Fragments Project; Smithsonian Tropical Research Institute FX We thank the Conselho Nacional de Desenvolvimento Cientifico e Technologic for permission to conduct this research, and the Instituto Nacional de Pesquisas da Amazonia, the Biological Dynamics of Forest Fragments Project, and the Smithsonian Tropical Research Institute for logistical and financial assistance. Fulbright U.S. Student Program, Margot Marsh Biodiversity Foundation, Primate Conservation, Inc., Organization for Tropical Studies, American Society of Primatologists, and Arizona State University provided funding to SAB. We thank A. M. dos Reis, O. F. da Silva, W. C. Lourenco, and L. R. da Silva for field assistance; P. Ribero for assistance with plant identification; and W. L. Laurance and A. Andrade for use of the tree database. Two reviewers and R. Jabaily provided feedback that improved the manuscript. This is publication 596 in the BDFFP/INPA-STRI technical series. NR 77 TC 11 Z9 11 U1 6 U2 46 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 AUG PY 2012 VL 93 IS 4 BP 959 EP 976 DI 10.1644/11-MAMM-A-286.1 PG 18 WC Zoology SC Zoology GA 009GN UT WOS:000309014200007 ER PT J AU Bravo, A Harms, KE Emmons, LH AF Bravo, Adriana Harms, Kyle E. Emmons, Louise H. TI Keystone resource (Ficus) chemistry explains lick visitation by frugivorous bats SO JOURNAL OF MAMMALOGY LA English DT Article DE Amazonia; bats; Carolliinae; figs; limiting resources; mineral licks; sodium; Stenodermatinae ID TAILED FRUIT BATS; PERUVIAN AMAZON; CAROLLIA-PERSPICILLATA; SOIL CHARACTERISTICS; SOUTHEASTERN PERU; AVIAN GEOPHAGY; PHYLLOSTOMIDAE; NITROGEN; MAMMALS; FIG AB Geophagy is a widespread behavior among plant-eating animals. In the Neotropics, mineral licks are activity hot spots for frugivorous bats (Stenodermatinae). Bats drink mineral-rich water accumulated in soil depressions made by geophagous mammals. Two mechanistic hypotheses have been proposed to explain this behavior: licks are reliable sources of limiting nutrients, especially sodium; and licks provide substances that render dietary toxins less harmful. We assessed the former by examining bats' diets in conjunction with lick chemistry in the Peruvian Amazon. We found that most bats that visit licks belong to the subfamily Stenodermatinae and are specialists on Ficus fruits-a keystone resource. In addition, although Ficus fruits are good sources of some minerals, their sodium content is limited in relation to the physiological requirement of a small mammal. In contrast, bats of the subfamily Carolliinae supplement their fruit diets with insects, potential sources of sodium. Complementary results among diets, Ficus chemistry, and lick-water chemistry strongly support the sodium-limitation hypothesis for bat lick use and suggest a mechanistic link between bats and ecosystem engineers that make soil-borne resources available. Because sodium is an essential nutrient for vertebrates and Ficus is a keystone resource for many animal species, our results may have implications for the community of frugivorous vertebrates in areas where sodium is limited. Licks may play a critical role as sodium sources and thus they should be considered as important conservation targets. C1 [Bravo, Adriana; Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Harms, Kyle E.] Smithsonian Trop Res Inst, Balboa, Panama. [Emmons, Louise H.] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. RP Bravo, A (reprint author), Amer Museum Nat Hist, Ctr Biodivers & Conservat, Cent Pk W & 79th St, New York, NY 10024 USA. EM abravo@amnh.org FU Peruvian Institute of Natural Resources (INRENA) [070-2005-INRENA-IFFS-DCB, 080-2007-INRENA-IFFS-DCB, 007-2008-INRENA-IFFS-DCB]; Amazon Conservation Association; American Society of Mammalogists; Bat Conservation International; Graduate Student Association-Biograds of Louisiana State University; Idea Wild; Louisiana Office of Environmental Education; Louisiana State University Graduate School; Rufford Small Grants; United States National Science Foundation FX We thank the Peruvian Institute of Natural Resources (INRENA) for providing research permits 070-2005-INRENA-IFFS-DCB, 080-2007-INRENA-IFFS-DCB, and 007-2008-INRENA-IFFS-DCB to conduct this study. For help in the field we thank the Asociacion para la Conservacion de la Cuenca Amazonica rangers, Y. Arteaga, M. Bravo, F. Carrasco, S. Claramunt, F. Cornejo, M. Cruz, Z. Ordonez, A. L. Rodales, M. Rodriguez, and W. Torres. We also thank N. Pitman, J. Ramos, and K. Salas for help with logistics. We are grateful to S. Claramunt, J. Eberhard, S. Galeano, F. Galvez, M. Gavilanez, M. Hafner, L. Hooper-Bui, J. Myers, V. Remsen, R. Stevens, and P. Stouffer for their insightful comments on this study and the manuscript. Financial support was provided by the Amazon Conservation Association (graduate student grant and seed grant award), American Society of Mammalogists, Bat Conservation International, Graduate Student Association-Biograds of Louisiana State University, Idea Wild, Louisiana Office of Environmental Education, Louisiana State University Graduate School, Rufford Small Grants, and the United States National Science Foundation (to KEH). NR 60 TC 3 Z9 3 U1 1 U2 39 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 AUG PY 2012 VL 93 IS 4 BP 1099 EP 1109 DI 10.1644/11-MAMM-A-333.1 PG 11 WC Zoology SC Zoology GA 009GN UT WOS:000309014200019 ER PT J AU Delaney, M AF Delaney, Michelle TI Peace Medals: Negotiating Power in Early America SO PUBLIC HISTORIAN LA English DT Book Review C1 [Delaney, Michelle] Smithsonian Inst, Washington, DC 20560 USA. RP Delaney, M (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 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 AUG PY 2012 VL 34 IS 3 BP 86 EP 87 PG 2 WC History SC History GA 010IM UT WOS:000309088100008 ER PT J AU Higgins, MA Asner, GP Perez, E Elespuru, N Tuomisto, H Ruokolainen, K Alonso, A AF Higgins, Mark A. Asner, Gregory P. Perez, Eneas Elespuru, Nydia Tuomisto, Hanna Ruokolainen, Kalle Alonso, Alfonso TI Use of Landsat and SRTM Data to Detect Broad-Scale Biodiversity Patterns in Northwestern Amazonia SO REMOTE SENSING LA English DT Article DE Amazonia; Landsat; SRTM; floristic composition; geology; soils; pteridophytes; vegetation mapping; NDVI ID RAIN-FOREST VEGETATION; ENVIRONMENTAL-CONTROL; FLORISTIC PATTERNS; SATELLITE IMAGERY; WESTERN AMAZONIA; TREES; BASIN; PERU; MELASTOMATACEAE; PTERIDOPHYTES AB Vegetation maps are the starting point for the design of protected areas and regional conservation plans. Accurate vegetation maps are missing for much of Amazonia, preventing the development of effective and compelling conservation strategies. Here we used a network of 160 inventories across northwestern Amazonia to evaluate the use of Landsat and Shuttle Radar Topography Mission (SRTM) data to identify floristic and edaphic patterns in Amazonian forests. We first calculated the strength of the relationship between these remotely-sensed data, and edaphic and floristic patterns in these forests, and asked how sensitive these results are to image processing and enhancement. We additionally asked if SRTM data can be used to model patterns in plant species composition in our study areas. We find that variations in Landsat and SRTM data are strongly correlated with variations in soils and plant species composition, and that these patterns can be mapped solely on the basis of SRTM data over limited areas. Using these data, we furthermore identified widespread patch-matrix floristic patterns across northwestern Amazonia, with implications for conservation planning and study. Our findings provide further evidence that Landsat and SRTM data can provide a cost-effective means for mapping these forests, and we recommend that maps generated from a combination of remotely-sensed and field data be used as the basis for conservation prioritization and planning in these vast and remote forests. C1 [Higgins, Mark A.; Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Perez, Eneas; Elespuru, Nydia] Univ Nacl Amazonia Peruana, Fac Ciencias Biol, Iquitos, Peru. [Tuomisto, Hanna; Ruokolainen, Kalle] Univ Turku, Dept Biol, FI-20100 Turku, Finland. [Tuomisto, Hanna; Ruokolainen, Kalle] Smithsonian Conservat Biol Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. RP Higgins, MA (reprint author), Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. EM higginsm@stanford.edu; gpa@stanford.edu; eneasperez@yahoo.com; nydia_valeria@hotmail.com; hanna.tuomisto@utu.fi; kalle.ruokolainen@utu.fi; alonsoa@si.edu RI Tuomisto, Hanna/G-6483-2012; Ruokolainen, Kalle/G-3141-2013; Asner, Gregory/G-9268-2013; OI Ruokolainen, Kalle/0000-0002-7494-9417; Asner, Gregory/0000-0001-7893-6421; Tuomisto, Hanna/0000-0003-1640-490X FU John D. and Catherine T. MacArthur Foundation (USA); Grantham Foundation for the Protection of the Environment (USA); Carnegie Institution for Science (USA); National Science Foundation (USA); Academy of Finland (Finland); American-Scandinavian Foundation (USA); Duke University (USA); Repsol Exploracion Peru (Peru) FX For field assistance we thank Fernando Ruiz (Pastaza-Tigre study area); Sulema Castro, Glenda Cardenas, and Wilber Bosmediano (Curaray study area); and Abel Sarmiento and Melchor Aguilar (Sucusari study area). For soil analyses, we thank Tapio Salo (MTT Agrifood Research Center, Finland) and Irma Puttonen. For logistic support at the Pastaza-Tigre study area we thank colleagues at the Instituto de Investigaciones de la Amazonia Peruana and the Universidad Nacional de la Amazonia Peruana. Additional logistic support at Pastaza-Tigre was provided by the PlusPetrol corporation (Argentina); logistic support at Curaray was provided by Repsol Exploracion Peru (Peru) and Global Geophysical Services (USA); and logistic support at Sucusari was provided by Explorama Tours (USA, Peru), and in particular Peter Jenson. We thank three anonymous reviewers for their constructive comments on the manuscript. This publication is contribution #9 of the Smithsonian Institution's Conservation Education and Sustainability Peru Biodiversity Program. Funding for this work was provided by the John D. and Catherine T. MacArthur Foundation (USA), the Grantham Foundation for the Protection of the Environment (USA), the Carnegie Institution for Science (USA), the National Science Foundation (USA), the Academy of Finland (Finland), the American-Scandinavian Foundation (USA), Duke University (USA), and Repsol Exploracion Peru (Peru). We thank the Instituto Nacional de Recursos Naturales (Peru) for permission to collect plant specimens; the ACEER Foundation (Peru, USA) for permission to work at the Sucusari study area; and the communities of the Rio Tigre for permission to work in their forests. NR 47 TC 17 Z9 17 U1 0 U2 42 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 2072-4292 J9 REMOTE SENS-BASEL JI Remote Sens. PD AUG PY 2012 VL 4 IS 8 BP 2401 EP 2418 DI 10.3390/rs4082401 PG 18 WC Remote Sensing SC Remote Sensing GA 003CW UT WOS:000308586800011 ER PT J AU Hark, RR Remus, JJ East, LJ Harmon, RS Wise, MA Tansi, BM Shughrue, KM Dunsin, KS Liu, CY AF Hark, Richard R. Remus, Jeremiah J. East, Lucille J. Harmon, Russell S. Wise, Michael A. Tansi, Benjamin M. Shughrue, Katrina M. Dunsin, Kehinde S. Liu, Chunyi TI Geographical analysis of "conflict minerals" utilizing laser-induced breakdown spectroscopy SO SPECTROCHIMICA ACTA PART B-ATOMIC SPECTROSCOPY LA English DT Article DE Laser-induced breakdown spectroscopy; LIBS; Conflict minerals; Columbite-tantalite; PLSDA ID PARTIAL LEAST-SQUARES; COLUMBITE; DISCRIMINATION; GEOCHEMISTRY; PEGMATITES; REGRESSION; TANTALITE; PATTERN AB Laser-induced breakdown spectroscopy (LIBS) offers a means of rapidly distinguishing different geographic sources for a mineral because the LIBS plasma emission spectrum provides information on the chemical composition (i.e. geochemical fingerprint) of a geomaterial. An application of this approach with potentially significant commercial and political importance is the spectral fingerprinting of "conflict minerals" such as columbite-tantalite ("coltan"). Following a successful pilot study of a columbite-tantalite suite from North America. a more geographically diverse set of 57 samples from 37 locations around the world was analyzed using a commercially available LIBS system. The LIBS spectra were analyzed using advanced multivariate statistical signal processing techniques. Partial least squares discriminant analysis (PLSDA) resulted in a correct place-level geographic classification at success rates above 90%. The possible role of rare-earth elements (REEs) as a factor contributing to the high levels of sample discrimination was explored. These results provide additional evidence that LIBS has the potential to be utilized in the field as a real-tirne screening tool to discriminate between columbite-tantalite ores of different provenance. (C) 2012 Elsevier B.V. All rights reserved. C1 [Hark, Richard R.; Tansi, Benjamin M.; Shughrue, Katrina M.] Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA. [Remus, Jeremiah J.; Dunsin, Kehinde S.] Clarkson Univ, Dept Elect & Comp Engn, Potsdam, NY 13699 USA. [East, Lucille J.; Liu, Chunyi] Appl Spectra Inc, Fremont, CA 94538 USA. [Harmon, Russell S.] N Carolina State Univ, Dept Marine Earth & Atmospher Sci, Raleigh, NC 27695 USA. [Wise, Michael A.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Hark, RR (reprint author), Juniata Coll, Dept Chem, Huntingdon, PA 16652 USA. EM hark@juniata.edu FU Army Research Laboratory; II-VI Foundation; Coulter Fellowship for the Transfer of Knowledge - Research Scholarship [43644] FX This research was made possible by Army Research Laboratory Fellow funding to R.S.H., financial support to R.R.H., K.M.S. and B.M.T. from the II-VI Foundation, and a Coulter Fellowship for the Transfer of Knowledge - Research Scholarship 43644 to K.S.D. The authors wish to thank Peter Torrione of New Folder Consulting, Durham, NC for LIBS GDT chemometric software, Applied Spectra, Inc. for technical support and use of instrumentation, and the following individuals and organizations for samples: Ulric Schwela (Tantalum-Niobium International Study Centre), David Miller (Global Advance Metals), Alexander Paiva (CIF Mineracao S.A.), and the Department of Mineral Sciences, Smithsonian Institution. Helpful comments from the anonymous reviewers helped to improve the final version of the manuscript. NR 27 TC 13 Z9 14 U1 2 U2 45 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0584-8547 J9 SPECTROCHIM ACTA B JI Spectroc. Acta Pt. B-Atom. Spectr. PD AUG-SEP PY 2012 VL 74-75 BP 131 EP 136 DI 10.1016/j.sab.2012.06.052 PG 6 WC Spectroscopy SC Spectroscopy GA 005UP UT WOS:000308775900021 ER PT J AU Hidalgo, P Ferrari, F Yanez, S Pino, P Escribano, R AF Hidalgo, Pamela Ferrari, Frank Yanez, Sonia Pino, Pamela Escribano, Ruben TI DEVELOPMENT OF RHINCALANUS NASUTUS (GIESBRECHT, 1888) (COPEPODA, RHINCALANIDAE) FROM THE HUMBOLDT CURRENT SYSTEM SO CRUSTACEANA LA English DT Article ID CENTRAL-SOUTHERN CHILE; NORTHERN CHILE; EUCALANUS-INERMIS; UPWELLING ZONE; 23-DEGREES-S; PATTERNS; NUMBERS AB Morphological changes in the exoskeleton of naupliar stages 2-6 and copepodid stages I-V of Rhincalanus nasutus are described. On the distal segment of naupliar antennule, one lateral seta and two medial setae are added during each molt to nauplius 3-6. A naupliar arthrite is a thick, distinctive structure on the coxa of antenna, and the exopod of this limb is patterned from the large proximal segment of that ramus. The coxal gnathobase of the mandible appears at nauplius 4. Buds of maxillule and maxilla are added during the molt to nauplius 5, and buds of maxilliped and swimming legs 1-2 are added during the molt to nauplius 6. The somite bearing maxilla clearly articulates completely with the somite bearing the maxilliped on the last two naupliar stages. This unusual articulation does not appear during copepodid development, and the somite bearing swimming leg 2 is the anterior articulating somite during this later phase. One articulating somite is added during molts to copepodid II-V. Segmentation of the antennule is completed by copepodid IV. Segmentation of the exopod of antenna does not change during the copepodid phase, but one segment is added to the endopod of maxilla. Segmentation and setation of the maxilliped follow the usual calanoid pattern. Buds of swimming legs 3-5 are ventrolateral on their smite. Their presumptive exopod has two attenuations; their presumptive endopod bears an attenuation and a seta. Segmentation of the rami of swimming legs 1-4 follows the common pattern for copepods except for the exopod and endopod of swimming leg 1 which are only 2-segmented. C1 [Hidalgo, Pamela; Yanez, Sonia; Escribano, Ruben] Univ Concepcion, Dept Oceanog, Ctr Oceanog Pacifico S Oriental COPAS, Dichato, Chile. [Ferrari, Frank] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitlant, DC USA. [Yanez, Sonia] Univ Antofagasta, Fac Recursos Mar, Programa Magister Ecol Ambientes, Angamos 601, Antofagasta, Chile. [Pino, Pamela] Univ Concepcion, Programa Magister Oceanog, Concepcion, Chile. RP Hidalgo, P (reprint author), Univ Concepcion, Dept Oceanog, Ctr Oceanog Pacifico S Oriental COPAS, POB 42, Dichato, Chile. EM pahidalg@udec.cl FU Chilean National Commission for Science a Technology (CONICYT) through FONDECYT [3070002, 11090146]; FONDECYT [1080037]; Center for Oceanographic Research in the Eastern South Pacific (COPAS) of the Concepcion University; FIP (Fondo Investigacion Pesquera, Chile) [2004-20, 2005-01] FX This study has been funded by the Chilean National Commission for Science a Technology (CONICYT) through FONDECYT Grant Nos 3070002 and 11090146 to P.H. and FONDECYT No. 1080037 to R.E., and Center for Oceanographic Research in the Eastern South Pacific (COPAS) of the Concepcion University and FIP (Fondo Investigacion Pesquera, Chile) Projects (PIP Nos 2004-20 and 2005-01). We are grateful to the COPAS time series team and the R/V Kay-Kay II crew for the sampling in the field works and PLAMZ (Pelagic Laboratory and Mesozooplankton) team of Marine Biology Station Dichato, Chile. We thank Dr. Hans-Uwe Dahms, Sangmyung University South Korea, for helpful discussions of naupliar development. NR 21 TC 2 Z9 2 U1 0 U2 6 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 AUG PY 2012 VL 85 IS 9 BP 1025 EP 1053 DI 10.1163/156854012X651673 PG 29 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 000JX UT WOS:000308383700001 ER PT J AU Emmons, LH Patton, JL AF Emmons, Louise H. Patton, James L. TI Taxonomic revision of Bolivian Juscelinomys (Rodentia, Cricetidae) with notes on morphology and ecology SO MAMMALIA LA English DT Article DE Akodontini; Cerrado; dentition; Oxymycterus; Sigmodontinae; systematics ID DIVERSIFICATION; SIGMODONTINAE; EVOLUTIONARY; OXYMYCTERUS; MAMMALIA AB The genus Juscelinomys includes three species of rare, Cerrado-endemic Sigmodontine mice: one from Central Brazil, now listed as extinct (IUCN), and two from Bolivia, originally known only from their holotypes and listed as data deficient. Additional specimens of Bolivian Juscelinomys have provided a basis for review of morphological and DNA characters. From these, we conclude that the segregation of Juscelinomys into two Bolivian species cannot be justified, so we revise the genus to include only two named taxa: J. candango Moojen, 1965, from central Brazil and J. huanchacae Emmons, 1999, from eastern Bolivia. We provide emended diagnoses for the genus and for the Bolivian species. We present new morphological details of the feet, dentition, and stomach of J. huanchacae, and we provide notes on its ecology. Juscelinomys huanchacae occurred sporadically in both space and time during a long-term trapping program. This may account for the rarity of the genus in collections. C1 [Emmons, Louise H.] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. [Patton, James L.] Univ Calif Berkeley, Museum Vertebrate Zool, Berkeley, CA 94720 USA. RP Emmons, LH (reprint author), Smithsonian Inst, Div Mammals, NHB W630,MRC 108, Washington, DC 20013 USA. EM emmonsl@si.edu FU A. Weedon and the Weedon Foundation; Douroucouli Foundation; National Geographic Society; Wildlife Conservation Society (WCS); W. Alton Jones Foundation through the Amazon Conservation Association FX Research in Bolivia was in collaboration with the Museo de Historia Natural Noel Kempff Mercado, Universidad Autonoma Gabriel Rene Moreno, Santa Cruz Bolivia (MNK). Its staff and students generously helped us throughout many years of study, especially K. Rivero, who smoothed our path over many obstacles. Permits to conduct studies in NKP were kindly granted by the Servicio Nacional de Areas Protegidas and the Direccion General de Biodiversidad de Bolivia. This project was supported by A. Weedon and the Weedon Foundation, The Douroucouli Foundation, The National Geographic Society, The Wildlife Conservation Society (WCS) and the W. Alton Jones Foundation through the Amazon Conservation Association. Part of the study was conducted under a research agreement between WCS and MNK. For cheerful and able field assistance, we are indebted to F. del Aguila, S. Angulo, S. Cabrera, V. Chavez, S. Coppeto, N. Rocha, R. Pena and M. Muir. For help and good company at El Refugio Huanchaca, we thank I. Phillips, the late B. Phillips, and Reynaldo Chore. D. Schmidt photographed the skulls. Ulyses Pardinas and an anonymous reviewer improved the manuscript with constructive comments. NR 29 TC 4 Z9 5 U1 0 U2 3 PU WALTER DE GRUYTER GMBH PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0025-1461 EI 1864-1547 J9 MAMMALIA JI Mammalia PD AUG PY 2012 VL 76 IS 3 BP 285 EP 294 DI 10.1515/mammalia-2012-0020 PG 10 WC Zoology SC Zoology GA 002RN UT WOS:000308551400007 ER PT J AU Heer, K Machado, CA Himler, AG Herre, EA Kalko, EKV Dick, CW AF Heer, Katrin Machado, Carlos A. Himler, Anna G. Herre, Edward Allen Kalko, Elisabeth K. V. Dick, Christopher W. TI ANONYMOUS AND EST-BASED MICROSATELLITE DNA MARKERS THAT TRANSFER BROADLY ACROSS THE FIG TREE GENUS (FICUS, MORACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Ficus insipida; hybridization; Moraceae; spatial genetic structure; tropical forests AB Premise of the study: We developed a set of microsatellite markers for broad utility across the species-rich pantropical tree genus Ficus (fig trees). The markers were developed to study population structure, hybridization, and gene flow in neotropical species. Methods and Results: We developed seven novel primer sets from expressed sequence tag (EST) libraries of F. citrifolia and F. popenoei (subgen. Urostigma sect. Americana) and optimized five previously developed anonymous loci for cross-species amplification. The markers were successfully tested on four species from the basal subgenus Pharmacosycea sect. Pharmacosycea (F. insipida, F. maxima, F. tonduzii, and F. yoponensis) and seven species of the derived subgenus Urostigma (F. citrifolia, F. colubrinae, F. costaricana, F. nymphaeifolia, F. obtusifolia, F. pertusa, and F. popenoei). The 12 markers amplified consistently and displayed polymorphism in all the species. Conclusions: This set of microsatellite markers is transferable across the phylogenetic breadth of Ficus, and should therefore be useful for studies of population structure and gene flow in approximately 750 fig species worldwide. C1 [Heer, Katrin; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Machado, Carlos A.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Himler, Anna G.] Univ Arizona, Dept Entomol, Tucson, AZ 85721 USA. [Herre, Edward Allen; Kalko, Elisabeth K. V.; Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Panama. [Dick, Christopher W.] Univ Michigan, Ann Arbor, MI 48109 USA. RP Heer, K (reprint author), Univ Ulm, Inst Expt Ecol, Ulm, Germany. EM katrin.heer@uni-ulm.de RI Dick, Christopher/A-8744-2008 FU German National Academic Foundation; National Science Foundation [DEB 0640379] FX The German National Academic Foundation provided financial support to K. H. C. W. D. acknowledges support from the National Science Foundation (DEB 0640379). We are grateful to Autoridad Nacional del Ambiente (ANAM) (Permit No. SC/AP-2-10 and SEX/AP-8-10) and Ministerio del Ambiente, Energia y Telecomunicaciones (MINET) (Permit No. 047-2010_SINAC) for granting research and export permits. The authors thank Juanita Choo, Ashley Thomson, and Wei Na for helpful advice with the laboratory work. NR 11 TC 4 Z9 4 U1 0 U2 10 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 AUG PY 2012 VL 99 IS 8 BP E330 EP E333 DI 10.3732/ajb.1200032 PG 4 WC Plant Sciences SC Plant Sciences GA 992VF UT WOS:000307807300010 PM 22847539 ER PT J AU Birnstiel, T Andrews, SM Ercolano, B AF Birnstiel, T. Andrews, S. M. Ercolano, B. TI Can grain growth explain transition disks? SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; protoplanetary disks; stars: pre-main sequence; planets and satellites: formation; circumstellar matter ID MAIN-SEQUENCE STARS; T-TAURI STARS; PROTOPLANETARY DISKS; DUST PARTICLES; SOLAR NEBULA; GM-AURIGAE; PLANETESIMAL FORMATION; PRETRANSITIONAL DISKS; AGGREGATE COLLISIONS; HYDRODYNAMIC MODELS AB Aims. Grain growth has been suggested as one possible explanation for the diminished dust optical depths in the inner regions of protoplanetary "transition" disks. In this work, we directly test this hypothesis in the context of current models of grain growth and transport. Methods. A set of dust evolution models with different disk shapes, masses, turbulence parameters, and drift efficiencies is combined with radiative transfer calculations in order to derive theoretical spectral energy distributions (SEDs) and images. Results. We find that grain growth and transport effects can indeed produce dips in the infrared SED, as typically found in observations of transition disks. Our models achieve the necessary reduction of mass in small dust by producing larger grains, yet not large enough to be fragmenting efficiently. However, this population of large grains is still detectable at millimeter wavelengths. Even if perfect sticking is assumed and radial drift is neglected, a large population of dust grains is left behind because the time scales on which they are swept up by the larger grains are too long. This mechanism thus fails to reproduce the large emission cavities observed in recent millimeter-wave interferometric images of accreting transition disks. C1 [Birnstiel, T.; Ercolano, B.] Univ Observ Munich, D-81679 Munich, Germany. [Birnstiel, T.; Ercolano, B.] Tech Univ Munich, D-85748 Garching, Germany. [Andrews, S. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Birnstiel, T (reprint author), Univ Observ Munich, Scheinerstr 1, D-81679 Munich, Germany. EM til.birnstiel@lmu.de OI Birnstiel, Tilman/0000-0002-1899-8783 NR 82 TC 46 Z9 46 U1 1 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 AUG PY 2012 VL 544 AR A79 DI 10.1051/0004-6361/201219262 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100079 ER PT J AU Bel, MC Rodriguez, J D'Avanzo, P Russell, DM Tomsick, J Corbel, S Lewis, FW Rahoui, F Buxton, M Goldoni, P Kuulkers, E AF Cadolle Bel, M. Rodriguez, J. D'Avanzo, P. Russell, D. M. Tomsick, J. Corbel, S. Lewis, F. W. Rahoui, F. Buxton, M. Goldoni, P. Kuulkers, E. TI Overview of an extensive multi-wavelength study of GX 339-4 during the 2010 outburst (vol 534, A119, 2011) SO ASTRONOMY & ASTROPHYSICS LA English DT Correction DE black hole physics; stars: individual: GX 339-4; X-rays: binaries; gamma rays: general; infrared: general; errata, addenda C1 [Cadolle Bel, M.; Kuulkers, E.] ISOC, ESAC, Madrid, Spain. [Rodriguez, J.; Corbel, S.] Univ Paris Diderot, CNRS, UMR 7158, Lab AIM,CEA DSM,IRFU SAp, Gif Sur Yvette, France. [D'Avanzo, P.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Russell, D. M.] Univ Amsterdam, Anton Pannekoek Inst, NL-1012 WX Amsterdam, Netherlands. [Tomsick, J.] Univ Calif Berkeley, SSL, Berkeley, CA 94720 USA. [Lewis, F. W.] Univ Glamorgan, Faulkes Telescope Project, Pontypridd CF37 1DL, M Glam, Wales. [Rahoui, F.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Rahoui, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Buxton, M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Goldoni, P.] Univ Paris Diderot, CNRS, UMR 7164, Lab APC,CEA DSM,IRFU SAp, Paris, France. RP Bel, MC (reprint author), ISOC, ESAC, Madrid, Spain. EM Marion.Cadolle@sciops.esa.int NR 1 TC 0 Z9 0 U1 1 U2 1 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 AUG PY 2012 VL 544 AR C2 DI 10.1051/0004-6361/201117684e PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100158 ER PT J AU de Boer, TJL Tolstoy, E Hill, V Saha, A Olszewski, EW Mateo, M Starkenburg, E Battaglia, G Walker, AG AF de Boer, T. J. L. Tolstoy, E. Hill, V. Saha, A. Olszewski, E. W. Mateo, M. Starkenburg, E. Battaglia, G. Walker, Andm. G. TI The star formation and chemical evolution history of the Fornax dwarf spheroidal galaxy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: dwarf; galaxies: evolution; galaxies: stellar content; Local Group; Hertzsprung-Russell and C-M diagrams ID MULTIELEMENT ABUNDANCE MEASUREMENTS; PHOTOMETRIC STANDARD STARS; COLOR-MAGNITUDE DIAGRAMS; GIANT BRANCH STARS; LOCAL GROUP; IRREGULAR GALAXY; MILKY-WAY; VLT/UVES ABUNDANCES; STELLAR POPULATIONS; SATELLITE GALAXIES AB We present deep photometry in the B, V and I filters from CTIO/MOSAIC for about 270 000 stars in the Fornax dwarf spheroidal galaxy, out to a radius of r(ell) approximate to 0.8 degrees. By combining the accurately calibrated photometry with the spectroscopic metallicity distributions of individual red giant branch stars we obtain the detailed star formation and chemical evolution history of Fornax. Fornax is dominated by intermediate age (1-10 Gyr) stellar populations, but also includes ancient (10-14 Gyr), and young (<= 1 Gyr) stars. We show that Fornax displays a radial age gradient, with younger, more metal-rich populations dominating the central region. This confirms results from previous works. Within an elliptical radius of 0.8 degrees, or 1.9 kpc from the centre, a total mass in stars of 4.3 x 10(7) M-circle dot was formed, from the earliest times until 250 Myr ago. Using the detailed star formation history, age estimates are determined for individual stars on the upper RGB, for which spectroscopic abundances are available, giving an age-metallicity relation of the Fornax dSph from individual stars. This shows that the average metallicity of Fornax went up rapidly from [Fe/H] <= -2.5 dex to [Fe/H] = -1.5 dex between 8-12 Gyr ago, after which a more gradual enrichment resulted in a narrow, well-defined sequence which reaches [Fe/H] approximate to -0.8 dex, approximate to 3 Gyr ago. These ages also allow us to measure the build-up of chemical elements as a function of time, and thus determine detailed time-scales for the evolution of individual chemical elements. A rapid decrease in [Mg/Fe] is seen for the stars with [Fe/H] >= -1.5 dex, with a clear trend in age. C1 [de Boer, T. J. L.; Tolstoy, E.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Hill, V.] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, Lab Cassiopee, F-06304 Nice 4, France. [Saha, A.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Olszewski, E. W.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Mateo, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Starkenburg, E.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Battaglia, G.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Walker, Andm. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP de Boer, TJL (reprint author), Univ Groningen, Kapteyn Astron Inst, Postbus 800, NL-9700 AV Groningen, Netherlands. EM deboer@astro.rug.nl RI Walker, Matthew/P-1777-2014; OI Walker, Matthew/0000-0003-2496-1925; Battaglia, Giuseppina/0000-0002-6551-4294 FU Netherlands Foundation for Scientific Research (NWO) through a VICI grant; NSF [AST0807498]; CITA National Fellowship; CIfAR's Junior Academy; ISSI (Bern) FX The authors thank ISSI (Bern) for support of the team "Defining the full life-cycle of dwarf galaxy evolution: the Local Universe as a template". T. d. B. and E. T. gratefully acknowledge the Netherlands Foundation for Scientific Research (NWO) for financial support through a VICI grant. E. O. is partially supported by NSF grant AST0807498. Partial support was provided to E. S. by a CITA National Fellowship and CIfAR's Junior Academy. The authors would like to thank the anonymous referee for his/her comments, that helped to improve the paper. NR 74 TC 55 Z9 55 U1 0 U2 0 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 AUG PY 2012 VL 544 AR A73 DI 10.1051/0004-6361/201219547 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100073 ER PT J AU Larsen, SS Strader, J Brodie, JP AF Larsen, S. S. Strader, J. Brodie, J. P. TI Constraints on mass loss and self-enrichment scenarios for the globular clusters of the Fornax dSph SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: individual: Fornax dSph; galaxies: star clusters: general; galaxies: stellar content ID MULTIPLE STELLAR POPULATIONS; DWARF SPHEROIDAL GALAXY; STAR-CLUSTERS; LOCAL GROUP; LUMINOSITY FUNCTION; FORMATION EFFICIENCIES; SYSTEMS; HALO; EVOLUTION; SPECTROSCOPY AB Recently, high-dispersion spectroscopy has demonstrated conclusively that four of the five globular clusters (GCs) in the Fornax dwarf spheroidal galaxy are very metal-poor with [Fe/H] < -2. The remaining cluster, Fornax 4, has [Fe/H] = -1.4. This is in stark contrast to the field star metallicity distribution which shows a broad peak around [Fe/H] approximate to -1 with only a few percent of the stars having [Fe/H] < -2. If we only consider stars and clusters with [Fe/H] < -2 we thus find an extremely high GC specific frequency, S-N approximate to 400, implying by far the highest ratio of GCs to field stars known anywhere. We estimate that about 1/5-1/4 of all stars in the Fornax dSph with [Fe/H] < -2 belong to the four most metal-poor GCs. These GCs could, therefore, at most have been a factor of 4-5 more massive initially. Yet, the Fornax GCs appear to share the same anomalous chemical abundance patterns known from Milky Way GCs, commonly attributed to the presence of multiple stellar generations within the clusters. The extreme ratio of metal-poor GC-versus field stars in the Fornax dSph is difficult to reconcile with scenarios for self-enrichment and early evolution of GCs in which a large fraction (90%-95%) of the first-generation stars have been lost. It also suggests that the GCs may not have formed as part of a larger population of now disrupted clusters with an initial power-law mass distribution. The Fornax dSph may be a rosetta stone for constraining theories of the formation, self-enrichment and early dynamical evolution of star clusters. C1 [Larsen, S. S.] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Strader, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Strader, J.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Brodie, J. P.] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. RP Larsen, SS (reprint author), Radboud Univ Nijmegen, Dept Astrophys, IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM S.larsen@astro.ru.nl FU NWO/VIDI; NSF [AST-1109878] FX We thank Charlie Conroy, Mark Gieles, Tom Richtler and the referee for valuable comments and discussion. S. S. L. acknowledges support by an NWO/VIDI grant and J.P.B. acknowledges NSF grant AST-1109878. NR 45 TC 43 Z9 43 U1 0 U2 0 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 AUG PY 2012 VL 544 AR L14 DI 10.1051/0004-6361/201219897 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100174 ER PT J AU Limousin, M Ebeling, H Richard, J Swinbank, AM Smith, GP Jauzac, M Rodionov, S Ma, CJ Smail, I Edge, AC Jullo, E Kneib, JP AF Limousin, M. Ebeling, H. Richard, J. Swinbank, A. M. Smith, G. P. Jauzac, M. Rodionov, S. Ma, C. -J. Smail, I. Edge, A. C. Jullo, E. Kneib, J. -P. TI Strong lensing by a node of the cosmic web The core of MACS J0717.5+3745 at z=0.55 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gravitational lensing: strong; galaxies: clusters: individual: MACS J0717.5+3745; large-scale structure of Universe; dark matter ID DARK-MATTER HALOS; SPACE-TELESCOPE OBSERVATIONS; HIGH-DENSITY ENVIRONMENTS; LUMINOUS GALAXY CLUSTERS; ALL-SKY SURVEY; DISCOVERY; UNIVERSE; DISTANT; Z-GREATER-THAN-0.5; ABELL-1689 AB We present results of a strong-lensing analysis of MACS J0717.5+3745 (here after MACS J0717), an extremely X-ray luminous galaxy cluster at z = 0.55. Observations at different wavelengths reveal a complex and dynamically very active cluster, whose core is connected to a large scale filament extended over several Mpc. Using multi-passband imaging data obtained with the Hubble Space Telescope's Advanced Camera for Surveys (ACS), we identify 15 multiply imaged systems across the full field of view of ACS, five of which we confirmed spectroscopically in ground-based follow-up observations with the Keck telescope. We use these multiply imaged systems to constrain a parametric model of the mass distribution in the cluster core, employing a new parallelized version of the LENSTOOL software. The main result is that the most probable description of the mass distribution comprises four cluster-scale dark matter haloes. The total mass distribution follows the light distribution but strongly deviates from the distribution of the intra-cluster gas as traced by the X-ray surface brightness. This confirms the complex morphology proposed by previous studies. We interpret this segregation of collisional and collisionless matter as strong evidence of multiple mergers and ongoing dynamical activity. MACS J0717 thus constitutes one of the most disturbed clusters presently known and, featuring a projected mass within the ACS field of view (R = 150" = 960 kpc) of 2.11 +/- 0.23 x 10(15) M-circle dot, the system is also one of the most massive known. C1 [Limousin, M.; Jauzac, M.; Rodionov, S.; Jullo, E.; Kneib, J. -P.] Univ Provence, CNRS, Lab Astrophys Marseille, UMR 6610, F-13388 Marseille 13, France. [Limousin, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Ebeling, H.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Richard, J.] Univ Lyon 1, Observ Lyon, CRAL, F-69561 St Genis Laval, France. [Swinbank, A. M.; Smail, I.; Edge, A. C.] Univ Durham, Dept Phys, Inst Computat Cosmol, Durham DH1 3LE, England. [Smith, G. P.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Smith, G. P.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Jauzac, M.] Univ KwaZulu Natal, Astrophys & Cosmol Res Unit, Sch Math Sci, ZA-4041 Durban, South Africa. [Ma, C. -J.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Ma, C. -J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jullo, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Limousin, M (reprint author), Univ Provence, CNRS, Lab Astrophys Marseille, UMR 6610, 38 Rue Frederic Joliot Curie, F-13388 Marseille 13, France. EM marceau.limousin@oamp.fr RI Rodionov, Sergey/K-2166-2013; Smail, Ian/M-5161-2013; Jauzac, Mathilde/B-1966-2015; Kneib, Jean-Paul/A-7919-2015; OI Rodionov, Sergey/0000-0002-9661-8221; Smail, Ian/0000-0003-3037-257X; Kneib, Jean-Paul/0000-0002-4616-4989; Edge, Alastair/0000-0002-3398-6916 FU Centre National de la Recherche Scientifique; STScI [GO-09722, GO-10420]; SAO [GO3-4168X]; Danish National Research Foundation FX M. L. thanks Massimo Meneghetti and Adi Zitrin for helpful discussions. M. L. and J. P. K. acknowledge the Centre National de la Recherche Scientifique for its support. H. E. acknowledges financial support from STScI grants GO-09722 and GO-10420 as well as SAO grant GO3-4168X. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work has been conducted using facilities offered by CeSAM (Centre de donneeS Astrophysiques de Marseille, http://lam.oamp.fr/cesam/. NR 40 TC 33 Z9 33 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 AUG PY 2012 VL 544 AR A71 DI 10.1051/0004-6361/201117921 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100071 ER PT J AU Roberts, JF Jimenez-Serra, I Gusdorf, A Martin-Pintado, J AF Roberts, J. F. Jimenez-Serra, I. Gusdorf, A. Martin-Pintado, J. TI The search for the magnetic precursor of C-type shocks in young molecular outflows SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: jets and outflows; shock waves; submillimeter: ISM; infrared: ISM ID SIO EMISSION; ROTATIONAL-EXCITATION; COLLIMATED OUTFLOW; STELLAR OBJECTS; LINE EMISSION; DENSE CORES; DARK CLOUD; NGC 1333; WAVES; EVOLUTION AB The detection of very narrow SiO emission and the higher degree of excitation of the ion fluid compared to the neutral one towards the protostar L1448-mm have been interpreted as signatures of the magnetic precursor of C-shocks. Since this is the only source where these features have been observed together, we carried out a survey to map the J = 2 -> 1 and 8 -> 7 lines of SiO, and the J = 1 -> 0 and 4 -> 3 lines of (HCO+)-C-13 (as the representative ion) and (HNC)-C-13 (as the representative neutral species) towards four class 0/I low-mass protostars known to have young outflows (L1448-IRS3, NGC 1333-IRAS 4A/B and SSV 13, VLA 1623 and IRAS 20353). As previously reported, towards L1448-IRS3 and NGC 1333 strong, narrow SiO 2 -> 1 is detected, and we also find a velocity component towards each outflow which shows high a (HCO+)-C-13 4 -> 3/1 -> 0 integrated intensity ratio compared to that of (HNC)-C-13. Towards VLA 1623, we find very weak, narrow SiO, and a component that is visible in (HCO)-C-13+ but not at all in (HNC)-C-13. For IRAS 20353, we find neither narrow SiO nor high (HCO+)-C-13 4 -> 3/1 -> 0 flux ratios. Previous work explained the higher degree of excitation of (HCO+)-C-13 by the selective excitation of ions by electrons, whose abundance is expected to increase at the precursor stage. Here, however, by considering a range of kinetic temperatures for the gas, we find that it is possible to fit the observations with a single temperature and density, without an increased electron abundance, despite the large differences in 4 -> 3/1 -> 0 ratio between the two molecules. The high (HCO+)-C-13 4 -> 3/1 -> 0 flux ratios may simply be due to protostellar heating. However, the hypothesis that narrow SiO is formed at the precursor stage of shocks remains plausible, since other explanations require either the presence of shocks with larger dynamical timescales, or predict the narrow SiO to have a larger spatial extent than it appears to have towards the sources L1448-IRS3 and VLA 1623. Larger scale maps of the narrow SiO emission are needed to confirm that it is confined to the regions around protostars (as would be expected in the precursor scenario), and mapping of different ion and neutral species is necessary to confirm whether there are indeed precursor regions surrounding young outflows where the ion and neutral species behave as separate fluids. C1 [Roberts, J. F.; Martin-Pintado, J.] INTA, CSIC, Ctr Astrobiol, Madrid 28850, Spain. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gusdorf, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Gusdorf, A.] Ecole Normale Super, CNRS, UMR 8112, Observ Paris,LERMA, F-75231 Paris 05, France. RP Roberts, JF (reprint author), INTA, CSIC, Ctr Astrobiol, Km 4, Madrid 28850, Spain. EM robertsj@cab.inta-csic.es RI Martin-Pintado, Jesus/H-6107-2015 OI Martin-Pintado, Jesus/0000-0003-4561-3508 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Spanish Ministerio de Ciencia e Innovacion [ESP2007-65812-C02-01]; Comunidad de Madrid Government under PRICIT project [S-0505/ESP-0237]; French Agence Nationale de la Recherche as part of the SCHISM project [ANR-09-BLAN-0231-01] FX We would like to thank the anonymous referee for helpful comments on an earlier draft of this paper. This paper is based on observations from the IRAM 30 m Telescope and the James Clerk Maxwell Telescope (project M10BU04). The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, The Netherlands Organisation for Scientific Research, and the National Research Council of Canada. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). This work has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This work has been partially supported by the Spanish Ministerio de Ciencia e Innovacion under project ESP2007-65812-C02-01, and by the Comunidad de Madrid Government under PRICIT project S-0505/ESP-0237 (ASTROCAM). A. Gusdorf acknowledges support by the grant ANR-09-BLAN-0231-01 from the French Agence Nationale de la Recherche as part of the SCHISM project. NR 45 TC 3 Z9 3 U1 1 U2 1 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 AUG PY 2012 VL 544 AR A150 DI 10.1051/0004-6361/201219024 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100150 ER PT J AU Zhang, B Reid, MJ Menten, KM Zheng, XW Brunthaler, A AF Zhang, B. Reid, M. J. Menten, K. M. Zheng, X. W. Brunthaler, A. TI The distance and size of the red hypergiant NML Cygni from VLBA and VLA astrometry SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrometry; masers; parallaxes; proper motions; stars: individual: NML Cyg; supergiants ID VY-CANIS-MAJORIS; LATE-TYPE STARS; PROPER MOTIONS; DUST SHELLS; TRIGONOMETRIC PARALLAXES; CIRCUMSTELLAR ENVELOPE; RADIO PHOTOSPHERES; RADIATIVE-TRANSFER; MASER EMISSION; MILKY-WAY AB Context. The red hypergiant NML Cyg has been assumed to be at part of the Cyg OB2 association, although its distance has never been measured directly. A reliable distance is crucial to study the properties of this prominent star. For example, its luminosity, and hence its position on the H-R diagram, is critical information to determine its evolutionary status. In addition, a detection of the radio photosphere would be complementary to other methods of determining the stellar size. Aims. We aim to understand the characteristics of NML Cyg with direct measurements of its absolute position, distance, kinematics, and size. Methods. We observe circumstellar 22 GHz H2O and 43 GHz SiO masers with the Very Long Baseline Array to determine the parallax and proper motion of NML Cyg. We observe continuum emission at 43 GHz from the radio photosphere of NML Cyg with the Very Large Array. Results. We measure the annual parallax of NML Cyg to be 0.620 +/- 0.047 mas, corresponding to a distance of 1.61(-0.11)(+0.13) kpc. The measured proper motion of NML Cyg is mu(x) = -1.55 +/- 0.42 mas yr(-1) eastward and mu(y) = -4.59 +/- 0.41 mas yr(-1) northward. Both the distance and proper motion are consistent with that of Cyg OB2, within their joint uncertainty, confirming their association. Taking into consideration molecular absorption signatures seen toward NML Cyg, we suggest that NML Cyg lies on the far side of the Cyg OB2 association. The stellar luminosity revised with our distance brings NML Cyg significantly below the empirical luminosity limit for a red supergiant. We partially resolve the radio photosphere of NML Cyg at 43 GHz and find its diameter is about 44 mas, suggesting an optical stellar diameter of 22 mas, if the size of radio photosphere is 2 times the optical photosphere. Based on the position of circumstellar SiO masers relative to the radio photosphere, we estimate the absolute position of NML Cyg at epoch 2008.868 to be alpha(J2000) = 20(h)46(m)25.(s)5382 +/- 0.(s)0010, delta(J2000) = 40 degrees 06'59.'' 379 +/- 0.'' 015. The peculiar motions of NML Cyg, the average of stars in Cyg OB2, and four other star-forming regions rules out that an expanding "Stromgren sphere" centered on Cyg OB2 is responsible for the kinematics of the Cygnus X region. C1 [Zhang, B.; Menten, K. M.; Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Zhang, B.] Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zheng, X. W.] Nanjing Univ, Dept Astron, Nanjing 210093, Jiangsu, Peoples R China. [Brunthaler, A.] Natl Radio Astron Observ, Socorro, NM 87801 USA. RP Zhang, B (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM bzhang@mpifr.de FU National Science Foundation of China [11073046, 11133008]; European Union [275596] FX We would like to thank the referee for very detailed and helpful comments. B. Zhang was supported by the National Science Foundation of China under grant 11073046, 11133008. A. Brunthaler was supported by a Marie Curie Outgoing International Fellowship (FP7) of the European Union (project number 275596). NR 51 TC 12 Z9 12 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 AUG PY 2012 VL 544 AR A42 DI 10.1051/0004-6361/201219587 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DS UT WOS:000308290100042 ER PT J AU Tornabene, LL Osinski, GR Mcewenb, AS Boyce, JM Bray, VJ Caudill, CM Grant, JA Hamilton, CW Mattson, S Mouginis-Mark, PJ AF Tornabene, Livio L. Osinski, Gordon R. McEwenB, Alfred S. Boyce, Joseph M. Bray, Veronica J. Caudill, Christy M. Grant, John A. Hamilton, Christopher W. Mattson, Sarah Mouginis-Mark, Peter J. TI Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process SO ICARUS LA English DT Article DE Mars, Surface; Cratering; Impact processes; Geological processes; Terrestrial planets ID SCIENCE EXPERIMENT HIRISE; GROUND ICE; EJECTA MORPHOLOGIES; ELYSIUM-PLANITIA; SINUS SABAEUS; DEPOSITS; REGIONS; UTOPIA; ORIGIN; MELT AB Recently acquired high-resolution images of martian impact craters provide further evidence for the interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of craters are nearly equally distributed between the two hemispheres, spanning from 53 degrees S to 62 degrees N latitude. They range in diameter from similar to 1 to 150 km, and are found at elevations between -5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clusters and range in size from similar to 10 m to as large as 3 km. Pit sizes scale with both the host crater's diameter and the host deposit size. These pits have subtle raised rims, and unlike primary and secondary impact craters, they lack well-defined ejecta deposits and overlapping stratigraphic relationships. They also lack any sign of any preferential alignment expected of volcanic or tectonic collapse features. Morphologic and stratigraphic evidence in support of an impact origin includes the observation that pitted materials primarily occur as ponded and flow-like deposits on crater floors, behind terraces, and infilling the lowest local topographic depressions atop the ejecta blanket similar to the distribution of impact melt-bearing bodies on the Moon. Based on the observations and comparisons to terrestrial and lunar analogs, we conclude that the pit-bearing materials are impactite deposits. The presence of these deposits in older craters, where preserved, suggests that they have formed on Mars throughout most of its geologic history; thus, understanding their origin may help to constrain the hydrological and climate history of Mars. (C) 2012 Elsevier Inc. All rights reserved. C1 [Tornabene, Livio L.; Osinski, Gordon R.] Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada. [McEwenB, Alfred S.; Bray, Veronica J.; Caudill, Christy M.; Mattson, Sarah] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Boyce, Joseph M.; Mouginis-Mark, Peter J.] Univ Hawaii, Hawaii Inst Geophys & Planetol, Manoa, HI 96822 USA. [Grant, John A.] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Hamilton, Christopher W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Tornabene, LL (reprint author), Univ Western Ontario, Ctr Planetary Sci & Explorat, London, ON N6A 5B7, Canada. EM ltornabe@uwo.ca FU NASA/JPL MRO project via the HiRISE Science and Operations team; Smithsonian Institution's "Charles Lindbergh" fellowship through the Center for Earth and Planetary Studies; NASA Postdoctoral Program at the Goddard Space Flight Center FX This work was supported by NASA/JPL MRO project via the HiRISE Science and Operations team, and the Smithsonian Institution's "Charles Lindbergh" fellowship through the Center for Earth and Planetary Studies. C.W.H. is supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. We would like to personally thank and acknowledge: Guy McArthur (CTX help), Patrick Russell (helpful discussions), the JMARS team, especially Eric Engle who personally helped me troubleshoot various GIS-related issues that were essential to the success of this study, Deanne Daigle who helped edit a final version of this manuscript, and the MRO and LRO, especially HiRISE, CTX and LROC teams, respectively, for all the wonderful crater-related data collected over the last few years. We'd also like to extend a special thanks to Horton Newsom and Seth Kadish for their invaluable time as reviewers and their efforts to help improve this manuscript for publication. NR 104 TC 33 Z9 33 U1 3 U2 17 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 AUG PY 2012 VL 220 IS 2 BP 348 EP 368 DI 10.1016/j.icarus.2012.05.022 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200006 ER PT J AU Harmon, JK Nolan, MC Husmann, DI Campbell, BA AF Harmon, John K. Nolan, Michael C. Husmann, Diana I. Campbell, Bruce A. TI Arecibo radar imagery of Mars: The major volcanic provinces SO ICARUS LA English DT Article DE Mars; Mars, Surface; Radar observations ID MEDUSAE FOSSAE FORMATION; DELAY-DOPPLER RADAR; MARTIAN FLOOD LAVAS; FAN-SHAPED DEPOSIT; THARSIS REGION; CERAUNIUS-FOSSAE; ELYSIUM PLANITIA; CERBERUS FOSSAE; ASCRAEUS MONS; PAVONIS MONS AB We present Earth-based radar images of Mars obtained with the upgraded Arecibo S-band (lambda = 12.6 cm) radar during the 2005-2012 oppositions. The imaging was done using the same long-code delay-Doppler technique as for the earlier (pre-upgrade) imaging but at a much higher resolution (similar to 3 km) and, for some regions, a more favorable sub-Earth latitude. This has enabled us to make a more detailed and complete mapping of depolarized radar reflectivity (a proxy for small-scale surface roughness) over the major volcanic provinces of Tharsis, Elysium, and Amazonis. We find that vast portions of these regions are covered by radar-bright lava flows exhibiting circular polarization ratios close to unity, a characteristic that is uncommon for terrestrial lavas and that is a likely indicator of multiple scattering from extremely blocky or otherwise highly disrupted flow surfaces. All of the major volcanoes have radar-bright features on their shields, although the brightness distribution on Olympus Mons is very patchy and the summit plateau of Pavonis Mons is entirely radar-dark. The older minor shields (paterae and tholi) are largely or entirely radar-dark, which is consistent with mantling by dust or pyroclastic material. Other prominent radar-dark features include: the "fan-shaped deposits", possibly glacial, associated with the three major Tharsis Montes shields; various units of the Medusae Fossae Formation; a region south and west of Biblis Patera where "Stealth" deposits appear to obscure Tharsis flows; and a number of "dark-halo craters" with radar-absorbing ejecta blankets deposited atop surrounding bright flows. Several major bright features in Tharsis are associated with off-shield lava flows; these include the Olympus Mons basal plains, volcanic fields east and south of Pavonis Mons, the Daedalia Planum flows south of Arsia Mons, and a broad expanse of flows extending east from the Tharsis Montes to Echus Chasma. The radar-bright lava plains in Elysium are concentrated mainly in Cerberus and include the fluvio-volcanic channels of Athabasca Valles, Grjota Valles, and Marte Valles, as well as an enigmatic region at the southern tip of the Cerberus basin. Some of the Cerberus bright features correspond to the distinctive "platy-ridged" flows identified in orbiter images. The radar-bright terrain in Amazonis Planitia comprises two distinct but contiguous sections: a northern section formed of lavas and sediments debouched from Marte Valles and a southern section whose volcanics may derive, in part, from local sources. This South Amazonis region shows perhaps the most complex radar-bright structure on Mars and includes features that correspond to platy-ridged flows similar to those in Cerberus. (C) 2012 Elsevier Inc. All rights reserved. C1 [Harmon, John K.; Nolan, Michael C.; Husmann, Diana I.] Arecibo Observ, Natl Astron & Ionosphere Ctr, Arecibo, PR 00612 USA. [Campbell, Bruce A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Harmon, JK (reprint author), 1902 Calle Cacique, San Juan, PR 00911 USA. EM harmon@naic.edu; nolan@naic.edu; campbellb@si.edu RI Nolan, Michael/H-4980-2012 OI Nolan, Michael/0000-0001-8316-0680 FU National Aeronautics and Space Administration (NASA); NSF FX The National Astronomy and Ionosphere Center (Arecibo Observatory) was operated, under a cooperative agreement with the National Science Foundation (NSF), by Cornell University (for the 2005-2010 observations) and by a consortium comprising SRI International, Universities Space Research Association (USRA), and Universidad Metropolitana (for the 2012 observations). The S-band radar observations were also made possible with support from the National Aeronautics and Space Administration (NASA). Diana Husmann's work at Arecibo was supported by a grant to Cornell University from the Research Experience for Undergraduates (REU) program of the NSF. We would like to thank the staff of Arecibo Observatory for their support, and in particular the following people: Victor Negron, Alfredo Santoni, and Joe Greene for transmitter maintenance and operations; Bill Sisk for digital hardware support; and Phil Perillat for datataking software support. We also thank John Chandler and Jon Giorgini for ephemeris support. We are grateful to Chris Magri for kindly volunteering to do Mars observations for us on October 14 and 15, 2005. Spacecraft images used in this paper were from the online Mars Global Data Sets, Planetary Data System (PDS) Node, Arizona State University http://www.mars.asu.edu/data/. The Mars Orbiter Laser Altimeter (MOLA) topographic data used in the delay-Doppler mapping were obtained from the PDS Geosciences Node, Washington University in St. Louis http://pds-geosciences.wustl.edu/missions/mgs/megdr.html. We wish to thank Lynn Carter and another, anonymous, reviewer for their constructive comments and suggestions. NR 179 TC 7 Z9 7 U1 3 U2 17 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 AUG PY 2012 VL 220 IS 2 BP 990 EP 1030 DI 10.1016/j.icarus.2012.06.030 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996AU UT WOS:000308057200052 ER PT J AU Engene, N Rottacker, EC Kastovsky, J Komarek, J Ellisman, MH Gerwick, WH Paul, V AF Engene, N. Rottacker, E. C. Kastovsky, J. Komarek, J. Ellisman, M. H. Gerwick, W. H. Paul, V TI TAXONOMIC REVISIONS OF MARINE CYANOBACTERIA TO FACILITATE NATURAL PRODUCTS DISCOVERIES AND HARMFUL ALGAE BLOOM MONITORING SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Engene, N.; Paul, V] Smithsonian Inst, Washington, DC 20560 USA. [Rottacker, E. C.; Ellisman, M. H.] Univ Calif San Diego, Natl Ctr Microscopy & Imaging Res, La Jolla, CA 92093 USA. [Kastovsky, J.; Komarek, J.] Univ S Bohemia, Fac Sci, Prague, Czech Republic. [Gerwick, W. H.] Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA USA. EM engenen@si.edu; erottack@ucsd.edu; hanys@prf.jcu.cz; komarek@butbn.cas.cz; mark.ellisman@gmail.com; wgerwick@ucsd.edu; Paul@si.edu NR 0 TC 0 Z9 0 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 2012 VL 48 SU 1 SI SI BP S26 EP S26 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 982NU UT WOS:000307053000073 ER PT J AU Fredericq, S Schmidt, WE Gabriel, D Sauvage, T Norris, JN Krayesky, D AF Fredericq, S. Schmidt, W. E. Gabriel, D. Sauvage, T. Norris, J. N. Krayesky, D. TI CHARACTERIZATION OF OFFSHORE RHODOLITH BEDS IN THE NW GULF OF MEXICO: TRIALS AND TRIBULATIONS SINCE THE BP DEEPWATER HORIZON OIL SPILL DISASTER SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Fredericq, S.; Schmidt, W. E.; Sauvage, T.] Univ Louisiana Lafayette, Lafayette, LA USA. [Norris, J. N.] Smithsonian Inst, Washington, DC 20560 USA. [Krayesky, D.] Slippery Rock Univ, Slippery Rock, PA 16057 USA. EM slf9209@louisiana.edu; weschmidt01@yahoo.com; danielalgabriel@gmail.com; tom.sauv@gamila.com; NORRISJ@si.edu; david.krayesky@sru.edu NR 0 TC 0 Z9 0 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 2012 VL 48 SU 1 SI SI BP S14 EP S14 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 982NU UT WOS:000307053000039 ER PT J AU Mark, WV Kibler, SR Holland, WC Tester, PA Schultz, TF Faust, MA Homes, MJ Chinain, M Litaker, RW AF Mark, Vandersea W. Kibler, S. R. Holland, W. C. Tester, P. A. Schultz, T. F. Faust, M. A. Homes, M. J. Chinain, M. Litaker, R. W. TI DEVELOPMENT OF SEMI-QUANTITATIVE PCR ASSAYS DETECTING AND ENUMERATING POTENTIALLY TOXIC CARIBBEAN GAMBIERDISCUS SPECIES SO JOURNAL OF PHYCOLOGY LA English DT Meeting Abstract C1 [Mark, Vandersea W.; Kibler, S. R.; Holland, W. C.; Tester, P. A.; Litaker, R. W.] NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC USA. [Schultz, T. F.] Duke Univ, Marine Lab, Marine Conservat Mol Facil, Beaufort, NC 28516 USA. [Faust, M. A.] Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, Suitland, MD USA. [Homes, M. J.] Queensland Dept Environm & Resource Man, Brisbane, Qld, Australia. [Chinain, M.] Inst Louis Malarde, Lab Microalgues Tox, Tahiti, Fr Polynesia. EM mark.w.vandersea@noaa.gov; steve.kibler@noaa.gov; chris.holland@noaa.gov; pat.tester@noaa.gov; tom.schultz@duke.edu; faustm@si.edu; michael.holmes@derm.qld.gov.au; MChinain@ilm.pf; Wayne.litaker@noaa.gov NR 0 TC 0 Z9 0 U1 2 U2 10 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 2012 VL 48 SU 1 SI SI BP S26 EP S27 PG 2 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 982NU UT WOS:000307053000074 ER PT J AU Hong, SK Grinolds, MS Maletinsky, P Walsworth, RL Lukin, MD Yacoby, A AF Hong, Sungkun Grinolds, Michael S. Maletinsky, Patrick Walsworth, Ronald L. Lukin, Mikhail D. Yacoby, Amir TI Coherent, Mechanical Control of a Single Electronic Spin SO NANO LETTERS LA English DT Article DE Electron spin; mechanical resonator; hybrid mechanical-spin system; nitrogen-vacancy (NV) center; nanoscale magnetometry; nanoscale motion sensor ID MAGNETIC-RESONANCE; QUANTUM CONTROL; NANOSCALE RESOLUTION; DIAMOND; MICROSCOPY; CENTERS; TIME AB We demonstrate coherent quantum control of a single spin driven by the motion of a mechanical resonator. The motion of a mechanical resonator is magnetically coupled to the electronic spin of a single nitrogen-vacancy center in diamond. Synchronization of spin-addressing protocols to the motion of the driven oscillator is used to fully exploit the coherence of this hybrid mechanical-spin system. We demonstrate applications of this coherent mechanical spin-control technique to nanoscale scanning magnetometry. C1 [Hong, Sungkun] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Grinolds, Michael S.; Maletinsky, Patrick; Walsworth, Ronald L.; Lukin, Mikhail D.; Yacoby, Amir] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yacoby, A (reprint author), LISE 6th Floor,11 Oxford St, Cambridge, MA 02138 USA. EM yacoby@physics.harvard.edu RI Hong, Sungkun/D-3282-2014; Maletinsky, Patrick/L-1851-2015 OI Hong, Sungkun/0000-0003-0985-6641; Maletinsky, Patrick/0000-0003-1699-388X FU NIST; DARPA; Kwanjeong Scholarship Foundation; Department of Defense (NDSEG program); NSF; Swiss National Science Foundation; National Science Foundation [ECS-0336765] FX We gratefully acknowledge G. Balasubramanian and P. R. Hemmer for fruitful technical discussions as well as B. Hausmann and M. Loncar for instruction in the fabrication of NV center containing nanostructures. We acknowledge financial support from NIST and DARPA. S.H. acknowledges support from the Kwanjeong Scholarship Foundation for fellowship funding. M.S.G. is supported through fellowships from the Department of Defense (NDSEG program) and the NSF. P.M. acknowledges support from the Swiss National Science Foundation. This work was carried out in part at the Center for Nanoscale Systems (CNS), a member of the National Nanotechnology Infrastructure Network (NNIN), which is supported by the National Science Foundation under NSF award no. ECS-0336765. CNS is part of Harvard University. NR 33 TC 34 Z9 34 U1 0 U2 37 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 J9 NANO LETT JI Nano Lett. PD AUG PY 2012 VL 12 IS 8 BP 3920 EP 3924 DI 10.1021/nl300775c PG 5 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 984SD UT WOS:000307211000008 PM 22800099 ER PT J AU Li, CH Chang, GQ Glenday, AG Langellier, N Zibrov, A Phillips, DF Kartner, FX Szentgyorgyi, A Walsworth, RL AF Li, Chih-Hao Chang, Guoqing Glenday, Alexander G. Langellier, Nicholas Zibrov, Alexander Phillips, David F. Kaertner, Franz X. Szentgyorgyi, Andrew Walsworth, Ronald L. TI Conjugate Fabry-Perot cavity pair for improved astro-comb accuracy SO OPTICS LETTERS LA English DT Article ID LASER FREQUENCY COMBS; SPECTROGRAPH; CALIBRATION AB We propose a new astro-comb mode-filtering scheme composed of two Fabry-Perot cavities (coined "conjugate Fabry-Perot cavity pair"). Simulations indicate that this new filtering scheme makes the accuracy of astro-comb spectral lines more robust against systematic errors induced by nonlinear processes associated with power-amplifying and spectral-broadening optical fibers. (C) 2012 Optical Society of America C1 [Li, Chih-Hao; Glenday, Alexander G.; Zibrov, Alexander; Phillips, David F.; Szentgyorgyi, Andrew; Walsworth, Ronald L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chang, Guoqing; Kaertner, Franz X.] MIT, Dept Elect Engn & Comp Sci, Cambridge, MA 02139 USA. [Chang, Guoqing; Kaertner, Franz X.] MIT, Elect Res Lab, Cambridge, MA 02139 USA. [Langellier, Nicholas; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Kaertner, Franz X.] DESY, Ctr Free Electron Laser Sci, D-22607 Hamburg, Germany. [Kaertner, Franz X.] Univ Hamburg, Dept Phys, D-22607 Hamburg, Germany. RP Li, CH (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM chli@cfa.harvard.edu FU National Science Foundation (NSF) [AST-0804441, ATI-0905214, ATI-1006503]; NASA [NNX09AC92G, NNX10AE68G] FX This work was performed with support from National Science Foundation (NSF) grants AST-0804441, ATI-0905214, and ATI-1006503; NASA grants NNX09AC92G and NNX10AE68G; and internal support from the Smithsonian Astrophysical Observatory. NR 14 TC 3 Z9 3 U1 1 U2 5 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD AUG 1 PY 2012 VL 37 IS 15 BP 3090 EP 3092 PG 3 WC Optics SC Optics GA 984XM UT WOS:000307226700028 PM 22859095 ER PT J AU Swenson, NG Erickson, DL Mi, XC Bourg, NA Forero-Montana, J Ge, XJ Howe, R Lake, JK Liu, XJ Ma, KP Pei, NC Thompson, J Uriarte, M Wolf, A Wright, SJ Ye, WH Zhang, JL Zimmerman, JK Kress, WJ AF Swenson, Nathan G. Erickson, David L. Mi, Xiangcheng Bourg, Norman A. Forero-Montana, Jimena Ge, Xuejun Howe, Robert Lake, Jeffrey K. Liu, Xiaojuan Ma, Keping Pei, Nancai Thompson, Jill Uriarte, Maria Wolf, Amy Wright, S. Joseph Ye, Wanhui Zhang, Jinlong Zimmerman, Jess K. Kress, W. John TI Phylogenetic and functional alpha and beta diversity in temperate and tropical tree communities SO ECOLOGY LA English DT Article ID MICROBIAL COMMUNITIES; EVOLUTIONARY PROCESSES; ECONOMICS SPECTRUM; PLANT-COMMUNITIES; SPECIES-RICHNESS; ASSEMBLY RULES; FOREST TREES; DRY FOREST; PATTERNS; TRAITS AB The study of biodiversity has tended to focus primarily on relatively information-poor measures of species diversity. Recently, many studies of local diversity (alpha diversity) have begun to use measures of functional and phylogenetic alpha diversity. Investigations into the phylogenetic and functional dissimilarity (beta diversity) of communities have been far less numerous, but these dissimilarity measures have the potential to infer the mechanisms underlying community assembly and dynamics. Here, we relate levels of phylogenetic and functional alpha diversity to levels of phylogenetic and functional beta diversity to infer the mechanism or mechanisms responsible for the assembly of tree communities in six forests located in tropical and temperate latitudes. The results show that abiotic filtering plays a role in structuring local assemblages and governing spatial turnover in community composition and that phylogenetic measures of alpha and beta diversity are not strong predictors of functional alpha and beta diversity in the forests studied. C1 [Swenson, Nathan G.; Lake, Jeffrey K.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Erickson, David L.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. [Mi, Xiangcheng; Liu, Xiaojuan; Ma, Keping; Zhang, Jinlong] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Bourg, Norman A.] Smithsonian Conservat Biol Inst, Ecol Grp, Front Royal, VA 22630 USA. [Forero-Montana, Jimena; Thompson, Jill; Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00936 USA. [Ge, Xuejun; Pei, Nancai; Ye, Wanhui] Chinese Acad Sci, Key Lab Plant Resource Conservat & Sustainable Ut, S China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Howe, Robert; Wolf, Amy] Univ Wisconsin, Dept Nat & Appl Sci, Green Bay, WI 54311 USA. [Pei, Nancai] Chinese Acad Forestry, Res Inst Trop Forestry, Guangzhou 510520, Guangdong, Peoples R China. [Thompson, Jill] Ctr Ecol & Hydrol Edinburgh, Penicuik EH26 0QB, Midlothian, Scotland. [Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Swenson, NG (reprint author), Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. EM swensonn@msu.edu RI Thompson, Jill/K-2200-2012; Swenson, Nathan/A-3514-2012; Uriarte, Maria/L-8944-2013; Wright, Stuart/M-3311-2013; Liu, Xiaojuan/B-4947-2017 OI Thompson, Jill/0000-0002-4370-2593; Swenson, Nathan/0000-0003-3819-9767; Wright, Stuart/0000-0003-4260-5676; FU F. H. Levinson Fund for BCI; Center for Tropical Forest Science research grant; Smithsonian Institution Global Earth Observatories (SIGEO) project; National Science Foundation [BSR-9015961, DEB-0516066, BSR-88111902, DEB-9411973, DEB-008538, DEB-0218039, DEB-0620910, 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]; Mellon Foundation; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Celera Foundation; HSBC Climate Partnership; SIGEO; Smithsonian Institution FX We thank NCEAS and their staff for computing support that made the calculations of fine-scale beta diversity possible. We also thank Jeannine Cavender-Bares, Ken Kozak, and David Ackerly for the invitation to contribute to this Special Issue. The collection of plant material for DNA sequencing and trait quantification was funded by the F. H. Levinson Fund for BCI and a Center for Tropical Forest Science research grant awarded to N. G. Swenson for Luquillo. DNA barcode sequencing and analyses for BCI and Luquillo were supported by funds from the Smithsonian Institution Global Earth Observatories (SIGEO) project. The Luquillo forest plot has been supported by National Science Foundation grants (BSR-9015961 and DEB-0516066) and from the Mellon Foundation. National Science Foundation funds to the Luquillo Long-Term Ecology Research Site (BSR-88111902, DEB-9411973, DEB-008538, DEB-0218039, and DEB-0620910) also supported this work. The BCI forest dynamics research project was made possible by 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, support from the Center for Tropical Forest Science, the Smithsonian Tropical Research Institute, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation, the Celera Foundation, and numerous private individuals, and through the hard work of over 100 people from 10 countries over the past two decades. Establishment of the SCBI plot by N. A. Bourg and W. J. McShea was funded by the HSBC Climate Partnership, SIGEO, and the Smithsonian Institution. All forest plots are part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 67 TC 57 Z9 68 U1 14 U2 203 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 AUG PY 2012 VL 93 IS 8 SU S BP S112 EP S125 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 985WY UT WOS:000307302400010 ER PT J AU Whitfeld, TJS Novotny, V Miller, SE Hrcek, J Klimes, P Weiblen, GD AF Whitfeld, Timothy J. S. Novotny, Vojtech Miller, Scott E. Hrcek, Jan Klimes, Petr Weiblen, George D. TI Predicting tropical insect herbivore abundance from host plant traits and phylogeny SO ECOLOGY LA English DT Article DE comparative methods; food webs; herbivory; Lepidoptera; lowland rain forest; New Guinea; plant defense ID LOWLAND RAIN-FOREST; PAPUA-NEW-GUINEA; HABITAT SPECIALIZATION; SPECIES COEXISTENCE; FUNCTIONAL TRAITS; DNA BARCODES; ECOLOGICAL COMMUNITIES; SUCCESSIONAL STATUS; AMAZONIAN FORESTS; FLOWERING PLANTS AB Phylogenetic ecology has identified patterns of diversity in communities that may find explanation in trophic interactions, and yet there have been few attempts to directly relate such patterns among trophic levels. Density-dependent processes involving pests and pathogens, for example, have been invoked to account for plant community phylogenetic patterns, but relatively little is known about how plant relatedness might affect community structure at other trophic levels. We examined the degree to which the abundance of herbivores in a rain forest community is explained by the phylogeny and functional traits of host plants. We destructively sampled all stems >= 5 cm diameter in two 1-ha plots of New Guinea primary and secondary lowland forest to test predicted relationships between herbivore abundance and plant resources. We analyzed per-tree caterpillar and leaf miner abundance, total leaf biomass (kg), percentage of immature foliage, specific leaf area (cm(2)/g), leaf nitrogen content (percentage of dry mass), and presence of exudates in the context of a plant community phylogeny estimated from DNA barcodes. Apart from nitrogen content and exudates, neither plant resources nor herbivore abundance showed evidence of phylogenetic signal in our community sample. The plant traits we measured could account for only 30% and 16% of variation in caterpillar and leaf miner abundance, respectively, among individual trees. Leaf biomass was a stronger predictor of herbivore abundance than either resource quality (leaf nitrogen content) or palatability (percentage of immature foliage, specific leaf area). The primary importance of resource quantity was also observed at the plant species level in analyses of species means and phylogenetic generalized least-squares regression. Plant relatedness did not account for much variation in herbivore abundance, but significant effects of exudates and leaf nitrogen content on caterpillar abundance illustrate how conserved traits at one trophic level may influence community-wide patterns at another. C1 [Whitfeld, Timothy J. S.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Novotny, Vojtech; Hrcek, Jan; Klimes, Petr] Acad Sci Czech Republic, Ctr Biol, Ceske Budejovice 37005, Czech Republic. [Novotny, Vojtech; Hrcek, Jan; Klimes, Petr] Univ S Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [Miller, Scott E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Weiblen, George D.] Univ Minnesota, Bell Museum, St Paul, MN 55108 USA. [Weiblen, George D.] Univ Minnesota, Dept Plant Biol, St Paul, MN 55108 USA. RP Whitfeld, TJS (reprint author), Univ Minnesota, Dept Forest Resources, 115 Green Hall,1530 Cleveland Ave N, St Paul, MN 55108 USA. EM whitf015@umn.edu RI Klimes, Petr/G-6823-2014; Novotny, Vojtech/G-9434-2014; Hrcek, Jan/D-7335-2015 OI Novotny, Vojtech/0000-0001-7918-8023; Hrcek, Jan/0000-0003-0711-6447 FU U.S. National Science Foundation [DEB-0515678]; Czech Science Foundation [P505/10/0673, 206/09/0115] FX We thank Jeannine Cavender-Bares, Kenneth Kozak, and David Ackerly for inviting our participation in the NCEAS ecophylogenetics working group, Robin Chazdon, Annika Moe, and Nathan Swenson for helpful criticism of the manuscript, Rebecca Montgomery for assistance with analysis, staff at the New Guinea Binatang Research Center for field assistance, Wanang landowners for access to field sites and assistance, Kipiro Damas and PNG Forest Research Institute for plant species identification, and John Kress and David Erickson of the Smithsonian Institution for plant DNA sequencing. This material is based upon work supported by the U.S. National Science Foundation under grant DEB-0515678 and the Czech Science Foundation under grants P505/10/0673 and 206/09/0115. NR 85 TC 33 Z9 33 U1 10 U2 117 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 AUG PY 2012 VL 93 IS 8 SU S BP S211 EP S222 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 985WY UT WOS:000307302400017 ER PT J AU Oliver, SJ Bock, J Altieri, B Amblard, A Arumugam, V Aussel, H Babbedge, T Beelen, A Bethermin, M Blain, A Boselli, A Bridge, C Brisbin, D Buat, V Burgarella, D Castro-Rodriguez, N Cava, A Chania, P Cirasuolo, M Clements, DL Conley, A Conversi, L Cooray, A Dowell, CD Dubois, EN Dwek, E Dye, S Eales, S Elbaz, D Farrah, D Feltre, A Ferrero, P Fiolet, N Fox, M Franceschini, A Gear, W Giovannoli, E Glenn, J Gong, Y Solares, EAG Griffin, M Halpern, M Harwit, M Hatziminaoglou, E Heinis, S Hurley, P Hwang, HS Hyde, A Ibar, E Ilbert, O Isaak, K Ivison, RJ Lagache, G Le Floc'h, E Levenson, L Lo Faro, B Lu, N Madden, S Maffei, B Magdis, G Mainetti, G Marchetti, L Marsden, G Marshall, J Mortier, AMJ Nguyen, HT O'Halloran, B Omont, A Page, MJ Panuzzo, P Papageorgiou, A Patel, H Pearson, CP Perez-Fournon, I Pohlen, M Rawlings, JI Raymond, G Rigopoulou, D Riguccini, L Rizzo, D Rodighiero, G Roseboom, IG Rowan-Robinson, M Portal, MS Schulz, B Scott, D Seymour, N Shupe, DL Smith, AJ Stevens, JA Symeonidis, M Trichas, M Tugwell, KE Vaccari, M Valtchanov, I Vieira, JD Viero, M Vigroux, L Wang, L Ward, R Wardlow, J Wright, G Xu, CK Zemcov, M AF Oliver, S. J. Bock, J. Altieri, B. Amblard, A. Arumugam, V. Aussel, H. Babbedge, T. Beelen, A. Bethermin, M. Blain, A. Boselli, A. Bridge, C. Brisbin, D. Buat, V. Burgarella, D. Castro-Rodriguez, N. Cava, A. Chania, P. Cirasuolo, M. Clements, D. L. Conley, A. Conversi, L. Cooray, A. Dowell, C. D. Dubois, E. N. Dwek, E. Dye, S. Eales, S. Elbaz, D. Farrah, D. Feltre, A. Ferrero, P. Fiolet, N. Fox, M. Franceschini, A. Gear, W. Giovannoli, E. Glenn, J. Gong, Y. Solares, E. A. Gonzalez Griffin, M. Halpern, M. Harwit, M. Hatziminaoglou, E. Heinis, S. Hurley, P. Hwang, H. S. Hyde, A. Ibar, E. Ilbert, O. Isaak, K. Ivison, R. J. Lagache, G. Le Floc'h, E. Levenson, L. Lo Faro, B. Lu, N. Madden, S. Maffei, B. Magdis, G. Mainetti, G. Marchetti, L. Marsden, G. Marshall, J. Mortier, A. M. J. Nguyen, H. T. O'Halloran, B. Omont, A. Page, M. J. Panuzzo, P. Papageorgiou, A. Patel, H. Pearson, C. P. Perez-Fournon, I. Pohlen, M. Rawlings, J. I. Raymond, G. Rigopoulou, D. Riguccini, L. Rizzo, D. Rodighiero, G. Roseboom, I. G. Rowan-Robinson, M. Portal, M. Sanchez Schulz, B. Scott, Douglas Seymour, N. Shupe, D. L. Smith, A. J. Stevens, J. A. Symeonidis, M. Trichas, M. Tugwell, K. E. Vaccari, M. Valtchanov, I. Vieira, J. D. Viero, M. Vigroux, L. Wang, L. Ward, R. Wardlow, J. Wright, G. Xu, C. K. Zemcov, M. TI The Herschel Multi-tiered Extragalactic Survey: HerMES SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE surveys; galaxies: evolution; infrared: galaxies; submillimetre: galaxies ID DEEP-FIELD-SOUTH; STAR-FORMATION HISTORY; LARGE-SCALE STRUCTURE; GOODS-N FIELD; SUBMILLIMETER-SELECTED GALAXIES; 1200-MU-M MAMBO SURVEY; MU-M OBSERVATIONS; SOURCE COUNTS; NUMBER COUNTS; INFRARED GALAXY AB The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling similar to 380?deg2. Fields range in size from 0.01 to similar to 20?deg2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500?mu m) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160?mu m), with an additional wider component of 270?deg2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100?000 galaxies at 5 sigma in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results. C1 [Oliver, S. J.; Dubois, E. N.; Farrah, D.; Hurley, P.; Roseboom, I. G.; Smith, A. J.; Wang, L.; Ward, R.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Bock, J.; Blain, A.; Bridge, C.; Cooray, A.; Dowell, C. D.; Levenson, L.; Lu, N.; Marshall, J.; Nguyen, H. T.; Schulz, B.; Shupe, D. L.; Vieira, J. D.; Viero, M.; Xu, C. K.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Bock, J.; Dowell, C. D.; Levenson, L.; Marshall, J.; Nguyen, H. T.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Altieri, B.; Amblard, A.; Conversi, L.; Portal, M. Sanchez; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Amblard, A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Amblard, A.; Arumugam, V.; Ivison, R. J.; Roseboom, I. G.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Amblard, A.; Aussel, H.; Elbaz, D.; Hwang, H. S.; Le Floc'h, E.; Magdis, G.; Riguccini, L.] Univ Paris Diderot, CE Saclay, Lab AIM Paris Saclay, F-91191 Gif Sur Yvette, France. [Babbedge, T.; Clements, D. L.; Fox, M.; Hyde, A.; Mortier, A. M. J.; O'Halloran, B.; Patel, H.; Rizzo, D.; Rowan-Robinson, M.] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England. [Beelen, A.; Bethermin, M.; Fiolet, N.; Lagache, G.] Univ Paris 11, IAS, F-91405 Orsay, France. [Amblard, A.; Beelen, A.; Bethermin, M.; Fiolet, N.; Lagache, G.] CNRS, UMR 8617, F-91405 Orsay, France. [Boselli, A.; Buat, V.; Burgarella, D.; Giovannoli, E.; Heinis, S.; Ilbert, O.] Univ Aix marseille, CNRS, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Brisbin, D.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Castro-Rodriguez, N.; Ferrero, P.; Perez-Fournon, I.] IAC, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Castro-Rodriguez, N.; Ferrero, P.; Perez-Fournon, I.] ULL, Dept Astrofis, E-38205 San Cristobal la Laguna, Tenerife, Spain. [Cava, A.] Univ Complutense Madrid, Dept Astrofis, Fac CC Fis, E-28040 Madrid, Spain. [Cirasuolo, M.; Ibar, E.; Ivison, R. J.; Wright, G.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Conley, A.; Glenn, J.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Cooray, A.; Gong, Y.; Wardlow, J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Dwek, E.] NASA, Observ Cosmol Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Dye, S.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Eales, S.; Gear, W.; Griffin, M.; Papageorgiou, A.; Pohlen, M.; Raymond, G.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, Wales. [Feltre, A.; Franceschini, A.; Lo Faro, B.; Mainetti, G.; Marchetti, L.; Rodighiero, G.; Vaccari, M.] Univ Padua, Dipartmento Astron, I-35122 Padua, Italy. [Fiolet, N.; Omont, A.; Vigroux, L.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Glenn, J.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Solares, E. A. Gonzalez] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Halpern, M.; Marsden, G.; Scott, Douglas] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Hatziminaoglou, E.] ESO, Garching, Germany. [Isaak, K.] ESTEC SRE SA, ESA Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [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, Oxford, England. [Page, M. J.; Rawlings, J. I.; Seymour, N.; Symeonidis, M.; Tugwell, K. E.] Univ Coll London, Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Pearson, C. P.; Rigopoulou, D.] Rutherford Appleton Lab, RAL Space, Chilton, England. [Pearson, C. P.] Univ Lethbridge, Inst Space Imaging Sci, Lethbridge, AB T1K 3M4, Canada. [Rigopoulou, D.] Univ Oxford, Dept Astrophys, Oxford OX1 3RH, England. [Seymour, N.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Trichas, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Oliver, SJ (reprint author), Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. RI Oliver, Seb/A-2479-2013; Magdis, Georgios/C-7295-2014; amblard, alexandre/L-7694-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Oliver, Seb/0000-0001-7862-1032; Magdis, Georgios/0000-0002-4872-2294; amblard, alexandre/0000-0002-2212-5395; Dye, Simon/0000-0002-1318-8343; Wardlow, Julie/0000-0003-2376-8971; 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; Bethermin, Matthieu/0000-0002-3915-2015; Rodighiero, Giulia/0000-0002-9415-2296; Altieri, Bruno/0000-0003-3936-0284 FU UK Science and Technology Facilities Council [ST/F002858/1, ST/I000976/1]; CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); UKSA (UK); NASA (USA) FX We acknowledge support from the UK Science and Technology Facilities Council, grant numbers ST/F002858/1 and ST/I000976/1. HCSS/HSPOT/HIPE are joint developments by the Herschel Science Ground Segment Consortium, consisting of ESA, the NASA Herschel Science Center and the HIFI, PACS and SPIRE consortia.; 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) and 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, UKSA (UK) and NASA (USA). NR 137 TC 264 Z9 263 U1 0 U2 8 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 AUG PY 2012 VL 424 IS 3 BP 1614 EP 1635 DI 10.1111/j.1365-2966.2012.20912.x PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300002 ER PT J AU Hardcastle, MJ Massaro, F Harris, DE Baum, SA Bianchi, S Chiaberge, M Morganti, R O'Dea, CP Siemiginowska, A AF Hardcastle, M. J. Massaro, F. Harris, D. E. Baum, S. A. Bianchi, S. Chiaberge, M. Morganti, R. O'Dea, C. P. Siemiginowska, A. TI The nature of the jet-driven outflow in the radio galaxy 3C 305 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: 3C 305; galaxies: ISM; galaxies: jets; X-rays: galaxies ID EMISSION-LINE NEBULAE; X-RAY; STATISTICAL PROPERTIES; INFRARED-EMISSION; GAS; KINEMATICS; SAMPLE; ABSORPTION; FEEDBACK; CLUSTERS AB We present Chandra X-ray and Very Large Array radio observations of the radio galaxy 3C?305. The X-ray observations reveal the details of the previously known extended X-ray halo around the radio galaxy. We show using X-ray spectroscopy that the X-ray emission is consistent with being shock-heated material and can be modelled with standard collisional-ionization models, rather than being photoionized by the active nucleus. On this basis, we can make a self-consistent model in which the X-ray-emitting plasma is responsible for the depolarization of some regions of the radio emission from the jets and hotspots, and to place lower and upper limits on the magnetic field strength in the depolarizing medium. On the assumption that the X-ray-emitting material, together with the previously known extended emission-line region and the outflow in neutral hydrogen, is all being driven out of the centre of the galaxy by an interaction with the jets, we derive a detailed energy budget for the radio galaxy, showing that the X-ray-emitting gas dominates the other phases in terms of its energy content. The power supplied by the jets must be similar to 1043?erg?s-1. C1 [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. [Massaro, F.; Harris, D. E.; O'Dea, C. P.; Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Massaro, F.] SLAC Natl Lab, Menlo Pk, CA 94025 USA. [Massaro, F.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Baum, S. A.] Rochester Inst Technol, Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [Baum, S. A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Bianchi, S.] Univ Roma Tre, Dipartimento Fis, I-00146 Rome, Italy. [Chiaberge, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Chiaberge, M.] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. [Chiaberge, M.] Ist Radioastron Bologna, INAF, I-40129 Bologna, Italy. [Morganti, R.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Morganti, R.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. RP Hardcastle, MJ (reprint author), Univ Hertfordshire, Sch Phys Astron & Math, Coll Lane, Hatfield AL10 9AB, Herts, England. EM m.j.hardcastle@herts.ac.uk RI Bianchi, Stefano/B-4804-2010; Massaro, Francesco/L-9102-2016; OI Bianchi, Stefano/0000-0002-4622-4240; Massaro, Francesco/0000-0002-1704-9850; Hardcastle, Martin/0000-0003-4223-1117 FU Royal Society; NASA [G01-12133A]; Fondazione Angelo Della Riccia; Foundation BLANCEFLOR Boncompagni-Ludovisi, nee Bildt FX We thank the referee, Clive Tadhunter, for constructive comments that have helped us to improve the paper. MJH thanks the Royal Society for a Research Fellowship which supported the early parts of this work. The work at SAO was supported by NASA grant G01-12133A. FM acknowledges the Fondazione Angelo Della Riccia for the grant awarded to support his research at SAO during 2011 and the Foundation BLANCEFLOR Boncompagni-Ludovisi, nee Bildt, for the grant awarded to him in 2010. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 62 TC 14 Z9 14 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 AUG PY 2012 VL 424 IS 3 BP 1774 EP 1789 DI 10.1111/j.1365-2966.2012.21247.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300013 ER PT J AU Tojeiro, R Percival, WJ Brinkmann, J Brownstein, JR Eisenstein, DJ Manera, M Maraston, C McBride, CK Muna, D Reid, B Ross, AJ Ross, NP Samushia, L Padmanabhan, N Schneider, DP Skibba, R Sanchez, AG Swanson, MEC Thomas, D Tinker, JL Verde, L Wake, DA Weaver, BA Zhao, GB AF Tojeiro, Rita Percival, Will J. Brinkmann, Jon Brownstein, Joel R. Eisenstein, Daniel J. Manera, Marc Maraston, Claudia McBride, Cameron K. Muna, Demitri Reid, Beth Ross, Ashley J. Ross, Nicholas P. Samushia, Lado Padmanabhan, Nikhil Schneider, Donald P. Skibba, Ramin Sanchez, Ariel G. Swanson, Molly E. C. Thomas, Daniel Tinker, Jeremy L. Verde, Licia Wake, David A. Weaver, Benjamin A. Zhao, Gong-Bo TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measuring structure growth using passive galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; Cosmology: observations; dark energy - large-scale structure of Universe ID DIGITAL SKY SURVEY; DARK ENERGY SURVEY; LUMINOUS RED GALAXIES; ACOUSTIC-OSCILLATIONS; COSMIC STRUCTURE; REDSHIFT SURVEY; DATA RELEASE; BIAS; SPACE; CONSTRAINTS AB We explore the benefits of using a passively evolving population of galaxies to measure the evolution of the rate of structure growth between z = 0.25 and 0.65 by combining data from the Sloan Digital Sky Survey (SDSS) I/II and SDSS-III surveys. The large-scale linear bias of a population of dynamically passive galaxies, which we select from both surveys, is easily modelled. Knowing the bias evolution breaks degeneracies inherent to other methodologies, and decreases the uncertainty in measurements of the rate of structure growth and the normalization of the galaxy power spectrum by up to a factor of 2. If we translate our measurements into a constraint on s8(z = 0) assuming a concordance cosmological model and general relativity (GR), we find that using a bias model improves our uncertainty by a factor of nearly 1.5. Our results are consistent with a flat ? cold dark matter model and with GR. C1 [Tojeiro, Rita; Percival, Will J.; Manera, Marc; Maraston, Claudia; Ross, Ashley J.; Samushia, Lado; Thomas, Daniel; Zhao, Gong-Bo] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Brinkmann, Jon] Apache Point Observ, Sunspot, NM 88349 USA. [Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Eisenstein, Daniel J.; McBride, Cameron K.; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muna, Demitri; Tinker, Jeremy L.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Reid, Beth; Ross, Nicholas P.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Padmanabhan, Nikhil; Wake, David A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Skibba, Ramin] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Verde, Licia] Univ Barcelona, ICREA, E-08028 Barcelona, Spain. [Verde, Licia] Univ Barcelona, ICC UB, E-08028 Barcelona, Spain. [Zhao, Gong-Bo] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Tojeiro, R (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England. EM rita.tojeiro@port.ac.uk OI Verde, Licia/0000-0003-2601-8770 FU European Research Council; National Science Foundation [AST-0901965]; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX RT and WJP are thankful for support from the European Research Council. MECS was supported by the National Science Foundation under Award No. AST-0901965. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 40 TC 48 Z9 48 U1 2 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 AUG PY 2012 VL 424 IS 3 BP 2339 EP 2344 DI 10.1111/j.1365-2966.2012.21404.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 982CC UT WOS:000307018300059 ER PT J AU van Putten, B Visser, MD Muller-Landau, HC Jansen, PA AF van Putten, Bram Visser, Marco D. Muller-Landau, Helene C. Jansen, Patrick A. TI Distorted-distance models for directional dispersal: a general framework with application to a wind-dispersed tree SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE anisotropic model; dispersal kernel; inverse modelling; Luehea seemannii; Matrushka property; pollen dispersal; ray-convex set; seed dispersal; seed shadow; stochastic model ID SEED DISPERSAL; POLLEN DISPERSAL; RECRUITMENT LIMITATION; ANISOTROPIC DISPERSAL; MECHANISTIC MODELS; PATTERNS; ENVIRONMENTS; FORESTS; IDENTIFICATION; CONSEQUENCES AB 1. Seed and pollen dispersal is often directionally biased, because of the inherent directionality of wind and many other dispersal vectors. Nevertheless, the vast majority of studies of seed and pollen dispersal fit isotropic dispersal kernels to data, implicitly assuming that dispersal is equally likely in all directions. 2. Here, we offer a flexible method for stochastic modelling of directional dispersal data. We show how anisotropic models can be constructed by combining standard dispersal functions with distorted-distance functions that transform the circular contour lines of any isotropic dispersal kernel into non-circular shapes. Many existing anisotropic phenomenological models of seed and pollen dispersal are special cases of our framework. 3. We present functional forms for the specific case of elliptic distorted-distance functions, under which contour lines of the seed shadow become non-concentric, nested ellipses, and show how models using these functions can be constructed and parameterized. R-code is provided. 4. We applied the elliptic anisotropic models to characterize seed dispersal in the wind-dispersed Neotropical tree Luehea seemannii (Malvaceae) on Barro Colorado Island, Panama. We used inverse modelling to fit alternative models to data of seed rain into seed traps, the locations of seed traps and adult trees, and tree size. 5. Our anisotropic model performed considerably better than commonly applied isotropic models, revealing that seed dispersal of L.similar to seemannii was strongly directional. The best-fitting model combined a 3-parameter elliptic distorted-distance function that captured the strong directional biases with a 1-parameter exponential dispersal kernel, a 1-parameter negative binomial probability distribution describing the clumping of seed rain and a 1-parameter function relating tree fecundity to tree diameter. 6. The framework presented in this paper enables more flexible and accurate modelling of directional dispersal data. It is applicable not only to studies of seed dispersal, but also to a wide range of other problems in which large numbers of particles disperse from one or more point sources. C1 [van Putten, Bram] Wageningen Univ, Math & Stat Methods Grp, NL-6700 AC Wageningen, Netherlands. [Visser, Marco D.; Muller-Landau, Helene C.; Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Visser, Marco D.] Radboud Univ Nijmegen, Dept Expt Plant Ecol, NL-6500 GL Nijmegen, Netherlands. [Jansen, Patrick A.] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. RP van Putten, B (reprint author), Wageningen Univ, Math & Stat Methods Grp, POB 100, NL-6700 AC Wageningen, Netherlands. EM bram.vanputten@wur.nl RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU Netherlands Foundation for Scientific Research [NWO-ALW 863-07-008, NWO-ALW 801-01-009]; Smithsonian Tropical Research Institute; HSBC Climate Partnership; C.T. de Wit Graduate School for Production Ecology and Resource Conservation; National Science Foundation [DEB 0614255, 0453665, 0640386, 0425651, 0346488, 0129874, 00753102, 9909347, 9615226, 9405933, 9221033, 9100058, 8906869, 8605042, 8206992, 792219]; Centre for Tropical Forest Science; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Small World Institute Fund FX We thank the Associate Editor and two anonymous referees for valuable comments that improved the manuscript. This study was supported by the Netherlands Foundation for Scientific Research (NWO-ALW 863-07-008 to PAJ; NWO-ALW 801-01-009 to MDV), the Smithsonian Tropical Research Institute (MDV), the HSBC Climate Partnership (HML) and the C.T. de Wit Graduate School for Production Ecology and Resource Conservation (HML). The case study datasets were collected with funding from the National Science Foundation (DEB 0614255, 0453665, 0640386, 0425651, 0346488, 0129874, 00753102, 9909347, 9615226, 9615226, 9405933, 9221033, 9100058, 8906869, 8605042, 8206992, 792219), the Smithsonian Tropical Research Institute, the Centre for Tropical Forest Science, the John D. and Catherine T. MacArthur Foundation, the Mellon Foundation and the Small World Institute Fund. NR 51 TC 5 Z9 6 U1 4 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD AUG PY 2012 VL 3 IS 4 BP 642 EP 652 DI 10.1111/j.2041-210X.2012.00208.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 981JA UT WOS:000306961700004 ER PT J AU Rowcliffe, JM Carbone, C Kays, R Kranstauber, B Jansen, PA AF Rowcliffe, J. Marcus Carbone, Chris Kays, Roland Kranstauber, Bart Jansen, Patrick A. TI Bias in estimating animal travel distance: the effect of sampling frequency SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE Barro Colorado Island; camera traps; daily distance; day range; movement models; radiotracking; random walk; telemetry; travel distance; tropical forest ID BIALOWIEZA-PRIMEVAL-FOREST; CORRELATED RANDOM-WALK; GPS TELEMETRY DATA; HOME RANGES; MOVEMENT DATA; BODY-SIZE; BEHAVIOR; MODELS; POLAND; ERROR AB 1. The distance travelled by animals is an important ecological variable that links behaviour, energetics and demography. It is usually measured by summing straight-line distances between intermittently sampled locations along continuous animal movement paths. The extent to which this approach underestimates travel distance remains a rarely addressed and unsolved problem, largely because true movement paths are rarely, if ever, available for comparison. Here, we use simulated movement paths parameterized with empirical movement data to study how estimates of distance travelled are affected by sampling frequency. 2. We used a novel method to obtain fine-scale characteristics of animal movement from camera trap videos for a set of tropical forest mammals and used these characteristics to generate detailed movement paths. We then sampled these paths at different frequencies, simulating telemetry studies, and quantified the accuracy of sampled travel distance estimation. 3. For our focal species, typical telemetry studies would underestimate distances travelled by 6793%, and extremely high sampling frequencies (several fixes per minute) would be required to get tolerably accurate estimates. The form of the relationship between tortuosity, sample frequency, and distance travelled was such that absolute distance cannot accurately be estimated by the infrequent samples used in typical tracking studies. 4. We conclude that the underestimation of distance travelled is a serious but underappreciated problem. Currently, there is no reliable, widely applicable method to obtain approximately unbiased estimates of distance travelled by animals. Further research on this problem is needed. C1 [Rowcliffe, J. Marcus; Carbone, Chris] ZSL Inst Zool, London NW 4RY, England. [Kays, Roland; Jansen, Patrick A.] Smithsonian Trop Res Inst, Panama City, Panama. [Kays, Roland] N Carolina Museum Nat Sci, Nat Res Ctr, Raleigh, NC 27601 USA. [Kranstauber, Bart] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Jansen, Patrick A.] Wageningen Univ, Ctr Ecosyst Studies, Wageningen, Netherlands. [Kranstauber, Bart; Jansen, Patrick A.] Univ Groningen, Ctr Ecol & Evolutionary Studies, Groningen, Netherlands. RP Rowcliffe, JM (reprint author), ZSL Inst Zool, Regents Pk, London NW 4RY, England. EM marcus.rowcliffe@ioz.ac.uk RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU NSF [DEB 0717071]; British Ecological Society; Netherlands Foundation of Scientific Research [NWO-ALW863-07-008] FX We thank Nadia Sitas, Anthony Turner, Daniel Rasmussen and Lennart Suselbeek for assistance in the field, as well as the Smithsonian Tropical Research Institute, and especially Oris Acevedo, for logistical support. We also thank four reviewers for their extremely diligent and constructive comments. Required permits for the work described in this article were obtained from the Autoridad Nacional del Ambiente, Panama, and the Smithsonian Tropical Research Institute. The work was funded by NSF (DEB 0717071) and the British Ecological Society. PAJ was funded by the Netherlands Foundation of Scientific Research (NWO-ALW863-07-008). NR 46 TC 28 Z9 28 U1 3 U2 92 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD AUG PY 2012 VL 3 IS 4 BP 653 EP 662 DI 10.1111/j.2041-210X.2012.00197.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 981JA UT WOS:000306961700005 ER PT J AU Simpson, RJ Povich, MS Kendrew, S Lintott, CJ Bressert, E Arvidsson, K Cyganowski, C Maddison, S Schawinski, K Sherman, R Smith, AM Wolf-Chase, G AF Simpson, R. J. Povich, M. S. Kendrew, S. Lintott, C. J. Bressert, E. Arvidsson, K. Cyganowski, C. Maddison, S. Schawinski, K. Sherman, R. Smith, A. M. Wolf-Chase, G. TI The Milky Way Project First Data Release: a bubblier Galactic disc SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; dust, extinction; H II regions; infrared: ISM ID H II REGIONS; TURBULENT MOLECULAR CLOUDS; MASSIVE-STAR-FORMATION; HII-REGIONS; GALAXY ZOO; INTERSTELLAR BUBBLES; INNER GALAXY; SUPERNOVA-REMNANTS; INFRARED SURVEY; MU-M AB We present a new catalogue of 5106 infrared bubbles created through visual classification via the online citizen science website The Milky Way Project. Bubbles in the new catalogue have been independently measured by at least five individuals, producing consensus parameters for their position, radius, thickness, eccentricity and position angle. Citizen scientists volunteers recruited online and taking part in this research have independently rediscovered the locations of at least 86 per?cent of three widely used catalogues of bubbles and H ii regions? whilst finding an order of magnitude more objects. 29 per cent of the Milky Way Project catalogue bubbles lie on the rim of a larger bubble, or have smaller bubbles located within them, opening up the possibility of better statistical studies of triggered star formation. Also outlined is the creation of a heat map of star formation activity in the Galactic plane. This online resource provides a crowd-sourced map of bubbles and arcs in the Milky Way, and will enable better statistical analysis of Galactic star formation sites. C1 [Simpson, R. J.; Lintott, C. J.; Smith, A. M.] Oxford Astrophys, Oxford OX1 3RH, England. [Povich, M. S.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Kendrew, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lintott, C. J.; Arvidsson, K.; Smith, A. M.; Wolf-Chase, G.] Adler Planetarium, Dept Astron, Chicago, IL 60605 USA. [Bressert, E.] ESO, D-87548 Garching, Germany. [Bressert, E.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Bressert, E.; Cyganowski, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maddison, S.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Schawinski, K.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Schawinski, K.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Sherman, R.; Wolf-Chase, G.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. RP Simpson, RJ (reprint author), Oxford Astrophys, Denys Wilkinson Bldg,Keble Rd, Oxford OX1 3RH, England. EM robert.simpson@astro.ox.ac.uk OI Bressert, Eli/0000-0002-6564-6182; Smith, Arfon/0000-0002-3957-2474; Schawinski, Kevin/0000-0001-5464-0888; Kendrew, Sarah/0000-0002-7612-0469 FU Leverhulme Trust; National Science Foundation CDI [DRL-0941610]; National Science Foundation [AST-0901646, AST-1003134]; NASA [PF9-00069, NAS8-03060]; Chandra X-ray Observatory Center FX The Milky Way Project and RJS. were supported by the Leverhulme Trust. The 'Talk' discussion tool used in the MWP was developed at the Adler Planetarium with support from the National Science Foundation CDI grant: DRL-0941610. MSP was supported by a National Science Foundation Astronomy & Astrophysics Postdoctoral Fellowship under award AST-0901646.; CJC is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003134. Support for the work of KS was provided by NASA through Einstein Postdoctoral Fellowship grant number PF9-00069 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. NR 56 TC 61 Z9 61 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 AUG PY 2012 VL 424 IS 4 BP 2442 EP 2460 DI 10.1111/j.1365-2966.2012.20770.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986ZB UT WOS:000307385100003 ER PT J AU Zhu, YC Davis, SW Narayan, R Kulkarni, AK Penna, RF McClintock, JE AF Zhu, Yucong Davis, Shane W. Narayan, Ramesh Kulkarni, Akshay K. Penna, Robert F. McClintock, Jeffrey E. TI The eye of the storm: light from the inner plunging region of black hole accretion discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; MHD; radiative transfer; methods: numerical; X-rays: binaries ID ACTIVE GALACTIC NUCLEI; 3-DIMENSIONAL MAGNETOHYDRODYNAMIC SIMULATIONS; MICROQUASAR XTE J1550-564; CONTINUUM-FITTING METHOD; MAGNETIC-FIELD GEOMETRY; RAY TRANSIENT A0620-00; CYGNUS X-1; DYNAMICAL MODEL; SLIM DISKS; HIGH-STATE AB It is generally thought that the light coming from the inner plunging region of black hole accretion discs contributes negligibly to the disc's overall spectrum, i.e. the plunging fluid is swallowed by the black hole before it has time to radiate. In the standard disc model used to fit X-ray observations of accretion discs, the plunging region is assumed to be perfectly dark. However, numerical simulations that include the full physics of the magnetized flow predict that a small fraction of the disc's total luminosity emanates from the plunging region. We investigate the observational consequences of this neglected inner light. We compute radiative-transfer-based disc spectra that correspond to 3D general relativistic magnetohydrodynamic simulated discs (which produce light inside their plunging regions). In the context of black hole spin estimation, we find that the neglected inner light only has a modest effect (this bias is less than typical observational systematic errors). For rapidly spinning black holes, we find that the combined emission from the plunging region produces a weak power-law tail at high energies. This indicates that infalling matter is the origin for some of the coronal emission observed in the thermal dominant and steep power-law states of X-ray binaries. C1 [Zhu, Yucong; Narayan, Ramesh; Kulkarni, Akshay K.; Penna, Robert F.; McClintock, Jeffrey E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Davis, Shane W.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H4, Canada. RP Zhu, YC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yzhu@cfa.harvard.edu; swd@cita.utoronto.ca; rnarayan@cfa.harvard.edu; akulkarni@cfa.harvard.edu; rpenna@cfa.harvard.edu; jem@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NSF [AST-0805832] FX The authors would like to thank Jack Steiner, Olek Sadowski and Lijun Gou for stimulating discussions and helpful suggestions. We also thank the anonymous referee for their insightful comments and feedback. We acknowledge support from NSF grant AST-0805832. The GRMHD simulations were made possible by the NSF through TeraGrid resources provided by NCSA (Abe), LONI (QueenBee) and NICS (Kraken), and by the NASA cluster Pleiades. TLUSTY spectral models were computed using the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 87 TC 39 Z9 39 U1 0 U2 5 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 AUG PY 2012 VL 424 IS 4 BP 2504 EP 2521 DI 10.1111/j.1365-2966.2012.21181.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986ZB UT WOS:000307385100008 ER PT J AU O'Sullivan, E Giacintucci, S Babul, A Raychaudhury, S Venturi, T Bildfell, C Mahdavi, A Oonk, JBR Murray, N Hoekstra, H Donahue, M AF O'Sullivan, Ewan Giacintucci, Simona Babul, Arif Raychaudhury, Somak Venturi, Tiziana Bildfell, Chris Mahdavi, Andisheh Oonk, J. B. R. Murray, Norman Hoekstra, Henk Donahue, Megan TI A Giant Metrewave Radio Telescope/Chandra view of IRAS 09104+4109: a type 2 QSO in a cooling flow SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: clusters: individual: CL 09104+4109; galaxies: individual: IRAS 09104+4109; quasars: general; radio continuum: galaxies; X-rays: galaxies: clusters ID DEEP CHANDRA OBSERVATION; ACTIVE GALACTIC NUCLEI; BRIGHTEST CLUSTER GALAXIES; X-RAY-EMISSION; BLACK-HOLES; STAR-FORMATION; JET POWER; ELLIPTIC GALAXIES; PERSEUS CLUSTER; INTERGALACTIC MEDIUM AB IRAS 09104+4109 is a rare example of a dust enshrouded type 2 quasi-stellar object (QSO) in the centre of a cool-core galaxy cluster. Previous observations of this z = 0.44 system showed that, as well as powering the hyperluminous infrared emission of the cluster-central galaxy, the QSO is associated with a double-lobed radio source. However, the steep radio spectral index and misalignment between the jets and ionized optical emission suggested that the orientation of the QSO had recently changed. We use a combination of new, multiband Giant Metrewave Radio Telescope observations and archival radio data to confirm that the jets are no longer powered by the QSO, and estimate their age to be 120-160?Myr. This is in agreement with the similar to 70-200 Myr age previously estimated for star formation in the galaxy. Previously unpublished Very Long Baseline Array data reveal a 200?pc scale double radio source in the galaxy core which is more closely aligned with the current QSO axis and may represent a more recent period of jet activity. These results suggest that the realignment of the QSO, the cessation of jet activity and the onset of rapid star formation may have been caused by a gas-rich galaxy merger. X-ray observations reveal a spiral structure in the intracluster medium (ICM) which suggests that the cluster is in the process of relaxation after a tidal encounter or merger with another system; such a merger could provide a mechanism for transporting a gas-rich galaxy into the cluster core without stripping its cold gas. A Chandra X-ray observation confirms the presence of cavities associated with the radio jets, and we estimate the energy required to inflate them to be similar to 7.7 x1060?erg. The mechanical power of the jets is sufficient to balance radiative cooling in the cluster, provided that they are efficiently coupled to the ICM. We find no evidence of direct radiative heating and conclude that the QSO either lacks the radiative luminosity to heat the ICM, or that it requires longer than 100-200?Myr to significantly impact its environment. C1 [O'Sullivan, Ewan; Raychaudhury, Somak] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [O'Sullivan, Ewan] Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, W Midlands, England. [Giacintucci, Simona] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, Simona] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. [Babul, Arif; Bildfell, Chris] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. [Venturi, Tiziana] Ist Radioastron, INAF, I-40129 Bologna, Italy. [Mahdavi, Andisheh] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94131 USA. [Oonk, J. B. R.] Netherlands Inst Radio Astron ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Murray, Norman] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Hoekstra, Henk] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Donahue, Megan] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. RP O'Sullivan, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ejos@star.sr.bham.ac.uk OI O'Sullivan, Ewan/0000-0002-5671-6900; Venturi, Tiziana/0000-0002-8476-6307; Babul, Arif/0000-0003-1746-9529; Hoekstra, Henk/0000-0002-0641-3231 FU European Community under the Marie Curie Research Training Network; Chandra Award number [AR1-12014X]; NASA through Einstein Postdoctoral Fellowship [PF0-110071]; Chandra X-ray Center (CXC); NSERC through the Discovery Grant program; [GO9-0143X] FX The authors thank the anonymous referee for their comments, which have improved the paper. We also thank D. Dallacasa, T. Clarke, G. Brunetti, A.J.R. Sanderson and D.J. Burke for useful discussions of the data and analysis, A. Siemiginowska for comments on the paper, and J. Hlavacek-Larrondo for providing her estimates of cavity location. E. O'Sullivan acknowledges support from the European Community under the Marie Curie Research Training Network and from Chandra Award number AR1-12014X. S. Giacintucci acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center (CXC), which is operated by the Smithsonian Astrophysical Observatory (SAO). AB and CB would like to acknowledge support from NSERC through the Discovery Grant program. AB also acknowledges the hospitality extended to him by the Astrophysics and Space Research Group at the University of Birmingham in 2011. MD acknowledges the support of a Chandra GO grant GO9-0143X. Chandra observation ObsID 10445 was proposed by K. Cavagnolo (now at 3B Scientific in Atlanta, GA), MD and G.M. Voit. MD acknowledges discussions with B. McNamara. 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. We would also like to thank the Lorentz Center in Leiden for hospitality and support during 2011 July during which time the present study was planned. We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 141 TC 18 Z9 18 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 AUG PY 2012 VL 424 IS 4 BP 2971 EP 2993 DI 10.1111/j.1365-2966.2012.21459.x PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986ZB UT WOS:000307385100047 ER PT J AU Sijacki, D Vogelsberger, M Keres, D Springel, V Hernquist, L AF Sijacki, Debora Vogelsberger, Mark Keres, Dusan Springel, Volker Hernquist, Lars TI Moving mesh cosmology: the hydrodynamics of galaxy formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: numerical; galaxies: formation; cosmology: theory ID SMOOTHED-PARTICLE HYDRODYNAMICS; GENERAL-RELATIVISTIC MAGNETOHYDRODYNAMICS; STAR-FORMATION; DARK-MATTER; CLUSTER MERGERS; SIMULATIONS; GAS; ENTROPY; SPH; QUASARS AB We present a detailed comparison between the well-known smoothed particle hydrodynamics (SPH) code gadget and the new moving-mesh code arepo on a number of hydrodynamical test problems. Through a variety of numerical experiments with increasing complexity we establish a clear link between simple test problems with known analytic solutions and systematic numerical effects seen in cosmological simulations of galaxy formation. Our tests demonstrate deficiencies of the SPH method in several sectors. These accuracy problems not only manifest themselves in idealized hydrodynamical tests, but also propagate to more realistic simulation set-ups of galaxy formation, ultimately affecting local and global gas properties in the full cosmological framework, as highlighted in companion papers by Vogelsberger et al. and Keres et al. We find that an inadequate treatment of fluid instabilities in gadget suppresses entropy generation by mixing, underestimates vorticity generation in curved shocks and prevents efficient gas stripping from infalling substructures. Moreover, in idealized tests of inside-out disc formation, the convergence rate of gas disc sizes is much slower in gadget due to spurious angular momentum transport. In simulations where we follow the interaction between a forming central disc and orbiting substructures in a massive halo, the final disc morphology is strikingly different in the two codes. In arepo, gas from infalling substructures is readily depleted and incorporated into the host halo atmosphere, facilitating the formation of an extended central disc. Conversely, gaseous sub-clumps are more coherent in gadget simulations, morphologically transforming the central disc as they impact it. The numerical artefacts of the SPH solver are particularly severe for poorly resolved flows, and thus inevitably affect cosmological simulations due to their inherently hierarchical nature. Taken together, our numerical experiments clearly demonstrate that arepo delivers a physically more reliable solution. C1 [Sijacki, Debora; Vogelsberger, Mark; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif San Diego, Ctr Astrophys & Space Sci, Dept Phys, La Jolla, CA 92093 USA. [Springel, Volker] Heidelberg Inst Theoret Studies, D-69118 Heidelberg, Germany. [Springel, Volker] Univ Heidelberg, ARI, Zentrum Astron, D-69120 Heidelberg, Germany. RP Sijacki, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dsijacki@cfa.harvard.edu FU NASA Hubble Fellowship [HST-HF-51282.01-A, HST-HF-51276.01-A]; FAS Science Division Research Computing Group at Harvard University FX We would like to thank Andrew MacFadyen and Daniel Eisenstein for very useful discussions and suggestions on the topic, and Manfred Kitzbichler and Diego Munoz for carefully reading the manuscript. We would like to thank the anonymous referee for many constructive suggestions, which helped to improve the presentation of the results. DS acknowledges NASA Hubble Fellowship through grant HST-HF-51282.01-A. DK acknowledges NASA Hubble Fellowship through grant HST-HF-51276.01-A. The computations in this paper were performed on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. NR 69 TC 92 Z9 92 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 AUG PY 2012 VL 424 IS 4 BP 2999 EP 3027 DI 10.1111/j.1365-2966.2012.21466.x PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986ZB UT WOS:000307385100049 ER PT J AU Wilson, CD Warren, BE Israel, FP Serjeant, S Attewell, D Bendo, GJ Butner, HM Chanial, P Clements, DL Golding, J Heesen, V Irwin, J Leech, J Matthews, HE Muhle, S Mortier, AMJ Petitpas, G Sanchez-Gallego, JR Sinukoff, E Shorten, K Tan, BK Tilanus, RPJ Usero, A Vaccari, M Wiegert, T Zhu, M Alexander, DM Alexander, P Azimlu, M Barmby, P Brar, R Bridge, C Brinks, E Brooks, S Coppin, K Cote, S Cote, P Courteau, S Davies, J Eales, S Fich, M Hudson, M Hughes, DH Ivison, RJ Knapen, JH Page, M Parkin, TJ Rigopoulou, D Rosolowsky, E Seaquist, ER Spekkens, K Tanvir, N van der Hulst, JM van der Werf, P Vlahakis, C Webb, TM Weferling, B White, GJ AF Wilson, C. D. Warren, B. E. Israel, F. P. Serjeant, S. Attewell, D. Bendo, G. J. Butner, H. M. Chanial, P. Clements, D. L. Golding, J. Heesen, V. Irwin, J. Leech, J. Matthews, H. E. Muhle, S. Mortier, A. M. J. Petitpas, G. Sanchez-Gallego, J. R. Sinukoff, E. Shorten, K. Tan, B. K. Tilanus, R. P. J. Usero, A. Vaccari, M. Wiegert, T. Zhu, M. Alexander, D. M. Alexander, P. Azimlu, M. Barmby, P. Brar, R. Bridge, C. Brinks, E. Brooks, S. Coppin, K. Cote, S. Cote, P. Courteau, S. Davies, J. Eales, S. Fich, M. Hudson, M. Hughes, D. H. Ivison, R. J. Knapen, J. H. Page, M. Parkin, T. J. Rigopoulou, D. Rosolowsky, E. Seaquist, E. R. Spekkens, K. Tanvir, N. van der Hulst, J. M. van der Werf, P. Vlahakis, C. Webb, T. M. Weferling, B. White, G. J. TI The JCMT Nearby Galaxies Legacy Survey - VIII. CO data and the LCO(3-2)-LFIR correlation in the SINGS sample SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE stars: formation; ISM: molecules; galaxies: ISM; galaxies: kinematics and dynamics; galaxies: spiral ID LUMINOUS INFRARED GALAXIES; HUBBLE-SPACE-TELESCOPE; WARM MOLECULAR GAS; STAR-FORMATION LAW; LOW-METALLICITY ENVIRONMENTS; SPECTRAL ENERGY-DISTRIBUTION; CO-TO-H-2 CONVERSION FACTOR; SPIRAL GALAXIES; VIRGO CLUSTER; INTERSTELLAR-MEDIUM AB The James Clerk Maxwell Telescope Nearby Galaxies Legacy Survey (NGLS) comprises an H?i-selected sample of 155 galaxies spanning all morphological types with distances less than 25?Mpc. We describe the scientific goals of the survey, the sample selection and the observing strategy. We also present an atlas and analysis of the CO J=3 - 2 maps for the 47 galaxies in the NGLS which are also part of the Spitzer Infrared Nearby Galaxies Survey. We find a wide range of molecular gas mass fractions in the galaxies in this sample and explore the correlation of the far-infrared luminosity, which traces star formation, with the CO luminosity, which traces the molecular gas mass. By comparing the NGLS data with merging galaxies at low and high redshift, which have also been observed in the CO J=3 - 2 line, we show that the correlation of far-infrared and CO luminosity shows a significant trend with luminosity. This trend is consistent with a molecular gas depletion time which is more than an order of magnitude faster in the merger galaxies than in nearby normal galaxies. We also find a strong correlation of the LFIR/LCO(3-2) ratio with the atomic-to-molecular gas mass ratio. This correlation suggests that some of the far-infrared emission originates from dust associated with atomic gas and that its contribution is particularly important in galaxies where most of the gas is in the atomic phase. C1 [Wilson, C. D.; Warren, B. E.; Attewell, D.; Golding, J.; Sinukoff, E.; Shorten, K.; Brooks, S.; Parkin, T. J.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Warren, B. E.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Israel, F. P.; van der Werf, P.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Serjeant, S.; White, G. J.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Bendo, G. J.] Univ Manchester, UK ALMA Reg Ctr Node, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England. [Butner, H. M.] James Madison Univ, Dept Phys & Astron, Harrisonburg, VA 22807 USA. [Chanial, P.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA DSM Irfu, CNRS,CE Saclay, F-91191 Gif Sur Yvette, France. [Clements, D. L.; Page, M.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Heesen, V.; Brinks, E.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Irwin, J.; Brar, R.; Courteau, S.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON K7L 3N6, Canada. [Leech, J.; Tan, B. K.; Rigopoulou, D.] Univ Oxford, Oxford OX1 3RH, England. [Matthews, H. E.] Natl Res Council Canada, Herzberg Inst Astrophys, DRAO, Penticton, BC V2A 69J, Canada. [Muhle, S.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Mortier, A. M. J.] Univ Edinburgh, Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Petitpas, G.; Azimlu, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sanchez-Gallego, J. R.; Knapen, J. H.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. [Sanchez-Gallego, J. R.; Knapen, J. H.] Univ La Laguna, Dept Astrofis, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Tilanus, R. P. J.; Weferling, B.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. [Usero, A.] Observ Madrid, OAN, E-28014 Madrid, Spain. [Vaccari, M.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Bellville, Cape Town, South Africa. [Wiegert, T.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Zhu, M.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Alexander, P.] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England. [Alexander, P.] Kavli Inst Cosmol Cambridge, Cambridge CB3 0HA, England. [Azimlu, M.; Barmby, P.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Bridge, C.] CALTECH, Pasadena, CA 91125 USA. [Coppin, K.; Webb, T. M.] McGill Univ, Dept Phys, Montreal, PQ H2A 2T8, Canada. [Cote, S.; Cote, P.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Davies, J.; Eales, S.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Fich, M.; Hudson, M.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Hughes, D. H.] INAOE, Puebla 72000, Mexico. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rigopoulou, D.] Rutherford Appleton Lab, RALSpace, Didcot OX11 0NL, Oxon, England. [Rosolowsky, E.; White, G. J.] Univ British Columbia, Kelowna, BC V1V 1V7, Canada. [Seaquist, E. R.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Spekkens, K.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [Tanvir, N.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [van der Hulst, J. M.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Vlahakis, C.] Joint ALMA Off, Santiago, Chile. RP Wilson, CD (reprint author), McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. EM wilson@physics.mcmaster.ca RI Hudson, Michael/H-3238-2012; Barmby, Pauline/I-7194-2016; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; OI Hudson, Michael/0000-0002-1437-3786; Barmby, Pauline/0000-0003-2767-0090; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Alexander, David/0000-0002-5896-6313 FU NSERC (Canada); UK Science and Technology Facilities Council; ALMA-CONICYT Fund for the Development of Chilean Astronomy [31090013]; Center of Excellence in Astrophysics and Associated Technologies [PBF 06]; National Aeronautics and Space Administration FX The James Clerk Maxwell Telescope is operated by The Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research and the National Research Council of Canada. The research of PB, PC, S. Courteau, MF, MH, JI,ER, ES, KS, TW and CDW is supported by grants from NSERC (Canada). AU has been supported through a Post Doctoral Research Assistantship from the UK Science and Technology Facilities Council. Travel support for BEW and TW was supplied by the National Research Council (Canada). We acknowledge the usage of the HyperLeda data base (http://leda.univ-lyon1.fr). CV received support from the ALMA-CONICYT Fund for the Development of Chilean Astronomy (Project 31090013) and from the Center of Excellence in Astrophysics and Associated Technologies (PBF 06). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 117 TC 24 Z9 24 U1 1 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 AUG PY 2012 VL 424 IS 4 BP 3050 EP 3080 DI 10.1111/j.1365-2966.2012.21453.x PG 31 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986ZB UT WOS:000307385100052 ER PT J AU Cygan, RT Post, JE Heaney, PJ Kubicki, JD AF Cygan, Randall T. Post, Jeffrey E. Heaney, Peter J. Kubicki, James D. TI Molecular models of birnessite and related hydrated layered minerals SO AMERICAN MINERALOGIST LA English DT Article DE Birnessite; rancieite; manganese; interlayer; water; hydration; molecular dynamics; DFT ID X-RAY-DIFFRACTION; CRYSTAL-STRUCTURE DETERMINATIONS; TOTAL-ENERGY CALCULATIONS; EFFECTIVE IONIC-RADII; AUGMENTED-WAVE METHOD; MANGANESE OXIDE; DYNAMICS SIMULATION; COMPUTER-SIMULATIONS; SYNTHETIC BIRNESSITE; SURFACE COMPLEXATION AB Birnessite and other charged layered manganese oxide minerals exhibit interlayers with variable cation-water behavior that controls many environmentally important cation exchange, adsorption, and redox processes. The occurrence of birnessite phases as fine-grained materials with corresponding high-surface areas makes them effective in controlling soil sediment and groundwater compositions, but difficult to structurally characterize using conventional analytical methods. Molecular simulations provide an alternative approach in which many details of bulk and interlayer structure can be ascertained to supplement and interpret the experimental findings. Classical and electronic structure methods are used to evaluate Na-, K-, and Ba-birnessite phases. Computational results compare favorably with structures obtained by synchrotron X-ray diffraction and difference electron Fourier mapping of the interlayer region. Based on the analysis of the 1 ns atomic trajectories, dynamics of water molecules is enhanced in the interlayer of K-birnessite relative to the limited motion of water molecules and cations in the other birnessite phases. Molecular dynamics simulations of rancieite, a complex layered manganese oxide having octahedral vacancies, indicate multiple sites for Ca2+ in the interlayer. In addition to manganese layer charge and layer structure, the hydration enthalpy for the interlayer cation affects the structure and dynamics of the interlayer in birnessite minerals. C1 [Cygan, Randall T.] Sandia Natl Labs, Dept Geochem, Albuquerque, NM 87185 USA. [Post, Jeffrey E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Heaney, Peter J.; Kubicki, James D.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. RP Cygan, RT (reprint author), Sandia Natl Labs, Dept Geochem, POB 5800, Albuquerque, NM 87185 USA. EM rtcygan@sandia.gov RI Kubicki, James/I-1843-2012 OI Kubicki, James/0000-0002-9277-9044 FU Geosciences Research Program of the U.S. Department of Energy, Office of Basic Energy Sciences; U.S. Department of Energy's National Nuclear Security Administration [DE-AC04-94AL85000]; NSF [EAR07-45374]; Center for Environmental Kinetics (CEKA), an NSF-DOE environmental molecular sciences institute [CHE-0431328] FX The authors acknowledge the expertise of Justin Durkin in the analysis of the many gigabytes of data associated with the MD trajectories. The senior author is grateful for the funding and long-term support provided by the Geosciences Research Program of the U.S. Department of Energy, Office of Basic Energy Sciences. Sandia National Laboratories is a multi-program laboratory managed and operated by Sandia Corporation, a wholly owned subsidiary of Lockheed Martin Corporation, for the U.S. Department of Energy's National Nuclear Security Administration under contract DE-AC04-94AL85000. Jeffrey Post and Peter Heaney were supported by funds from NSF grant EAR07-45374. James Kubicki was supported by the Center for Environmental Kinetics (CEKA, CHE-0431328), an NSF-DOE environmental molecular sciences institute. Computational support for DFT calculations was provided by CEKA and the Research and Cyberinfrastructure Center at The Pennsylvania State University. NR 63 TC 12 Z9 12 U1 8 U2 64 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 AUG-SEP PY 2012 VL 97 IS 8-9 BP 1505 EP 1514 DI 10.2138/am.2012.3957 PG 10 WC Geochemistry & Geophysics; Mineralogy SC Geochemistry & Geophysics; Mineralogy GA 987KF UT WOS:000307415100027 ER PT J AU Zimbelman, JR Williams, SH Johnston, AK AF Zimbelman, James R. Williams, Steven H. Johnston, Andrew K. TI Cross-sectional profiles of sand ripples, megaripples, and dunes: a method for discriminating between formational mechanisms SO EARTH SURFACE PROCESSES AND LANDFORMS LA English DT Article DE topography; sand ripples; granule ripples; megaripples; reversing dune; transverse dunes ID TRANSVERSE AEOLIAN RIDGES; SEDIMENT TRANSPORT; REVERSING DUNE; SILVER PEAK; EOLIAN SAND; AIR-FLOW; WIND; MARS; MODEL; BEDFORMS AB Cross-sectional profiles of sand ripples, megaripples, and sand dunes provide a useful tool for discriminating between formation by ripple and dune processes. Feature width, defined as the basal break in slope along the profile to either side of the crest, represents a good standard for comparison of profile attributes across more than three orders of magnitude. Aspect ratio (height/width) as a function of log width separates measurements into clusters representing differing mechanisms of formation. Scaling both height and distance for individual profiles by feature width facilitates comparison of profile shapes across three orders of magnitude in width. The data presented here should prove useful for evaluating possible mechanisms of origin for aeolian features observed remotely, including on planetary bodies. Copyright (c) 2012 John Wiley & Sons, Ltd. C1 [Zimbelman, James R.; Johnston, Andrew K.] Smithsonian Inst, CEPS, NASM, Washington, DC 20013 USA. [Williams, Steven H.] Smithsonian Inst, Natl Air & Space Museum, Educ Div, Washington, DC 20013 USA. RP Zimbelman, JR (reprint author), Smithsonian Inst, CEPS, NASM, MRC 315, Washington, DC 20013 USA. EM zimbelmanj@si.edu FU Becker and Walcott portions of the Smithsonian Endowments; NASA [NNX08AK90G] FX This work was supported primarily by funds from the Becker and Walcott portions of the Smithsonian Endowments. Additional support for some of the work came from NASA Mars Data Analysis Program grant NNX08AK90G. Comments by M. Balme, an anonymous reviewer, and the special issue Editor were very helpful during revision of this manuscript. NR 54 TC 9 Z9 9 U1 1 U2 21 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0197-9337 J9 EARTH SURF PROC LAND JI Earth Surf. Process. Landf. PD AUG PY 2012 VL 37 IS 10 BP 1120 EP 1125 DI 10.1002/esp.3243 PG 6 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 983LU UT WOS:000307121600009 ER PT J AU Gingerich, O AF Gingerich, Owen TI The Cambridge Photographic Star Atlas SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 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 AUG PY 2012 VL 43 BP 359 EP 359 PN 3 PG 1 WC History & Philosophy Of Science SC History & Philosophy of Science GA 980HC UT WOS:000306883200008 ER PT J AU Vandersea, MW Kibler, SR Holland, WC Tester, PA Schultz, TF Faust, MA Holmes, MJ Chinain, M Litaker, RW AF Vandersea, Mark W. Kibler, Steven R. Holland, William C. Tester, Patricia A. Schultz, Thomas F. Faust, Maria A. Holmes, Michael J. Chinain, Mirelle Litaker, R. Wayne TI DEVELOPMENT OF SEMI-QUANTITATIVE PCR ASSAYS FOR THE DETECTION AND ENUMERATION OF GAMBIERDISCUS SPECIES (GONYAULACALES, DINOPHYCEAE) SO JOURNAL OF PHYCOLOGY LA English DT Article DE qPCR; ciguatera; Gambierdiscus belizeanus; Gambierdiscus caribaeus; Gambierdiscus carolinianus; Gambierdiscus carpenteri; Gambierdiscus ruetzleri; Gambierdiscus ribotype 2; SYBR green ID REAL-TIME PCR; SP-NOV; DINOFLAGELLATE GAMBIERDISCUS; TOXIC DINOFLAGELLATE; CIGUATERA; QUANTIFICATION; SAMPLES; WATER; OCEAN AB Ciguatera fish poisoning (CFP) is a serious health problem in tropical regions and is caused by the bioaccumulation of lipophilic toxins produced by dinoflagellates in the genus Gambierdiscus. Gambierdiscus species are morphologically similar and are difficult to distinguish from one another even when using scanning electron microscopy. Improved identification and detection methods that are sensitive and rapid are needed to identify toxic species and investigate potential distribution and abundance patterns in relation to incidences of CFP. This study presents the first species-specific, semi-quantitative polymerase chain reaction (qPCR) assays that can be used to address these questions. These assays are specific for five Gambierdiscus species and one undescribed ribotype. The assays utilized a SYBR green format and targeted unique sequences found within the SSU, ITS, and the D1/D3 LSU ribosomal domains. Standard curves were constructed using known concentrations of cultured cells and 10-fold serial dilutions of rDNA PCR amplicons containing the target sequence for each specific assay. Assay sensitivity and accuracy were tested using DNA extracts purified from known concentrations of multiple Gambierdiscus species. The qPCR assays were used to assess Gambierdiscus species diversity and abundance in samples collected from nearshore areas adjacent to Ft. Pierce and Jupiter, Florida USA. The results indicated that the practical limit of detection for each assay was 10 cells per sample. Most interestingly, the qPCR analysis revealed that as many as four species of Gambierdiscus were present in a single macrophyte sample. C1 [Vandersea, Mark W.; Kibler, Steven R.; Holland, William C.; Tester, Patricia A.] NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. [Schultz, Thomas F.] Duke Univ, Marine Lab, Marine Conservat Mol Facil, Nicholas Sch Environm, Beaufort, NC 28516 USA. [Faust, Maria A.] Smithsonian Inst, Dept Bot, US Natl Herbarium, Natl Museum Nat Hist, Suitland, MD 20746 USA. [Holmes, Michael J.] Natl Univ Singapore, Trop Marine Sci Inst, Singapore 119223, Singapore. [Holmes, Michael J.] Aquat Ecosyst Hlth, Dept Environm & Resource Management, Brisbane, Qld 4001, Australia. [Litaker, R. Wayne] NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, Beaufort, NC 28516 USA. RP Vandersea, MW (reprint author), NOAA, NOS, Ctr Coastal Fisheries & Habitat Res, 101 Pivers Isl Rd, Beaufort, NC 28516 USA. EM mark.w.vandersea@noaa.gov OI Schultz, Thomas/0000-0001-9694-9920 FU NOAA's Center for Sponsored Coastal Ocean Research, Ecology and Oceanography of Harmful Algal Bloom Program; Smithsonian Institution Caribbean Coral Reef Ecosystem Program (CCRE); Smithsonian Institution Hunterdon Oceanographic Research Endownment; NOAA FX We thank Valerie Paul, Sherry Reed, and William Lee at the Smithsonian Marine Station at Fort Pierce for their support. Rance Hardison is kindly acknowledged for helping to conduct the multisizer cell enumerations. We also thank three anonymous reviewers for their constructive, critical reviews of this manuscript. Reference to tradenames does not imply product endorsement by the National Ocean Service, NOAA. This work was partially supported by a grant from NOAA's Center for Sponsored Coastal Ocean Research, Ecology and Oceanography of Harmful Algal Bloom Program. ECOHAB contribution number 671. Support for the research also came from grants provided by the Smithsonian Institution Caribbean Coral Reef Ecosystem Program (CCRE), the Smithsonian Institution Hunterdon Oceanographic Research Endownment and NOAA program funds. NR 34 TC 16 Z9 17 U1 4 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-3646 J9 J PHYCOL JI J. Phycol. PD AUG PY 2012 VL 48 IS 4 BP 902 EP 915 DI 10.1111/j.1529-8817.2012.01146.x PG 14 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 982BM UT WOS:000307016700008 PM 27009001 ER PT J AU Hong, T AF Hong, Terry TI Ru. 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 AUG PY 2012 VL 137 IS 13 BP 89 EP 89 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 990CD UT WOS:000307607700138 ER PT J AU Chang, D Duda, TF AF Chang, Dan Duda, Thomas F., Jr. TI Extensive and Continuous Duplication Facilitates Rapid Evolution and Diversification of Gene Families SO MOLECULAR BIOLOGY AND EVOLUTION LA English DT Article DE duplication; rapid evolution; Conus; species interaction; gene turnover ID NICOTINIC ACETYLCHOLINE-RECEPTOR; MAXIMUM-LIKELIHOOD; TREE RECONSTRUCTION; MOLECULAR EVOLUTION; DIFFERENTIAL LOSS; GASTROPOD CONUS; VENOM EVOLUTION; SELECTION; CONOTOXIN; MODEL AB The origin of novel gene functions through gene duplication, mutation, and natural selection represents one of the mechanisms by which organisms diversify and one of the possible paths leading to adaptation. Nonetheless, the extent, role, and consequences of duplications in the origins of ecological adaptations, especially in the context of species interactions, remain unclear. To explore the evolution of a gene family that is likely linked to species associations, we investigated the evolutionary history of the A-superfamily of conotoxin genes of predatory marine cone snails (Conus species). Members of this gene family are expressed in the venoms of Conus species and are presumably involved in predator-prey associations because of their utility in prey capture. We recovered sequences of this gene family from genomic DNA of four closely related species of Conus and reconstructed the evolutionary history of these genes. Our study is the first to directly recover conotoxin genes from Conus genomes to investigate the evolution of conotoxin gene families. Our results revealed a phenomenon of rapid and continuous gene turnover that is coupled with heightened rates of evolution. This continuous duplication pattern has not been observed previously, and the rate of gene turnover is at least two times higher than estimates from other multigene families. Conotoxin genes are among the most rapidly evolving protein-coding genes in metazoans, a phenomenon that may be facilitated by extensive gene duplications and have driven changes in conotoxin functions through neofunctionalization. Together these mechanisms led to dramatically divergent arrangements of A-superfamily conotoxin genes among closely related species of Conus. Our findings suggest that extensive and continuous gene duplication facilitates rapid evolution and drastic divergence in venom compositions among species, processes that may be associated with evolutionary responses to predator-prey interactions. C1 [Chang, Dan; Duda, Thomas F., Jr.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Chang, Dan; Duda, Thomas F., Jr.] Univ Michigan, Museum Zool, Ann Arbor, MI 48109 USA. [Chang, Dan] Univ Michigan, Dept Stat, Ann Arbor, MI 48109 USA. [Duda, Thomas F., Jr.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Chang, D (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. EM changdan@umich.edu FU University of Michigan Rackham Graduate School; Rackham/Department of Ecology and Evolutionary; National Science Foundation [IOS-0718379] FX We thank Jon-Paul Bingham (University of Hawaii) for providing C. quercinus specimens. We thank David A. Roberts for his help with simulations. We acknowledge Jianzhi Zhang, Alex S. Kondrashov, Taehwan Lee, and Celia K. C. Churchill for their suggestions on the manuscript. We thank the three anonymous reviewers and the associate editor Todd Oakley for their valuable suggestions and comments. This work was supported by funds from the University of Michigan Rackham Graduate School and a Rackham/Department of Ecology and Evolutionary Block Grant awarded to Dan Chang and a National Science Foundation award (IOS-0718379) to Thomas F. Duda Jr. The authors declare no competing financial interests. NR 80 TC 48 Z9 49 U1 1 U2 39 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 AUG PY 2012 VL 29 IS 8 BP 2019 EP 2029 DI 10.1093/molbev/mss068 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 984EA UT WOS:000307171300012 PM 22337864 ER PT J AU Balunas, MJ Pavlik, CM Wong, CYB Lopez, DD Engene, N McPhail, K Gerwick, WH AF Balunas, M. J. Pavlik, C. M. Wong, C. Y. B. Lopez, D. D. Engene, N. McPhail, K. Gerwick, W. H. TI Discovery and development of Santacruzamate A, a potent and selective histone deacetylase inhibitor SO PLANTA MEDICA LA English DT Meeting Abstract CT International Congress on Natural Products Research on Global Change, Natural Products and Human Health/8th Joint Meeting of AFERP, ASP, GA, PSE and SIF CY JUL 28-AUG 01, 2012 CL New York, NY SP Amer Soc Pharmacognosy (ASP), Soc Med Plant & Nat Prod Res (GA), Italian Soc Phytochem (SIF), Phytochem Soc Europe (PSE), French Speaking Soc Pharmacognosy (AFERP) C1 [Balunas, M. J.; Pavlik, C. M.] Univ Connecticut, Dept Pharmaceut Sci, Div Med Chem, Storrs, CT USA. [Balunas, M. J.; Engene, N.; Gerwick, W. H.] Univ Calif San Diego, Ctr Marine Biotechnol & Biomed, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Balunas, M. J.; Gerwick, W. H.] Smithsonian Trop Res Inst, Panama City, Panama. [Balunas, M. J.; Wong, C. Y. B.; Lopez, D. D.] INDICASAT, Panama City, Panama. [McPhail, K.] Oregon State Univ, Coll Pharm, Corvallis, OR 97331 USA. NR 0 TC 0 Z9 0 U1 0 U2 9 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD AUG PY 2012 VL 78 IS 11 BP 1050 EP 1050 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 982KT UT WOS:000307042800076 ER PT J AU Salvador, LA Taori, K Ostrov, D Biggs, JS Paul, VJ Luesch, H AF Salvador, L. A. Taori, K. Ostrov, D. Biggs, J. S. Paul, V. J. Luesch, H. TI Novel elastase inhibitors from marine cyanobacteria: Structural diversity, target-bound crystal structures and cellular effects SO PLANTA MEDICA LA English DT Meeting Abstract CT International Congress on Natural Products Research on Global Change, Natural Products and Human Health/8th Joint Meeting of AFERP, ASP, GA, PSE and SIF CY JUL 28-AUG 01, 2012 CL New York, NY SP Amer Soc Pharmacognosy (ASP), Soc Med Plant & Nat Prod Res (GA), Italian Soc Phytochem (SIF), Phytochem Soc Europe (PSE), French Speaking Soc Pharmacognosy (AFERP) C1 [Salvador, L. A.; Taori, K.; Luesch, H.] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Ostrov, D.] Univ Florida, Dept Pathol Immunol & Lab Med, Gainesville, FL 32610 USA. [Biggs, J. S.] Univ Guam, Marine Lab, UOG Stn, Mangilao, GU 96923 USA. [Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. NR 0 TC 0 Z9 0 U1 0 U2 2 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD AUG PY 2012 VL 78 IS 11 BP 1058 EP 1058 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 982KT UT WOS:000307042800107 ER PT J AU Montaser, R Paul, VJ Luesch, H AF Montaser, R. Paul, V. J. Luesch, H. TI Chemistry and biology of novel cyanobacterial secondary metabolites from Guam SO PLANTA MEDICA LA English DT Meeting Abstract CT International Congress on Natural Products Research on Global Change, Natural Products and Human Health/8th Joint Meeting of AFERP, ASP, GA, PSE and SIF CY JUL 28-AUG 01, 2012 CL New York, NY SP Amer Soc Pharmacognosy (ASP), Soc Med Plant & Nat Prod Res (GA), Italian Soc Phytochem (SIF), Phytochem Soc Europe (PSE), French Speaking Soc Pharmacognosy (AFERP) C1 [Montaser, R.; Luesch, H.] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD AUG PY 2012 VL 78 IS 11 BP 1148 EP 1148 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 982KT UT WOS:000307042800518 ER PT J AU Tidgewell, K Moy, J Herrera, L Spadafora, C Gerwick, WH AF Tidgewell, K. Moy, J. Herrera, L. Spadafora, C. Gerwick, W. H. TI Secondary metabolites from Panamanian mat forming cyanobacteria SO PLANTA MEDICA LA English DT Meeting Abstract CT International Congress on Natural Products Research on Global Change, Natural Products and Human Health/8th Joint Meeting of AFERP, ASP, GA, PSE and SIF CY JUL 28-AUG 01, 2012 CL New York, NY SP Amer Soc Pharmacognosy (ASP), Soc Med Plant & Nat Prod Res (GA), Italian Soc Phytochem (SIF), Phytochem Soc Europe (PSE), French Speaking Soc Pharmacognosy (AFERP) C1 [Tidgewell, K.; Gerwick, W. H.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. [Tidgewell, K.; Moy, J.] Smithsonian Trop Res Inst, Panama City, Panama. [Herrera, L.; Spadafora, C.] INDICASAT, Panama City, Panama. NR 0 TC 0 Z9 0 U1 0 U2 10 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 J9 PLANTA MED JI Planta Med. PD AUG PY 2012 VL 78 IS 11 BP 1149 EP 1149 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA 982KT UT WOS:000307042800523 ER PT J AU Thongphakdee, A Berg, D Tharasanit, T Thongtipsiridech, S Tipkantha, W Keawmai, U Noimoon, S Thongkittidilok, C Punkong, C Kamolnorranath, S Comizzoli, P Siriaroonrat, B AF Thongphakdee, A. Berg, D. Tharasanit, T. Thongtipsiridech, S. Tipkantha, W. Keawmai, U. Noimoon, S. Thongkittidilok, C. Punkong, C. Kamolnorranath, S. Comizzoli, P. Siriaroonrat, B. TI Eld's deer embryos produced in vitro can develop to term after transfer into recipient females SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Meeting Abstract CT 17th International Congress on Animal Reproduction (ICAR) CY JUL 29-AUG 02, 2012 CL Vancouver, CANADA SP Bioniche, Merial, Sanofi Co, Pfizer Anim Hlth, MSD Anim Hlth, Imv Technol, Minitube, Semex, Canadian Food Inspect Agcy DE Eld's deer; embryo devlopment; in vitro fertilization; embryo transfer C1 [Thongphakdee, A.; Tipkantha, W.; Keawmai, U.; Noimoon, S.; Punkong, C.; Kamolnorranath, S.; Siriaroonrat, B.] Zool Pk Org Royal Patronage HM King, Bangkok, Thailand. [Berg, D.] AgResearch Ltd, Hamilton, New Zealand. [Tharasanit, T.; Thongkittidilok, C.] Chulalongkorn Univ, Fac Vet Sci, Bangkok, Thailand. [Thongtipsiridech, S.] Kasetsart Univ, Fac Vet Med, Nakhon Pathom, Thailand. [Comizzoli, P.] Smithsonian Conservat Biol Inst, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0936-6768 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD AUG PY 2012 VL 47 SU 4 SI SI BP 454 EP 454 PG 1 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 980UG UT WOS:000306918700162 ER PT J AU Buarpung, S Tharasanit, T Thongkittidilok, C Comizzoli, P Techakumphu, M AF Buarpung, S. Tharasanit, T. Thongkittidilok, C. Comizzoli, P. Techakumphu, M. TI In vitro development of feline embryos after intracytoplasmic sperm injection with 7-day refrigerated testicular sperm SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Meeting Abstract CT 17th International Congress on Animal Reproduction (ICAR) CY JUL 29-AUG 02, 2012 CL Vancouver, CANADA SP Bioniche, Merial, Sanofi Co, Pfizer Anim Hlth, MSD Anim Hlth, Imv Technol, Minitube, Semex, Canadian Food Inspect Agcy DE Testicular sperm; cold storage; domestic cat; ICSI; embryo C1 [Buarpung, S.; Tharasanit, T.; Thongkittidilok, C.; Techakumphu, M.] Chulalongkorn Univ, Fac Vet Sci, Dept Obstet Gynaecol & Reprod, Bangkok, Thailand. [Comizzoli, P.] Smithsonian Conservat Biol Inst, Dept Reprod Sci, Washington, DC USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0936-6768 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD AUG PY 2012 VL 47 SU 4 SI SI BP 516 EP 516 PG 1 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 980UG UT WOS:000306918700334 ER PT J AU Kim, SM Fujihara, M Sahare, M Minami, N Yamada, M Imai, H AF Kim, S-M Fujihara, M. Sahare, M. Minami, N. Yamada, M. Imai, H. TI The role of GalNAc glycan residues associated adhesion and self-renewal in cultured bovine gonocytes SO REPRODUCTION IN DOMESTIC ANIMALS LA English DT Meeting Abstract CT 17th International Congress on Animal Reproduction (ICAR) CY JUL 29-AUG 02, 2012 CL Vancouver, CANADA SP Bioniche, Merial, Sanofi Co, Pfizer Anim Hlth, MSD Anim Hlth, Imv Technol, Minitube, Semex, Canadian Food Inspect Agcy DE Gonocytes; spermatogonial stem cells; bovine testis; glycoconjugates; lectin C1 [Kim, S-M; Fujihara, M.; Sahare, M.; Minami, N.; Yamada, M.; Imai, H.] Kyoto Univ, Grad Sch Agr, Reprod Biol Lab, Kyoto, Japan. [Fujihara, M.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0936-6768 J9 REPROD DOMEST ANIM JI Reprod. Domest. Anim. PD AUG PY 2012 VL 47 SU 4 SI SI BP 588 EP 589 PG 2 WC Agriculture, Dairy & Animal Science; Reproductive Biology; Veterinary Sciences SC Agriculture; Reproductive Biology; Veterinary Sciences GA 980UG UT WOS:000306918700540 ER PT J AU Cranmer, SR van Ballegooijen, AA AF Cranmer, Steven R. van Ballegooijen, Adriaan A. TI PROTON, ELECTRON, AND ION HEATING IN THE FAST SOLAR WIND FROM NONLINEAR COUPLING BETWEEN ALFVENIC AND FAST-MODE TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); plasmas; solar wind; Sun: corona; turbulence; waves ID ANISOTROPIC MAGNETOHYDRODYNAMIC TURBULENCE; LOW-FREQUENCY WAVES; ULTRAVIOLET CORONAGRAPH SPECTROMETER; STRONG IMBALANCED TURBULENCE; DOMINATED ACCRETION FLOWS; SLOW MAGNETOSONIC WAVES; MAGNETIC-FIELD LINES; MHD TURBULENCE; DENSITY-FLUCTUATIONS; CYCLOTRON WAVES AB In the parts of the solar corona and solar wind that experience the fewest Coulomb collisions, the component proton, electron, and heavy ion populations are not in thermal equilibrium with one another. Observed differences in temperatures, outflow speeds, and velocity distribution anisotropies are useful constraints on proposed explanations for how the plasma is heated and accelerated. This paper presents new predictions of the rates of collisionless heating for each particle species, in which the energy input is assumed to come from magnetohydrodynamic (MHD) turbulence. We first created an empirical description of the radial evolution of Alfven, fast-mode, and slow-mode MHD waves. This model provides the total wave power in each mode as a function of distance along an expanding flux tube in the high-speed solar wind. Next, we solved a set of cascade advection-diffusion equations that give the time-steady wavenumber spectra at each distance. An approximate term for nonlinear coupling between the Alfven and fast-mode fluctuations is included. For reasonable choices of the parameters, our model contains enough energy transfer from the fast mode to the Alfven mode to excite the high-frequency ion cyclotron resonance. This resonance is efficient at heating protons and other ions in the direction perpendicular to the background magnetic field, and our model predicts heating rates for these species that agree well with both spectroscopic and in situ measurements. Nonetheless, the high-frequency waves comprise only a small part of the total Alfvenic fluctuation spectrum, which remains highly two dimensional as is observed in interplanetary space. C1 [Cranmer, Steven R.; van Ballegooijen, Adriaan A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU National Aeronautics and Space Administration (NASA) [NNX09AB27G, NNX10AC11G, NNX10AQ27G] FX The authors are indebted to Ben Chandran for indispensable contributions to this work. We also acknowledge Greg Howes, Phil Isenberg, Peera Pongkitiwanichakul, Bill Matthaeus, Steve Spangler, and the anonymous referee for many helpful comments and discussions. This work was supported by the National Aeronautics and Space Administration (NASA) under grants NNX09AB27G, NNX10AC11G, and NNX10AQ27G to the Smithsonian Astrophysical Observatory. NR 223 TC 26 Z9 26 U1 0 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 AUG 1 PY 2012 VL 754 IS 2 AR 92 DI 10.1088/0004-637X/754/2/92 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700013 ER PT J AU Hatchell, J Terebey, S Huard, T Mamajek, EE Allen, L Bourke, TL Dunham, MM Gutermuth, R Harvey, PM Jorgensen, JK Merin, B Noriega-Crespo, A Peterson, DE AF Hatchell, J. Terebey, S. Huard, T. Mamajek, E. E. Allen, L. Bourke, T. L. Dunham, M. M. Gutermuth, R. Harvey, P. M. Jorgensen, J. K. Merin, B. Noriega-Crespo, A. Peterson, D. E. TI THE SPITZER SURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. V. OPHIUCHUS NORTH OBSERVED WITH IRAC AND MIPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: evolution; stars: formation ID YOUNG STELLAR OBJECTS; MAIN-SEQUENCE STARS; NEARBY OB ASSOCIATIONS; LARGE-MAGELLANIC-CLOUD; SKY SURVEY 2MASS; T-TAURI STARS; MOLECULAR CLOUDS; C2D SURVEY; SCORPIO-CENTAURUS; SCUBA SURVEY AB We present Spitzer IRAC (2.1 deg(2)) and MIPS (6.5 deg(2)) observations of star formation in the Ophiuchus North (Oph N) molecular clouds. This fragmentary cloud complex lies on the edge of the Sco-Cen OB association, several degrees to the north of the well-known rho Oph star-forming region, at an approximate distance of 130 pc. The Oph N clouds were mapped as part of the Spitzer Gould Belt project under the working name "Scorpius." In the regions mapped, selected to encompass all the cloud with visual extinction A(V) > 3, 11 young stellar object (YSO) candidates are identified, 8 from IRAC/MIPS color-based selection and 3 from Two Micron All Sky Survey (2MASS) K-S/MIPS colors. Adding to one source previously identified in L43, this increases the number of YSOcs identified in Oph N to 12. During the selection process, four color-based YSOcs were rejected as probable asymptotic giant branch stars and one as a known galaxy. The sources span the full range of YSOc classifications from Class 0/1 to Class III, and starless cores are also present. Twelve high extinction (A(V) > 10) cores are identified with a total mass of similar to 100 M-circle dot. These results confirm that there is little ongoing star formation in this region (instantaneous star formation efficiency <0.34%) and that the bottleneck lies in the formation of dense cores. The influence of the nearby Upper Sco OB association, including the 09V star zeta Oph, is seen in dynamical interactions and raised dust temperatures but has not enhanced levels of star formation in Oph N. C1 [Hatchell, J.] Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England. [Terebey, S.] Calif State Univ Los Angeles, Dept Phys & Astron PS315, Los Angeles, CA 90032 USA. [Huard, T.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Huard, T.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Mamajek, E. E.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Allen, L.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Bourke, T. L.; Peterson, D. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunham, M. M.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Gutermuth, R.] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. [Harvey, P. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Jorgensen, J. K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, J. K.] Univ Copenhagen, Ctr Star & Planet Format, DK-2100 Copenhagen O, Denmark. [Merin, B.] European Space Astron Ctr ESA, Herschel Sci Ctr, Madrid 28691, Spain. [Noriega-Crespo, A.] CALTECH, Ctr Sci, Pasadena, CA 91125 USA. RP Hatchell, J (reprint author), Univ Exeter, Astrophys Grp, Exeter EX4 4QL, Devon, England. EM hatchell@astro.ex.ac.uk; sterebe@calstatela.edu; thuard@astro.umd.edu; emamajek@pas.rochester.edu; lallen@noao.edu; tbourke@cfa.harvard.edu; michael.dunham@yale.edu; rgutermu@astro.umass.edu; pmh@astro.as.utexas.edu; jeskj@nbi.dk; Bruno.Merin@sciops.esa.int; alberto@ipac.caltech.edu FU STFC; NSF [AST-1008908]; National Aeronautics and Space Administration FX We thank the anonymous referee for constructive suggestions. S.T. thanks Deborah Padgett for help with the WISE data. J.H. acknowledges support from the STFC Advanced Fellowship program. E.E.M. acknowledges support from the NSF award AST-1008908. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France; 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; and data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles; and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 94 TC 16 Z9 16 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 104 DI 10.1088/0004-637X/754/2/104 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700025 ER PT J AU Hayashida, M Madejski, GM Nalewajko, K Sikora, M Wehrle, AE Ogle, P Collmar, W Larsson, S Fukazawa, Y Itoh, R Chiang, J Stawarz, L Blandford, RD Richards, JL Max-Moerbeck, W Readhead, A Buehler, R Cavazzuti, E Ciprini, S Gehrels, N Reimer, A Szostek, A Tanaka, T Tosti, G Uchiyama, Y Kawabata, KS Kino, M Sakimoto, K Sasada, M Sato, S Uemura, M Yamanaka, M Greiner, J Kruehler, T Rossi, A Macquart, JP Bock, DCJ Villata, M Raiteri, CM Agudo, I Aller, HD Aller, MF Arkharov, AA Bach, U Benitez, E Berdyugin, A Blinov, DA Blumenthal, K Bottcher, M Buemi, CS Carosati, D Chen, WP Di Paola, A Dolci, M Efimova, NV Forne, E Gomez, JL Gurwell, MA Heidt, J Hiriart, D Jordan, B Jorstad, SG Joshi, M Kimeridze, G Konstantinova, TS Kopatskaya, EN Koptelova, E Kurtanidze, OM Lahteenmaki, A Lamerato, A Larionov, VM Larionova, EG Larionova, LV Leto, P Lindfors, E Marscher, AP McHardy, IM Molina, SN Morozova, DA Nikolashvili, MG Nilsson, K Reinthal, R Roustazadeh, P Sakamoto, T Sigua, LA Sillanpaa, A Takalo, L Tammi, J Taylor, B Tornikoski, M Trigilio, C Troitsky, IS Umana, G AF Hayashida, M. Madejski, G. M. Nalewajko, K. Sikora, M. Wehrle, A. E. Ogle, P. Collmar, W. Larsson, S. Fukazawa, Y. Itoh, R. Chiang, J. Stawarz, L. Blandford, R. D. Richards, J. L. Max-Moerbeck, W. Readhead, A. Buehler, R. Cavazzuti, E. Ciprini, S. Gehrels, N. Reimer, A. Szostek, A. Tanaka, T. Tosti, G. Uchiyama, Y. Kawabata, K. S. Kino, M. Sakimoto, K. Sasada, M. Sato, S. Uemura, M. Yamanaka, M. Greiner, J. Kruehler, T. Rossi, A. Macquart, J. P. Bock, D. C. -J. Villata, M. Raiteri, C. M. Agudo, I. Aller, H. D. Aller, M. F. Arkharov, A. A. Bach, U. Benitez, E. Berdyugin, A. Blinov, D. A. Blumenthal, K. Boettcher, M. Buemi, C. S. Carosati, D. Chen, W. P. Di Paola, A. Dolci, M. Efimova, N. V. Forne, E. Gomez, J. L. Gurwell, M. A. Heidt, J. Hiriart, D. Jordan, B. Jorstad, S. G. Joshi, M. Kimeridze, G. Konstantinova, T. S. Kopatskaya, E. N. Koptelova, E. Kurtanidze, O. M. Lahteenmaki, A. Lamerato, A. Larionov, V. M. Larionova, E. G. Larionova, L. V. Leto, P. Lindfors, E. Marscher, A. P. McHardy, I. M. Molina, S. N. Morozova, D. A. Nikolashvili, M. G. Nilsson, K. Reinthal, R. Roustazadeh, P. Sakamoto, T. Sigua, L. A. Sillanpaa, A. Takalo, L. Tammi, J. Taylor, B. Tornikoski, M. Trigilio, C. Troitsky, I. S. Umana, G. TI THE STRUCTURE AND EMISSION MODEL OF THE RELATIVISTIC JET IN THE QUASAR 3C 279 INFERRED FROM RADIO TO HIGH-ENERGY gamma-RAY OBSERVATIONS IN 2008-2010 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; gamma rays: galaxies; quasars: individual (3C 279); radiation mechanisms: non-thermal; X-rays: galaxies ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; MULTIBAND IMAGING PHOTOMETER; FERMI-DETECTED BLAZARS; MULTIWAVELENGTH OBSERVATIONS; SPACE-TELESCOPE; ABSOLUTE CALIBRATION; GASP-WEBT; X-RAY; ELECTROMAGNETIC-SPECTRUM AB We present time-resolved broadband observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears to be delayed with respect to the gamma-ray emission by about 10 days. X-ray observations reveal a pair of "isolated" flares separated by similar to 90 days, with only weak gamma-ray/optical counterparts. The spectral structure measured by Spitzer reveals a synchrotron component peaking in the mid-infrared band with a sharp break at the far-infrared band during the gamma-ray flare, while the peak appears in the millimeter (mm)/submillimeter (sub-mm) band in the low state. Selected spectral energy distributions are fitted with leptonic models including Comptonization of external radiation produced in a dusty torus or the broad-line region. Adopting the interpretation of the polarization swing involving propagation of the emitting region along a curved trajectory, we can explain the evolution of the broadband spectra during the gamma-ray flaring event by a shift of its location from similar to 1 pc to similar to 4 pc from the central black hole. On the other hand, if the gamma-ray flare is generated instead at sub-pc distance from the central black hole, the far-infrared break can be explained by synchrotron self-absorption. We also model the low spectral state, dominated by the mm/sub-mm peaking synchrotron component, and suggest that the corresponding inverse-Compton component explains the steady X-ray emission. C1 [Hayashida, M.; Madejski, G. M.; Chiang, J.; Blandford, R. D.; Buehler, R.; Reimer, A.; Szostek, A.; Tanaka, T.; Uchiyama, Y.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Hayashida, M.] Kyoto Univ, Dept Astron, Grad Sch Sci, Sakyo Ku, Kyoto 6068502, Japan. [Nalewajko, K.] Univ Colorado, Boulder, CO 80309 USA. [Nalewajko, K.; Sikora, M.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Wehrle, A. E.] Space Sci Inst, Boulder, CO 80301 USA. [Ogle, P.] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Collmar, W.; Greiner, J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Larsson, S.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Fukazawa, Y.; Itoh, R.; Sakimoto, K.; Sasada, M.; Yamanaka, M.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Stawarz, L.] JAXA, Inst Space & Astronaut Sci, Chuo Ku, Sagamihara, Kanagawa 2525210, Japan. [Stawarz, L.; Szostek, A.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Richards, J. L.; Max-Moerbeck, W.; Readhead, A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Cavazzuti, E.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Ciprini, S.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Gehrels, N.; Sakamoto, T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Kawabata, K. S.; Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Kino, M.; Sato, S.] Nagoya Univ, Dept Phys & Astrophys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kruehler, T.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Rossi, A.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Macquart, J. P.] Curtin Univ Technol, Bentley, WA 6845, Australia. [Macquart, J. P.] Int Ctr Radio Astron Res, Bentley, WA 6845, Australia. [Bock, D. C. -J.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Villata, M.; Raiteri, C. M.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, TO, Italy. [Agudo, I.; Gomez, J. L.; Molina, S. N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Agudo, I.; Blumenthal, K.; Jorstad, S. G.; Joshi, M.; Marscher, A. P.; Taylor, B.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Arkharov, A. A.; Efimova, N. V.; Larionov, V. M.] Pulkovo Observ, St Petersburg 196140, Russia. [Bach, U.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Benitez, E.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Berdyugin, A.; Lindfors, E.; Reinthal, R.; Sillanpaa, A.; Takalo, L.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Blinov, D. A.; Efimova, N. V.; Jorstad, S. G.; Konstantinova, T. S.; Kopatskaya, E. N.; Larionov, V. M.; Larionova, E. G.; Larionova, L. V.; Morozova, D. A.; Troitsky, I. S.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Boettcher, M.; Lamerato, A.; Roustazadeh, P.] Ohio Univ, Dept Phys & Astron, Inst Astrophys, Athens, OH 45701 USA. [Buemi, C. S.; Leto, P.; Trigilio, C.; Umana, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Carosati, D.] EPT Observ, Tijarafe, La Palma, Spain. [Carosati, D.] TNG Fdn Galileo Galilei, INAF, La Palma, Spain. [Chen, W. P.; Koptelova, E.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taiwan. [Dolci, M.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Roma, Italy. [Dolci, M.] Osservatorio Astron Collurania Vincenzo Cerruli, INAF, I-64100 Teramo, Italy. [Forne, E.] Agrupacio Astron Sabadell, Sabadell 08206, Spain. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heidt, J.] Heidelberg Univ, ZAH, Landesternwarte, D-69117 Heidelberg, Germany. [Hiriart, D.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada, Baja California, Mexico. [Jordan, B.] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin 2, Ireland. [Kimeridze, G.; Kurtanidze, O. M.; Nikolashvili, M. G.; Sigua, L. A.] Abastumani Observ, GE-0301 Abastumani, Rep of Georgia. [Koptelova, E.] Natl Taiwan Univ, Dept Phys, Taipei 106, Taiwan. [Lahteenmaki, A.; Tammi, J.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [McHardy, I. M.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Nilsson, K.] Univ Turku, Finnish Ctr Astron ESO FINCA, FI-21500 Piikiio, Finland. [Taylor, B.] Lowell Observ, Flagstaff, AZ 86001 USA. RP Hayashida, M (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, 2575 Sand Hill Rd,M-S 29, Menlo Pk, CA 94025 USA. EM mahaya@slac.stanford.edu; madejski@slac.stanford.edu; knalew@Colorado.edu; sikora@camk.edu.pl RI Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Macquart, Jean-Pierre/B-5306-2013; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Larionova, Elena/H-7287-2013; Efimova, Natalia/I-2196-2013; Blinov, Dmitry/G-9925-2013 OI Umana, Grazia/0000-0002-6972-8388; Leto, Paolo/0000-0003-4864-2806; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Dolci, Mauro/0000-0001-8000-5642; Buemi, Carla Simona/0000-0002-7288-4613; Villata, Massimo/0000-0003-1743-6946; Larionova, Liudmila/0000-0002-0274-1481; Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Elena/0000-0002-2471-6500; Efimova, Natalia/0000-0002-8071-4753; Blinov, Dmitry/0000-0003-0611-5784 FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Smithsonian Institution; Academia Sinica; Russian RFBR foundation [09-02-00092]; MICIIN (Spain) [AYA2010-14844]; CEIC (Andalucia) [P09-FQM-4784]; Academy of Finland [212656, 210338, 121148]; NASA Fermi GI [NNX08AV65G, NNX08AV61G, NNX09AT99G, NNX09AU10G]; NSF [AST-0907893, AST-0607523]; BU; Lowell Observatory; UK Science and Technology Facilities Council; Georgian National Science Foundation [GNSF/ST09/521 4-320]; NASA; NASA [NNX09AU16G, NNX10AP16G, NNX11AO13G]; University of Michigan; Japan Society for the Promotion of Science for Young Scientists; Polish MNiSW [N N203 301635, N N203 386337]; Polish ASTRONET [621/E-78/SN-0068/2007]; Polish NCN [DEC-2011/01/B/ST9/04845] FX The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK), and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council, and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The St. Petersburg University team acknowledges support from the Russian RFBR foundation via grant 09-02-00092. AZT-24 observations are made within an agreement between Pulkovo, Rome, and Teramo observatories. This paper is partly based on observations carried out at the German-Spanish Calar Alto Observatory, which is jointly operated by the MPIA and the IAA-CSIC. Acquisition of the MAPCAT data is supported in part by MICIIN (Spain) grant and AYA2010-14844, and by CEIC (Andalucia) grant P09-FQM-4784. The Metsaahovi team acknowledges the support from the Academy of Finland to our observing projects (numbers 212656, 210338, 121148, and others). The Medicina and Noto telescopes are operated by INAF-Istituto di Radioastronomia. The research at Boston University was supported by NASA Fermi GI grants NNX08AV65G, NNX08AV61G, NNX09AT99G, and NNX09AU10G, and NSF grant AST-0907893. 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 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 Abastumani Observatory team acknowledges financial support by the Georgian National Science Foundation through grant GNSF/ST09/521 4-320. The research at the University of Michigan has been funded by a series of grants from NASA and from the NSF. Specific grant numbers are NASA grants NNX09AU16G, NNX10AP16G, NNX11AO13G, and NSF grant AST-0607523. Funding for the operation of UMRAO was provided by the University of Michigan.; M.H. is supported by the Research Fellowships of the Japan Society for the Promotion of Science for Young Scientists. This work was partially supported by the Polish MNiSW grants N N203 301635 and N N203 386337, the Polish ASTRONET grant 621/E-78/SN-0068/2007, and the Polish NCN grant DEC-2011/01/B/ST9/04845. NR 99 TC 58 Z9 58 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 AUG 1 PY 2012 VL 754 IS 2 AR 114 DI 10.1088/0004-637X/754/2/114 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700035 ER PT J AU Miller, BP Gallo, E Wright, JT Dupree, AK AF Miller, Brendan P. Gallo, Elena Wright, Jason T. Dupree, Andrea K. TI ON THE DETECTABILITY OF STAR-PLANET INTERACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: activity; stars: individual (WASP-18); stars: magnetic field ID EXTRASOLAR GIANT PLANETS; X-RAY-EMISSION; SOLAR-LIKE STARS; CA II H; HOT JUPITERS; HOST STARS; CHROMOSPHERIC ACTIVITY; MAGNETIC ACTIVITY; YOUNG STARS; TAU-BOOTIS AB Magnetic (or tidal) interactions between "hot Jupiters" and their host stars can potentially enhance chromospheric and coronal activity. An ideal test bed for investigating this effect is provided by the extreme WASP-18 system, which features a massive (similar to 10 times Jupiter) close-in (less than or similar to 1 day period) transiting planet orbiting a young F6 star. Optical and X-ray observations of WASP-18 were conducted in 2011 November. The high-resolution echelle spectrograph Magellan Inamori Kyocera Echelle was used on the 6.5 m Magellan Clay Telescope to obtain 13 spectra spanning planetary orbital phases of 0.7-1.4, while the X-ray Telescope on Swift provided contemporaneous monitoring with a stacked exposure of similar to 50 ks. The cores of the Ca II H and K lines do not show significant variability over multiple orbits spanning similar to 8 days, in contrast to the expectation of phase-dependent chromospheric activity enhancements for efficient star-planet interaction. The star is also X-ray faint, with log L-X < 27.6, indicating that coronal activity is likewise low. The lack of detectable star-planet interaction in this extreme system requires that any such effect here must be transient, if indeed present. We demonstrate that searches for Ca II H and K variability can potentially mistake a stellar hotspot, if observed over a short segment of the rotation period, for planet-induced activity. Taken together, these results suggest that the utility of star-planet interaction as a robust method of estimating exoplanet magnetic field strengths may be limited. C1 [Miller, Brendan P.; Gallo, Elena] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wright, Jason T.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Wright, Jason T.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Dupree, Andrea K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Miller, BP (reprint author), Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. OI Wright, Jason/0000-0001-6160-5888 FU Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium FX We thank Mario Mateo for essential assistance with the Magellan observing run, Niel Gehrels and the Swift Science Team for approving and carrying out our Target of Opportunity observations of WASP-18, and an anonymous referee for helpful comments. This paper includes data gathered with the 6.5 meter Magellan Telescopes located at Las Campanas Observatory, Chile. This research has made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. 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. NR 52 TC 16 Z9 16 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 AUG 1 PY 2012 VL 754 IS 2 AR 137 DI 10.1088/0004-637X/754/2/137 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700058 ER PT J AU Roediger, E Kraft, RP Machacek, ME Forman, WR Nulsen, PEJ Jones, C Murray, SS AF Roediger, E. Kraft, R. P. Machacek, M. E. Forman, W. R. Nulsen, P. E. J. Jones, C. Murray, S. S. TI IRREGULAR SLOSHING COLD FRONTS IN THE NEARBY MERGING GROUPS NGC 7618 AND UGC 12491: EVIDENCE FOR KELVIN-HELMHOLTZ INSTABILITIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: individual (NGC 7618, UGC 12491); galaxies: clusters: intracluster medium; hydrodynamics; instabilities; X-rays: galaxies: clusters ID GALAXY CLUSTERS; INTERGALACTIC MEDIUM; XMM-NEWTON; CHANDRA OBSERVATIONS; PERSEUS CLUSTER; MAGNETIC-FIELD; VIRGO CLUSTER; GAS; BUBBLES; MERGER AB We present results from two similar to 30 ks Chandra observations of the hot atmospheres of the merging galaxy groups centered around NGC 7618 and UGC 12491. Our images show the presence of arc-like sloshing cold fronts (CFs) wrapped around each group center and similar to 100 kpc long spiral tails in both groups. Most interestingly, the CFs are highly distorted in both groups, exhibiting "wings" along the fronts. These features resemble the structures predicted from non-viscous hydrodynamic simulations of gas sloshing, where Kelvin-Helmholtz instabilities (KHIs) distort the CFs. This is in contrast to the structure seen in many other sloshing and merger CFs, which are smooth and featureless at the current observational resolution. Both magnetic fields and viscosity have been invoked to explain the absence of KHIs in these smooth CFs, but the NGC 7618/UGC 12491 pair are two in a growing number of both sloshing and merger CFs that appear distorted. Magnetic fields and/or viscosity may be able to suppress the growth of KHIs at the CFs in some clusters and groups, but clearly not in all. We propose that the presence or absence of KHI distortions in CFs can be used as a measure of the effective viscosity and/or magnetic field strengths in the intracluster medium. C1 [Roediger, E.] Jacobs Univ Bremen, Sch Sci & Engn, D-28759 Bremen, Germany. [Roediger, E.; Kraft, R. P.; Machacek, M. E.; Forman, W. R.; Nulsen, P. E. J.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Roediger, E (reprint author), Jacobs Univ Bremen, Sch Sci & Engn, Campus Ring 1, D-28759 Bremen, Germany. EM e.roediger@jacobs-university.de OI Nulsen, Paul/0000-0003-0297-4493; Forman, William/0000-0002-9478-1682 FU DFG (German Research Foundation) [1177, 1573]; Julich Supercomputing Center [NIC 3711, 4368]; Smithsonian Astrophysical Observatory; Nasa [NNX07AH65G, NAS8-03060] FX E.R. acknowledges support by the Priority Programmes 1177 ("Witnesses of Cosmic History") and 1573 ("Physics of the Interstellar Medium") of the DFG (German Research Foundation), the supercomputing grants NIC 3711 and 4368 at the Julich Supercomputing Center, a visiting scientist fellowship of the Smithsonian Astrophysical Observatory, and the hospitality of the Center for Astrophysics in Cambridge. M.E.M. acknowledges support by the Nasa grant NNX07AH65G. This work was supported by NASA grant NAS8-03060. We thank the referee for helpful and constructive comments. NR 37 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2012 VL 754 IS 2 AR 147 DI 10.1088/0004-637X/754/2/147 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700068 ER PT J AU Tappe, A Rho, J Boersma, C Micelotta, ER AF Tappe, A. Rho, J. Boersma, C. Micelotta, E. R. TI POLYCYCLIC AROMATIC HYDROCARBON PROCESSING IN THE BLAST WAVE OF THE SUPERNOVA REMNANT N132D SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: individual objects (N132D); ISM: molecules; ISM: supernova remnants; shock waves ID SPITZER-SPACE-TELESCOPE; RICH PROTOPLANETARY NEBULAE; INFRARED SPECTROGRAPH; MAGELLANIC CLOUD; DUST DESTRUCTION; MU-M; EMISSION; SPECTROSCOPY; G11.2-0.3; YOUNG AB We present Spitzer Infrared Spectrograph 14-36 mu m mapping observations of the supernova remnant N132D in the Large Magellanic Cloud. This study focuses on the processing of polycyclic aromatic hydrocarbons (PAHs) that we previously identified in the southern blast wave. The mid-infrared spectra show strong continuum emission from shock-heated dust and a unique, nearly featureless plateau in the 15-20 mu m region, which we attribute to PAH molecules. The typical PAH emission bands observed in the surrounding interstellar medium ahead of the blast wave disappear, which indicates shock processing of PAH molecules. The PAH plateau appears most strongly at the outer edge of the blast wave and coincides with diffuse X-ray emission that precedes the brightest X-ray and optical filaments. This suggests that PAH molecules in the surrounding medium are swept up and processed in the hot gas of the blast wave shock, where they survive the harsh conditions long enough to be detected. We also observe a broad emission feature at 20 mu m appearing with the PAH plateau. We speculate that this feature is either due to FeO dust grains or connected to the processing of PAHs in the supernova blast wave shock. C1 [Tappe, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rho, J.] NASA, SOFIA Sci Mission Operat USRA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Micelotta, E. R.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. RP Tappe, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS-72, Cambridge, MA 02138 USA. EM atappe@cfa.harvard.edu RI Boersma, Christiaan/L-7696-2014; OI Boersma, Christiaan/0000-0002-4836-217X; Micelotta, Elisabetta/0000-0002-6555-5109 FU NASA [NNX10AQ84G]; NASA at Ames Research Center FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA funding through the Spitzer GO program and the Astrophysics Data Analysis Program NNX10AQ84G (awarded to J. Rho). C. Boersma is supported by an appointment to the NASA Postdoctoral Program at Ames Research Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 33 TC 5 Z9 5 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 AUG 1 PY 2012 VL 754 IS 2 AR 132 DI 10.1088/0004-637X/754/2/132 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700053 ER PT J AU Tomsick, JA Bodaghee, A Chaty, S Rodriguez, J Rahoui, F Halpern, J Kalemci, E Arabaci, MO AF Tomsick, John A. Bodaghee, Arash Chaty, Sylvain Rodriguez, Jerome Rahoui, Farid Halpern, Jules Kalemci, Emrah Arabaci, Mehtap Ozbey TI LOCALIZING INTEGRAL SOURCES WITH CHANDRA: X-RAY AND MULTI-WAVELENGTH IDENTIFICATIONS AND ENERGY SPECTRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; stars: individual (IGR J01545+6437, IGR J03103+5706, IGR J04069+5042, IGR J06552-1146, IGR J09189-4418, IGR J12489-6243, IGR J13402-6428, IGR J15293-5609, IGR J15368-5102, IGR J15391-5307, IGR J15415-5029, IGR J16173-5023, IGR J16206-5253, IGR J16413-4046, IGR J16560-4958, IGR J21188+4901); stars: neutron; white dwarfs; X-rays: galaxies; X-rays: stars ID GALACTIC PLANE SURVEY; IGR J16318-4848; OPTICAL SPECTROSCOPY; CATALOG; LOCALIZATIONS; EXTINCTION; ABSORPTION; ABUNDANCES; TRANSIENT; BINARIES AB We report on Chandra observations of 18 hard X-ray (>20 keV) sources discovered with the INTEGRAL satellite near the Galactic plane. For 14 of the INTEGRAL sources, we have uncovered one or two potential Chandra counterparts per source. These provide soft X-ray (0.3-10 keV) spectra and subarcsecond localizations, which we use to identify counterparts at other wavelengths, providing information about the nature of each source. Despite the fact that all of the sources are within 5 degrees of the plane, four of the IGR sources are active galactic nuclei (AGNs; IGR J01545+6437, IGR J15391-5307, IGR J15415-5029, and IGR J21565+5948) and four others are likely AGNs (IGR J03103+5706, IGR J09189-4418, IGR J16413-4046, and IGR J16560-4958) based on each of them having a strong IR excess and/or extended optical or near-IR emission. We compare the X-ray and near-IR fluxes of this group of sources to those of AGNs selected by their 2-10 keV emission in previous studies and find that these IGR AGNs are in the range of typical values. There is evidence in favor of four of the sources being Galactic (IGR J12489-6243, IGR J15293-5609, IGR J16173-5023, and IGR J16206-5253), but only IGR J15293-5609 is confirmed as a Galactic source as it has a unique Chandra counterpart and a parallax measurement from previous optical observations that puts its distance at 1.56 +/- 0.12 kpc. The 0.3-10 keV luminosity for this source is (1.4(-0.4)(+1.0)) x 10(32) erg s(-1), and its optical/IR spectral energy distribution is well described by a blackbody with a temperature of 4200-7000 K and a radius of 12.0-16.4 R-circle dot. These values suggest that IGR J15293-5609 is a symbiotic binary with an early K-type giant and a white dwarf accretor. We also obtained likely Chandra identifications for IGR J13402-6428 and IGR J15368-5102, but follow-up observations are required to constrain their source types. C1 [Tomsick, John A.; Bodaghee, Arash] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Chaty, Sylvain; Rodriguez, Jerome] Univ Paris Diderot, CNRS, AIM, CEA,DSM,Irfu Serv Astrophys,Ctr Saclay,UMR E 9005, FR-91191 Gif Sur Yvette, France. [Chaty, Sylvain] Inst Univ France, F-75005 Paris, France. [Rahoui, Farid] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Rahoui, Farid] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Halpern, Jules] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Kalemci, Emrah] Sabanci Univ, Fac Engn & Nat Sci, TR-34956 Istanbul, Turkey. [Arabaci, Mehtap Ozbey] Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey. RP Tomsick, JA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM jtomsick@ssl.berkeley.edu OI Rodriguez, Jerome/0000-0002-4151-4468; Chaty, Sylvain/0000-0002-5769-8601 FU NASA [GO1-12046X, NAS8-03060] FX J.A.T. and A.B. acknowledge partial support from NASA through Chandra Award Number GO1-12046X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory under NASA contract NAS8-03060. We acknowledge useful comments from an anonymous referee. This research has made use of the IGR Sources page maintained by J. Rodriguez and A. Bodaghee (http://irfu.cea.fr/Sap/IGR-Sources), the VizieR catalog access tool and the SIMBAD database, which are both operated at CDS, Strasbourg, France. We also acknowledge the use of the 2MASS, USNO, DENIS, and WISE catalogs. NR 58 TC 11 Z9 11 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 AUG 1 PY 2012 VL 754 IS 2 AR 145 DI 10.1088/0004-637X/754/2/145 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700066 ER PT J AU Tsang, BTH Pun, CSJ Di Stefano, R Li, KL Kong, AKH AF Tsang, B. T. H. Pun, C. S. J. Di Stefano, R. Li, K. L. Kong, A. K. H. TI THE DISCOVERY OF AN X-RAY/UV STELLAR FLARE FROM THE LATE-K/EARLY-M DWARF LMC 335 SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: activity; stars: coronae; stars: flare; stars: individual (LMC 335); stars: late-type; X-rays: stars ID LOW-MASS STARS; XMM-NEWTON; SOLAR NEIGHBORHOOD; ULTRAVIOLET EMISSION; PROXIMA-CENTAURI; MAIN-SEQUENCE; SKY SURVEY; EV LAC; QUIESCENT; ABUNDANCES AB We report the discovery of an X-ray/UV stellar flare from the source LMC 335, captured by XMM-Newton in the field of the Large Magellanic Cloud. The flare event was recorded continuously in X-ray for its first 10 hr from the precursor to the late decay phases. The observed fluxes increased by more than two orders of magnitude at its peak in X-ray and at least one in the UV as compared to quiescence. The peak 0.1-7.0 keV X-ray flux is derived from the two-temperature APEC model to be similar to(8.4 +/- 0.6) x 10(-12) erg cm(-2) s(-1). Combining astrometric information from multiple X-ray observations in the quiescent and flare states, we identify the NIR counterpart of LMC 335 as the Two Micron All Sky Survey source J05414534-6921512. The NIR color relations and spectroscopic parallax characterize the source as a Galactic K7-M4 dwarf at a foreground distance of (100-264) pc, implying a total energy output of the entire event of similar to(0.4-2.9) x 10(35) erg. This report comprises detailed analyses of this late-K/early-M dwarf flare event that has the longest time coverage yet reported in the literature. The flare decay can be modeled with two exponential components with timescales of similar to 28 minutes and similar to 4 hr, with a single-component decay firmly ruled out. The X-ray spectra during flare can be described by two components, a dominant high-temperature component of similar to 40-60 MK and a low-temperature component of similar to 10 MK, with a flare loop length of about 1.1-1.3 stellar radius. C1 [Tsang, B. T. H.; Pun, C. S. J.; Kong, A. K. H.] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Di Stefano, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, K. L.; Kong, A. K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. [Li, K. L.; Kong, A. K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. RP Tsang, BTH (reprint author), Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. FU HKU; National Science Council of the Republic of China (Taiwan) [NSC100-2628-M-007-002-MY3]; Kenda Foundation Golden Jade Fellowship; RGC/GRF from the government of the Hong Kong SAR [704709] FX We thank the anonymous referee for the helpful comments on the characterization of the spectral type of the source. B.T.H.T. acknowledges valuable discussions with Dr. Jifeng Liu and Dr. Frank Primini, and the support from HKU under the grant of Postgraduate Studentship. A.K.H.K. gratefully acknowledges support from the National Science Council of the Republic of China (Taiwan) through grant NSC100-2628-M-007-002-MY3 and a Kenda Foundation Golden Jade Fellowship. This research has made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. This research has also made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This was also supported by the use of observations made with the European Southern Observatory telescopes obtained from the ESO/ST-ECF Science Archive Facility. This investigation was supported by the RGC/GRF grant 704709 from the government of the Hong Kong SAR. NR 57 TC 2 Z9 2 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 AUG 1 PY 2012 VL 754 IS 2 AR 107 DI 10.1088/0004-637X/754/2/107 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700028 ER PT J AU Wang, Y Beuther, H Zhang, QZ Bik, A Rodon, JA Jiang, ZB Fallscheer, C AF Wang, Yuan Beuther, Henrik Zhang, Qizhou Bik, Arjan Rodon, Javier A. Jiang, Zhibo Fallscheer, Cassandra TI DIFFERENT EVOLUTIONARY STAGES IN THE MASSIVE STAR-FORMING REGION W3 MAIN COMPLEX SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (W3); ISM: jets and outflows; ISM: molecules; stars: formation; stars: massive ID YOUNG STELLAR OBJECTS; FAR-INFRARED OBSERVATIONS; GIANT MOLECULAR CLOUD; ORION-KL; LINE SURVEY; PROTOSTELLAR CORES; CHEMICAL-STRUCTURE; ARRAY OBSERVATIONS; APERTURE SYNTHESIS; RADIO-CONTINUUM AB We observed three high-mass star-forming regions in the W3 high-mass star formation complex with the Submillimeter Array and IRAM 30 m telescope. These regions, i.e., W3 SMS1 (W3 IRS5), SMS2 (W3 IRS4) and SMS3, are in different evolutionary stages and are located within the same large-scale environment, which allows us to study rotation and outflows as well as chemical properties in an evolutionary sense. While we find multiple millimeter continuum sources toward all regions, these three subregions exhibit different dynamical and chemical properties, which indicate that they are in different evolutionary stages. Even within each subregion, massive cores of different ages are found, e. g., in SMS2, sub-sources from the most evolved ultracompact HII region to potential starless cores exist within 30,000 AU of each other. Outflows and rotational structures are found in SMS1 and SMS2. Evidence for interactions between the molecular cloud and the HII regions is found in the (CO)-C-13 channel maps, which may indicate triggered star formation. C1 [Wang, Yuan; Jiang, Zhibo] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Wang, Yuan; Jiang, Zhibo] Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Peoples R China. [Wang, Yuan; Beuther, Henrik; Bik, Arjan] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Wang, Yuan] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rodon, Javier A.] European So Observ, Santiago 19, Chile. [Fallscheer, Cassandra] Univ Victoria, Dept Phys & Astron, STN CSC, Victoria, BC V8W 3P6, Canada. [Fallscheer, Cassandra] Natl Res Council Canada, Victoria, BC V9E 2E7, Canada. RP Wang, Y (reprint author), Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. EM ywang@pmo.ac.cn OI Bik, Arjan/0000-0001-8068-0891; Zhang, Qizhou/0000-0003-2384-6589 FU NSFC, China [10873037, 10921063, 10733030] FX We thank the anonymous referee for useful comments. We thank the observers at the SMA and 30 m telescopes. We thank Dr. Tieftrunck for providing the VLA continuum maps. Y.W. thanks the productive discussions with Dr. Min Fang. This work is supported by the NSFC 10873037 and 10921063, 10733030, China. NR 92 TC 7 Z9 7 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 AUG 1 PY 2012 VL 754 IS 2 AR 87 DI 10.1088/0004-637X/754/2/87 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 977MO UT WOS:000306666700008 ER PT J AU Mayor, JR Schuur, EAG Mack, MC Hollingsworth, TN Baath, E AF Mayor, Jordan R. Schuur, Edward A. G. Mack, Michelle C. Hollingsworth, Terresa N. Baath, Erland TI Nitrogen Isotope Patterns in Alaskan Black Spruce Reflect Organic Nitrogen Sources and the Activity of Ectomycorrhizal Fungi SO ECOSYSTEMS LA English DT Article DE 15N; black spruce; denitrifier method; dissolved organic nitrogen; ectomycorrhiza; isotope fractionation; mixing models ID NATURAL N-15 ABUNDANCE; ECOSYSTEM CARBON STORAGE; FATTY-ACID ANALYSIS; MYCORRHIZAL FUNGI; BOREAL FOREST; ARCTIC TUNDRA; MICROBIAL BIOMASS; SOIL N; AGRICULTURAL ABANDONMENT; SPECIES COMPOSITION AB Global patterns in soil, plant, and fungal stable isotopes of N (delta N-15) show promise as integrated metrics of N cycling, particularly the activity of ectomycorrhizal (ECM) fungi. At small spatial scales, however, it remains difficult to differentiate the underlying causes of plant delta N-15 variability and this limits the application of such measurements to better understand N cycling. We conducted a landscape-scale analysis of delta N-15 values from 31 putatively N-limited monospecific black spruce (Picea mariana) stands in central Alaska to assess the two main hypothesized sources of plant delta N-15 variation: differing sources and ECM fractionation. We found roughly 20% of the variability in black spruce foliar N and delta N-15 values to be correlated with the concentration and delta N-15 values of soil NH4 (+) and dissolved organic N (DON) pools, respectively. However, N-15-based mixing models from 24 of the stands suggested that fractionation by ECM fungi obscures the N-15 signature of soil N pools. Models, regressions, and N abundance data all suggested that increasing dependence on soil DON to meet black spruce growth demands predicates increasing reliance on ECM-derived N and that black spruce, on average, received 53% of its N from ECM fungi. Future research should partition the delta N-15 values within the soil DON pool to determine how choice of soil delta N-15 values influence modeled ECM activity. The C balance of boreal forests is tightly linked to N cycling and delta N-15 values may be useful metrics of changes to these connections. C1 [Mayor, Jordan R.; Schuur, Edward A. G.; Mack, Michelle C.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Mayor, Jordan R.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. [Hollingsworth, Terresa N.] Univ Alaska Fairbanks, USDA, US Forest Serv, Pacific NW Res Stn,Boreal Ecol Cooperat Res Unit, Fairbanks, AK 99775 USA. [Baath, Erland] Lund Univ, Dept Biol, Microbial Ecol Grp, S-22362 Lund, Sweden. RP Mayor, JR (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM clavulina@gmail.com OI Baath, Erland/0000-0002-2616-1342 FU NSF [DGE-0221599]; Mycological Society of America; International Association of GeoChemistry Student Research Grant; Riewald-Olowo Graduate Research Award; University of Florida Graduate Student Council; DOE FX This study was partially supported by an NSF Doctoral Dissertation award (DGE-0221599), a Forest Fungal Ecology Research award of the Mycological Society of America, an International Association of GeoChemistry Student Research Grant, a Riewald-Olowo Graduate Research Award, and University of Florida Graduate Student Council Travel awards to JRM; DOE and NSF funding to EAGS; and, the logistical support offered by the Ecosystem Ecology Laboratory at the University of Alaska, Fairbanks and the Bonanza Creek Long-Term Ecological Research site. Martin Lavoie, Emily Tissier, Dominique Ardura, Rady Ho, Dat Nyguen, and Rachel Rubin provided field or laboratory assistance. Gary Laursen assisted with fungal identifications. The manuscript benefited from the input of John Hobbie and two anonymous reviewers. Raw data to be made available at the Bonanza Creek LTER database (http://www.lter.uaf.edu/data_b.cfm). NR 112 TC 17 Z9 18 U1 5 U2 90 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1432-9840 EI 1435-0629 J9 ECOSYSTEMS JI Ecosystems PD AUG PY 2012 VL 15 IS 5 BP 819 EP 831 DI 10.1007/s10021-012-9548-9 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 981FN UT WOS:000306952400010 ER PT J AU Kolowski, JM Alonso, A AF Kolowski, Joseph M. Alonso, Alfonso TI Primate Abundance in an Unhunted Region of the Northern Peruvian Amazon and the Influence of Seismic Oil Exploration SO INTERNATIONAL JOURNAL OF PRIMATOLOGY LA English DT Article DE Anthropogenic; Ateles; Disturbance; Hydrocarbon; Lagothrix; Line-transect ID LAGOTHRIX-LAGOTRICHA-POEPPIGII; ATELES-BELZEBUTH-BELZEBUTH; NATIONAL-PARK; WOODLAND CARIBOU; RAIN-FOREST; NORTHEASTERN ALBERTA; POPULATION-DENSITIES; UNFLOODED FORESTS; FEEDING ECOLOGY; SEED DISPERSAL AB The western Amazon, a relatively remote and unstudied region, is experiencing unprecedented levels of oil and gas exploration. Despite the widespread use of seismic reflection technology for oil and gas exploration, no studies have investigated the response of primate populations to this disturbance in the Amazon. We conducted distance sampling along transects in pristine, unhunted lowland rain forest inside a large oil concession (Block 39) in the northern Peruvian Amazon with ongoing 2D seismic exploration. We aimed to investigate seismic exploration effects on local primate abundance, with a particular focus on the region's most endangered primates, lowland woolly monkeys (Lagothrix poeppigii) and white-bellied spider monkeys (Ateles belzebuth). We sampled transects before the arrival of exploration crews (control) and during the seismic operation (disturbance) and compared primate counts using mixed-effect models. We confirmed the presence of nine species of primates along sampled transects. Abundance of primate groups (species pooled) was not different between the control and disturbance period, yet abundance of primate individuals was significantly lower in the disturbance period. Although we encountered groups of Ateles belzebuth equally often during the control and disturbance periods, overall counts of individuals of this species were lower during the disturbance period owing to lower subgroup sizes. This suggests this species may have responded, at least temporarily, with localized spatial avoidance, and that it may be particularly sensitive to human disturbance regardless of hunting pressure. Our overall density estimate for Lagothrix poeppigii (30.6/km(2)) approaches the highest reported for the species. Although the relatively temporary nature of 2D seismic exploration may limit its effect on primate species, our data indicate some species may respond more negatively than others. C1 [Kolowski, Joseph M.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Alonso, Alfonso] Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Kolowski, JM (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Front Royal, VA 22630 USA. EM kolowskij@si.edu FU Repsol Exploracion Peru FX We thank Gegner Pastor, Enrique Pinedo, Luis Fernando, Guillermo Jipa, Antonio Pastrana, and Anibal Lachi Perez for their invaluable field support and local knowledge of the forest and its fauna. Special thanks to Repsol Exploracion Peru personnel in Lima and in Block 39, and Repsol YPF personnel in Madrid and Houston. We also thank the staff of Global Geophysical Services for their generous assistance with field support. Sulema Castro provided critical project coordination and organization. We are very grateful to two anonymous reviewers as well as Tremie Gregory, all of whom provided important suggestions that greatly improved this manuscript. Funding for this project and generous logistical support were provided by Repsol Exploracion Peru. This research was conducted under permit no. 016-2008-INRENA-IFFS-DCB. This publication is contribution no. 8 of the Peru Biodiversity Program. NR 59 TC 10 Z9 10 U1 1 U2 27 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0164-0291 J9 INT J PRIMATOL JI Int. J. Primatol. PD AUG PY 2012 VL 33 IS 4 BP 958 EP 971 DI 10.1007/s10764-012-9627-y PG 14 WC Zoology SC Zoology GA 979DJ UT WOS:000306794800017 ER PT J AU Adams, ER Ciardi, DR Dupree, AK Gautier, TN Kulesa, C McCarthy, D AF Adams, E. R. Ciardi, D. R. Dupree, A. K. Gautier, T. N., III Kulesa, C. McCarthy, D. TI ADAPTIVE OPTICS IMAGES OF KEPLER OBJECTS OF INTEREST SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; instrumentation: adaptive optics; planets and satellites: detection ID PLANET CANDIDATES; MULTIPLE SYSTEM; STAR; CAMERA AB All transiting planets are at risk of contamination by blends with nearby, unresolved stars. Blends dilute the transit signal, causing the planet to appear smaller than it really is, or produce a false-positive detection when the target star is blended with eclipsing binary stars. This paper reports on high spatial-resolution adaptive optics images of 90 Kepler planetary candidates. Companion stars are detected as close as 0.'' 1 from the target star. Images were taken in the near-infrared (J and Ks bands) with ARIES on the MMT and PHARO on the Palomar Hale 200 inch telescope. Most objects (60%) have at least one star within 6 '' separation and a magnitude difference of 9. Eighteen objects (20%) have at least one companion within 2 '' of the target star; six companions (7%) are closer than 0.'' 5. Most of these companions were previously unknown, and the associated planetary candidates should receive additional scrutiny. Limits are placed on the presence of additional companions for every system observed, which can be used to validate planets statistically using the BLENDER method. Validation is particularly critical for low-mass, potentially Earth-like worlds, which are not detectable with current-generation radial velocity techniques. High-resolution images are thus a crucial component of any transit follow-up program. C1 [Adams, E. R.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, D. R.] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Gautier, T. N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kulesa, C.; McCarthy, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Ciardi, David/0000-0002-5741-3047 NR 20 TC 61 Z9 61 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD AUG PY 2012 VL 144 IS 2 AR 42 DI 10.1088/0004-6256/144/2/42 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600013 ER PT J AU Kryukova, E Megeath, ST Gutermuth, RA Pipher, J Allen, TS Allen, LE Myers, PC Muzerolle, J AF Kryukova, E. Megeath, S. T. Gutermuth, R. A. Pipher, J. Allen, T. S. Allen, L. E. Myers, P. C. Muzerolle, J. TI LUMINOSITY FUNCTIONS OF SPITZER-IDENTIFIED PROTOSTARS IN NINE NEARBY MOLECULAR CLOUDS SO ASTRONOMICAL JOURNAL LA English DT Article DE infrared: stars; stars: formation; stars: luminosity function, mass function; stars: protostars ID YOUNG STELLAR OBJECTS; INITIAL MASS FUNCTION; 2-DIMENSIONAL RADIATIVE-TRANSFER; MULTIBAND IMAGING PHOTOMETER; ARRAY CAMERA IRAC; T-TAURI STARS; DENSE CORES; PROTOSTELLAR ENVELOPES; C2D SURVEY; EVOLUTIONARY SIGNATURES AB We identify protostars in Spitzer surveys of nine star-forming (SF) molecular clouds within 1 kpc: Serpens, Perseus, Ophiuchus, Chamaeleon, Lupus, Taurus, Orion, Cep OB3, and Mon R2, which combined host over 700 protostar candidates. These clouds encompass a variety of SF environments, including both low-mass and high-mass SF regions, as well as dense clusters and regions of sparsely distributed star formation. Our diverse cloud sample allows us to compare protostar luminosity functions in these varied environments. We combine near-and mid-infrared photometry from the Two Micron All Sky Survey and Spitzer to create 1-24 mu m spectral energy distributions (SEDs). Using protostars from the c2d survey with well-determined bolometric luminosities, we derive a relationship between bolometric luminosity, mid-IR luminosity (integrated from 1-24 mu m), and SED slope. Estimations of the bolometric luminosities for protostar candidates are combined to create luminosity functions for each cloud. Contamination due to edge-on disks, reddened Class II sources, and galaxies is estimated and removed from the luminosity functions. We find that luminosity functions for high-mass SF clouds (Orion, Mon R2, and Cep OB3) peak near 1L(circle dot) and show a tail extending toward luminosities above 100L(circle dot). The luminosity functions of the low-mass SF clouds (Serpens, Perseus, Ophiuchus, Taurus, Lupus, and Chamaeleon) do not exhibit a common peak, however the combined luminosity function of these regions peaks below 1L(circle dot). Finally, we examine the luminosity functions as a function of the local surface density of young stellar objects. In the Orion molecular clouds, we find a significant difference between the luminosity functions of protostars in regions of high and low stellar density, the former of which is biased toward more luminous sources. This may be the result of primordial mass segregation, although this interpretation is not unique. We compare our luminosity functions to those predicted by models and find that our observed luminosity functions are best matched by models that invoke competitive accretion, although we do not find strong agreement between the high-mass SF clouds and any of the models. C1 [Kryukova, E.; Megeath, S. T.; Allen, T. S.] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Pipher, J.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Allen, L. E.] Natl Opt Astron Observ, Tucson, AZ USA. [Myers, P. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Muzerolle, J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Kryukova, E (reprint author), Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. NR 90 TC 42 Z9 42 U1 0 U2 1 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 AUG PY 2012 VL 144 IS 2 AR 31 DI 10.1088/0004-6256/144/2/31 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600002 ER PT J AU Mace, GN Prato, L Torres, G Wasserman, LH Mathieu, RD McLean, IS AF Mace, G. N. Prato, L. Torres, G. Wasserman, L. H. Mathieu, R. D. McLean, I. S. TI DYNAMICAL MEASUREMENTS OF THE YOUNG UPPER SCORPIUS TRIPLE NTTS 155808-2219 SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: evolution; stars: pre-main sequence ID LOW-MASS STARS; SEQUENCE SPECTROSCOPIC BINARIES; CENTAURUS OB ASSOCIATION; KECK-II-TELESCOPE; ECHELLE SPECTROGRAPH; ROTATION; SYSTEMS; MULTIPLICITY; COMPONENTS; OPHIUCHUS AB The young, low-mass, triple system NTTS 155808-2219 (ScoPMS 20) was previously identified as a similar to 17 day period single-lined spectroscopic binary (SB) with a tertiary component at 0.21 arcsec. Using high-resolution infrared spectra, acquired with NIRSPEC on Keck II, both with and without adaptive optics (AO), we measured radial velocities (RVs) of all three components. Reanalysis of the single-lined visible light observations, made from 1987 to 1993, also yielded RV detections of the three stars. Combining visible light and infrared data to compute the orbital solution produces orbital parameters consistent with the single-lined solution and a mass ratio of q = 0.78 +/- 0.01 for the SB. We discuss the consistency between our results and previously published data on this system, our RV analysis with both observed and synthetic templates, and the possibility that this system is eclipsing, providing a potential method for the determination of the stars' absolute masses. Over the similar to 20 year baseline of our observations, we have measured the acceleration of the SB's center of mass in its orbit with the tertiary. Long-term, AO imaging of the tertiary will eventually yield dynamical data useful for component mass estimates. C1 [Mace, G. N.; McLean, I. S.] Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. [Prato, L.; Wasserman, L. H.] Lowell Observ, Flagstaff, AZ 86001 USA. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mathieu, R. D.] Univ Wisconsin, Dept Astron, Madison, WI 53726 USA. RP Mace, GN (reprint author), Univ Calif Los Angeles, Div Astron & Astrophys, Los Angeles, CA 90095 USA. EM gmace@astro.ucla.edu FU NASA Keck PI Data Award; NSF [AST-0444017, AST-1009136, AST-1007992]; NOAO through the Telescope System Instrumentation Program (TSIP); NSF; National Aeronautics and Space Administration; National Science Foundation; W. M. Keck Foundation FX We thank our collaborators for their contributions: T. Barman for producing our synthetic template library, and M. Simon for discussions on choosing the optimal cross-correlation templates. We sincerely thank the Keck staff for their support of this science, in particular T. Stickel, J. Rivera, S. Magee, G. Puniwai, C. Wilburn, G. Hill, and B. Schaefer. We are grateful to the anonymous referee for a timely and Succinct report. This research was funded in part by a NASA Keck PI Data Award, administerd by the NASA Exoplanet Science Institute, and NSF Grants AST-0444017 and AST-1009136 (to LP). G.T. acknowledges partial support from the NSF through grant AST-1007992. Some of the data described herein was taken on the Keck II telescope with time granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. This work made use of the SIMBAD reference database, the NASA Astrophysics Data System, and the data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Widefield Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize and acknowledge the significant cultural role that the summit of Mauna Kea plays within the indigenous Hawaiian community and are grateful for the opportunity to conduct observations from this special mountain. NR 44 TC 5 Z9 5 U1 0 U2 1 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 AUG PY 2012 VL 144 IS 2 AR 55 DI 10.1088/0004-6256/144/2/55 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600026 ER PT J AU O'Gorman, E Harper, GM Brown, JM Brown, A Redfield, S Richter, MJ Requena-Torres, MA AF O'Gorman, Eamon Harper, Graham M. Brown, Joanna M. Brown, Alexander Redfield, Seth Richter, Matthew J. Requena-Torres, Miguel A. TI CARMA CO(J=2-1) OBSERVATIONS OF THE CIRCUMSTELLAR ENVELOPE OF BETELGEUSE SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; radio lines: stars; stars: individual (alpha Ori); stars: late-type; stars: massive; supergiants ID LATE-TYPE STARS; ORIONIS M2 IAB; SUPERGIANT ALPHA-ORIONIS; MASS-LOSS; CO EMISSION; EXTENDED ATMOSPHERE; OUTER ATMOSPHERE; RADIAL-VELOCITY; EVOLVED STARS; LINE EMISSION AB We report radio interferometric observations of the (CO)-C-12-O-16 1.3 mm J = 2 - 1 emission line in the circumstellar envelope of the Msupergiant alpha Ori and have detected and separated both the S1 and S2 flow components for the first time. Observations were made with the Combined Array for Research in Millimeter- wave Astronomy (CARMA) interferometer in the C, D, and E antenna configurations. We obtain good u-v coverage (5-280 k lambda) by combining data from all three configurations allowing us to trace spatial scales as small as 0.'' 9 over a 32 '' field of view. The high spectral and spatial resolution C configuration line profile shows that the inner S1 flow has slightly asymmetric outflow velocities ranging from -9.0 km s(-1) to +10.6 km s(-1) with respect to the stellar rest frame. We find little evidence for the outer S2 flow in this configuration because the majority of this emission has been spatially filtered (resolved out) by the array. We also report a SOFIA-GREAT CO(J = 12 - 11) emission line profile, which we associate with this inner higher excitation S1 flow. The outer S2 flow appears in the D and E configuration maps and its outflow velocity is found to be in good agreement with high-resolution optical spectroscopy of Ki obtained at the McDonald Observatory. We image both S1 and S2 in the multi-configuration maps and see a gradual change in the angular size of the emission in the high absolute velocity maps. We assign an outer radius of 4 '' to S1 and propose that S2 extends beyond CARMA's field of view (32 '' at 1.3 mm) out to a radius of 17 '', which is larger than recent single-dish observations have indicated. When azimuthally averaged, the intensity falloff for both flows is found to be proportional to R-1, where R is the projected radius, indicating optically thin winds with rho alpha R-2. C1 [O'Gorman, Eamon; Harper, Graham M.] Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. [Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Redfield, Seth] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. [Richter, Matthew J.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Requena-Torres, Miguel A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP O'Gorman, E (reprint author), Trinity Coll Dublin, Sch Phys, Dublin 2, Ireland. OI Redfield, Seth/0000-0003-3786-3486 FU CARMA partner universities; Universities Space Research Association, Inc., under NASA [NAS2-97001]; Deutsches SOFIA Institut under DLR [50 OK 0901]; Science Foundation Ireland [SFI11/RFP.1/AST/3064]; Trinity College Dublin; National Science Foundation FX Support for CARMA construction was derived from the states of California, Illinois, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. This work is based (in part) on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy. SOFIA Science Mission Operations are conducted jointly by the Universities Space Research Association, Inc., under NASA contract NAS2-97001, and the Deutsches SOFIA Institut under DLR contract 50 OK 0901. GREAT is a development by the MPI fur Radioastronomie and the KOSMA/Universitat zu Koln, in cooperation with the MPI fur Sonnensystemforschung and the DLR Institut fur Planetenforschung. We thank Sarah Kennelly for providing us with archival Herschel spectra. This publication has emanated from research conducted with the financial support of Science Foundation Ireland under Grant Number SFI11/RFP.1/AST/3064, and a grant from Trinity College Dublin. NR 42 TC 6 Z9 6 U1 0 U2 1 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 AUG PY 2012 VL 144 IS 2 AR 36 DI 10.1088/0004-6256/144/2/36 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 976PK UT WOS:000306596600007 ER PT J AU Moisan, P Labandeira, CC Matushkina, NA Wappler, T Voigt, S Kerp, H AF Moisan, Philippe Labandeira, Conrad C. Matushkina, Natalia A. Wappler, Torsten Voigt, Sebastian Kerp, Hans TI Lycopsid-arthropod associations and odonatopteran oviposition on Triassic herbaceous Isoetites SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Quillwort; Odonatoptera; Archizygoptera; Oviposition; Madygen; Mesozoic ID FOSSIL INSECT EGGS; ENDOPHYTIC OVIPOSITION; 1ST RECORD; FOOD-WEB; PLANT; LEAVES; GERMANY; ODONATA; INDIA; PALEOECOLOGY AB Associations between lycopsid and herbivorous arthropods are rare in the fossil record and equally sparse among the three surviving lineages of Lycopodiaceae. Selaginellaceae and Isoetaceae. However, from the Middle Upper Triassic Madygen Formation of southwestern Kyrgyzstan, we describe the first association between an isoetalean host, Isoetites (a quillwort), and a pattern of elliptical egg insertion scars that altered the host's live plant tissues. This ovipositional damage, in some cases deployed in a stereotypical zigzag pattern, was most likely caused by small damselfly-like insects from the extinct suborder Archizygoptera of the order Odonatoptera (dragonflies). If this identification is correct, it indicates considerable behavioral stasis of dragonflies extending deep into the Mesozoic. Our detection of lycopsid ovipositional damage adds to the list of major plant hosts from the preangiospermous Mesozoic that were resources for host use by egg-laying dragonflies, particularly horsetails, ferns, and seed plants that included conifers, peltasperms, corystosperms, ginkgophytes, bennettitaleans and probably cycads. (C) 2012 Elsevier B.V. All rights reserved. C1 [Moisan, Philippe; Kerp, Hans] Univ Munster, Forsch Sstelle Paltiobot, Inst Geol & Palaontol, D-48143 Munster, Germany. [Labandeira, Conrad C.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. [Matushkina, Natalia A.] Kyiv Natl Univ, Dept Zool, Fac Biol, UA-01033 Kiev, Ukraine. [Wappler, Torsten] Univ Bonn, Steinmann Inst Geol, D-53115 Bonn, Germany. [Voigt, Sebastian] Tech Univ Bergakad Freiberg, Inst Geol, D-09599 Freiberg, Germany. RP Moisan, P (reprint author), Univ Munster, Forsch Sstelle Paltiobot, Inst Geol & Palaontol, Hindenburgpl 57, D-48143 Munster, Germany. EM f_mois01@uni-muenster.de RI Wappler, Torsten/D-4287-2011 OI Wappler, Torsten/0000-0003-1592-0988 FU Deutscher Akademischer Austausch Dienst (DAAD) [A/06/27956]; Deutsche Forschungsgemeinschaft (DFG) [VO 1466/1-1] FX This research was supported in part by the Deutscher Akademischer Austausch Dienst (DAAD grant A/06/27956 to P.M.) and the Deutsche Forschungsgemeinschaft (DFG grant VO 1466/1-1 to S.V.). The first author thanks Christian Pott (Stockholm) for providing relevant literature. This is contribution 248 of the Evolution of Terrestrial Ecosystems Consortium at the National Museum of Natural History, in Washington D.C. The comments and suggestions by two anonymous reviewers greatly improved this manuscript. NR 141 TC 16 Z9 16 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-0182 J9 PALAEOGEOGR PALAEOCL JI Paleogeogr. Paleoclimatol. Paleoecol. PD AUG 1 PY 2012 VL 344 BP 6 EP 15 DI 10.1016/j.palaeo.2012.05.016 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 978DV UT WOS:000306721700002 ER PT J AU Estrada, A Raboy, BE Oliveira, LC AF Estrada, Alejandro Raboy, Becky E. Oliveira, Leonardo C. TI Agroecosystems and Primate Conservation in The Tropics: A Review SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Review DE agriculture; agricultural matrix; human-primate conflict; neotropics; paleotropics; primate persistence ID HEADED LION TAMARIN; WILD HOWLER MONKEYS; LINDU-NATIONAL-PARK; SEED DISPERSAL; FOREST FRAGMENTS; PROTECTED AREAS; TARSIUS-DIANAE; LEONTOPITHECUS-CHRYSOMELAS; ERYTHROCEBUS-PATAS; RANGING PATTERNS AB Agroecosystems cover more than one quarter of the global land area (ca. 50 million km2) as highly simplified (e.g. pasturelands) or more complex systems (e.g. polycultures and agroforestry systems) with the capacity to support higher biodiversity. Increasingly more information has been published about primates in agroecosystems but a general synthesis of the diversity of agroecosystems that primates use or which primate taxa are able to persist in these anthropogenic components of the landscapes is still lacking. Because of the continued extensive transformation of primate habitat into human-modified landscapes, it is important to explore the extent to which agroecosystems are used by primates. In this article, we reviewed published information on the use of agroecosystems by primates in habitat countries and also discuss the potential costs and benefits to human and nonhuman primates of primate use of agroecosystems. The review showed that 57 primate taxa from four regions: Mesoamerica, South America, Sub-Saharan Africa (including Madagascar), and South East Asia, used 38 types of agroecosystems as temporary or permanent habitats. Fifty-one percent of the taxa recorded in agroecosystems were classified as least concern in the IUCN Red List, but the rest were classified as endangered (20%), vulnerable (18%), near threatened (9%), or critically endangered (2%). The large proportion of threatened primates in agroecosystems suggests that agroecosystems may play an important role in landscape approaches to primate conservation. We conclude by discussing the value of agroecosystems for primate conservation at a broad scale and highlight priorities for future research. Am. J. Primatol. 74:696-711, 2012. (c) 2012 Wiley Periodicals, Inc. C1 [Estrada, Alejandro] Univ Nacl Autonoma Mexico, Estn Biol Trop Los Tuxtlas, Inst Biol, Mexico City 04510, DF, Mexico. [Raboy, Becky E.] Smithsonian Inst, Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Raboy, Becky E.; Oliveira, Leonardo C.] Inst Estudos Socioambientais Sul Bahia IESB, Ilheus, BA, Brazil. [Oliveira, Leonardo C.] Univ Fed Rio de Janeiro, Programa Posgrad Ecol, Rio De Janeiro, Brazil. [Oliveira, Leonardo C.] Univ Estadual Santa Cruz, Programa Posgrad Ecol & Conservacao Biodiversidad, Ilheus, BA, Brazil. [Oliveira, Leonardo C.] Bicho do Mato Inst Pesquisa, Belo Horizonte, MG, Brazil. RP Estrada, A (reprint author), Univ Nacl Autonoma Mexico, Estn Biol Trop Los Tuxtlas, Inst Biol, Mexico City 04510, DF, Mexico. EM aestrada@primatesmx.com RI Oliveira, Leonardo/G-1290-2012 OI Oliveira, Leonardo/0000-0002-1774-0713 NR 137 TC 29 Z9 29 U1 13 U2 97 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 J9 AM J PRIMATOL JI Am. J. Primatol. PD AUG PY 2012 VL 74 IS 8 BP 696 EP 711 DI 10.1002/ajp.22033 PG 16 WC Zoology SC Zoology GA 975CK UT WOS:000306484200003 PM 22605526 ER PT J AU Chevance, M Weijmans, AM Damjanov, I Abraham, RG Simard, L van den Bergh, S Caris, E Glazebrook, K AF Chevance, Melanie Weijmans, Anne-Marie Damjanov, Ivana Abraham, Roberto G. Simard, Luc van den Bergh, Sidney Caris, Evelyn Glazebrook, Karl TI ON THE SHAPES AND STRUCTURES OF HIGH-REDSHIFT COMPACT GALAXIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: fundamental parameters; galaxies: statistics; galaxies: structure ID SIMILAR-TO 2; SUPERDENSE MASSIVE GALAXIES; HUBBLE-SPACE-TELESCOPE; INSIDE-OUT GROWTH; ULTRA-DEEP-FIELD; SIZE EVOLUTION; QUIESCENT GALAXIES; ELLIPTIC GALAXIES; STAR-FORMATION; PASSIVE GALAXIES AB Recent deep Hubble Space Telescope WFC3 imaging suggests that amajority of compact quiescent massive galaxies at z similar to 2 may contain disks. To investigate this claim, we have compared the ellipticity distribution of 31 carefully selected high-redshift massive quiescent compact galaxies to a set of mass-selected ellipticity and Sersic index distributions obtained from two-dimensional structural fits to similar to 40,000 nearby galaxies from the Sloan Digital Sky Survey. A Kolmogorov-Smirnov test shows that the distribution of ellipticities for the high-redshift galaxies is consistent with the ellipticity distribution of a similarly chosen sample of massive early-type galaxies. However, the distribution of Sersic indices for the high-redshift sample is inconsistent with that of local early-type galaxies, and instead resembles that of local disk-dominated populations. The mismatch between the properties of high-redshift compact galaxies and those of both local early-type and disk-dominated systems leads us to conclude that the basic structures of high-redshift compact galaxies probably do not closely resemble those of any single local galaxy population. Any galaxy population analog to the high-redshift compact galaxies that exists at the current epoch is either a mix of different types of galaxies, or possibly a unique class of objects on their own. C1 [Chevance, Melanie; Damjanov, Ivana; Abraham, Roberto G.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Chevance, Melanie; Weijmans, Anne-Marie] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Chevance, Melanie] Ecole Normale Super, Dept Phys, F-94235 Cachan, France. [Damjanov, Ivana] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Simard, Luc; van den Bergh, Sidney] Natl Res Council Canada, Dominion Astrophys Observ, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Caris, Evelyn; Glazebrook, Karl] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Chevance, M (reprint author), Univ Toronto, Dept Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada. RI Glazebrook, Karl/N-3488-2015 OI Glazebrook, Karl/0000-0002-3254-9044 NR 44 TC 17 Z9 17 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 AUG 1 PY 2012 VL 754 IS 2 AR L24 DI 10.1088/2041-8205/754/2/L24 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 975QY UT WOS:000306527200006 ER PT J AU Naoz, S Farr, WM Rasio, FA AF Naoz, Smadar Farr, Will M. Rasio, Frederic A. TI ON THE FORMATION OF HOT JUPITERS IN STELLAR BINARIES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: general; planetary systems ID SPIN-ORBIT ALIGNMENT; SOLAR-TYPE STARS; EXTRASOLAR PLANETS; TIDAL EVOLUTION; SYSTEMS; MULTIPLICITY; MIGRATION; COMPANIONS; EXOPLANETS; ECCENTRICITY AB We study the production of hot Jupiters (HJs) in stellar binaries. We show that the "eccentric Kozai-Lidov" (EKL) mechanism can play a key role in the dynamical evolution of a star-planet-star triple system. We run a large set of Monte Carlo simulations including the secular evolution of the orbits, general relativistic precession, and tides, and we determine the semimajor axis, eccentricity, inclination, and spin-orbit angle distributions of the HJs that are produced. We explore the effect of different tidal friction parameters on the results. We find that the efficiency of forming HJs when taking the EKL mechanism into account is higher then previously estimated. Accounting for the frequency of stellar binaries, we find that this production mechanism can account for about 30% of the observed HJ population. Current observations of spin-orbit angles are consistent with this mechanism producing similar to 30% of all HJs, and up to 100% of the misaligned systems. Based on the properties of binaries without an HJ in our simulations, we predict the existence of many Jupiter-like planets with moderately eccentric and inclined orbits and semimajor axes of several AU. C1 [Naoz, Smadar] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Naoz, Smadar; Farr, Will M.; Rasio, Frederic A.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Rasio, Frederic A.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Naoz, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. OI Rasio, Frederic/0000-0002-7132-418X; Naoz, Smadar/0000-0002-9802-9279 FU NASA [NNX12AI86G] FX This research was supported in part by NASA grant NNX12AI86G, and through the computational resources and staff contributions provided by Information Technology at Northwestern University as part of its shared cluster program, Quest. We thank Yoram Lithwick, Josh Winn, John Johnson, Dan Fabrycky, Amaury Triaud, and Simon Albrecht. This research made use of the Exoplanet Orbit Database and the Exoplanet Data Explorer at exoplanets.org. NR 49 TC 79 Z9 80 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 AUG 1 PY 2012 VL 754 IS 2 AR L36 DI 10.1088/2041-8205/754/2/L36 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 975QY UT WOS:000306527200018 ER PT J AU Amador-Vargas, S AF Amador-Vargas, S. TI Behavioral responses of acacia ants correlate with age and location on the host plant SO INSECTES SOCIAUX LA English DT Article DE Division of labor; Acacia ants; Age polyethism; Behavioral castes ID DIVISION-OF-LABOR; TEMPORAL POLYETHISM; CENTRAL AMERICA; FORMICIDAE; SPECIALIZATION; HYMENOPTERA; MUTUALISM; COLONIES; CASTES AB In social insects, worker specialization in location-related tasks could occur if they return to the same location over time. Location and task fidelity was tested in the acacia ants Pseudomyrmex spinicola, which nest inside the swollen spines of the tree, and all workers enter the spines at night and during rain. Workers were marked and followed at three locations: on the leaves, tree trunk, and ground near the plant. Behavioral tests were performed, testing the reactions of marked ants toward the food used to feed the larvae (Beltian Bodies, "BB"), and to brood outside the spines. Marked ants and ants of known age were tested for responses to disturbance of the spines. Ants were more likely to occur in the location where they were originally marked. Trunk-marked ants discarded the BB when it had a foliole fragment attached to it, while leaf-marked ants carried it to the spine. Trunk-marked ants left larvae and exited from disturbed spines more frequently than other ants. Leaf-marked ants carried larvae and pupae more often than trunk-marked ants. Spine-marked ants left pupae more often than trunk- or leaf-marked ants. When considering age, older ants reacted aggressively when threatened, whereas younger ants protected the brood. However, younger ants reacted more aggressively when older ants were absent, and older ants were more aggressive in the presence of larvae. In sum, the spatial segregation of the ants coincided with behavioral differences, and different behavioral responses are related to the age of the ant. C1 [Amador-Vargas, S.] Univ Costa Rica, San Jose, Costa Rica. [Amador-Vargas, S.] Smithsonian Trop Res Inst, Panama City, Panama. RP Amador-Vargas, S (reprint author), Univ Texas Austin, Patterson Labs, 1 Univ Stn,C0900, Austin, TX 78712 USA. EM samadorv@utexas.edu OI Amador Vargas, Sabrina/0000-0001-8738-4876 FU Don and Beverly Stone Fund; Glaxo Fund; Smithsonian Tropical Research Institute FX I dedicate this work to Rodolfo Amador and Sodelba Vargas. I thank Frank Joyce, Gilbert Barrantes, and especially William Eberhard for valuable comments on previous versions of the manuscript; W. Eberhard and G. Barrantes for long discussions about the results; William Wcislo and other members of the Wcislo Lab for support at STRI; Heil Martin for information about nectar composition; the staff at Palo Verde for their support, especially Romelio Campos; Maga Gei for feeding the ants in my absence; and the staff at Parque Natural Metropolitano. The Don and Beverly Stone Fund and the Glaxo Fund managed by the Organization for Tropical Studies and a Short Term Fellowship from the Smithsonian Tropical Research Institute funded this investigation. Research was conducted under scientific permit no. 74-2007 from the MINAE and SE/A-709 from the ANAM, in accordance with the laws of the Republic of Costa Rica and Panama NR 23 TC 5 Z9 5 U1 0 U2 36 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD AUG PY 2012 VL 59 IS 3 BP 341 EP 350 DI 10.1007/s00040-012-0226-x PG 10 WC Entomology SC Entomology GA 974IY UT WOS:000306429000006 ER PT J AU Farji-Brener, AG Morueta-Holme, N Chinchilla, F Willink, B Ocampo, N Bruner, G AF Farji-Brener, A. G. Morueta-Holme, N. Chinchilla, F. Willink, B. Ocampo, N. Bruner, G. TI Leaf-cutting ants as road engineers: the width of trails at branching points in Atta cephalotes SO INSECTES SOCIAUX LA English DT Article DE Ants; Building behavior; Costa Rica; Foraging trails; Trail design ID TRAFFIC ORGANIZATION; WALKING SPEED; MAINTENANCE; COLOMBICA AB We used a simple engineering principle, which suggests that the width of a road needed for a smooth traffic flow is proportional to the peak traffic volume ("engineering hypothesis"), to analyze the adaptive significance of trail width at branching points in the leaf-cutting ant Atta cephalotes. Since the flow of outgoing ants splits at trail bifurcations and merges when ants return to the nest through the same paths, the sum of branch widths should equal the width of the trail section upstream of the bifurcation. We measured the width of branches and their preceding trail section and also performed field measurements and manipulations to analyze ant flow, number of collisions, and ant speed in different trail sectors. Contrary to the prediction of the "engineering hypothesis", the sum of branch widths was larger than the width of the trail immediately before the bifurcation. Our data contradict the "trail addition hypothesis" and support the "border effect hypothesis" to explain this pattern. First, the width of the widest branch was smaller than the width of the trail upstream of the bifurcation, an unexpected result if one branch is merely the continuation of the basal trail. Second, ants collided with obstacles more often in the margin than in the central portion of the trail, relocated ants from central to margin trail sectors reduced their speed, and ant flow was higher in the central sections of the trail. Since the delaying effect of trail margins increases as the trail width decreases, ants may build branches wider than expected to reduce the border effect. The delaying effect of trail margins should be included in the analysis of costs and benefits to fully understand the adaptive value of the design of ant trail networks. C1 [Farji-Brener, A. G.] Lab Ecotono CRUB UNCOma INIBIOMA CONICET, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. [Morueta-Holme, N.] Aarhus Univ, Ecoinformat & Biodivers Grp, Dept Biosci, DK-8000 Aarhus C, Denmark. [Chinchilla, F.] Estn Biol, Monteverde, Puntarenas, Costa Rica. [Willink, B.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. [Ocampo, N.] Fdn Horizonte Verde, Bogota, Colombia. [Bruner, G.] Smithsonian Trop Res Inst, Panama City, Panama. RP Farji-Brener, AG (reprint author), Lab Ecotono CRUB UNCOma INIBIOMA CONICET, Pasaje Gutierrez 1125, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. EM alefarji@yahoo.com RI Willink, Beatriz/J-9931-2015; Morueta-Holme, Naia/J-4952-2013; OI Willink, Beatriz/0000-0002-4579-6909; Morueta-Holme, Naia/0000-0002-0776-4092; Farji-Brener, Alejandro Gustavo/0000-0001-7251-3866 NR 26 TC 2 Z9 2 U1 6 U2 31 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 J9 INSECT SOC JI Insect. Soc. PD AUG PY 2012 VL 59 IS 3 BP 389 EP 394 DI 10.1007/s00040-012-0231-0 PG 6 WC Entomology SC Entomology GA 974IY UT WOS:000306429000011 ER PT J AU McKenzie, LA Brooks, RC Johnston, EL AF McKenzie, Louise A. Brooks, Robert C. Johnston, Emma L. TI A widespread contaminant enhances invasion success of a marine invader SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE Bryozoans; contamination; copper; metamorphosis; non-indigenous species; propagule pressure; recruitment; trade-off ID HEAVY-METALS; WATERSIPORA-SUBTORQUATA; BIOLOGICAL INVASIONS; PROPAGULE PRESSURE; SPECIES RICHNESS; RAPID EVOLUTION; LARVAL SIZE; COPPER; COMMUNITIES; RESISTANCE AB 1. The global transfer of species by human vectors is continuing despite the use of managerial controls such as antifouling biocides and pesticide applications. The process of introduction now exposes species to novel conditions which may select for tolerance to a contaminant. Invader establishment success is influenced by both the supply of invasive propagules and disturbance. Therefore, it is important to understand whether tolerance to an anthropogenic disturbance, such as contamination, can change the parameters of supply in a way that inadvertently augments the invasion process. 2. To test whether the invasion process is influenced by a widespread contaminant, we investigated how recruitment of the invasive hull-fouling bryozoan Watersipora subtorquata is affected by exposure to copper-based antifouling paint. We quantified settlement patterns in control and copper environments and then assessed post-settlement survival and fitness components. 3. Copper significantly increased total recruitment success despite greater post-settlement mortality. Surviving recruits differed morphologically, with shorter ancestrulae and smaller colonies in high copper treatments. These results show a strong positive affiliation between larval W.similar to subtorquata and high levels of copper although there are associated fitness costs. 4. Syntheses and applications. We found a direct positive effect of contamination on recruitment of a common invasive species. This process is likely to be relevant to other non-indigenous species (NIS) that exhibit a positive affiliation with metal contamination. Copper can potentially enhance success at multiple stages of the invasion process, including facilitating transport and establishment, by increasing the supply and retention of individuals into anthropogenically disturbed environments. Identification of tolerance to contamination as a species trait may also aid in predicting a species invasiveness and spread. Management of metal pollution through remediation and alternative copper-free antifouling techniques would help prevent the spread and establishment of many marine NIS. C1 [McKenzie, Louise A.; Brooks, Robert C.; Johnston, Emma L.] Univ New S Wales, Evolut & Ecol Res Ctr, Sch Biol Earth & Environm Sci, Sydney, NSW 2052, Australia. RP McKenzie, LA (reprint author), Smithsonian Environm Res Ctr, Marine Invas Lab, POB 28, Edgewater, MD 21037 USA. EM mckenziel@si.edu RI Brooks, Robert/A-1251-2008; Johnston, Emma/B-7210-2009 OI Brooks, Robert/0000-0001-6926-0781; Johnston, Emma/0000-0002-2117-366X FU Australian Government; Australian Research Council FX We are grateful to the Subtidal Ecology and Ecotoxicology laboratory members for assistance in the field. The authors were supported by the Australian Government and Australian Research Council through Research Fellowships, Postgraduate Awards and Grants. We thank Burraneer Marina for the use of their facilities. We thank K. A. Dafforn and G. F. Clark for their comments on improving the manuscript. NR 62 TC 5 Z9 5 U1 2 U2 74 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD AUG PY 2012 VL 49 IS 4 BP 767 EP 773 DI 10.1111/j.1365-2664.2012.02158.x PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 974ZU UT WOS:000306477000003 ER PT J AU Gschweng, M Kalko, EKV Berthold, P Fiedler, W Fahr, J AF Gschweng, Marion Kalko, Elisabeth K. V. Berthold, Peter Fiedler, Wolfgang Fahr, Jakob TI Multi-temporal distribution modelling with satellite tracking data: predicting responses of a long-distance migrant to changing environmental conditions SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE Eleonora's falcon; Madagascar; maxent; migratory species; remote sensing; species distribution modelling; wintering area ID SPECIES-DISTRIBUTION MODELS; HABITAT SUITABILITY; MAXIMUM-ENTROPY; TELEMETRY DATA; MIGRATION; ECOLOGY; MADAGASCAR; ACCURACY; TURTLES; AFRICA AB 1. Despite the wealth of data available from satellite tracking (ST) studies, such data have rarely been used to model species distributions. Using a novel method, we show how to exploit satellite data to analyse whether and how a migratory species responds to fluctuating environmental conditions in its wintering area. This is particularly crucial for establishing comprehensive conservation measures for rare species in areas that are threatened by increasing land use and climate change. 2. We use ST data of Eleonoras falcon Falco eleonorae, a long-distance migratory raptor that winters in Madagascar, and assess the performance of static species distribution models (SDM) as well as multi-temporal models. ST data were derived from seven falcons tracked during three consecutive wintering periods and for a total of 2410 bearings, of which 512 locations were used in SDMs. We employed environmental predictors (climate, topography and land cover) with a spatial resolution of 30 arc seconds (c. 1 km2) to match rigorously filtered ST data with an accuracy of =1 km. 3. We first created a model with low temporal but high spatial resolution (half-year). To predict suitable habitat for each month of the wintering season, we took advantage of the high temporal resolution inherent in ST data and employed temporally corresponding remote sensing data [Normalized Difference Vegetation Index (NDVI) 10-day composites] together with other variables to create monthly models. 4. We show that ST data are suited to build robust and transferable SDMs despite a low number of tracked individuals. Multi-temporal SMDs further revealed seasonal responses of the study species to changing environmental conditions in its wintering area. 5. Synthesis and applications. We present a transferable approach to predict the potential distribution of organisms as well as their dynamic response to changing environmental conditions. Future conservation management plans could include the prediction of a species reaction to changing land-use practices or climate change based on the methodology proposed here. This would provide an early warning system for the decline of populations wintering in remote areas that underlie strong climatic fluctuations. C1 [Fahr, Jakob] Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, D-38106 Braunschweig, Germany. [Gschweng, Marion; Kalko, Elisabeth K. V.; Fahr, Jakob] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Berthold, Peter; Fiedler, Wolfgang; Fahr, Jakob] Max Planck Inst Ornithol, D-78315 Radolfzell am Bodensee, Germany. RP Fahr, J (reprint author), Tech Univ Carolo Wilhelmina Braunschweig, Inst Zool, Mendelssohnstr 4, D-38106 Braunschweig, Germany. EM jakob.fahr@gmail.com RI Fahr, Jakob/E-8831-2012; OI Fahr, Jakob/0000-0002-9174-1204; Fiedler, Wolfgang/0000-0003-1082-4161 FU German Academic Exchange Programme (DAAD); BIOTA programme; German Federal Ministry of Education and Research (BMBF) [01LC0411]; Falcon Fund FX Matthias Herkt and Gunter Barnikel (Ulm University) provided much appreciated GIS support; Martin Wegmann (University of Wurzburg & DLR) calculated the environmental layers of topodiversity. The German Academic Exchange Programme (DAAD) funded fieldwork in Madagascar (MG). JF was supported by the BIOTA programme, funded by the German Federal Ministry of Education and Research (BMBF, project 01LC0411). The 'Direction des Eaux et Forets' and the ANGAP (Association National pour la Gestion des Aires Protegees) granted permits to conduct faunal surveys in Madagascar. BirdLife International Madagascar Programme, Voninavoko Raminoarisoa, helped in receiving permits and supported literature research. Frank Hawkins (Conservation International) gave valuable information on the occurrence of Eleonora's falcon in Madagascar and Sama Zefania assisted with fieldwork. Sadly, Elisabeth K. V. Kalko, co-author of this manuscript and supervisor of the PhD thesis of MG from which this publication derives, deceased during fieldwork in September 2011. We are greatly indebted for her contribution to the Falcon Fund, which financially supported fieldwork in Madagascar. We thank two anonymous reviewers for their comments on a former version of this manuscript and both the editor and associate editor for their kind support during the revision process. The authors declare that there is no conflict of interest related to this publication. NR 53 TC 17 Z9 17 U1 11 U2 87 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD AUG PY 2012 VL 49 IS 4 BP 803 EP 813 DI 10.1111/j.1365-2664.2012.02170.x PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 974ZU UT WOS:000306477000007 ER PT J AU Ugan, A Neme, G Gil, A Coltrain, J Tykot, R Novellino, P AF Ugan, Andrew Neme, Gustavo Gil, Adolfo Coltrain, Joan Tykot, Robert Novellino, Paula TI Geographic variation in bone carbonate and water delta O-18 values in Mendoza, Argentina and their relationship to prehistoric economy and settlement SO JOURNAL OF ARCHAEOLOGICAL SCIENCE LA English DT Article DE Stable isotopes; delta O-18; Water; Argentina; Mendoza; Archaeology; Settlement pattern; Mobility; Agriculture ID CENTRAL-WESTERN ARGENTINA; OXYGEN-ISOTOPE ANALYSIS; STABLE-ISOTOPES; MAIZE-CONSUMPTION; PHOSPHATE; FRACTIONATION; TEOTIHUACAN; PHYSIOLOGY; RATIOS; TEETH AB Questions of mobility, settlement pattern, and their relation to economic organization and resource use are central to ongoing work in central-western Argentina. Here we analyze geographic patterns in the distribution of 178 human bone carbonate delta O-18 samples, 46 human tooth enamel carbonate delta O-18 samples, and 48 water delta O-18 samples from throughout the Andean Cordillera and Monte Desert and evaluate their implications for prehistoric mobility and economy. We confirm and refine previous generalizations regarding a highland/lowland dichotomy in water delta O-18 values and show that the range of human carbonate delta O-18 values generally reflect available water sources. While there is little within-lifetime change in patterns of water use, we show that most individuals have stable isotope signatures consistent with water use from multiple areas or areas other than where they were ultimately interred. These data indicate high levels of residential mobility, and we conclude by discussing their implications for our understanding of regional prehistory. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Ugan, Andrew; Neme, Gustavo; Gil, Adolfo] Museo Hist Nat San Rafael, RA-5600 Mendoza, Argentina. [Ugan, Andrew] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ugan, Andrew; Coltrain, Joan] Univ Utah, Dept Anthropol, Salt Lake City, UT 84112 USA. [Gil, Adolfo] Univ Nacl Cuyo, Fac Filosofa & Letras, RA-5500 Mendoza, Argentina. [Tykot, Robert] Univ S Florida, Dept Anthropol, Tampa, FL 33620 USA. [Novellino, Paula] Museo Ciencias Nat & Antropol JC Moyano, Mendoza, Argentina. RP Ugan, A (reprint author), Museo Hist Nat San Rafael, Parque Moriano Moreno, RA-5600 Mendoza, Argentina. EM andrew.ugan@gmail.com; gustavoneme@arqueologiamendoza.com; adolfogil@arqueologiamendoza.org; joan.coltrain@anthro.utah.edu; rtykot@usf.edu; pnovel@hotmail.com FU NSF [0754353]; la Agencia Nacional de Ciencia y Tecnologia [PICT 2006-00046, IDAC-ICES 2007/610]; la Universidad Nacional de Cuyo FX We would like to thank Alejandra Guerci and Clara Otaola for their help with sample collection and Craig Cook and Brad Erkkila at the University of Wyoming Stable Isotope Facility and SIRFER for processing. This work was funded in part by NSF Grant 0754353, la Agencia Nacional de Ciencia y Tecnologia (PICT 2006-00046 and IDAC-ICES 2007/610), and la Universidad Nacional de Cuyo. NR 75 TC 12 Z9 12 U1 1 U2 17 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0305-4403 EI 1095-9238 J9 J ARCHAEOL SCI JI J. Archaeol. Sci. PD AUG PY 2012 VL 39 IS 8 BP 2752 EP 2763 DI 10.1016/j.jas.2012.04.013 PG 12 WC Anthropology; Archaeology; Geosciences, Multidisciplinary SC Anthropology; Archaeology; Geology GA 970WT UT WOS:000306163700016 ER PT J AU Richards-Zawacki, CL Wang, IJ Summers, K AF Richards-Zawacki, Corinne L. Wang, Ian J. Summers, Kyle TI Mate choice and the genetic basis for colour variation in a polymorphic dart frog: inferences from a wild pedigree SO MOLECULAR ECOLOGY LA English DT Article DE heritability; mate choice; pedigree; polymorphism; sexual selection; speciation ID STRAWBERRY POISON FROG; DEL-TORO-ARCHIPELAGO; DENDROBATES-PUMILIO; SEXUAL SELECTION; CICHLID FISH; PATERNITY ASSESSMENT; MATING PREFERENCES; BROOD CARE; SPECIATION; POPULATIONS AB Understanding how reproductive barriers evolve during speciation remains an important question in evolution. Divergence in mating preferences may be a common first step in this process. The striking colour pattern diversity of strawberry dart frog (Dendrobates pumilio) populations has likely been shaped by sexual selection. Previous laboratory studies have shown that females attend to male coloration and prefer to court with males of their own colour, suggesting that divergent morphs may be reproductively isolated. To test this hypothesis, we used molecular data to estimate pedigree relationships from a polymorphic population. Whereas in the laboratory both red and yellow females preferred to court with males of their own phenotype, our pedigree shows a pattern of assortative mating only for red females. In the wild, yellow females appear to be less choosy about their mates, perhaps because they incur higher costs associated with searching than females of the more common red phenotype. We also used our pedigree to investigate the genetic basis for colour-pattern variation. The phenotype frequencies we observed were consistent with those expected if dorsal background coloration is controlled by a single locus, with complete dominance of red over yellow. Our results not only help clarify the role of sexual selection in reducing gene flow, but also shed light on the mechanisms underlying colour-pattern variation among sympatric colour morphs. The difference we observed between mating preferences measured under laboratory conditions and the pattern of mate choice observed in the wild highlight the importance of field studies for understanding behavioural reproductive isolation. C1 [Richards-Zawacki, Corinne L.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Richards-Zawacki, Corinne L.] Smithsonian Trop Res Inst, Ancon, Panama, Panama. [Wang, Ian J.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Summers, Kyle] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. RP Richards-Zawacki, CL (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, 400 Lindy Boggs Bldg, New Orleans, LA 70118 USA. EM cori@tulane.edu RI Wang, Ian/G-3260-2010; Richards-Zawacki, Corinne/F-2731-2011 OI Wang, Ian/0000-0003-2554-9414; Richards-Zawacki, Corinne/0000-0002-4212-041X FU STRI; National Science Foundation (NSF) [0701165]; University of California President's Office; NSF [1003227]; University of Michigan [09765, 2007-17-12-15-07] FX We thank Narissa Bax, Sebastian Castillo, Ricardo Cossio, Deyvis Gonzalez, Tracy Stetzinger, Geoff Zawacki, Amanda Zellmer, Tom Richards and Becky Richards for help with mark-recapture. The STRI provided logistical support for this project, and we are particularly grateful to Gabriel Jacome and Plinio Gondola of the Bocas del Toro Field Station. This study was financially supported by a short-term fellowship from STRI, postdoctoral fellowships from the National Science Foundation (NSF, Award No. 0701165) and the University of California President's Office to CRZ, and an NSF postdoctoral fellowship to IJW (Award No. 1003227). The Panamanian National Authority for the Environment (ANAM) provided research and export permission for this study. This work complied with IACUC protocols (University of Michigan No. 09765 and STRI No. 2007-17-12-15-07). NR 71 TC 22 Z9 23 U1 3 U2 83 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD AUG PY 2012 VL 21 IS 15 BP 3879 EP 3892 DI 10.1111/j.1365-294X.2012.05644.x PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 975AL UT WOS:000306478800020 PM 22650383 ER PT J AU McKeon, CS Stier, AC McIlroy, SE Bolker, BM AF McKeon, C. Seabird Stier, Adrian C. McIlroy, Shelby E. Bolker, Benjamin M. TI Multiple defender effects: synergistic coral defense by mutualist crustaceans SO OECOLOGIA LA English DT Article DE Alpheus; Coral reefs; Exosymbiont; Multiple predator effects; Trapezia ID OF-THORNS STARFISH; ECOLOGICAL COMMUNITIES; REEF CORALS; DIVERSITY; PREDATOR; SYMBIONTS; TRAPEZIA; PACIFIC; CRABS; HOST AB The majority of our understanding of mutualisms comes from studies of pairwise interactions. However, many hosts support mutualist guilds, and interactions among mutualists make the prediction of aggregate effects difficult. Here, we apply a factorial experiment to interactions of 'guard' crustaceans that defend their coral host from seastar predators. Predation was reduced by the presence of mutualists (15% reduction in predation frequency and 45% in volume of coral consumed). The frequency of attacks with both mutualists was lower than with a single species, but it did not differ significantly from the expected frequency of independent effects. In contrast, the combined defensive efficacy of both mutualist species reduced the volume of coral tissue lost by 73%, significantly more than the 38% reduction expected from independent defensive efforts, suggesting the existence of a cooperative synergy in defensive behaviors of 'guard' crustaceans. These emergent 'multiple defender effects' are statistically and ecologically analogous to the emergent concept of 'multiple predator effects' known from the predation literature. C1 [McKeon, C. Seabird] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Stier, Adrian C.; Bolker, Benjamin M.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [McIlroy, Shelby E.] SUNY Buffalo, Dept Geol, Buffalo, NY 14260 USA. RP McKeon, CS (reprint author), Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM McKeons@si.edu OI Bolker, Benjamin/0000-0002-2127-0443 FU NSF [OCE-0242312]; University of Florida; BIOCODE Moorea; Ocean Bridges program FX We thank Craig Osenberg, Todd Palmer, and Gustav Paulay for discussion and comments, and the staff at the Gump station for their logistical support. Jay Stachowicz and anonymous reviewers aided the manuscript greatly. This project was funded by NSF (OCE-0242312; to Osenberg, St. Mary and Bolker), an Alumni Fellowship from University of Florida to C.S. McKeon, the BIOCODE Moorea project to G. Paulay, and the Ocean Bridges program (Partnership University Fund of the French American Cultural Exchange). This is a contribution from the University of California Berkeley's Richard B. Gump South Pacific Research Station. NR 46 TC 16 Z9 16 U1 0 U2 78 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD AUG PY 2012 VL 169 IS 4 BP 1095 EP 1103 DI 10.1007/s00442-012-2275-2 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 975GA UT WOS:000306494800023 PM 22374368 ER PT J AU Dieckmann, ME Bret, A Sarri, G Alvaro, EP Kourakis, I Borghesi, M AF Dieckmann, M. E. Bret, A. Sarri, G. Perez Alvaro, E. Kourakis, I. Borghesi, M. TI Particle simulation study of electron heating by counter-streaming ion beams ahead of supernova remnant shocks SO PLASMA PHYSICS AND CONTROLLED FUSION LA English DT Article ID QUASI-PERPENDICULAR SHOCKS; MAGNETIC-FIELD; TRANSITION REGION; COSMIC-RAYS; ACCELERATION; PLASMA; INSTABILITIES; DYNAMICS; AMPLIFICATION; TURBULENCE AB The growth and saturation of Buneman-type instabilities is examined with a particle-in-cell (PIC) simulation for parameters that are representative for the foreshock region of fast supernova remnant shocks. A dense ion beam and the electrons correspond to the upstream plasma and a fast ion beam to the shock-reflected ions. The purpose of the 2D simulation is to identify the nonlinear saturation mechanisms, the electron heating and potential secondary instabilities that arise from anisotropic electron heating and result in the growth of magnetic fields. We confirm that the instabilities between both ion beams and the electrons saturate by the formation of phase space holes by the beam-aligned modes. The slower oblique modes accelerate some electrons, but they cannot heat up the electrons significantly before they are trapped by the faster beam-aligned modes. Two circular electron velocity distributions develop, which are centred around the velocity of each ion beam. They develop due to the scattering of the electrons by the electrostatic wave potentials. The growth of magnetic fields is observed, but their amplitude remains low. C1 [Dieckmann, M. E.; Sarri, G.; Kourakis, I.; Borghesi, M.] Queens Univ Belfast, Ctr Plasma Phys, Belfast BT7 1NN, Antrim, North Ireland. [Bret, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bret, A.; Perez Alvaro, E.] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Bret, A.; Perez Alvaro, E.] Inst Invest Energet & Aplicac Ind, Ciudad Real 13071, Spain. RP Dieckmann, ME (reprint author), Queens Univ Belfast, Ctr Plasma Phys, Belfast BT7 1NN, Antrim, North Ireland. RI Dieckmann, Mark Eric/C-8591-2009; Borghesi, Marco/K-2974-2012; Bret, Antoine/C-9112-2009; Kourakis, Ioannis/B-7885-2010; OI Dieckmann, Mark Eric/0000-0003-4055-0552; Bret, Antoine/0000-0003-2030-0046; Kourakis, Ioannis/0000-0002-4027-0166; Sarri, Gianluca/0000-0003-1800-343X FU Vetenskapsradet [DNR 2010-4063]; EPSRC [EP/D043808/1, EP/D06337X/1, EP/I031766/1]; Consejeria de Educacion y Ciencia [ENE2009-09276]; Leverhulme Trust [ECF-2011-383]; Junta de Comunidades de Castilla-La Mancha [PAI08-0182-3162] FX This work was supported by Vetenskapsradet (DNR 2010-4063), by EPSRC (EP/D043808/1, EP/D06337X/1, EP/I031766/1), by Consejeria de Educacion y Ciencia (ENE2009-09276), by the Leverhulme Trust (ECF-2011-383) and by the Junta de Comunidades de Castilla-La Mancha (PAI08-0182-3162). Computer time and support was provided by the HPC2N in Umea. NR 46 TC 6 Z9 6 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0741-3335 J9 PLASMA PHYS CONTR F JI Plasma Phys. Control. Fusion PD AUG PY 2012 VL 54 IS 8 AR 085015 DI 10.1088/0741-3335/54/8/085015 PG 11 WC Physics, Fluids & Plasmas SC Physics GA 974HN UT WOS:000306423700018 ER PT J AU Troxler, TG Ikenaga, M Scinto, L Boyer, JN Condit, R Perez, R Gann, GD Childers, DL AF Troxler, Tiffany G. Ikenaga, Makoto Scinto, Leonard Boyer, Joseph N. Condit, Richard Perez, Rolando Gann, George D. Childers, Daniel L. TI Patterns of Soil Bacteria and Canopy Community Structure Related to Tropical Peatland Development SO WETLANDS LA English DT Article DE Plant; Ombrotrophy; PCR-DGGE; Phosphorus; Wetland; Bacteria; Acidobacteria; Respiration; Enzyme activity; Forest; Bog ID PHOSPHORUS LIMITATION; TERRESTRIAL ECOSYSTEMS; DIVERSITY GRADIENT; NUTRIENT GRADIENTS; SPECIES-DIVERSITY; PLANT DIVERSITY; NATURAL-WATERS; SWAMP FOREST; RAIN-FOREST; NEW-ZEALAND AB Natural environmental gradients provide important information about the ecological constraints on plant and microbial community structure. In a tropical peatland of Panama, we investigated community structure (forest canopy and soil bacteria) and microbial community function (soil enzyme activities and respiration) along an ecosystem development gradient that coincided with a natural P gradient. Highly structured plant and bacterial communities that correlated with gradients in phosphorus status and soil organic matter content characterized the peatland. A secondary gradient in soil porewater NH4 described significant variance in soil microbial respiration and beta-1-4-glucosidase activity. Covariation of canopy and soil bacteria taxa contributed to a better understanding of ecological classifications for biotic communities with applicability for tropical peatland ecosystems of Central America. Moreover, plants and soils, linked primarily through increasing P deficiency, influenced strong patterning of plant and bacterial community structure related to the development of this tropical peatland ecosystem. C1 [Troxler, Tiffany G.; Scinto, Leonard; Boyer, Joseph N.] Florida Int Univ, SE Environm Res Ctr, Miami, FL 33199 USA. [Ikenaga, Makoto] Ritsumeikan Univ, Coll Life Sci, Dept Biosci & Biotechnol, Kusatsu, Shiga 5258577, Japan. [Condit, Richard; Perez, Rolando] Smithsonian Trop Res Inst, Ancon, Panama, Panama. [Gann, George D.] Inst Reg Conservat, Miami, FL 33176 USA. [Childers, Daniel L.] Arizona State Univ, Global Inst Sustainabil, Tempe, AZ 85287 USA. [Childers, Daniel L.] Arizona State Univ, Sch Sustainabil, Tempe, AZ 85287 USA. RP Troxler, TG (reprint author), Florida Int Univ, SE Environm Res Ctr, 11200 SW 8th St,OE 148, Miami, FL 33199 USA. EM troxlert@fiu.edu FU Smithsonian Tropical Research Institute; National Science Foundation [DBI-0620409, DEB-9910514] FX The authors would like to acknowledge B. Giraldo, G. Jacome, P. Gondola, E. Brown, M. Barry, D. Johnson and I. Mendoza for field, lab and logistical assistance. Drs. S. Davis, D. Liptzin and J. Edmonds provided helpful comments on earlier drafts of this manuscript. We are grateful to the Smithsonian Tropical Research Institute and R. Collins for assistance with travel funding through a fellowship to T. Troxler. This material is based upon work supported by the National Science Foundation through the Florida Coastal Everglades Long-Term Ecological Research program under Grants No. DBI-0620409 and No. DEB-9910514. This is contribution #548 of the Southeast Environmental Research Center at Florida International University. NR 61 TC 7 Z9 7 U1 1 U2 31 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 EI 1943-6246 J9 WETLANDS JI Wetlands PD AUG PY 2012 VL 32 IS 4 BP 769 EP 782 DI 10.1007/s13157-012-0310-z PG 14 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 976ON UT WOS:000306594300015 ER PT J AU Hershler, R Liu, HP Clark, WH AF Hershler, Robert Liu, Hsiu-Ping Clark, William H. TI Comments on "The absence of genotypic diversity in a successful parthenogenetic invader" by Mark Dybdahl and Devin Drown [Biological Invasions 13 (2011), 1663-1672] SO BIOLOGICAL INVASIONS LA English DT Editorial Material DE Invasive species; New Zealand mudsnail; Microsatellites; Genetic diversity; Allele scoring ID POTAMOPYRGUS-ANTIPODARUM; MICROSATELLITE LOCI; GENETIC-VARIATION; MUTATION HISTORY; POPULATIONS; SNAIL; RECONSTRUCTION; PATTERNS; ALLELE AB We contend that a recent study of microsatellite variation in invasive populations of the New Zealand mudsnail in the United States (Dybdahl and Drown 2011) underestimated genotypic diversity because it inappropriately focused on allelic size ranges that were previously documented for (invasive) British populations. The authors ignored peaks that were "far outside" of these size ranges, thus precluding recognition of additional alleles, including those that have been reported in other populations of this species. We are also concerned about the lack of reproducibility in the scoring methods utilized because the authors did not define a threshold for deciding when peaks should be ignored. The extent to which genotypic diversity consequently has been underestimated and otherwise inaccurately described cannot be ascertained based on the data provided in this study. C1 [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Liu, Hsiu-Ping] Metropolitan State Coll Denver, Dept Biol, Denver, CO 80217 USA. [Clark, William H.] Coll Idaho, Orma J Smith Museum Nat Hist, Caldwell, ID 83605 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, POB 37012,NHB W-305,MRC 163, Washington, DC 20013 USA. EM hershlerr@si.edu NR 13 TC 2 Z9 2 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD AUG PY 2012 VL 14 IS 8 BP 1643 EP 1645 DI 10.1007/s10530-012-0184-2 PG 3 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 973DL UT WOS:000306334500011 ER PT J AU Swenson, NG Enquist, BJ Pither, J Kerkhoff, AJ Boyle, B Weiser, MD Elser, JJ Fagan, WF Forero-Montana, J Fyllas, N Kraft, NJB Lake, JK Moles, AT Patino, S Phillips, OL Price, CA Reich, PB Quesada, CA Stegen, JC Valencia, R Wright, IJ Wright, SJ Andelman, S Jorgensen, PM Lacher, TE Monteagudo, A Nunez-Vargas, MP Vasquez-Martinez, R Nolting, KM AF Swenson, Nathan G. Enquist, Brian J. Pither, Jason Kerkhoff, Andrew J. Boyle, Brad Weiser, Michael D. Elser, James J. Fagan, William F. Forero-Montana, Jimena Fyllas, Nikolaos Kraft, Nathan J. B. Lake, Jeffrey K. Moles, Angela T. Patino, Sandra Phillips, Oliver L. Price, Charles A. Reich, Peter B. Quesada, Carlos A. Stegen, James C. Valencia, Renato Wright, Ian J. Wright, S. Joseph Andelman, Sandy Jorgensen, Peter M. Lacher, Thomas E., Jr. Monteagudo, Abel Percy Nunez-Vargas, M. Vasquez-Martinez, Rodolfo Nolting, Kristen M. TI The biogeography and filtering of woody plant functional diversity in North and South America SO GLOBAL ECOLOGY AND BIOGEOGRAPHY LA English DT Article DE Biogeography; functional diversity; functional traits; latitudinal gradient; species richness ID COMMUNITY ASSEMBLY RULES; GLOBAL PATTERNS; SEED SIZE; FOREST IMPLICATIONS; ECONOMICS SPECTRUM; SPECIES RICHNESS; TRAIT; PHOSPHORUS; STOICHIOMETRY; TEMPERATURE AB Aim In recent years evidence has accumulated that plant species are differentially sorted from regional assemblages into local assemblages along local-scale environmental gradients on the basis of their function and abiotic filtering. The favourability hypothesis in biogeography proposes that in climatically difficult regions abiotic filtering should produce a regional assemblage that is less functionally diverse than that expected given the species richness and the global pool of traits. Thus it seems likely that differential filtering of plant traits along local-scale gradients may scale up to explain the distribution, diversity and filtering of plant traits in regional-scale assemblages across continents. The present work aims to address this prediction. Location North and South America. Methods We combine a dataset comprising over 5.5 million georeferenced plant occurrence records with several large plant functional trait databases in order to: (1) quantify how several critical traits associated with plant performance and ecology vary across environmental gradients; and (2) provide the first test of whether the woody plants found within 1 degrees and 5 degrees map grid cells are more or less functionally diverse than expected, given their species richness, across broad gradients. Results The results show that, for many of the traits studied, the overall distribution of functional traits in tropical regions often exceeds the expectations of random sampling given the species richness. Conversely, temperate regions often had narrower functional trait distributions than their smaller species pools would suggest. Main conclusion The results show that the overall distribution of function does increase towards the equator, but the functional diversity within regional-scale tropical assemblages is higher than that expected given their species richness. These results are consistent with the hypothesis that abiotic filtering constrains the overall distribution of function in temperate assemblages, but tropical assemblages are not as tightly constrained. C1 [Swenson, Nathan G.; Lake, Jeffrey K.; Nolting, Kristen M.] Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. [Enquist, Brian J.; Boyle, Brad; Stegen, James C.] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ 85721 USA. [Enquist, Brian J.; Andelman, Sandy] Conservat Int, Arlington, VA 22202 USA. [Enquist, Brian J.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Pither, Jason] Univ British Columbia, Dept Biol & Phys Geog, Kelowna, BC, Canada. [Kerkhoff, Andrew J.] Kenyon Coll, Dept Biol, Gambier, OH 43022 USA. [Kerkhoff, Andrew J.] Kenyon Coll, Dept Math, Gambier, OH 43022 USA. [Weiser, Michael D.] N Carolina State Univ, Dept Zool, Raleigh, NC 27695 USA. [Elser, James J.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Forero-Montana, Jimena] Univ Puerto Rico, Dept Biol, Rio Piedras, PR 00931 USA. [Fyllas, Nikolaos; Phillips, Oliver L.; Quesada, Carlos A.] Univ Leeds, Sch Geog, Leeds LS2 9JT, W Yorkshire, England. [Kraft, Nathan J. B.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Moles, Angela T.] Univ New S Wales, Sch Biol Earth & Environm Sci, Evolut & Ecol Res Ctr, Sydney, NSW 2052, Australia. [Patino, Sandra] Univ Nacl Colombia Amazonia, Amazonas, Colombia. [Price, Charles A.] Univ Western Australia, Sch Plant Biol, Crawley, WA 6009, Australia. [Reich, Peter B.] Univ Minnesota, Dept Forest Resources, St Paul, MN 55108 USA. [Valencia, Renato] Univ Catolica Ecuador, Escuela Ciencias Biol, Lab Ecol Plantas, Quito, Ecuador. [Wright, Ian J.] Macquarie Univ, Dept Biol Sci, Sydney, NSW 2109, Australia. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Monteagudo, Abel; Vasquez-Martinez, Rodolfo] Missouri Bot Garden, Proyecto Flora Peru, St Louis, MO 63166 USA. [Lacher, Thomas E., Jr.] Texas A&M Univ, Dept Wildlife & Fisheries Sci, College Stn, TX 77843 USA. [Percy Nunez-Vargas, M.] Univ San Antonio Abad Cusco, Herbario Vargas, Cuzco, Peru. RP Swenson, NG (reprint author), Michigan State Univ, Dept Plant Biol, E Lansing, MI 48824 USA. EM swensonn@msu.edu RI Kraft, Nathan/A-2817-2012; Phillips, Oliver/A-1523-2011; Price, Charles/B-1171-2011; Elser, James/A-7082-2008; Weiser, Michael/E-6215-2011; Swenson, Nathan/A-3514-2012; Wright, Ian/G-4979-2012; Wright, Stuart/M-3311-2013; Moles, Angela/C-3083-2008; Stegen, James/Q-3078-2016 OI Enquist, Brian/0000-0002-6124-7096; Fyllas, Nikolaos/0000-0002-5651-5578; Kraft, Nathan/0000-0001-8867-7806; Phillips, Oliver/0000-0002-8993-6168; Elser, James/0000-0002-1460-2155; Weiser, Michael/0000-0001-9080-0834; Swenson, Nathan/0000-0003-3819-9767; Wright, Ian/0000-0001-8338-9143; Wright, Stuart/0000-0003-4260-5676; Moles, Angela/0000-0003-2041-7762; Stegen, James/0000-0001-9135-7424 FU Michigan State University; NSF; Missouri Botanical Gardens; Conservational International FX N.G.S. is supported by Michigan State University. B.J.E. is supported by funding from the NSF. This work was made possible by support from the Missouri Botanical Gardens and Conservational International. NR 47 TC 58 Z9 60 U1 9 U2 116 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1466-822X EI 1466-8238 J9 GLOBAL ECOL BIOGEOGR JI Glob. Ecol. Biogeogr. PD AUG PY 2012 VL 21 IS 8 BP 798 EP 808 DI 10.1111/j.1466-8238.2011.00727.x PG 11 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 972JW UT WOS:000306274400003 ER PT J AU Hinde, K German, JB AF Hinde, Katie German, J. Bruce TI Food in an evolutionary context: insights from mother's milk SO JOURNAL OF THE SCIENCE OF FOOD AND AGRICULTURE LA English DT Article DE lactation; infant development; gene-culture co-evolution; dairy; personalised medicine; obesity; nutrition; mammalian evolution ID MACACA-MULATTA; LACTATION; TEMPERAMENT; PREFERENCES; ADAPTATIONS; BEHAVIOR; GENOME; BREAST; CATTLE; ACIDS AB In the emergence of diverse animal life forms, food is the most insistent and pervasive of environmental pressures. As the life sciences begin to understand organisms in genomic detail, evolutionary perspectives provide compelling insights into the results of these dynamic interactions between food and consumer. Such an evolutionary perspective is particularly needed today in the face of unprecedented capabilities to alter the food supply. What should we change? Answering this question for food production, safety and sustainability will require a much more detailed understanding of the complex interplay between humans and their food. Many organisms that we grow, produce, process and consume as foods naturally evolved adaptations in part to avoid being eaten. Crop breeding and processing have been the tools to convert overtly toxic and antinutritious commodities into foods that are safe to eat. Now the challenge is to enhance the nutritional quality and thereby contribute to improving human health. We posit that the Rosetta stone of food and nourishment is mammalian lactation and mother's milk. The milk that a mammalian mother produces for her young is a complete and comprehensive diet. Moreover, the capacity of the mammary gland as a remarkable bioreactor to synthesise milk, and the infant to utilise milk, reflects 200 million years of symbiotic co-evolution between producer and consumer. Here we present emerging transdisciplinary research decoding mother's milk from humans and other mammals. We further discuss how insights from mother's milk have important implications for food science and human health. Copyright (C) 2012 Society of Chemical Industry C1 [German, J. Bruce] Univ Calif Davis, Dept Food Sci & Technol, Davis, CA 95616 USA. [Hinde, Katie] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Hinde, Katie] Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA USA. [Hinde, Katie] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. [Hinde, Katie; German, J. Bruce] Univ Calif Davis, Foods Hlth Inst, Davis, CA 95616 USA. RP German, JB (reprint author), Univ Calif Davis, Dept Food Sci & Technol, Davis, CA 95616 USA. EM jbgerman@ucdavis.edu OI Hinde, Katie/0000-0002-0528-866X FU University of California Discovery Grant Program; National Institute on Environmental Health Sciences Superfund [P42 ES02710]; Childhood Autism Risks from Genetics and the Environment Study [P01 ES11269]; National Institutes of Health-National Institute of Child Health and Human Development Awards [5R01HD059127, 1R01HD061923]; National Science Foundation [BCS-0921978] FX We thank Alexandra Carrick for providing the opportunity to write this perspective, and two anonymous reviewers for their thoughtful comments on an earlier draft of the manuscript. This publication was made possible in part by support from the University of California Discovery Grant Program, the National Institute on Environmental Health Sciences Superfund P42 ES02710, the Childhood Autism Risks from Genetics and the Environment Study Grant P01 ES11269, the National Institutes of Health-National Institute of Child Health and Human Development Awards 5R01HD059127 and 1R01HD061923 and the National Science Foundation Grant BCS-0921978. NR 35 TC 11 Z9 12 U1 0 U2 51 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-5142 J9 J SCI FOOD AGR JI J. Sci. Food Agric. PD AUG PY 2012 VL 92 IS 11 BP 2219 EP 2223 DI 10.1002/jsfa.5720 PG 5 WC Agriculture, Multidisciplinary; Chemistry, Applied; Food Science & Technology SC Agriculture; Chemistry; Food Science & Technology GA 973ZX UT WOS:000306400500001 PM 22729619 ER PT J AU White, M Myers, AD Ross, NP Schlegel, DJ Hennawi, JF Shen, Y McGreer, I Strauss, MA Bolton, AS Bovy, J Fan, X Miralda-Escude, J Palanque-Delabrouille, N Paris, I Petitjean, P Schneider, DP Viel, M Weinberg, DH Yeche, C Zehavi, I Pan, K Snedden, S Bizyaev, D Brewington, H Brinkmann, J Malanushenko, V Malanushenko, E Oravetz, D Simmons, A Sheldon, A Weaver, BA AF White, Martin Myers, Adam D. Ross, Nicholas P. Schlegel, David J. Hennawi, Joseph F. Shen, Yue McGreer, Ian Strauss, Michael A. Bolton, Adam S. Bovy, Jo Fan, X. Miralda-Escude, Jordi Palanque-Delabrouille, N. Paris, I. Petitjean, P. Schneider, D. P. Viel, M. Weinberg, David H. Yeche, Ch Zehavi, I. Pan, K. Snedden, S. Bizyaev, D. Brewington, H. Brinkmann, J. Malanushenko, V. Malanushenko, E. Oravetz, D. Simmons, A. Sheldon, A. Weaver, Benjamin A. TI The clustering of intermediate-redshift quasars as measured by the Baryon Oscillation Spectroscopic Survey SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE quasars: general; cosmology: observations; large-scale structure of Universe ID DIGITAL-SKY-SURVEY; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; PHOTOMETRICALLY CLASSIFIED QUASARS; STAR-FORMING GALAXIES; 2-POINT CORRELATION-FUNCTION; LUMINOUS RED GALAXIES; DARK-MATTER HALOES; DATA RELEASE; TARGET SELECTION AB We measure the quasar two-point correlation function over the redshift range 2.2 < z < 2.8 using data from the Baryon Oscillation Spectroscopic Survey. We use a homogeneous subset of the data consisting of 27 129 quasars with spectroscopic redshifts by far the largest such sample used for clustering measurements at these redshifts to date. The sample covers 3600 deg(2), corresponding to a comoving volume of 9.7 (h(-1) Gpc)(3) assuming a fiducial Lambda cold dark matter cosmology, and it has a median absolute i-band magnitude of -26, k-corrected to z= 2. After accounting for redshift errors we find that the redshift-space correlation function is fitted well by a power law of slope -2 and amplitude s(0)=(9.7 +/- 0.5)h(-1) Mpc over the range 3 < s < 25 h(-1) Mpc. The projected correlation function, which integrates out the effects of peculiar velocities and redshift errors, is fitted well by a power law of slope -1 and r(0)=(8.4 +/- 0.6)h(-1) Mpc over the range 4 < R < 16 h(-1) Mpc. There is no evidence for strong luminosity or redshift dependence to the clustering amplitude, in part because of the limited dynamic range in our sample. Our results are consistent with, but more precise than, previous measurements at similar redshifts. Our measurement of the quasar clustering amplitude implies a bias factor of b similar or equal to 3.5 for our quasar sample. We compare the data to models to constrain the manner in which quasars occupy dark matter haloes at z similar to 2.4 and infer that such quasars inhabit haloes with a characteristic mass of < M > similar or equal to 10(12) h(-1) M-circle dot with a duty cycle for the quasar activity of 1 per cent. C1 [White, Martin; Ross, Nicholas P.; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [White, Martin] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Myers, Adam D.; Hennawi, Joseph F.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McGreer, Ian] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Bolton, Adam S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Bovy, Jo; Fan, X.] Inst Adv Study, Princeton, NJ 08540 USA. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis Avancats, Barcelona 08010, Spain. [Miralda-Escude, Jordi] Inst Ciencies Cosmos IEEC UB, Barcelona 08034, Spain. [Palanque-Delabrouille, N.; Yeche, Ch] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Paris, I.; Petitjean, P.] Univ Paris 06, F-75014 Paris, France. [Paris, I.; Petitjean, P.] Inst Astrophys Paris, CNRS, F-75014 Paris, France. [Schneider, D. P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, D. P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Viel, M.] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Zehavi, I.] Case Western Reserve Univ, Dept Astron, Cleveland, OH 44106 USA. [Pan, K.; Snedden, S.; Brewington, H.; Brinkmann, J.; Malanushenko, V.; Malanushenko, E.; Oravetz, D.; Simmons, A.; Sheldon, A.] Apache Point Observ, Sunspot, NM 88349 USA. [Bizyaev, D.; Weaver, Benjamin A.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. RP White, M (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, 1 Cyclotron Rd, Berkeley, CA 94720 USA. EM mwhite@berkeley.edu RI White, Martin/I-3880-2015; OI White, Martin/0000-0001-9912-5070; Miralda-Escude, Jordi/0000-0002-2316-8370; Viel, Matteo/0000-0002-2642-5707; Bovy, Jo/0000-0001-6855-442X FU Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; US Department of Energy Office of Science; NSF; NASA [HST-HF-51285.01]; Spanish grants [AYA2009-09745, PR2011-0431]; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the US Department of Energy Office of Science. The SDSS-III website is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University.; MW was supported by the NSF and NASA. ADM is a research fellow of the Alexander von Humboldt Foundation of Germany. JM-E is supported by Spanish grants AYA2009-09745 and PR2011-0431. JB was partially supported by a NASA Hubble Fellowship (HST-HF-51285.01). NR 142 TC 74 Z9 74 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 AUG PY 2012 VL 424 IS 2 BP 933 EP 950 DI 10.1111/j.1365-2966.2012.21251.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800011 ER PT J AU Hayward, CC Jonsson, P Keres, D Magnelli, B Hernquist, L Cox, TJ AF Hayward, Christopher C. Jonsson, Patrik Keres, Dusan Magnelli, Benjamin Hernquist, Lars Cox, T. J. TI How to distinguish starbursts and quiescently star-forming galaxies: the 'bimodal' submillimetre galaxy population as a case study SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE radiative transfer; stars: formation; galaxies: high-redshift; galaxies: starburst; infrared: galaxies; submillimetre: galaxies ID SIMILAR-TO 2; ULTRALUMINOUS INFRARED GALAXIES; SMOOTHED PARTICLE HYDRODYNAMICS; SPECTRAL ENERGY-DISTRIBUTIONS; DEGREE EXTRAGALACTIC SURVEY; ACTIVE GALACTIC NUCLEI; HIGH-REDSHIFT GALAXIES; QUASAR LUMINOSITY FUNCTION; SUPERMASSIVE BLACK-HOLES; CO-H2 CONVERSION FACTOR AB In recent work, we have suggested that the high-redshift (z similar to 24) bright submillimetre galaxy (SMG) population is heterogeneous, with major mergers contributing both at early stages, where quiescently star-forming discs are blended into one submm source (galaxy-pair SMGs), and at late stages, where mutual tidal torques drive gas inflows and cause strong starbursts. Here we combine hydrodynamic simulations of major mergers with 3D dust radiative transfer calculations to determine observational diagnostics that can distinguish between quiescently star-forming SMGs and starburst SMGs via integrated data alone. We fit the far-infrared (FIR) spectral energy distributions of the simulated galaxies with the optically thin single-temperature modified blackbody, the full form of the single-temperature modified blackbody and a power-law temperature distribution model. The effective dust temperature, Td, and power-law index of the dust emissivity in the FIR, beta, derived can significantly depend on the fitting form used, and the intrinsic beta of the dust is not recovered. However, for all forms used here, there is Td above which almost all simulated galaxies are starbursts, so a Td cut is very effective at selecting starbursts. Simulated merger-induced starbursts also have higher LIR/Mgas and LIR/LFUV than quiescently star-forming galaxies and lie above the star formation ratestellar mass relation. These diagnostics can be used to test our claim that the SMG population is heterogeneous and to observationally determine what star formation mode dominates a given galaxy population. We comment on applicability of these diagnostics to ultraluminous IR galaxies (ULIRGs) that would not be selected as SMGs. These hot-dust ULIRGs are typically starburst galaxies lower in mass than SMGs, but they can also simply be SMGs observed from a different viewing angle. C1 [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. [Hayward, Christopher C.; Jonsson, Patrik; Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Keres, Dusan] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Keres, Dusan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Magnelli, Benjamin] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. RP Hayward, CC (reprint author), Heidelberger Inst Theoret Studien, Schloss Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany. EM christopher.hayward@h-its.org RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU NASA [HST-HF-51276.01-A]; W. M. Keck Foundation; FAS Research Computing Group at Harvard University FX CCH thanks Emanuele Daddi for motivation for this work, Padelis Papadopoulos and Rahul Shetty for lively discussion of IR SED fitting and Shane Bussmann, Diego Munoz and Dominik Riechers for insight into submm interferometry. We thank the anonymous referee, Caitlin Casey, Helmut Dannerbauer, Michal Michalowski, Alex Pope and Amy Stutz for helpful comments on the manuscript. We thank Volker Springel for providing the non-public version of GADGET-2 used for this work and Brant Robertson for use of his code to scale the initial conditions to high redshift. DK is supported by NASA through Hubble Fellowship grant HST-HF-51276.01-A. PJ acknowledges support by a grant from the W. M. Keck Foundation. The simulations in this paper were performed on the Odyssey cluster supported by the FAS Research Computing Group at Harvard University. NR 203 TC 53 Z9 53 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 AUG PY 2012 VL 424 IS 2 BP 951 EP 970 DI 10.1111/j.1365-2966.2012.21254.x PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800012 ER PT J AU Tremblay, GR O'Dea, CP Baum, SA Clarke, TE Sarazin, CL Bregman, JN Combes, F Donahue, M Edge, AC Fabian, AC Ferland, GJ McNamara, BR Mittal, R Oonk, JBR Quillen, AC Russell, HR Sanders, JS Salome, P Voit, GM Wilman, RJ Wise, MW AF Tremblay, G. R. O'Dea, C. P. Baum, S. A. Clarke, T. E. Sarazin, C. L. Bregman, J. N. Combes, F. Donahue, M. Edge, A. C. Fabian, A. C. Ferland, G. J. McNamara, B. R. Mittal, R. Oonk, J. B. R. Quillen, A. C. Russell, H. R. Sanders, J. S. Salome, P. Voit, G. M. Wilman, R. J. Wise, M. W. TI Multiphase signatures of active galactic nucleus feedback in Abell 2597 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: individual: Abell 2597; galaxies: clusters: intracluster medium; galaxies: star formation ID X-RAY SPECTROSCOPY; RADIO GALAXIES; CHANDRA OBSERVATION; GASEOUS ATMOSPHERE; BUOYANT BUBBLES; STAR-FORMATION; EMITTING GAS; CLUSTERS; FILAMENTS; A2597 AB We present new Chandra X-ray observations of the brightest cluster galaxy (BCG) in the cool-core cluster Abell 2597 (z= 0.0821). The data reveal an extensive kpc-scale X-ray cavity network as well as a 15-kpc filament of soft-excess gas exhibiting strong spatial correlation with archival Very Large Array radio data. In addition to several possible scenarios, multiwavelength evidence may suggest that the filament is associated with multiphase (103107 K) gas that has been entrained and dredged-up by the propagating radio source. Stemming from a full spectral analysis, we also present profiles and 2D spectral maps of modelled X-ray temperature, entropy, pressure and metal abundance. The maps reveal an arc of hot gas which in projection borders the inner edge of a large X-ray cavity. Although limited by strong caveats, we suggest that the hot arc may be (a) due to a compressed rim of cold gas pushed outwards by the radio bubble or (b) morphologically and energetically consistent with cavity-driven active galactic nucleus heating models invoked to quench cooling flows, in which the enthalpy of a buoyant X-ray cavity is locally thermalized as ambient gas rushes to refill its wake. If confirmed, this would be the first observational evidence for this model. C1 [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. [Tremblay, G. R.; O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Tremblay, G. R.; Baum, S. A.; Mittal, R.] Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [O'Dea, C. P.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Baum, S. A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Clarke, T. E.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Bregman, J. N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Combes, F.; Salome, P.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Edge, A. C.; Wilman, R. J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ferland, G. J.] Univ Kentucky, Dept Phys, Lexington, KY 40506 USA. [McNamara, B. R.; Russell, H. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [Oonk, J. B. R.; Wise, M. W.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Quillen, A. C.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Tremblay, GR (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM grant.tremblay@eso.org OI Edge, Alastair/0000-0002-3398-6916; Tremblay, Grant/0000-0002-5445-5401; Sanders, Jeremy/0000-0003-2189-4501; Combes, Francoise/0000-0003-2658-7893; Ferland, Gary/0000-0003-4503-6333; Voit, Gerard/0000-0002-3514-0383 FU NASA/NY Space Grant Consortium; European Southern Observatory (ESO); European Community [229517]; NASA through JPL/Caltech; Radcliffe Institute for Advanced Study at Harvard University; NASA [G06-7115B, NAS8-39073, RSA 1373266, RSA P12-78175, G01-12169X, NAS8-03060, 5-26555]; 6.1 Base funds FX The authors thank Drs Elaine Sadler, Robert Laing, Andy Robinson, Joel Kastner and Bill Sparks for thoughtful discussions. We also thank the anonymous referee for constructive feedback. GRT is grateful to Ruth Smith, and acknowledges support from the NASA/NY Space Grant Consortium, as well as a European Southern Observatory (ESO) Fellowship partially funded by the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. Partial support was provided by NASA through an award issued by JPL/Caltech, as well as the Radcliffe Institute for Advanced Study at Harvard University. TEC was partially supported by NASA through Chandra award G06-7115B issued by the Chandra X-ray Observatory Center for and on behalf of NASA under contract NAS8-39073. Basic research into radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funds. CLS was supported in part by NASA Herschel Grants RSA 1373266, RSA P12-78175 and Chandra Grant G01-12169X. ACF thanks the Royal Society. This paper is based upon observations with the Chandra X-ray Observatory, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. We also make use of previously published observations by 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 5-26555. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities Inc. We have made extensive use of the NASA Astrophysics Data System bibliographic services and the NASA/IPAC Extragalactic Database, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 50 TC 9 Z9 9 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 AUG PY 2012 VL 424 IS 2 BP 1026 EP 1041 DI 10.1111/j.1365-2966.2012.21281.x PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800017 ER PT J AU Tremblay, GR O'Dea, CP Baum, SA Clarke, TE Sarazin, CL Bregman, JN Combes, F Donahue, M Edge, AC Fabian, AC Ferland, GJ McNamara, BR Mittal, R Oonk, JBR Quillen, AC Russell, HR Sanders, JS Salome, P Voit, GM Wilman, RJ Wise, MW AF Tremblay, G. R. O'Dea, C. P. Baum, S. A. Clarke, T. E. Sarazin, C. L. Bregman, J. N. Combes, F. Donahue, M. Edge, A. C. Fabian, A. C. Ferland, G. J. McNamara, B. R. Mittal, R. Oonk, J. B. R. Quillen, A. C. Russell, H. R. Sanders, J. S. Salome, P. Voit, G. M. Wilman, R. J. Wise, M. W. TI Residual cooling and persistent star formation amid active galactic nucleus feedback in Abell 2597 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Review DE galaxies: active; galaxies: clusters: general; galaxies: clusters: individual: Abell 2597; galaxies: clusters: intracluster medium; galaxies: star formation ID BRIGHTEST CLUSTER GALAXIES; POWERFUL RADIO GALAXIES; RAY-LUMINOUS CLUSTERS; FAR-ULTRAVIOLET OBSERVATIONS; MOLECULAR-HYDROGEN EMISSION; DEEP CHANDRA OBSERVATION; H-ALPHA FILAMENTS; FLOW CLUSTERS; XMM-NEWTON; PERSEUS CLUSTER AB New Chandra X-ray and Herschel Far-Infrared (FIR) observations enable a multiwavelength study of active galactic nucleus (AGN) heating and intracluster medium (ICM) cooling in the brightest cluster galaxy (BCG) of Abell 2597 (z= 0.0821). The new Chandra observations reveal the central ?30 kpc X-ray cavity network to be more extensive than previously thought, and associated with enough enthalpy to theoretically inhibit the inferred classical cooling flow. Nevertheless, we present new evidence, consistent with previous results, that a moderately strong residual cooling flow is persisting at 48 per cent of the classically predicted rates in a spatially structured manner amid the feedback-driven excavation of the X-ray cavity network. New Herschel observations are used to estimate warm and cold dust masses, a lower limit gas-to-dust ratio and a star formation rate consistent with previous measurements. [O i] and CO(2-1) line profiles are used to constrain the kinematics of the similar to 109 M? reservoir of cold molecular gas. The cooling time profile of the ambient X-ray atmosphere is used to map the locations of the observational star formation entropy threshold as well as the theoretical thermal instability threshold. Both lie just outside the ?30-kpc central region permeated by X-ray cavities, and star formation as well as ionized and molecular gas lie interior to both. The young stars are distributed in an elongated region that is aligned with the radio lobes, and their estimated ages are both younger and older than the X-ray cavity network, suggesting both jet-triggered as well as persistent star formation over the current AGN feedback episode. Bright X-ray knots that are coincident with extended Lya and far-ultraviolet continuum filaments motivate a discussion of structured cooling from the ambient hot atmosphere along a projected axis that is perpendicular to X-ray cavity and radio axis. We conclude that the cooling ICM is the dominant contributor of the cold gas reservoir fuelling star formation and AGN activity in the Abell 2597 BCG. C1 [Tremblay, G. R.] European So Observ, D-85748 Garching, Germany. [Tremblay, G. R.; O'Dea, C. P.] Rochester Inst Technol, Dept Phys, Rochester, NY 14623 USA. [Tremblay, G. R.; Baum, S. A.; Mittal, R.] Chester F Carlson Ctr Imaging Sci, Rochester, NY 14623 USA. [O'Dea, C. P.; McNamara, B. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Baum, S. A.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. [Clarke, T. E.] USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Bregman, J. N.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Combes, F.; Salome, P.] CNRS, Observ Paris, LERMA, F-75014 Paris, France. [Donahue, M.; Voit, G. M.] Michigan State Univ, Dept Phys & Astron, E Lansing, MI 48824 USA. [Edge, A. C.; Wilman, R. J.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Fabian, A. C.; Sanders, J. S.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Ferland, G. J.] Univ Kentucky, Dept Phys, Lexington, KY 40506 USA. [McNamara, B. R.; Russell, H. R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. [Oonk, J. B. R.; Wise, M. W.] Netherlands Inst Radio Astron, ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Quillen, A. C.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. RP Tremblay, GR (reprint author), European So Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM grant.tremblay@eso.org OI Edge, Alastair/0000-0002-3398-6916; Combes, Francoise/0000-0003-2658-7893; Tremblay, Grant/0000-0002-5445-5401; Ferland, Gary/0000-0003-4503-6333; Sanders, Jeremy/0000-0003-2189-4501; Voit, Gerard/0000-0002-3514-0383 FU NASA/NY Space Grant Consortium; European Southern-Observatory (ESO); European Community [229517]; NASA through JPL/Caltech; Radcliffe Institute for Advanced Study at Harvard University; NASA through Chandra award [G06-7115B]; NASA [NAS8-39073, RSA 1373266, RSA P12-78175, NAS8-03060, 5-26555]; 6.1 Base funds; Chandra Grant [G01-12169X] FX The authors thank Drs Elaine Sadler, Robert Laing, Andy Robinson, Joel Kastner and Bill Sparks for thoughtful discussions. We also thank the anonymous referee for constructive feedback. GRT is grateful to Ruth Smith, and acknowledges support from the NASA/NY Space Grant Consortium, as well as a European Southern-Observatory (ESO) Fellowship partially funded by the European Community's Seventh Framework Programme (/FP7/2007-2013/) under grant agreement No. 229517. Partial support was provided by NASA through an award issued by JPL/Caltech, as well as the Radcliffe Institute for Advanced Study at Harvard University. TEC was partially supported by NASA through Chandra award G06-7115B issued by the Chandra X-ray Observatory Center for and on behalf of NASA under contract NAS8-39073. Basic research into radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funds. CLS was supported in part by NASA Herschel Grants RSA 1373266, RSA P12-78175 and Chandra Grant G01-12169X. ACF thanks the Royal Society. This paper is based upon observations with the Chandra X-ray Observatory, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. We also present observations made with the Herschel Space Observatory, a European Space Agency Cornerstone Mission with significant participation by NASA. We make use of previously published observations by 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 5-26555. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities Inc. We have made extensive use of the NASA Astrophysics Data System bibliographic services and the NASA/IPAC Extragalactic Database, operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. NR 183 TC 15 Z9 16 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 AUG PY 2012 VL 424 IS 2 BP 1042 EP 1060 DI 10.1111/j.1365-2966.2012.21278.x PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800018 ER PT J AU Wyatt, MC Kennedy, G Sibthorpe, B Moro-Martin, A Lestrade, JF Ivison, RJ Matthews, B Udry, S Greaves, JS Kalas, P Lawler, S Su, KYL Rieke, GH Booth, M Bryden, G Horner, J Kavelaars, JJ Wilner, D AF Wyatt, M. C. Kennedy, G. Sibthorpe, B. Moro-Martin, A. Lestrade, J. -F. Ivison, R. J. Matthews, B. Udry, S. Greaves, J. S. Kalas, P. Lawler, S. Su, K. Y. L. Rieke, G. H. Booth, M. Bryden, G. Horner, J. Kavelaars, J. J. Wilner, D. TI Herschel imaging of 61 Vir: implications for the prevalence of debris in low-mass planetary systems SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: formation; planet-disc interactions; circumstellar matter; planetary systems ID SOLAR-TYPE STARS; SUN-LIKE STARS; STEADY-STATE EVOLUTION; TERRESTRIAL PLANETS; GIANT PLANETS; NEARBY STARS; SUPER-EARTHS; HOT DUST; HD 69830; DISKS AB This paper describes Herschel observations of the nearby (8.5 pc) G5V multi-exoplanet host star 61 Vir at 70, 100, 160, 250, 350 and 500 m carried out as part of the DEBRIS survey. These observations reveal emission that is significantly extended out to a distance of >15 arcsec with a morphology that can be fitted by a nearly edge-on (77 degrees inclination) radially broad (from 30 au out to at least 100 au) debris disc of fractional luminosity 2.7 x 10(-5), with two additional (presumably unrelated) sources nearby that become more prominent at longer wavelengths. Chance alignment with a background object seen at 1.4 GHz provides potential for confusion, however, the stars 1.4 arcsec yr-1 proper motion allows archival Spitzer 70 m images to confirm that what we are interpreting as disc emission really is circumstellar. Although the exact shape of the discs inner edge is not well constrained, the region inside 30 au must be significantly depleted in planetesimals. This is readily explained if there are additional planets outside those already known (i.e. in the 0.530 au region), but is also consistent with collisional erosion. We also find tentative evidence that the presence of detectable debris around nearby stars correlates with the presence of the lowest mass planets that are detectable in current radial velocity surveys. Out of an unbiased sample of the nearest 60 G stars, 11 are known to have planets, of which six (including 61 Vir) have planets that are all less massive than Saturn, and four of these have evidence for debris. The debris towards one of these planet hosts (HD 20794) is reported here for the first time. This fraction (4/6) is higher than that expected for nearby field stars (15 per cent), and implies that systems that form low-mass planets are also able to retain bright debris discs. We suggest that this correlation could arise because such planetary systems are dynamically stable and include regions that are populated with planetesimals in the formation process where the planetesimals can remain unperturbed over Gyr time-scales. C1 [Wyatt, M. C.; Kennedy, G.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Sibthorpe, B.; Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Moro-Martin, A.] Ctr Astrobiol CSIC INTA, Madrid 28850, Spain. [Lestrade, J. -F.] Observ Paris, F-75014 Paris, France. [Matthews, B.; Booth, M.; Kavelaars, J. J.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Udry, S.] Observ Univ Geneve, CH-1290 Versoix, Switzerland. [Greaves, J. S.] Univ St Andrews, Scottish Univ Phys Alliance, St Andrews KY16 9SS, Fife, Scotland. [Kalas, P.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kalas, P.] SETI Inst, Mountain View, CA 94043 USA. [Lawler, S.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Su, K. Y. L.; Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Booth, M.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 5C2, Canada. [Bryden, G.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Horner, J.] Univ New S Wales, Sch Phys, Dept Astrophys & Opt, Sydney, NSW 2052, Australia. [Wilner, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wyatt, MC (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM wyatt@ast.cam.ac.uk RI Ivison, R./G-4450-2011; OI Ivison, R./0000-0001-5118-1313; Booth, Mark/0000-0001-8568-6336; Horner, Jonti/0000-0002-1160-7970; Su, Kate/0000-0002-3532-5580; Kennedy, Grant/0000-0001-6831-7547 FU European Union through ERC [279973] FX The authors are grateful to Ben Zuckerman for helpful comments on the paper. This work was supported by the European Union through ERC grant number no. 279973. NR 93 TC 52 Z9 52 U1 0 U2 5 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 AUG PY 2012 VL 424 IS 2 BP 1206 EP 1223 DI 10.1111/j.1365-2966.2012.21298.x PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800030 ER PT J AU Heida, M Jonker, PG Torres, MAP Mineo, S AF Heida, M. Jonker, P. G. Torres, M. A. P. Mineo, S. TI Accurate positions for the ultraluminous X-ray sources NGC 7319-X4 and NGC 5474-X1 and limiting magnitudes for their optical counterparts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: individual: NGC 5474; galaxies: individual: NGC 7319; X-rays: binaries; X-rays: individual: NGC 5474-X1; X-rays: individual: NGC 7319-X4 ID SUPERMASSIVE BLACK-HOLES; SKY SURVEY; GALAXIES; SUPERNOVAE; EMISSION; MASS; CALIBRATION; BINARIES; REDSHIFT; SYSTEMS AB In this paper, we report accurate Chandra positions for two ultraluminous X-ray sources (ULXs): NGC 7319-X4 at Right Ascension (RA) = 339029 17(2), Declination (Dec.) = 33974 76(2) and NGC 5474-X1 at RA = 211248 59(3), Dec. = 53635 84(3). We perform bore-sight corrections on the Chandra X-ray satellite observations of these sources to get these accurate positions of the X-ray sources and match these positions with archival optical data from the Wide Field Planetary Camera 2 (WFPC2) onboard the Hubble Space Telescope. We do not find the optical counterparts; the limiting absolute magnitudes of the observations in the WFPC2 standard magnitude system are B=-7.9, V=-8.7 and I=-9.3 for NGC 7319-X4 and U=-6.4 for NGC 5474-X1. We report on the X-ray spectral properties and find evidence for X-ray variability in NGC 5474-X1. Finally, we briefly discuss several options for the nature of these ULXs. C1 [Heida, M.; Jonker, P. G.; Torres, M. A. P.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Heida, M.; Jonker, P. G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.; Torres, M. A. P.; Mineo, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Heida, M (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM m.heida@astro.ru.nl OI Mineo, Stefano/0000-0003-2908-0879 FU NASA [NAS 5-26555] FX MH and PGJ thank Richard Mushotzky for bringing NGC 7319-X4 to their attention. This research has made use of data obtained from the Chandra Data Archive, the Chandra Source Catalog and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. This paper is based on observations made with the NASA/ESA HST, obtained from the data archive at the Space Telescope Institute. STScI is operated by the association of Universities for Research in Astronomy, Inc. under the NASA contract NAS 5-26555. NR 38 TC 0 Z9 0 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 AUG PY 2012 VL 424 IS 2 BP 1563 EP 1569 DI 10.1111/j.1365-2966.2012.21370.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 973JQ UT WOS:000306356800060 ER PT J AU Collin, R AF Collin, Rachel TI Temperature-mediated trade-offs and changes in life-history integration in two slipper limpets (Gastropoda: Calyptraeidae) with planktotrophic development SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE adaptive phenotypic plasticity; phenotypic covariance; P-matrix; temperature-size rule ID FLY SCATHOPHAGA-STERCORARIA; EGG SIZE; PHENOTYPIC PLASTICITY; OFFSPRING SIZE; HATCHING SIZE; BODY-SIZE; CELL-SIZE; MARINE-INVERTEBRATES; REPRODUCTIVE OUTPUT; NUMBER AB Intraspecific variation in egg size and hatching size, and the genetic and environmental trade-offs that contribute to variation, are the basis of the evolution of life histories. The present study examined both univariate and multivariate temperature-mediated plasticity of life-history traits, as well as temperature-mediated trade-offs in egg size and clutch size, in two planktotrophic species of marine slipper limpets, Crepidula. Previous work with two species of Crepidula with large eggs and lecithotrophic development has shown a significant effect of temperature on egg size and hatching size. To further examine the effect of temperature on egg size in Crepidula, the effects of temperature on egg size and hatching size, as well as the possible trade-offs with other the life-history features, were examined for two planktotrophic species: Crepidula incurva and Crepidula cf. marginalis. Field-collected juveniles were raised at 23 or 28 degrees C and egg size, hatching size, capsules/brood, eggs/capsule, time to hatch, interbrood interval, and final body weight were recorded. Consistent with results for the lecithotrophic Crepidula, egg size and hatching size decreased with temperature in the planktotrophic species. The affects of maternal identity and individual brood account for more than half of the intraspecific variation in egg size and hatching size. Temperature also showed a significant effect on reproductive rate, with time to hatch and interbrood interval both decreasing with increasing temperature. However, temperature had contrasting effects on the number of offspring. Crepidula cf. marginalis has significantly more eggs/capsule and therefore more eggs per brood at 28 degrees C compared to 23 degrees C, although capsules/brood did not vary with temperature. Crepidula incurva, on the other hand, produced significantly more capsules/brood and more eggs per brood at the lower temperature, whereas the number of eggs/capsule did not vary with temperature. The phenotypic variancecovariance matrix of life-history variables showed a greater response to temperature in C. incurva than in C. cf. marginalis, and temperature induced trade-offs between offspring size and number differ between the species. These differences suggest that temperature changes as a result of seasonal upwelling along the coast of Panama will effect the reproduction and evolution of life histories of these two co-occurring species differently. (c) 2012 The Linnean Society of London, Biological Journal of the Linnean Society, 2012, , . C1 Smithsonian Trop Res Inst, Balboa, Panama. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Box 0843-03092, Balboa, Panama. EM collinr@si.edu FU Smithsonian Tropical Research Institute; United States National Science Foundation [IOS-1019727] FX I thank Maricela Salazar, Trinidad Prado, and Arianne Magallon for their help with animal maintenance and measurements. Katie McDonald wrote the IMAGEJ macro to measure larval shells and provided the equations for larval volume. I thank members of the Collin Laboratory discussion group and two anonymous reviewers for their helpful commented on previous versions of the manuscript. This project was supported by the Smithsonian Tropical Research Institute, and grant IOS-1019727 from the United States National Science Foundation. NR 64 TC 9 Z9 9 U1 1 U2 27 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD AUG PY 2012 VL 106 IS 4 BP 763 EP 775 DI 10.1111/j.1095-8312.2012.01908.x PG 13 WC Evolutionary Biology SC Evolutionary Biology GA 971RD UT WOS:000306220600005 ER PT J AU Chisholm, RA Levin, SA AF Chisholm, Ryan A. Levin, Simon A. TI Linking Dispersal and Immigration in Multidimensional Environments SO BULLETIN OF MATHEMATICAL BIOLOGY LA English DT Article DE Dispersal; Immigration ID INVADING ORGANISMS; COMMUNITIES; DYNAMICS; SPREAD; MODEL AB Many problems in ecology require the estimation of rates of dispersal of individuals or propagules across physical boundaries. Such problems arise in invasion ecology, forest dynamics, and the neutral theory of biodiversity. In a forest plot, for example, one might ask what proportion of the seed rain originates from outside the plot. A recent study presented analytical approximations that relate the rate of immigration across a boundary to plot geometry and to the parameters of a dispersal kernel in one- and two-dimensional environments. In this study, we provide a more rigorous derivation of these expressions and we derive a more general expression that applies in environments of arbitrary dimension. We discuss potential applications of the one-, two-, and three-dimensional results to ecological problems. C1 [Chisholm, Ryan A.; Levin, Simon A.] 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 USA. EM ryan.chis@gmail.com RI Chisholm, Ryan/H-8033-2012 FU Microstates to Macrodynamics: A New Mathematics of Biology, Defense Advanced Research Projects Agency [HR0011-05-1-0057] FX We thank William Allard, Frank Morgan, James O'Dwyer, Rachel Ward, and Hyam Rubenstein for helpful discussion. We thank two anonymous reviewers for comments that improved the manuscript. This research was partly funded by the grant, Microstates to Macrodynamics: A New Mathematics of Biology, Defense Advanced Research Projects Agency (HR0011-05-1-0057). NR 16 TC 3 Z9 3 U1 0 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0092-8240 J9 B MATH BIOL JI Bull. Math. Biol. PD AUG PY 2012 VL 74 IS 8 BP 1754 EP 1763 DI 10.1007/s11538-012-9734-0 PG 10 WC Biology; Mathematical & Computational Biology SC Life Sciences & Biomedicine - Other Topics; Mathematical & Computational Biology GA 970IP UT WOS:000306121900004 PM 22576454 ER PT J AU Sonsthagen, SA McClaren, EL Doyle, FI Titus, K Sage, GK Wilson, RE Gust, JR Talbot, SL AF Sonsthagen, Sarah A. McClaren, Erica L. Doyle, Frank I. Titus, Kimberly Sage, George K. Wilson, Robert E. Gust, Judy R. Talbot, Sandra L. TI Identification of metapopulation dynamics among Northern Goshawks of the Alexander Archipelago, Alaska, and Coastal British Columbia SO CONSERVATION GENETICS LA English DT Article DE Accipiter gentilis; Alexander Archipelago; British Columbia; Gene flow; Genetic structure; Metapopulation dynamics; Northern Goshawk ID EFFECTIVE POPULATION-SIZE; POLYMORPHIC MICROSATELLITE MARKERS; MAXIMUM-LIKELIHOOD-ESTIMATION; ALLELE FREQUENCY DATA; GENE FLOW; COALESCENT APPROACH; COMPUTER-PROGRAM; MIGRATION RATES; LOCI; DNA AB Northern Goshawks occupying the Alexander Archipelago, Alaska, and coastal British Columbia nest primarily in old-growth and mature forest, which results in spatial heterogeneity in the distribution of individuals across the landscape. We used microsatellite and mitochondrial data to infer genetic structure, gene flow, and fluctuations in population demography through evolutionary time. Patterns in the genetic signatures were used to assess predictions associated with the three population models: panmixia, metapopulation, and isolated populations. Population genetic structure was observed along with asymmetry in gene flow estimates that changed directionality at different temporal scales, consistent with metapopulation model predictions. Therefore, Northern Goshawk assemblages located in the Alexander Archipelago and coastal British Columbia interact through a metapopulation framework, though they may not fit the classic model of a metapopulation. Long-term population sources (coastal mainland British Columbia) and sinks (Revillagigedo and Vancouver islands) were identified. However, there was no trend through evolutionary time in the directionality of dispersal among the remaining assemblages, suggestive of a rescue-effect dynamic. Admiralty, Douglas, and Chichagof island complex appears to be an evolutionarily recent source population in the Alexander Archipelago. In addition, Kupreanof island complex and Kispiox Forest District populations have high dispersal rates to populations in close geographic proximity and potentially serve as local source populations. Metapopulation dynamics occurring in the Alexander Archipelago and coastal British Columbia by Northern Goshawks highlight the importance of both occupied and unoccupied habitats to long-term population persistence of goshawks in this region. C1 [Sonsthagen, Sarah A.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds & Labs Analyt Biol, Washington, DC 20013 USA. [McClaren, Erica L.] Minist Environm, Black Creek, BC V9J 1K1, Canada. [Doyle, Frank I.] Wildlife Dynam Consulting, Smithers, BC V0J 2N0, Canada. [Titus, Kimberly] Alaska Dept Fish & Game, Div Wildlife Conservat, Juneau, AK 99802 USA. [Wilson, Robert E.] Univ Alaska Fairbanks, Dept Biol & Wildlife, Fairbanks, AK 99775 USA. RP Sonsthagen, SA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Birds & Labs Analyt Biol, Washington, DC 20013 USA. EM ssonsthagen@usgs.gov FU Brigham Young University; US Geological Survey Alaska Science Center; US Forest Service; Environment Canada; US Fish and Wildlife Service FX This paper would not have been possible without the help from many individuals who provided field, logistic, and laboratory assistance. Funding was provided by Brigham Young University, US Geological Survey Alaska Science Center, US Forest Service, Environment Canada, and the US Fish and Wildlife Service. Technological support was provided by Shawn Houston, University of Alaska Life Science Informatics computer cluster (NIH P20RR016466). We especially thank the Bird Treatment and Learning Center in Anchorage, Alaska, for providing samples useful in marker development. CR Dial, J Rearick, and J Unland rendered laboratory assistance. The manuscript was improved by comments from P Beerli, Florida State University; S Boyce, US Forest Service; V Penteriani, Estacion Biologica de Donana, C.S.I.C.; and two anonymous reviewers. Mention of trade names or commercial products does not constitute endorsement or recommendation for use. NR 78 TC 4 Z9 4 U1 1 U2 36 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 AUG PY 2012 VL 13 IS 4 BP 1045 EP 1057 DI 10.1007/s10592-012-0352-z PG 13 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 969OD UT WOS:000306064100014 ER PT J AU Van Bael, SA Seid, MA Wcislo, WT AF Van Bael, Sunshine A. Seid, Marc A. Wcislo, William T. TI Endophytic fungi increase the processing rate of leaves by leaf-cutting ants (Atta) SO ECOLOGICAL ENTOMOLOGY LA English DT Article DE Atta colombica; Attini; foliar endophytes; insect agriculture; symbiosis ID CEPHALOTES L HYMENOPTERA; FORMICIDAE; GARDENS AB 1. Fungal endophytes are microfungi that reside asymptomatically inside of leaf tissues, increasing in density and diversity through time after leaves flush. Previous studies have suggested that the presence of fungal endophytes in the harvest material of leaf-cutting ants (Atta colombica, Guerin-Meneville) may negatively affect the ants and their fungal cultivar. 2. In the present study, it was tested whether the presence and diversity of fungal endophytes affected the amount of time necessary for leaf-cutter ants to cut, process, and plant leaf material in their fungal garden. It was found that ants took 3043% longer to cut, carry, clean, and plant leaf tissue with high relative to low endophyte abundance, and that the ants responded similarly to leaf tissue with high or low endophyte diversity. 3. It was further investigated whether the fungal cultivars' colonisation rate was greater on leaf material without fungal endophytes. No difference in the ants' cultivar colonisation rate on leaf tissue with high or low endophyte abundance was observed. C1 [Van Bael, Sunshine A.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Van Bael, Sunshine A.; Seid, Marc A.; Wcislo, William T.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Van Bael, SA (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. EM svanbael@tulane.edu FU NSF [DEB-0949602]; SENACYT [FID10-091]; Smithsonian Institute; Smithsonian Tropical Research Institute FX We thank H. Fernandez-Marin, H. Herz, and two anonymous reviewers for helpful advice. For help in the field and laboratory, we thank J. Urriola, K. Schaffer, E. Rojas, C. Estrada, T. Tascon, M. Sosa, and F. Santos. For logistical support we thank R. Urriola and A. Ruiz. This work was funded by NSF DEB-0949602 to S.A.V. and W.T.W., and SENACYT FID10-091 to S.A.V. and W.T.W., the Smithsonian Institute and the Smithsonian Tropical Research Institute. Permission was granted to do this research by Panama's Authority on the Evironment (ANAM). NR 14 TC 8 Z9 8 U1 1 U2 32 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6946 J9 ECOL ENTOMOL JI Ecol. Entomol. PD AUG PY 2012 VL 37 IS 4 BP 318 EP 321 DI 10.1111/j.1365-2311.2012.01364.x PG 4 WC Entomology SC Entomology GA 971RT UT WOS:000306222200007 ER PT J AU Van Bocxlaer, B Schultheiss, R Plisnier, PD Albrecht, C AF Van Bocxlaer, Bert Schultheiss, Roland Plisnier, Pierre-Denis Albrecht, Christian TI Does the decline of gastropods in deep water herald ecosystem change in Lakes Malawi and Tanganyika? SO FRESHWATER BIOLOGY LA English DT Article DE anthropogenic stress; benthic invertebrate conservation; climate change; deoxygenation; stratification ID AFRICAN GREAT-LAKES; EAST-AFRICA; CLIMATE-CHANGE; CAPE MACLEAR; SPECIES FLOCK; ANCIENT LAKES; VICTORIA; NYASA; CERITHIOIDEA; ENDEMISM AB 1. Ancient, deep lakes have traditionally been considered as stable, ecological islands, well buffered from environmental change because of their great depth. However, they are not immune to anthropogenic and climatic stress. Ecosystems of the permanently stratified warm Lakes Malawi and Tanganyika in the Great East African Rift are particularly delicate. Their stratification regime has historically limited the distribution of benthic biota to a bathtub ring of biodiversity, namely substrata in the upper, oxygenated water layer. 2. We use historical data on the endemic deep-water molluscs of these lakes to assess present-day stress on their benthic ecosystems. During the 20th century, these molluscs have probably decreased in abundance and migrated to shallower water. 3. These apparent trends have a significance beyond species-based conservation, foremost because deep-water organisms heavily rely on the position and temporal stability of the oxycline and therefore provide an early warning of large-scale changes in the distribution of dissolved oxygen. Oxygen demands have increased in the East African Great Lakes over the last century whereas ventilation of deep water has remained the same or declined. 4. The combination of these factors is resulting in a narrowing of the ring of biodiversity and a changed nutrient flux through this ring. Reduction in the habitat available inevitably puts biota at risk, whereas changes in nutrient flux may cause shifts in the entire ecosystem or the collapse of parts of it. 5. Considering the socioeconomic value of these lakes and the potentially grave implications for their faunal biodiversity and entire ecosystems, existing evidence of faunal decline, especially in taxa that depend strongly on the stratification regime, is of great concern. Moreover, because the factors responsible are widespread and include surface-water warming, increased run-off and eutrophication, respiration stress may also develop in other tropical and subtropical lakes. C1 [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Univ Ghent, Dept Geol & Soil Sci, Res Unit Palaeontol, B-9000 Ghent, Belgium. [Schultheiss, Roland; Albrecht, Christian] Univ Giessen, Dept Anim Ecol & Systemat, Giessen, Germany. [Plisnier, Pierre-Denis] Royal Museum Cent Africa, Dept Earth Sci, Tervuren, Belgium. RP Van Bocxlaer, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM vanbocxlaerb@si.edu RI Van Bocxlaer, Bert/N-1965-2016 OI Van Bocxlaer, Bert/0000-0003-2033-326X FU Flanders Research Foundation; Ghent University research council (BOF); Leopold III-Fund; Belgian American Educational Foundation; Smithsonian Institution; SYNTHESYS grant [GB-TAF-3455]; BELSPO [SD/AR/04A]; DFG [SCHR352/9-1, AL 1076/6-2, AL 1076/7-1] FX We are grateful to A. S. Cohen for suggesting that we tackle this subject. D. H. Eccles, M. Glaubrecht, P. Kat, T. Kristensen, E. Michel and J. A. Todd kindly provided unpublished information on deep-water mollusc sampling. We thank A. S. Cohen, D. H. Eccles, R. E. Hecky, G. Hunt, D. Van Damme, D. Verschuren, M. Vollmer and T. Wilke for constructive advice, and A. Hildrew for the excellent editing. We are obliged to F. Schrenk, H. Simfukwe, T. Geertz, J. Tembo and D. Simbeye for fieldwork support. Funding was received from the Flanders Research Foundation, the Ghent University research council (BOF), the Leopold III-Fund, the Belgian American Educational Foundation and a Peter Buck Fellowship of the Smithsonian Institution to B. V. B., from SYNTHESYS grant GB-TAF-3455 to R. S., from BELSPO SD/AR/04A (CHOLTIC project) to P.-D.P., and the DFG projects SCHR352/9-1, AL 1076/6-2 and AL 1076/7-1 to C.A. NR 92 TC 9 Z9 10 U1 1 U2 36 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0046-5070 J9 FRESHWATER BIOL JI Freshw. Biol. PD AUG PY 2012 VL 57 IS 8 BP 1733 EP 1744 DI 10.1111/j.1365-2427.2012.02828.x PG 12 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 970NV UT WOS:000306139300017 ER PT J AU Kitajima, K Llorens, AM Stefanescu, C Timchenko, MV Lucas, PW Wright, SJ AF Kitajima, Kaoru Llorens, Anna-Maria Stefanescu, Carla Timchenko, Marta Vargas Lucas, Peter W. Wright, S. Joseph TI How cellulose-based leaf toughness and lamina density contribute to long leaf lifespans of shade-tolerant species SO NEW PHYTOLOGIST LA English DT Article DE anti-herbivory defence; cellulose; herbivory; lamina density; leaf lifespan; leaf toughness; seedling survival; shade tolerance ID LOWLAND TROPICAL FOREST; RAIN-FOREST; FRACTURE-TOUGHNESS; CARBON GAIN; BIOMECHANICAL PROPERTIES; PHOTOSYNTHETIC CAPACITY; RESOURCE AVAILABILITY; MECHANICAL-PROPERTIES; LITTER DECOMPOSITION; NEOTROPICAL FOREST AB Cell wall fibre and lamina density may interactively affect leaf toughness and leaf lifespan. Here, we tested this with seedlings of 24 neotropical tree species differing in shade tolerance and leaf lifespan under standardized field conditions (140867 d in gaps; longer in shade). We quantified toughness with a cutting test, explicitly seeking a mechanistic linkage to fibre. Lamina density, but not fracture toughness, exhibited a plastic response to gaps vs shade, while neither trait was affected by leaf age. Toughness corrected for lamina density, a recently recognized indicator of material strength per unit mass, was linearly correlated with cellulose content per unit dry mass. Leaf lifespan was positively correlated with cellulose and toughness in shade-tolerant species but only weakly in gap-dependent species. Leaf lifespan was uncorrelated with lamina thickness, phenolics and tannin concentrations. In path analysis including all species, leaf lifespan was directly enhanced by density and toughness, and indirectly by cellulose via its effect on toughness. Different suites of leaf traits were correlated with early seedling survival in gaps vs shade. In conclusion, cellulose and lamina density jointly enhance leaf fracture toughness, and these carbon-based physical traits, rather than phenolic-based defence, explain species differences in herbivory, leaf lifespan and shade survival. C1 [Kitajima, Kaoru; Stefanescu, Carla] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Kitajima, Kaoru; Llorens, Anna-Maria; Timchenko, Marta Vargas; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. [Lucas, Peter W.] Kuwait Univ, Dept Bioclin Sci, Kuwait, Kuwait. RP Kitajima, K (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM kitajima@ufl.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU NSF [0093033]; Smithsonian Tropical Research Institute FX We thank: Roberto Cordero and Sebastian Bernal for the field data collection; Ann Hagerman, Michelle Mack, Kris Callis and Anne Baker for making tannin and fibre analyses possible; and Amy Zanne for help with phylogenetic analysis. The study was supported by NSF 0093033 to K. K. and by the Smithsonian Tropical Research Institute. NR 85 TC 36 Z9 37 U1 5 U2 62 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0028-646X J9 NEW PHYTOL JI New Phytol. PD AUG PY 2012 VL 195 IS 3 BP 640 EP 652 DI 10.1111/j.1469-8137.2012.04203.x PG 13 WC Plant Sciences SC Plant Sciences GA 971CB UT WOS:000306179200017 PM 22709147 ER PT J AU Pinto, CM Kalko, EKV Cottontail, L Wellinghausen, N Cottontail, VM AF Pinto, C. Miguel Kalko, Elisabeth K. V. Cottontail, Lain Wellinghausen, Nele Cottontail, Veronika M. TI TcBat a bat-exclusive lineage of Trypanosoma cruzi in the Panama Canal Zone, with comments on its classification and the use of the 18S rRNA gene for lineage identification SO INFECTION GENETICS AND EVOLUTION LA English DT Article DE Artibeus jamaicensis; Bat; Chagas disease; Chiroptera; Missing data; Reservoir host ID MISSING DATA; PHYLOGENETIC ANALYSES; MAXIMUM-LIKELIHOOD; ORIGINS; HYBRIDIZATION; INFECTION; ALIGNMENT; ECUADOR; DISEASE; HYBRIDS AB We report TcBat, a recently described genetic lineage of Trypanosoma cruzi, in fruit-eating bats Artibeus from Panama. Infections were common (11.6% prevalence), but no other T. cruzi cruzi genotypes were detected. Phylogenetic analyses show an unambiguous association with Brazilian TcBat, but raise questions about the phylogenetic placement of this genotype using the 18S rRNA gene alone. However, analyses with three concatenated genes (18S rRNA, cytb, and H2B) moderately support TcBat as sister to the discrete typing unit (DTU) Tcl. We demonstrate that short fragments (>500 bp) of the 185 rRNA gene are useful for identification of DTUs of T. cruzi, and provide reliable phylogenetic signal as long as they are analyzed within a matrix with reference taxa containing additional informative genes. TcBat forms a very distinctive monophyletic group that may be recognized as an additional DTU within T. cruzi cruzi. (C) 2012 Elsevier B.V. All rights reserved. C1 [Pinto, C. Miguel] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Pinto, C. Miguel] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. [Pinto, C. Miguel] CUNY, Grad Ctr, New York, NY USA. [Pinto, C. Miguel] Pontificia Univ Catolica Ecuador, Quito, Ecuador. [Kalko, Elisabeth K. V.; Cottontail, Veronika M.] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Cottontail, Lain] Kbo Isar Amper Klinikum, Taujkirchen Vils, Germany. [Wellinghausen, Nele] Gaertner & Collegues Lab, Ravensburg, Germany. [Wellinghausen, Nele; Cottontail, Veronika M.] Univ Ulm, Inst Med Microbiol & Hyg, Ulm, Germany. RP Pinto, CM (reprint author), Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. EM mpinto@amnh.org FU Promotionsprogramm in Experimental Medicine of the University of Ulm and the Cusanuswerk; STRI trust funds; Annette Kade Fellowship through the American Museum of Natural History; [SEX/A-145-05] FX We thank Robin M.D. Beck, Carlos A. Flores-Lopez, Edmundo Gonzalez-Santillan, Mario J. Grijalva, Susan L Perkins, Nancy B. Simmons, Daniel Zurita, and two anonymous reviewers for comments on the analyses and the manuscript. We are grateful for the funding support from Grants of the Promotionsprogramm in Experimental Medicine of the University of Ulm and the Cusanuswerk (VMC), STRI trust funds (EKVK), and an Annette Kade Fellowship through the American Museum of Natural History (CMP). Research and export permits were granted to VMC by the Panamanian Autoridad Nacional del Ambiente (# SEX/A-145-05). NR 35 TC 31 Z9 32 U1 1 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1567-1348 J9 INFECT GENET EVOL JI Infect. Genet. Evol. PD AUG PY 2012 VL 12 IS 6 BP 1328 EP 1332 DI 10.1016/j.meegid.2012.04.013 PG 5 WC Infectious Diseases SC Infectious Diseases GA 969DA UT WOS:000306034700023 PM 22543008 ER PT J AU Luan, FB Santelli, CM Hansel, CM Burgos, WD AF Luan, Fubo Santelli, Cara M. Hansel, Colleen M. Burgos, William D. TI Defining manganese(II) removal processes in passive coal mine drainage treatment systems through laboratory incubation experiments SO APPLIED GEOCHEMISTRY LA English DT Article ID BIOGENIC MN OXIDES; MN(II) OXIDATION; MICROBIAL COMMUNITIES; DISSOLVED METALS; STRAIN SG-1; FUNGI; SOIL; BACTERIAL; BIOMASS; WATERS AB Oxic limestone beds are commonly used for the passive removal of Mn(II) from coal mine drainage (CMD). Aqueous Mn(II) is removed via oxidative precipitation of Mn(III/IV) oxides catalyzed by Mn(II)-oxidizing microbes and Mn oxide (MnOx) surfaces. The relative importance of these two processes for Mn removal was examined in laboratory experiments conducted with sediments and CMD collected from eight Mn(II)-removal beds in Pennsylvania and Tennessee, USA. Sterile and non-sterile sediments were incubated in the presence/absence of air and presence/absence of fungicides to operationally define the relative contributions of Mn removal processes. Relatively fast rates of Mn removal were measured in four of the eight sediments where 63-99% of Mn removal was due to biological oxidation. In contrast, in the four sediments with slow rates of Mn(II) removal, 25-63% was due to biological oxidation. Laboratory rates of Mn(II) removal were correlated (R-2 = 0.62) to bacterial biomass concentration (measured by phospholipid fatty acids (PLFA)). Furthermore, laboratory rates of Mn(II) removal were correlated (R-2 = 0.87) to field-scale performance of the Mn(II)-removal beds. A practical recommendation from this study is to include MnOx-coated limestone (and associated biomass) from an operating bed as "seed'' material when constructing new Mn(II)-removal beds. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Luan, Fubo; Burgos, William D.] Penn State Univ, Dept Civil & Environm Engn, University Pk, PA 16802 USA. [Santelli, Cara M.] Smithsonian Inst, Washington, DC 20013 USA. [Hansel, Colleen M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RP Burgos, WD (reprint author), Penn State Univ, Dept Civil & Environm Engn, 212 Sackett Bldg, University Pk, PA 16802 USA. EM wdb3@psu.edu OI Santelli, Cara/0000-0001-8617-0008 FU Office of Surface Mining [S07AP12478]; National Science Foundation [EAR-0846715] FX This research was supported by the Office of Surface Mining under Cooperative Agreement S07AP12478 and funds provided by the National Science Foundation, Grant Number EAR-0846715, awarded to CMH. NR 49 TC 12 Z9 12 U1 2 U2 51 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0883-2927 J9 APPL GEOCHEM JI Appl. Geochem. PD AUG PY 2012 VL 27 IS 8 BP 1567 EP 1578 DI 10.1016/j.apgeochem.2012.03.010 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 966AR UT WOS:000305809500012 ER PT J AU Becker, NI Encarnacao, JA Kalko, EKV Tschapka, M AF Becker, Nina I. Encarnacao, Jorge A. Kalko, Elisabeth K. V. Tschapka, Marco TI The effects of reproductive state on digestive efficiency in three sympatric bat species of the same guild SO COMPARATIVE BIOCHEMISTRY AND PHYSIOLOGY A-MOLECULAR & INTEGRATIVE PHYSIOLOGY LA English DT Article DE Food processing; Digestion; Alimentary tract; Gleaner; Calorimetry; Bats; Energy demand; Reproductive status ID MALE DAUBENTONS BATS; BASAL METABOLIC-RATE; PLECOTUS-AURITUS; MYOTIS-LUCIFUGUS; GASTROINTESTINAL-TRACT; ENERGY-UTILIZATION; DAILY TORPOR; ENERGETICS; LACTATION; FLEXIBILITY AB The functional link between food as an energy source and metabolizable energy is the digestive tract The digestive organs may change in size, structure, or retention time in response to energetic demands of the animal. Very efficient digestive tracts may be better at processing food but require higher energetic investments for maintenance even when post-absorptive. These costs influence the resting metabolic rate (RMR) that is defined as the energy necessary to fuel vital metabolic functions in a resting animal. In bats a trade-off between the necessity for a highly efficient digestive tract and moderate energetic maintenance costs may be particularly important We hypothesized that low RMR coincides with low digestive efficiency (defined as apparent metabolizable energy coefficient (MEC)) and that phases of increased energetic demand are compensated for by increased digestive efficiency. We measured RMR and apparent MEC in the bats species Myotis nattereri, M. bechsteinii, and Plecotus auritus. In support of our hypothesis, M. nattereri has the lowest mass-specific RMR of the three species and the lowest apparent MEC. However, apparent MEC did not change during phases with differing energetic demands in any of the bat species, probably because bats operate at the limit of their sustainable energy demand. (C) 2012 Elsevier Inc. All rights reserved. C1 [Becker, Nina I.; Kalko, Elisabeth K. V.; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Becker, Nina I.; Encarnacao, Jorge A.] Univ Giessen, Mammalian Ecol Grp, Dept Anim Ecol & Systemat, D-35392 Giessen, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Becker, NI (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM nina.becker@uni-ulm.de FU Landesgraduiertenforderung Baden-Wurttemberg FX We want to thank Berry Pinshow very much for his help and useful comments on the manuscript The work was done with the permission of the Regierungsprasidium Giessen. The study was supported by a stipend of the Landesgraduiertenforderung Baden-Wurttemberg to N.I. Becker. NR 65 TC 10 Z9 10 U1 0 U2 16 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 1095-6433 J9 COMP BIOCHEM PHYS A JI Comp. Biochem. Physiol. A-Mol. Integr. Physiol. PD AUG PY 2012 VL 162 IS 4 BP 386 EP 390 DI 10.1016/j.cbpa.2012.04.021 PG 5 WC Biochemistry & Molecular Biology; Physiology; Zoology SC Biochemistry & Molecular Biology; Physiology; Zoology GA 964WA UT WOS:000305726200014 PM 22561664 ER PT J AU Rubilar-Rogers, D Otero, RA Yury-Yanez, RE Vargas, AO Gutstein, CS AF Rubilar-Rogers, David Otero, Rodrigo A. Yury-Yanez, Roberto E. Vargas, Alexander O. Gutstein, Carolina S. TI An overview of the dinosaur fossil record from Chile SO JOURNAL OF SOUTH AMERICAN EARTH SCIENCES LA English DT Article DE Dinosaurs; Birds; Mesozoic; Cenozoic; Chile ID BAHIA INGLESA FORMATION; NORTH-CENTRAL CHILE; SOUTH-AMERICA; EOCENE PENGUINS; ATACAMA DESERT; NEOGENE; MIOCENE; SPHENISCUS; SAUROPOD; BIRDS AB In Chile, the record of dinosaurs in Jurassic and Cretaceous sediments is often restricted to footprints, with few skeletal remains. Tetanuran theropods are known in the Upper Jurassic, and bones of titanosaur sauropods in the Late Cretaceous, including partial skeletons (e.g. Atacamatitan chilensis Kellner et al.). Also from the late Cretaceous, an ornithopod vertebra, a pair of theropod teeth and one tarsometatarsus of a gaviiform bird (Neogaeornis wetzeli Lambrecht) have been reported. The Cenozoic fossil record comprises abundant and well-preserved marine birds from Eocene and Miocene units, with a specially abundant record of Sphenisciformes and less frequently, Procellariiformes. There is an excellent Miocene -Pliocene record of other birds such as Odontopterygiformes, including the most complete skeleton ever found of a pelagornithid, Pelagornis chilensis Mayr and Rubilar-Rogers. Fossil birds are also known from Pliocene and Pleistocene strata. A remarkable collection of birds was discovered in lacustrine sediments of late Pleistocene age associated to human activity. The perspectives in the study of dinosaurs in Chile are promising because plenty of material stored in institutional collections is not described yet. The record of Chilean dinosaurs is relevant for understanding the dynamics and evolution of this group of terrestrial animals in the western edge of Gondwana, while Cenozoic birds from the Region may contribute to the understanding of current biogeography for instance, the effect of the emergence and establishment of the Humboldt Current. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Rubilar-Rogers, David; Otero, Rodrigo A.] Museo Nacl Hist Nat, Area Paleontol, Santiago, Chile. [Yury-Yanez, Roberto E.] Univ Chile, Fac Ciencias, Dept Ciencias Ecol, Lab Zool Vertebrados, Santiago, Chile. [Vargas, Alexander O.] Univ Chile, Fac Ciencias, Dept Biol, Lab Ontogenia & Filogenia, Santiago, Chile. [Gutstein, Carolina S.] Univ Chile, Fac Ciencias, Dept Ciencias Ecol, Lab Ecofisiol, Santiago, Chile. [Gutstein, Carolina S.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Rubilar-Rogers, D (reprint author), Museo Nacl Hist Nat, Area Paleontol, Casilla 787, Santiago, Chile. EM drubilar@mnhn.cl OI Gutstein, Carolina/0000-0002-0823-2434 FU Conicyt-Chile FX We are very grateful of the editors of JSES specially of Timothy Horscroft for his invitation to publish this paper. Many thanks to Jocelyn Navarro who made the line drawings of Atacamasaurus chilensis. Conicyt-Chile funded PhD degree of D. R.-R. and C.S.G. and master degree of R. Y.-Y. We thank Jurassic Foundation for field support. NR 138 TC 5 Z9 8 U1 1 U2 10 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0895-9811 J9 J S AM EARTH SCI JI J. South Am. Earth Sci. PD AUG PY 2012 VL 37 BP 242 EP 255 DI 10.1016/j.jsames.2012.03.003 PG 14 WC Geosciences, Multidisciplinary SC Geology GA 961UF UT WOS:000305494300018 ER PT J AU Zhang, LQ Wang, L Gowda, V Wang, M Li, XF Kan, XZ AF Zhang, Liqin Wang, Li Gowda, Vinita Wang, Ming Li, Xifeng Kan, Xianzhao TI The mitochondrial genome of the Cinnamon Bittern, Ixobrychus cinnamomeus (Pelecaniformes: Ardeidae): sequence, structure and phylogenetic analysis SO MOLECULAR BIOLOGY REPORTS LA English DT Article DE Ardeidae; Ixobrychus cinnamomeus; Mitochondrial genome; Pelecaniformes; Phylogenetics ID D-LOOP REGION; BIRDS; AVES; DNA; NUCLEOTIDE; EVOLUTION; SELECTION; ACCURACY AB Ixobrychus cinnamomeus is a member of the large wading bird family, known as Ardeidae. In the present study, we determined the complete mitochondrial genome of I. cinnamomeus for use in future phylogenetic analysis. This circular mitochondrial genome is 17,180 bp in length and composed of 13 protein-coding genes, 22 tRNA genes, two rRNA genes and one putative control region. Three conserved domains and a minisatellite of 17 nucleotides with 22 tandem repeats were detected at the end of the control region. Phylogenetic relationships were reconstructed using the nucleotide and corresponding amino acid datasets of 12 concatenated protein-coding genes from the mitochondrial genome. Using maximum likelihood, maximum parsimony and Bayesian inference methods, the monophyly of Ciconiidae, Ardeidae and Threskiornithidae were confirmed; however, the monophyly of traditional Ciconiiformes and Pelecaniformes failed to be recovered. Although further studies are recommended to clarify relationships among and within the orders of Ciconiiformes, Pelecaniformes, Suliformes and Phaethontiformes, our results provide preliminary exploratory results that can be useful in the current understanding of avian phylogenetics. C1 [Zhang, Liqin; Wang, Ming; Li, Xifeng; Kan, Xianzhao] Anhui Normal Univ, Coll Life Sci, Prov Key Lab Conservat & Exploitat Res Biol Resou, Wuhu 241000, Peoples R China. [Wang, Li] Beijing Forestry Univ, Coll Forestry, Beijing 100083, Peoples R China. [Gowda, Vinita] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Kan, XZ (reprint author), Anhui Normal Univ, Coll Life Sci, Prov Key Lab Conservat & Exploitat Res Biol Resou, Wuhu 241000, Peoples R China. EM xianzhaokan@yahoo.com.cn OI Kan, Xianzhao/0000-0002-9225-407X FU National Natural Science Foundation of China [30870172]; Key Lab of Biotic Environment and Ecology Safety in Anhui Province FX We would like to thank Binghua Li, Gabe Johnson, Chaoju Qian, Jian Yuan for assistance, suggestions, and comments. We greatly appreciate the constructive criticisms and suggestions by three anonymous reviewers. This study was supported by a grant from the National Natural Science Foundation of China (No. 30870172) and the Key Lab of Biotic Environment and Ecology Safety in Anhui Province. NR 39 TC 18 Z9 18 U1 0 U2 14 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0301-4851 EI 1573-4978 J9 MOL BIOL REP JI Mol. Biol. Rep. PD AUG PY 2012 VL 39 IS 8 BP 8315 EP 8326 DI 10.1007/s11033-012-1681-1 PG 12 WC Biochemistry & Molecular Biology SC Biochemistry & Molecular Biology GA 965EI UT WOS:000305749200052 PM 22699875 ER PT J AU Schirtzinger, EE Tavares, ES Gonzales, LA Eberhard, JR Miyaki, CY Sanchez, JJ Hernandez, A Mueller, H Graves, GR Fleischer, RC Wright, TF AF Schirtzinger, Erin E. Tavares, Erika S. Gonzales, Lauren A. Eberhard, Jessica R. Miyaki, Cristina Y. Sanchez, Juan J. Hernandez, Alexis Mueeller, Heinrich Graves, Gary R. Fleischer, Robert C. Wright, Timothy F. TI Multiple independent origins of mitochondrial control region duplications in the order Psittaciformes SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Ancestral state reconstruction; Control region; Control region duplication; Gene duplication; Mitochondrial genomes; Parrots ID D-LOOP REGION; CONCERTED EVOLUTION; GENE ORDER; DNA REPLICATION; PARROTS PSITTACIFORMES; TANDEM DUPLICATION; SEQUENCE EVOLUTION; GENOME SEQUENCES; RAPID EVOLUTION; RNA GENES AB mitochondrial genomes are generally thought to be under selection for compactness, due to their small size, consistent gene content, and a lack of introns or intergenic spacers. As more animal mitochondrial genomes are fully sequenced, rearrangements and partial duplications are being identified with increasing frequency, particularly in birds (Class Ayes). In this study, we investigate the evolutionary history of mitochondrial control region states within the avian order Psittaciformes (parrots and cockatoos). To this aim, we reconstructed a comprehensive multi-locus phylogeny of parrots, used PCR of three diagnostic fragments to classify the mitochondrial control region state as single or duplicated, and mapped these states onto the phylogeny. We further sequenced 44 selected species to validate these inferences of control region state. Ancestral state reconstruction using a range of weighting schemes identified six independent origins of mitochondrial control region duplications within Psittaciformes. Analysis of sequence data showed that varying levels of mitochondrial gene and tRNA homology and degradation were present within a given clade exhibiting duplications. Levels of divergence between control regions within an individual varied from 0-10.9% with the differences occurring mainly between 51 and 225 nucleotides 3' of the goose hairpin in domain I. Further investigations into the fates of duplicated mitochondrial genes, the potential costs and benefits of having a second control region, and the complex relationship between evolutionary rates, selection, and time since duplication are needed to fully explain these patterns in the mitochondrial genome. (C) 2012 Elsevier Inc. All rights reserved. C1 [Schirtzinger, Erin E.; Gonzales, Lauren A.; Wright, Timothy F.] New Mexico State Univ, Dept Biol, Las Cruces, NM 88003 USA. [Tavares, Erika S.] Royal Ontario Museum, Dept Nat Hist, Toronto, ON M5S 2C6, Canada. [Eberhard, Jessica R.] Louisiana State Univ, Dept Biol, Baton Rouge, LA 70803 USA. [Eberhard, Jessica R.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Tavares, Erika S.; Miyaki, Cristina Y.] Univ Sao Paulo, Dept Genet & Biol Evolut, Sao Paulo, Brazil. [Sanchez, Juan J.; Hernandez, Alexis] Inst Nacl Toxicol & Ciencias Forenses, Tenerife 38320, Canary Islands, Spain. [Mueeller, Heinrich] Loro Parque Fdn, Dept Vet Med, Tenerife 3840, Spain. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Graves, Gary R.] Univ Copenhagen, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. [Fleischer, Robert C.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. RP Schirtzinger, EE (reprint author), New Mexico State Univ, Dept Biol, POB 30001,MSC 3AF, Las Cruces, NM 88003 USA. EM eesem@nmsu.edu RI Miyaki, Cristina/J-2431-2015; publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017 OI Miyaki, Cristina/0000-0002-9708-9202; FU NIH [S06 GM008136]; Sigma Xi; Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP); Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) FX We thank the following institutions and people for the generous loan of tissue specimens: American Museum of Natural History (P. Sweet), Academy of Natural Sciences of Philadelphia (L. Joseph), the African Safari Zoo, the Australian National Wildlife Collection (L. Joseph), the Field Museum of Natural History (D. Willard), Fundacao Crax, University of Kansas Museum of Natural History (M. Robbins), Loro Parque Fundacion, Louisiana State University Museum of Natural Science (R. Brumfield), Museu Paraense Emilio Goeldi, Parque Ecologic do Tiete, the San Diego Zoological Park (N. Lamberski), Universidade Estadual Paulista (UNESP), the US National Museum of Natural History, the New Mexico State University Vertebrate Museum (P. Houde), Zoologico de Sorocaba, Zoologico de Americana, Zoologico Cyro-Gevaerd and several breeders. We particularly thank David Waugh, Sara Cappelli and Julia Scharpegge of the Loro Parque Fundacion and Tania Matsumoto for generous assistance in obtaining data from critical specimens. We thank Rogerio Lourenco for providing some of the sequences, Sergio L. Pereira for suggestions, and Elizabeth Moseman for many useful comments on the manuscript. Research support was provided by NIH grant S06 GM008136 (TFW), Sigma Xi Grant-in-Aid-of-Research (EES), Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) (EST), Coordenacao de Aperfeicoamento de Pessoal de Nivel Superior (CAPES) (EST) and Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) (EST). CYM has a CNPq research productivity fellowship. This study was approved by the Institutional Animal Care and Use Committee of New Mexico State University. NR 86 TC 30 Z9 30 U1 3 U2 30 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 AUG PY 2012 VL 64 IS 2 BP 342 EP 356 DI 10.1016/j.ympev.2012.04.009 PG 15 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 960FY UT WOS:000305374600009 PM 22543055 ER PT J AU Winter, FH Neufeld, MJ Dougherty, K AF Winter, Frank H. Neufeld, Michael J. Dougherty, Kerrie TI Was the rocket invented or accidentally discovered? Some new observations on its origins SO ACTA ASTRONAUTICA LA English DT Article DE Rocket; China; Taoism; Newton; Invention; Discovery AB The history of spaceflight would not have been possible without a single object, the rocket-one of the most complex engineering feats in human history. However, a closer examination of the earliest history of the basic rocket, a gunpowder-propelled device developed in China around 900 years ago, suggests that it originated as an accidental discovery rather than as a deliberately planned invention. This paper will examine the evidence in support of the idea of accidental discovery, including new observations on the earliest concepts of rocket motion, not only in China but also in the West. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. [Dougherty, Kerrie] Powerhouse Museum, Sydney, NSW 2010, Australia. RP Winter, FH (reprint author), 9525 Draycott Court, Burke, VA 22015 USA. EM fhwinter@gmail.com; neufeldm@si.edu; kerried@phm.gov.au NR 30 TC 0 Z9 0 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0094-5765 J9 ACTA ASTRONAUT JI Acta Astronaut. PD AUG-SEP PY 2012 VL 77 BP 131 EP 137 DI 10.1016/j.actaastro.2012.03.014 PG 7 WC Engineering, Aerospace SC Engineering GA 959HO UT WOS:000305303700014 ER PT J AU Jansen, PA Hirsch, BT Emsens, WJ Zamora-Gutierrez, V Wikelski, M Kays, R AF Jansen, Patrick A. Hirsch, Ben T. Emsens, Willem-Jan Zamora-Gutierrez, Veronica Wikelski, Martin Kays, Roland TI Thieving rodents as substitute dispersers of megafaunal seeds SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Pleistocene extinctions; seed predation; cache pilferage; telemetry ID PALM ASTROCARYUM-STANDLEYANUM; TROPICAL FORESTS; SPATIAL-PATTERNS; ACORN DISPERSAL; RAIN-FOREST; AGOUTI; RECRUITMENT; PREDATION; TRACKING; SURVIVAL AB The Neotropics have many plant species that seem to be adapted for seed dispersal by megafauna that went extinct in the late Pleistocene. Given the crucial importance of seed dispersal for plant persistence, it remains a mystery how these plants have survived more than 10,000 y without their mutualist dispersers. Here we present support for the hypothesis that secondary seed dispersal by scatter-hoarding rodents has facilitated the persistence of these large-seeded species. We used miniature radio transmitters to track the dispersal of reputedly megafaunal seeds by Central American agoutis, which scatter-hoard seeds in shallow caches in the soil throughout the forest. We found that seeds were initially cached at mostly short distances and then quickly dug up again. However, rather than eating the recovered seeds, agoutis continued to move and recache the seeds, up to 36 times. Agoutis dispersed an estimated 35% of seeds for > 100 m. An estimated 14% of the cached seeds survived to the next year, when a new fruit crop became available to the rodents. Serial video-monitoring of cached seeds revealed that the stepwise dispersal was caused by agoutis repeatedly stealing and recaching each other's buried seeds. Although previous studies suggest that rodents are poor dispersers, we demonstrate that communities of rodents can in fact provide highly effective long-distance seed dispersal. Our findings suggest that thieving scatter-hoarding rodents could substitute for extinct megafaunal seed dispersers of tropical large-seeded trees. C1 [Jansen, Patrick A.; Hirsch, Ben T.; Wikelski, Martin; Kays, Roland] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa Ancon, Panama. [Jansen, Patrick A.; Emsens, Willem-Jan; Zamora-Gutierrez, Veronica] Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. [Jansen, Patrick A.] Univ Groningen, Fac Math & Nat Sci, Ctr Ecol & Evolutionary Studies, NL-9700 CC Groningen, Netherlands. [Hirsch, Ben T.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Emsens, Willem-Jan] Univ Antwerp, Dept Biol, Ecosyst Management Res Grp, B-2610 Antwerp, Belgium. [Zamora-Gutierrez, Veronica] Univ Cambridge, Dept Zool, Conservat Sci Grp, Cambridge CB2 3EJ, England. [Wikelski, Martin] Max Planck Inst Ornithol, D-78315 Radolfzell am Bodensee, Germany. [Wikelski, Martin] Univ Konstanz, Dept Ornithol, D-78543 Constance, Germany. [Kays, Roland] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Kays, Roland] N Carolina Museum Nat Sci, Nat Res Ctr, Raleigh, NC 27601 USA. RP Jansen, PA (reprint author), Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Balboa Ancon, Panama. EM patrick.jansen@wur.nl RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 FU National Science Foundation [NSF-DEB-0717071]; Netherlands Foundation for Scientific Research [NWO-WOTRO W85-239, NWO-ALW 863-07-008]; Leiden University Fund; Huygens Scholarship program; Leiden University Lustra Scholarship; Fonds voor Onderzoek ten behoeve van het Natuurbehoud; Smithsonian Tropical Research Institute; Frank Levinson Family Foundation FX We thank Tom Garin (Advanced Telemetry Systems), Daniel Obando, Alejandro Ortega, and Meg Crofoot for technical support; Lieneke Bakker, Reyna Bell, Chris Carson, Matt McElroy, Veronica Pereira, Torrey Rodgers, Sumana Serchan, Michiel Veldhuis, and Brian Watts for field assistance; Joe Wright for the original idea of automated radio-tracking of seeds; John Terborgh and two anonymous reviewers for comments; and the Smithsonian Tropical Research Institute for facilities and administrative support. Financial support was provided by National Science Foundation Grant NSF-DEB-0717071 (to R.K. and M.W.), Netherlands Foundation for Scientific Research Grants NWO-WOTRO W85-239 and NWO-ALW 863-07-008 (to P.A.J.), the Leiden University Fund, the Huygens Scholarship program, a Leiden University Lustra Scholarship, the "Fonds voor Onderzoek ten behoeve van het Natuurbehoud" (to V.Z.-G.), the Smithsonian Tropical Research Institute, and the Frank Levinson Family Foundation. NR 63 TC 76 Z9 78 U1 15 U2 87 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 JUL 31 PY 2012 VL 109 IS 31 BP 12610 EP 12615 DI 10.1073/pnas.1205184109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 989CQ UT WOS:000307538200069 PM 22802644 ER PT J AU Hansel, CM Zeiner, CA Santelli, CM Webb, SM AF Hansel, Colleen M. Zeiner, Carolyn A. Santelli, Cara M. Webb, Samuel M. TI Mn(II) oxidation by an ascomycete fungus is linked to superoxide production during asexual reproduction SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE biomineralization; oxidative burst ID MANGANESE OXIDES; PHANEROCHAETE-CHRYSOSPORIUM; ASPERGILLUS-NIDULANS; NADPH OXIDASES; STRAIN SG-1; SEAWATER; PEROXIDASE; CHELATORS; DIFFERENTIATION; CHEMISTRY AB Manganese (Mn) oxides are among the most reactive minerals within the environment, where they control the bioavailability of carbon, nutrients, and numerous metals. Although the ability of microorganisms to oxidize Mn(II) to Mn(III/IV) oxides is scattered throughout the bacterial and fungal domains of life, the mechanism and physiological basis for Mn(II) oxidation remains an enigma. Here, we use a combination of compound-specific chemical assays, microspectroscopy, and electron microscopy to show that a common Ascomycete filamentous fungus, Stilbella aciculosa, oxidizes Mn(II) to Mn oxides by producing extracellular superoxide during cell differentiation. The reactive Mn oxide phase birnessite and the reactive oxygen species superoxide and hydrogen peroxide are colocalized at the base of asexual reproductive structures. Mn oxide formation is not observed in the presence of superoxide scavengers (e.g., Cu) and inhibitors of NADPH oxidases (e.g., diphenylene iodonium chloride), enzymes responsible for superoxide production and cell differentiation in fungi. Considering the recent identification of Mn(II) oxidation by NADH oxidase-based superoxide production by a common marine bacterium (Roseobacter sp.), these results introduce a surprising homology between some prokaryotic and eukaryotic organisms in the mechanisms responsible for Mn(II) oxidation, where oxidation appears to be a side reaction of extracellular superoxide production. Given the versatility of superoxide as a redox reactant and the widespread ability of fungi to produce superoxide, this microbial extracellular superoxide production may play a central role in the cycling and bioavailability of metals (e.g., Hg, Fe, Mn) and carbon in natural systems. C1 [Hansel, Colleen M.; Zeiner, Carolyn A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Santelli, Cara M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Webb, Samuel M.] Stanford Synchrotron Radiat Lightsource, Menlo Pk, CA 94025 USA. RP Hansel, CM (reprint author), Woods Hole Oceanog Inst, Marine Chem & Geochem Dept, Woods Hole, MA 02543 USA. EM chansel@whoi.edu RI Webb, Samuel/D-4778-2009; OI Webb, Samuel/0000-0003-1188-0464; Santelli, Cara/0000-0001-8617-0008 FU Department of Energy, Office of Biological and Environmental Research; National Institutes of Health, National Center for Research Resources; Department of Energy's Office of Biological and Environmental Research and located at Pacific Northwest National Laboratory; National Science Foundation [EAR-0846715] FX The authors thank Alice Dohnalkova (Environmental Molecular Sciences Laboratory) for assistance in transmission electron microscopy collection and analysis, and three anonymous reviewers for their valuable contributions to this manuscript. Portions of this research were carried out at the Stanford Synchrotron Radiation Lightsource, a national user facility operated by Stanford University on behalf of the US Department of Energy, Office of Basic Energy Sciences. The Stanford Synchrotron Radiation Lightsource Structural Molecular Biology Program is supported by the Department of Energy, Office of Biological and Environmental Research, and by the National Institutes of Health, National Center for Research Resources, Biomedical Technology Program. A portion of this research was also performed using the Environmental Molecular Sciences Laboratory, a national scientific user facility sponsored by the Department of Energy's Office of Biological and Environmental Research and located at Pacific Northwest National Laboratory. This project was funded by the National Science Foundation, Grant EAR-0846715 (to C. M. H.). NR 40 TC 45 Z9 49 U1 7 U2 76 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 JUL 31 PY 2012 VL 109 IS 31 BP 12621 EP 12625 DI 10.1073/pnas.1203885109 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 989CQ UT WOS:000307538200071 PM 22802654 ER PT J AU Martin, A Papa, R Nadeau, NJ Hill, RI Counterman, BA Halder, G Jiggins, CD Kronforst, MR Long, AD McMillan, WO Reed, RD AF Martin, Arnaud Papa, Riccardo Nadeau, Nicola J. Hill, Ryan I. Counterman, Brian A. Halder, Georg Jiggins, Chris D. Kronforst, Marcus R. Long, Anthony D. McMillan, W. Owen Reed, Robert D. TI Diversification of complex butterfly wing patterns by repeated regulatory evolution of a Wnt ligand SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Mullerian mimicry; Wnt pathway; Mendelian genetics; evolutionary-developmental biology ID HEPARAN-SULFATE PROTEOGLYCANS; HELICONIUS-BUTTERFLIES; MULLERIAN MIMICRY; COLOR PATTERN; POSITIONAL INFORMATION; CONVERGENT EVOLUTION; PARALLEL EVOLUTION; HYBRID ZONES; LINKAGE MAP; GENE AB Although animals display a rich variety of shapes and patterns, the genetic changes that explain how complex forms arise are still unclear. Here we take advantage of the extensive diversity of Heliconius butterflies to identify a gene that causes adaptive variation of black wing patterns within and between species. Linkage mapping in two species groups, gene-expression analysis in seven species, and pharmacological treatments all indicate that cis-regulatory evolution of the WntA ligand underpins discrete changes in color pattern features across the Heliconius genus. These results illustrate how the direct modulation of morphogen sources can generate a wide array of unique morphologies, thus providing a link between natural genetic variation, pattern formation, and adaptation. C1 [Martin, Arnaud; Papa, Riccardo; Long, Anthony D.; Reed, Robert D.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. [Martin, Arnaud; Jiggins, Chris D.; McMillan, W. Owen; Reed, Robert D.] Smithsonian Trop Res Inst, Balboa, Panama. [Papa, Riccardo] Univ Puerto Rico, Dept Biol, Ctr Appl Trop Ecol & Conservat, Rio Piedras, PR 00931 USA. [Nadeau, Nicola J.; Jiggins, Chris D.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Hill, Ryan I.; Kronforst, Marcus R.] Harvard Univ, FAS Ctr Syst Biol, Cambridge, MA 02138 USA. [Counterman, Brian A.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA. [Halder, Georg] Univ Texas MD Anderson Canc Ctr, Dept Biochem & Mol Biol, Houston, TX 77030 USA. RP Martin, A (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. EM heliconiuswing@gmail.com RI Jiggins, Chris/B-9960-2008; Nadeau, Nicola/E-1149-2011; Reed, Robert/A-2419-2008; Halder, Georg/F-2966-2015; OI Jiggins, Chris/0000-0002-7809-062X; Nadeau, Nicola/0000-0002-9319-921X; Halder, Georg/0000-0001-7580-3236; Long, Tony/0000-0002-5007-8514; Martin, Arnaud/0000-0002-5980-2249 FU National Science Foundation [DEB-0844244, DEB-1020355, IOS-1052541]; Biotechnology and Biological Sciences Research Council [BB/H01439X/1] FX We thank D. Kapan, S. Rusza, M. Abanto, P. Etter, J. Davey, H. Hines, A. Morrison, N. Gillingham, T. Douglas, J. Olander, A. Tapia, C. Pardo-Diaz, L. Maroja, and L. Gilbert for laboratory help and breeding work; and governmental agencies from Panama, Costa Rica, Ecuador, and French Guiana for permits. This work was funded by National Science Foundation Grants DEB-0844244, DEB-1020355, and IOS-1052541; and Biotechnology and Biological Sciences Research Council Grant BB/H01439X/1. NR 53 TC 60 Z9 60 U1 5 U2 74 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 JUL 31 PY 2012 VL 109 IS 31 BP 12632 EP 12637 DI 10.1073/pnas.1204800109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 989CQ UT WOS:000307538200073 PM 22802635 ER PT J AU Wolfe, E Yelin, SF AF Wolfe, Elie Yelin, S. F. TI Quantum bounds for inequalities involving marginal expectation values SO PHYSICAL REVIEW A LA English DT Article ID NONLOCALITY AB We review and develop an algorithm to determine arbitrary quantum bounds based on the seminal work of Tsirelson [Lett. Math. Phys. 4, 93 (1980)]. The potential of this algorithm is demonstrated by both deriving marginal-involving number-valued quantum bounds and identifying a generalized class of function-valued quantum bounds. Those results facilitate an eight-dimensional volume analysis of quantum mechanics which extends the work of Cabello [Phys. Rev. A 72, 012113 (2005)]. We contrast the quantum volume defined by these bounds to that of macroscopic locality, defined by the inequalities corresponding to the first level of the hierarchy of Navascues et al. [New J. Phys. 10, 073013 (2008)], proving our function-valued quantum bounds to be more complete. C1 [Wolfe, Elie; Yelin, S. F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S. F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Wolfe, E (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM wolfe@phys.uconn.edu RI Wolfe, Elie/F-7888-2014 OI Wolfe, Elie/0000-0002-6960-3796 FU NSF FX We thank B. S. Tsirelson of Tel Aviv University for his input and discussions that enhanced this paper considerably, as well as Roger Colbeck of the Perimeter Institute for Theoretical Physics. We wish to thank the NSF for funding. NR 30 TC 2 Z9 2 U1 0 U2 3 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 JUL 30 PY 2012 VL 86 IS 1 AR 012123 DI 10.1103/PhysRevA.86.012123 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 980VH UT WOS:000306921800003 ER PT J AU Berrocoso, AJ Huber, BT MacLeod, KG Petrizzo, MR Lees, JA Wendler, I Coxall, H Mweneinda, AK Falzoni, F Birch, H Singano, JM Haynes, S Cotton, L Wendler, J Bown, PR Robinson, SA Gould, J AF Berrocoso, Alvaro Jimenez Huber, Brian T. MacLeod, Kenneth G. Petrizzo, Maria Rose Lees, Jacqueline A. Wendler, Ines Coxall, Helen Mweneinda, Amina K. Falzoni, Francesca Birch, Heather Singano, Joyce M. Haynes, Shannon Cotton, Laura Wendler, Jens Bown, Paul R. Robinson, Stuart A. Gould, Jeremy TI Lithostratigraphy, biostratigraphy and chemostratigraphy of Upper Cretaceous and Paleogene sediments from southern Tanzania: Tanzania Drilling Project Sites 27-35 SO JOURNAL OF AFRICAN EARTH SCIENCES LA English DT Article DE Tanzania Drilling Project; Kilwa Group; Upper Cretaceous biostratigraphy; Turonian glassy foraminifera; Holococcoliths; Cretaceous-Paleogene boundary ID COASTAL TANZANIA; FORAMINIFERAL ASSEMBLAGES; PLANKTONIC-FORAMINIFERA; EVOLUTIONARY HISTORY; INDIAN-OCEAN; KILWA GROUP; EOCENE; SECTION; TETHYS; PALEOECOLOGY AB The 2008 Tanzania Drilling Project (TOP) expedition recovered common planktonic foraminifera (PF), calcareous nannofossils (CN) and calcareous dinoflagellates with extraordinary shell preservation at multiple Cenomanian-Campanian sites that will be used for paleoclimatic, paleoceanographic, and biostratigraphic studies. New cores confirm the existence of a more expanded and continuous Upper Cretaceous sequence than had previously been documented in the Lindi and Kilwa regions of southeastern coastal Tanzania. This TDP expedition cored 684.02 m at eight Upper Cretaceous sites (TOP Sites 28-35) and a thin Paleocene section (TDP Site 27). TDP Sites 29, 30, 31 and 34 together span the lowermost Turonian to Coniacian (PF Whiteinella archaeocretacea to Dicarinella concavata Zones and CN Zones UC6a-9b), with TDP Site 31 being the most biostratigraphically complete Turonian section found during TOP drilling. A discontinuous section from the Santonian-upper Campanian (PF D. asymetrica to Radotruncana calcarata Zones and CN Zones UC12-16) was collectively recovered at TOP Sites 28, 32 and 35, while thin sequences of the lower Cenomanian (PF Thalmanninella globotruncanoides Zone and CN subzones UC3a-b) and middle Paleocene (Selandian; PF Zone P3a and CN Zone NP5) were cored in TOP Sites 33 and 27, respectively. Records of delta C-13(org) and delta C-13(carb) from bulk sediments generated for all the Cretaceous sites show largely stable values through the sections. Only a few parallel delta C-13(org) and delta C-13(carb) shifts have been found and they are interpreted to reflect local processes. The delta O-18(carb) record, however, is consistent with Late Cretaceous cooling trends from the Turonian into the Campanian. Lithologies of these sites include thick intervals of claystones and silt-stones with locally abundant, finely-laminated fabrics, irregular occurrences of thin sandstone layers, and sporadic bioclastic debris (e.g., inoceramids, ammonites). Minor lithologies represent much thinner units of up to medium-grained, massive sandstones. The %CaCO3 (similar to 5-40%) and %C-org (similar to 0.1-2%) are variable, with the highest %CaCO3 in the lower Campanian and the highest %C-org in the Turonian. Lithofacies analysis suggests that deposition of these sediments occurred in outer shelf-upper slope, a setting that agrees well with inferences from benthic foraminifera and calcareous dinoflagellates. (C) 2012 Elsevier Ltd. All rights reserved. C1 [Berrocoso, Alvaro Jimenez] Univ Manchester, Sch Earth Atmospher & Environm Sci, Manchester M13 9PL, Lancs, England. [Huber, Brian T.; Wendler, Ines; Wendler, Jens] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [MacLeod, Kenneth G.; Haynes, Shannon] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. [Petrizzo, Maria Rose; Falzoni, Francesca] Univ Milan, Dipartimento Sci Terra Ardito Desio, Milan, Italy. [Lees, Jacqueline A.; Bown, Paul R.; Robinson, Stuart A.; Gould, Jeremy] UCL, Dept Earth Sci, London WC1E 6BT, England. [Coxall, Helen; Mweneinda, Amina K.; Birch, Heather; Cotton, Laura] Cardiff Univ, Sch Earth Ocean & Planetary Sci, Cardiff CF10 3YE, S Glam, Wales. [Singano, Joyce M.] Tanzania Petr Dev Corp, Dar Es Salaam, Tanzania. RP Berrocoso, AJ (reprint author), Univ Manchester, Sch Earth Atmospher & Environm Sci, Oxford Rd, Manchester M13 9PL, Lancs, England. EM alvaro.jimenezberrocoso@manchester.ac.uk RI Robinson, Stuart/C-4808-2011; MacLeod, Kenneth/C-4042-2017; Petrizzo, Maria Rose/M-8672-2013; OI Robinson, Stuart/0000-0003-4329-1058; MacLeod, Kenneth/0000-0002-6016-0837; Petrizzo, Maria Rose/0000-0002-9584-8471; LEES, JACKIE/0000-0003-0737-8826; Falzoni, Francesca/0000-0002-5694-9827; Bown, Paul/0000-0001-6777-4463 FU USA National Science Foundation [EAR 0642993]; Smithsonian Walcott Fund; NERC [NE/G004986/1]; MIUR-Prin [2007-2007W9B2WE 001]; Universita degli Studi di Milano FX The Tanzania Petroleum Development Corporation and the Tanzania Commission for Science and Technology are acknowledged for logistical support and permission to carry out this research in the field. We appreciate the generous hospitality and valuable technical assistance of Ephrem Mchana, the late Michael Mkereme, and Elvis Mgaya (Mr. K). Field work and drilling were funded by a USA National Science Foundation grant to KGM and BTH (EAR 0642993) and a Smithsonian Walcott Fund grant to BTH. JAL was funded by the NERC (Grant NE/G004986/1). Financial support to MRP was provided by MIUR-Prin 2007-2007W9B2WE 001. The PhD program of the Universita degli Studi di Milano is acknowledged for funding FF. All authors participated in the 2008 drilling season. AJB did the sedimentological and facies analysis. BTH, MRP, HC, FF, HB and LC did the planktonic foraminiferal biostratigraphy. JAL and PRB did the calcareous nannofossil biostratigraphy. LW and JW did the benthic foraminiferal and dinoflagellates analyses, respectively. KGM and SH carried out the chemostratigraphic measurements. AJB, BTH, KGM, MRP, JAL, HC, HB, IW, JW, PRB and SH collaborated on writing the manuscript. NR 43 TC 13 Z9 15 U1 2 U2 23 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1464-343X J9 J AFR EARTH SCI JI J. Afr. Earth Sci. PD JUL 27 PY 2012 VL 70 BP 36 EP 57 DI 10.1016/j.jafrearsci.2012.05.006 PG 22 WC Geosciences, Multidisciplinary SC Geology GA 978DN UT WOS:000306720900005 ER PT J AU Lemeshko, M Krems, RV Weimer, H AF Lemeshko, Mikhail Krems, Roman V. Weimer, Hendrik TI Nonadiabatic Preparation of Spin Crystals with Ultracold Polar Molecules (vol 109, 035301, 2012) SO PHYSICAL REVIEW LETTERS LA English DT Correction C1 [Krems, Roman V.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Krems, Roman V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. NR 1 TC 0 Z9 0 U1 1 U2 11 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 JUL 26 PY 2012 VL 109 IS 4 AR 049901 DI 10.1103/PhysRevLett.109.049901 PG 1 WC Physics, Multidisciplinary SC Physics GA 980ZP UT WOS:000306933000013 ER PT J AU Sanchis-Ojeda, R Fabrycky, DC Winn, JN Barclay, T Clarke, BD Ford, EB Fortney, JJ Geary, JC Holman, MJ Howard, AW Jenkins, JM Koch, D Lissauer, JJ Marcy, GW Mullally, F Ragozzine, D Seader, SE Still, M Thompson, SE AF Sanchis-Ojeda, Roberto Fabrycky, Daniel C. Winn, Joshua N. Barclay, Thomas Clarke, Bruce D. Ford, Eric B. Fortney, Jonathan J. Geary, John C. Holman, Matthew J. Howard, Andrew W. Jenkins, Jon M. Koch, David Lissauer, Jack J. Marcy, Geoffrey W. Mullally, Fergal Ragozzine, Darin Seader, Shawn E. Still, Martin Thompson, Susan E. TI Alignment of the stellar spin with the orbits of a three-planet system SO NATURE LA English DT Article ID EXTRASOLAR PLANETS; STAR; STARSPOTS; TRANSITS; MASS AB The Sun's equator and the planets' orbital planes are nearly aligned, which is presumably a consequence of their formation from a single spinning gaseous disk. For exoplanetary systems this well-aligned configuration is not guaranteed: dynamical interactions may tilt planetary orbits, or stars may be misaligned with the protoplanetary disk through chaotic accretion(1), magnetic interactions(2) or torques from neighbouring stars. Indeed, isolated 'hot Jupiters' are often misaligned and even orbiting retrograde(3,4). Here we report an analysis of transits of planets over starspots(5-7) on the Sun-like star Kepler-30 (ref. 8), and show that the orbits of its three planets are aligned with the stellar equator. Furthermore, the orbits are aligned with one another to within a few degrees. This configuration is similar to that of our Solar System, and contrasts with the isolated hot Jupiters. The orderly alignment seen in the Kepler-30 system suggests that high obliquities are confined to systems that experienced disruptive dynamical interactions. Should this be corroborated by observations of other coplanar multi-planet systems, then star-disk misalignments would be ruled out as the explanation for the high obliquities of hot Jupiters, and dynamical interactions would be implicated as the origin of hot Jupiters. C1 [Sanchis-Ojeda, Roberto; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Fabrycky, Daniel C.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Barclay, Thomas; Still, Martin] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Barclay, Thomas; Clarke, Bruce D.; Jenkins, Jon M.; Koch, David; Lissauer, Jack J.; Mullally, Fergal; Seader, Shawn E.; Still, Martin; Thompson, Susan E.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Clarke, Bruce D.; Jenkins, Jon M.; Mullally, Fergal; Seader, Shawn E.; Thompson, Susan E.] SETI Inst, Mountain View, CA USA. [Ford, Eric B.] Univ Florida, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Geary, John C.; Holman, Matthew J.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howard, Andrew W.; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Sanchis-Ojeda, R (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM rsanchis86@gmail.com; daniel.fabrycky@gmail.com RI Sanchis-Ojeda, Roberto/B-6574-2013; Ragozzine, Darin/C-4926-2013; OI Sanchis-Ojeda, Roberto/0000-0002-6193-972X; Fortney, Jonathan/0000-0002-9843-4354; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]; NASA through Hubble Fellowship [HF-51272.01-A]; STScI; NASA through the Kepler Participating Scientist programme FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission was provided by NASA's Science Mission Directorate. The data presented in this Letter were obtained from the Mikulski Archive for Space Telescopes (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. S. Albrecht, E. Agol, J. A. Carter, L. Doyle and A. Shporer provided comments on the manuscript. D. C. F. acknowledges NASA support through Hubble Fellowship grant HF-51272.01-A, awarded by STScI. D. R. acknowledges the Harvard Institute for Theory and Computation. E. B. F., M. J. H. and J.N.W. acknowledge NASA support through the Kepler Participating Scientist programme. NR 20 TC 92 Z9 92 U1 0 U2 8 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 26 PY 2012 VL 487 IS 7408 BP 449 EP 453 DI 10.1038/nature11301 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979KD UT WOS:000306815300031 PM 22836999 ER PT J AU Greenberg, R Cadena, V Danner, RM Tattersall, G AF Greenberg, Russell Cadena, Viviana Danner, Raymond M. Tattersall, Glenn TI Heat Loss May Explain Bill Size Differences between Birds Occupying Different Habitats SO PLOS ONE LA English DT Article ID DARWINS FINCHES; MARSH SPARROWS; ALLENS RULE; EVOLUTION; TEMPERATURE; ADAPTATION; MORPHOLOGY; ECOLOGY; POPULATION; RESPONSES AB Background: Research on variation in bill morphology has focused on the role of diet. Bills have other functions, however, including a role in heat and water balance. The role of the bill in heat loss may be particularly important in birds where water is limiting. Song sparrows localized in coastal dunes and salt marsh edge (Melospiza melodia atlantica) are similar in size to, but have bills with a 17% greater surface area than, those that live in mesic habitats (M. m. melodia), a pattern shared with other coastal sparrows. We tested the hypotheses that sparrows can use their bills to dissipate "dry" heat, and that heat loss from the bill is higher in M. m. atlantica than M. m. melodia, which would indicate a role of heat loss and water conservation in selection for bill size. Methodology/Principal Findings: Bill, tarsus, and body surface temperatures were measured using thermal imaging of sparrows exposed to temperatures from 15-37 degrees C and combined with surface area and physical modeling to estimate the contribution of each body part to total heat loss. Song sparrow bills averaged 5-10 degrees C hotter than ambient. The bill of M. m atlantica dissipated up to 33% more heat and 38% greater proportion of total heat than that of M. m. melodia. This could potentially reduce water loss requirements by approximately 7.7%. Conclusions/Significance: This >30% higher heat loss in the bill of M. m. atlantica is independent of evaporative water loss and thus could play an important role in the water balance of sparrows occupying the hot and exposed dune/salt marsh environments during the summer. Heat loss capacity and water conservation could play an important role in the selection for bill size differences between bird populations and should be considered along with trophic adaptations when studying variation in bill size. C1 [Greenberg, Russell; Danner, Raymond M.] Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Washington, DC USA. [Cadena, Viviana; Tattersall, Glenn] Brock Univ, Dept Biol Sci, St Catharines, ON L2S 3A1, Canada. [Danner, Raymond M.] Virginia Polytech Inst & State Univ, Avian Ecol Grp, Dept Biol Sci, Blacksburg, VA 24061 USA. RP Greenberg, R (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC USA. EM greenbergr@si.edu RI Tattersall, Glenn/D-3469-2009; Danner, Raymond/J-8350-2013 OI Tattersall, Glenn/0000-0002-6591-6760; Danner, Raymond/0000-0002-3999-8141 FU Abbott Endowment; Smithsonian Institution FX Research was supported by the Abbott Endowment, short-term visitor award, and Research Equipment Pool Grants of the Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 27 Z9 27 U1 9 U2 58 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 JUL 25 PY 2012 VL 7 IS 7 AR e40933 DI 10.1371/journal.pone.0040933 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979GX UT WOS:000306806600030 PM 22848413 ER PT J AU Pham, LM Bar-Gill, N Belthangady, C Le Sage, D Cappellaro, P Lukin, MD Yacoby, A Walsworth, RL AF Pham, L. M. Bar-Gill, N. Belthangady, C. Le Sage, D. Cappellaro, P. Lukin, M. D. Yacoby, A. Walsworth, R. L. TI Enhanced solid-state multispin metrology using dynamical decoupling SO PHYSICAL REVIEW B LA English DT Article ID NANOSCALE RESOLUTION; ELECTRONIC SPIN; DIAMOND SPINS; COHERENCE; BATH AB We use multipulse dynamical decoupling to increase the coherence lifetime (T-2) of large numbers of nitrogen-vacancy (NV) electronic spins in room temperature diamond, thus enabling scalable applications of multispin quantum information processing and metrology. We realize an order-of-magnitude extension of the NV multispin T-2 in three diamond samples with widely differing spin impurity environments. In particular, for samples with nitrogen impurity concentration less than or similar to 1 ppm, we extend T-2 to >2 ms, comparable to the longest coherence time reported for single NV centers, and demonstrate a tenfold enhancement in NV multispin sensing of ac magnetic fields. C1 [Pham, L. M.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Bar-Gill, N.; Belthangady, C.; Le Sage, D.; Walsworth, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bar-Gill, N.; Lukin, M. D.; Yacoby, A.; Walsworth, R. L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Cappellaro, P.] MIT, Nucl Sci & Engn Dept, Cambridge, MA 02139 USA. RP Pham, LM (reprint author), Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. RI Cappellaro, Paola/B-1413-2010; OI Cappellaro, Paola/0000-0003-3207-594X; Le Sage, David/0000-0003-1678-9491 FU NIST; NSF; DARPA (QuEST program); DARPA (QuASAR program) FX This work was supported by NIST, NSF, and DARPA (QuEST and QuASAR programs). We gratefully acknowledge the provision of diamond samples by Element Six and Apollo and helpful technical discussions with Daniel Twitchen and Matthew Markham. NR 34 TC 36 Z9 36 U1 2 U2 34 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 JUL 24 PY 2012 VL 86 IS 4 AR 045214 DI 10.1103/PhysRevB.86.045214 PG 5 WC Physics, Condensed Matter SC Physics GA 977UB UT WOS:000306689200004 ER PT J AU Cohen, EB Moore, FR Fischer, RA AF Cohen, Emily B. Moore, Frank R. Fischer, Richard A. TI Experimental Evidence for the Interplay of Exogenous and Endogenous Factors on the Movement Ecology of a Migrating Songbird SO PLOS ONE LA English DT Article ID CATBIRDS DUMETELLA-CAROLINENSIS; PASSERINE MIGRANTS; HABITAT SELECTION; REPRODUCTIVE-PERFORMANCE; INSECTIVOROUS BIRDS; FOOD AVAILABILITY; STOPOVER ECOLOGY; SPATIAL-BEHAVIOR; FAT; COMPETITION AB Movement patterns during songbird migration remain poorly understood despite their expected fitness consequences in terms of survival, energetic condition and timing of migration that will carry over to subsequent phases of the annual cycle. We took an experimental approach to test hypotheses regarding the influence of habitat, energetic condition, time of season and sex on the hour-by-hour, local movement decisions of a songbird during spring stopover. To simulate arrival of nocturnal migrants at unfamiliar stopover sites, we translocated and continuously tracked migratory red-eyed vireos (Vireo olivaceus) throughout spring stopover with and without energetic reserves that were released in two replicates of three forested habitat types. Migrants moved the most upon release, during which time they selected habitat characterized by greater food abundance and higher foraging attack rates. Presumably under pressure to replenish fuel stores necessary to continue migration in a timely fashion, migrants released in poorer energetic condition moved faster and further than migrants in better condition and the same pattern was true for migrants released late in spring relative to those released earlier. However, a migrant's energetic condition had less influence on their behavior when they were in poor quality habitat. Movement did not differ between sexes. Our study illustrates the importance of quickly finding suitable habitat at each stopover site, especially for energetically constrained migrants later in the season. If an initial period prior to foraging were necessary at each stop along a migrant's journey, non-foraging periods would cumulatively result in a significant energetic and time cost to migration. However, we suggest behavior during stopover is not solely a function of underlying resource distributions but is a complex response to a combination of endogenous and exogenous factors. C1 [Cohen, Emily B.; Moore, Frank R.] Univ So Mississippi, Dept Biol Sci, Hattiesburg, MS 39406 USA. [Fischer, Richard A.] United States Army Engn Res & Dev Ctr, Environm Lab, Vicksburg, MS USA. RP Cohen, EB (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Migratory Bird Ctr, Washington, DC USA. EM cohene@si.edu FU The University of Southern Mississippi; Department of Defense Strategic Environmental Research and Development Program (SERDP) [SI-1469] FX Funding for this project was provided by The University of Southern Mississippi and the Department of Defense Strategic Environmental Research and Development Program (SERDP Project SI-1469). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 58 TC 17 Z9 17 U1 1 U2 44 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 JUL 23 PY 2012 VL 7 IS 7 AR e41818 DI 10.1371/journal.pone.0041818 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 977TM UT WOS:000306687700155 PM 22844528 ER PT J AU Fauchald, K Berke, SK Woodin, SA AF Fauchald, Kristian Berke, Sarah Kosting Woodin, Sarah Ann TI Diopatra (Onuphidae: Polychaeta) from intertidal sediments in southwestern Europe SO ZOOTAXA LA English DT Article DE Annelida; SW Europe; Atlantic Ocean; Intertidal ID ANNELIDA AB Intertidal populations of Diopatra from Spanish, Portuguese and French Atlantic beaches have traditionally been identified as D. neapolitana. This species is present, mainly in Spain and Portugal. However, at least some French beaches are occupied by a distinct species, D. biscayensis, here described as new. In addition, in Portugal and Spain, a third species, here described as new, D. cryptornata, will also key out as D. neapolitana using standard keys, but is morphologically distinct. The three species can be separated not only on traditional characters, but also on obvious differences in anterior morphology not usually considered in descriptions. The French habitats now occupied by D. biscayensis, previously had populations of D. neapolitana alone as documented by collections in the Paris Museum made by Quatrefages and Saint-Joseph in the mid-late 1800s. Diopatra marocensis has recently been reported from Atlantic waters, from both intertidal and subtidal areas. Since this species can be confused with the three species named above, a partial re-description based on paratype material is included here. Finally, a fifth species, D. micrura, has recently been described from the area and is here briefly characterized based on the original description. A key to all five species has been constructed. C1 [Fauchald, Kristian] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Berke, Sarah Kosting; Woodin, Sarah Ann] Univ S Carolina, Dept Biol Sci, Columbia, SC 29208 USA. [Berke, Sarah Kosting] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. RP Fauchald, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 0163,POB 37012, Washington, DC 20013 USA. EM FAUCHALD@si.edu RI Woodin, Sarah/K-8481-2014 OI Woodin, Sarah/0000-0001-5615-2212 FU ONR [N00014-0310352]; NOAA [NA04NOS4780264]; NASA [NNG04GE43G, NNX07AF20G, NNX11AP77]; NSF [OCE1039513, OCE1129401] FX KF is grateful to his two co-authors for making this interesting material available and for their patience in waiting for him to complete the descriptions. In addition he is very grateful for the careful work done by two reviewers; thanks to them, this is a much better paper than it otherwise would have been. We thank D. Wethey and F. Lima for field assistance, G. Bachelet for the donation of specimens from the shallow subtidal off the mouth of the Gironde, and Meziane Tarik of the Paris Museum for loan of the types of Diopatra gallica collected by Quatrefages and of the specimens collected by Saint-Joseph from the Arcachon area. This research was supported by ONR (N00014-0310352), NOAA (NA04NOS4780264), NASA (NNG04GE43G, NNX07AF20G, NNX11AP77), and NSF (OCE1039513, OCE1129401). NR 8 TC 7 Z9 7 U1 1 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 JUL 23 PY 2012 IS 3395 BP 47 EP 58 PG 12 WC Zoology SC Zoology GA 976MP UT WOS:000306589200005 ER PT J AU Finkbeiner, SD Briscoe, AD Reed, RD AF Finkbeiner, Susan D. Briscoe, Adriana D. Reed, Robert D. TI The benefit of being a social butterfly: communal roosting deters predation SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE communal roosting; collective aposematism; dilution effect; aggregation; predation; Heliconius ID HELICONIUS BUTTERFLIES; COSTA-RICA; HOME RANGE; LEPIDOPTERA NYMPHALIDAE; AVIAN PREDATORS; RAIN-FOREST; EVOLUTION; GREGARIOUSNESS; PATTERNS; SPECIALIZATION AB Aposematic passion-vine butterflies from the genus Heliconius form communal roosts on a nightly basis. This behaviour has been hypothesized to be beneficial in terms of information sharing and/or anti-predator defence. To better understand the adaptive value of communal roosting, we tested these two hypotheses in field studies. The information-sharing hypothesis was addressed by examining following behaviour of butterflies departing from natural roosts. We found no evidence of roost mates following one another to resources, thus providing no support for this hypothesis. The anti-predator defence hypothesis was tested using avian-indiscriminable Heliconius erato models placed singly and in aggregations at field sites. A significantly higher number of predation attempts were observed on solitary models versus aggregations of models. This relationship between aggregation size and attack rate suggests that communally roosting butterflies enjoy the benefits of both overall decreased attack frequency as well as a prey dilution effect. Communal roosts probably deter predators through collective aposematism in which aggregations of conspicuous, unpalatable prey communicate a more effective repel signal to predators. On the basis of our results, we propose that predation by birds is a key selective pressure maintaining Heliconius communal roosting behaviour. C1 [Finkbeiner, Susan D.; Briscoe, Adriana D.; Reed, Robert D.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. [Reed, Robert D.] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Finkbeiner, SD (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. EM sfinkbei@uci.edu RI Briscoe, Adriana/E-8963-2010 OI Briscoe, Adriana/0000-0001-8514-4983 FU Smithsonian Tropical Research Institue; Organization for Tropical Studies; U.S. Department of Education GAANN; National Geographic Society; National Science Foundation (NSF) [DGE-0808392]; NSF [IOS-1025106] FX We thank Kailen Mooney for aid in project design and statistical analyses; Jim Mallet for advice and comments; Christian Salcedo and Daniel Osorio for feedback on the manuscript; Nancy Burley, Owen McMillan and Larry Gilbert for advice; Jasmine Velez, Talia Gustafson, Jimena Golcher and Maranatha Kellinger for aid in field observations and assisting in the preparation of butterfly models; Johannes Spaethe, Chris Jiggins and Patricio Salazar for tips on butterfly models; Dave Krueger and UCI ImageWorks for aid in designing and printing models; the Smithsonian Tropical Research Institute (STRI) and Organization for Tropical Studies (OTS) for use of field sites; La Autoridad Nacional del Ambiente (ANAM, Panama) and El Ministerio del Ambiente, Energia, y Telecomunicaciones (MINAET, Costa Rica) for research permit approval; and our funding sources: the Smithsonian Tropical Research Institue, the Organization for Tropical Studies, the U.S. Department of Education GAANN, the National Geographic Society; this material is based upon work supported by the National Science Foundation (NSF) Graduate Research Fellowship under award no. DGE-0808392 to S.D.F. and NSF grant no. IOS-1025106 to A.D.B. and R.D.R. NR 68 TC 25 Z9 27 U1 2 U2 68 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 JUL 22 PY 2012 VL 279 IS 1739 BP 2769 EP 2776 DI 10.1098/rspb.2012.0203 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 959ED UT WOS:000305294500009 PM 22438492 ER PT J AU Brown, WR Cohen, JG Geller, MJ Kenyon, SJ AF Brown, Warren R. Cohen, Judith G. Geller, Margaret J. Kenyon, Scott J. TI THE NATURE OF HYPERVELOCITY STARS AND THE TIME BETWEEN THEIR FORMATION AND EJECTION SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; Galaxy: halo; Galaxy: kinematics and dynamics; stars: early-type; stars: individual (SDSS J091759.47+672238.35) ID LARGE-MAGELLANIC-CLOUD; MASSIVE BLACK-HOLE; GALACTIC-CENTER; STELLAR ORBITS; RUNAWAY STARS; THEORETICAL ISOCHRONES; PHOTOMETRIC SYSTEMS; YOUNG STARS; B-STARS; S-STARS AB We obtain Keck HIRES spectroscopy of HVS5, one of the fastest unbound stars in the Milky Way halo. We show that HVS5 is a 3.62 +/- 0.11 M-circle dot main-sequence B star at a distance of 50 +/- 5 kpc. The difference between its age and its flight time from the Galactic center is 105 +/- 18 (stat) +/- 30 (sys) Myr; flight times from locations elsewhere in the Galactic disk are similar. This 10(8) yr "arrival time" between formation and ejection is difficult to reconcile with any ejection scenario involving massive stars that live for only 10(7) yr. For comparison, we derive arrival times of 10(7) yr for two unbound runaway B stars, consistent with their disk origin where ejection results from a supernova in a binary system or dynamical interactions between massive stars in a dense star cluster. For HVS5, ejection during the first 10(7) yr of its lifetime is ruled out at the 3 sigma level. Together with the 10(8) yr arrival times inferred for three other well-studied hypervelocity stars (HVSs), these results are consistent with a Galactic center origin for the HVSs. If the HVSs were indeed ejected by the central black hole, then the Galactic center was forming stars similar or equal to 200 Myr ago, and the progenitors of the HVSs took similar or equal to 100 Myr to enter the black hole's loss cone. C1 [Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Cohen, Judith G.] CALTECH, Palomar Observ, Pasadena, CA 91125 USA. RP Brown, WR (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM wbrown@cfa.harvard.edu; jlc@astro.caltech.edu; mgeller@cfa.harvard.edu; skenyon@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU Smithsonian Institution; NSF [AST-0908139] FX This work was supported in part by the Smithsonian Institution. J. Cohen acknowledges partial support from NSF grant AST-0908139. This research makes use of NASA's Astrophysics Data System Bibliographic Services. We are grateful to the many people who have worked to make the Keck Telescopes and their instruments a reality, and who operate and maintain these observatories. The authors extend special thanks to those of Hawaiian ancestry on whose sacred mountain we are privileged to be guests. Without their generous hospitality, none of the observations presented herein would have been possible NR 50 TC 18 Z9 18 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 JUL 20 PY 2012 VL 754 IS 1 AR L2 DI 10.1088/2041-8205/754/1/L2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 971XF UT WOS:000306238800002 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Decerprit, G Dickherber, R Duke, C Dumm, J Dwarkadas, VV Errando, M Falcone, A Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Godambe, S Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Humensky, TB Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Lee, K Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R Nunez, PD Ong, RA Orr, M Otte, AN Pandel, D Park, N Perkins, JS Pohl, M Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Skole, C Smith, AW Staszak, D Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Tyler, J Varlotta, A Vincent, S Vivier, M Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Welsing, R Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Decerprit, G. Dickherber, R. Duke, C. Dumm, J. Dwarkadas, V. V. Errando, M. Falcone, A. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Godambe, S. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. Nunez, P. D. Ong, R. A. Orr, M. 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. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Skole, C. Smith, A. W. Staszak, D. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Tyler, J. Varlotta, A. Vincent, S. Vivier, M. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Welsing, R. Williams, D. A. Zitzer, B. TI VERITAS OBSERVATIONS OF THE NOVA IN V407 CYGNI SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general; novae, cataclysmic variables; white dwarfs ID GAMMA-RAY EMISSION; RS-OPHIUCHI; CHERENKOV TELESCOPES; GALACTIC PLANE; 2006 OUTBURST; BLAST WAVE; DISCOVERY; ARRAY AB We report on very high energy (E > 100 GeV) gamma-ray observations of V407 Cygni, a symbiotic binary that underwent a nova outburst producing 0.1-10 GeV gamma rays during 2010 March 10-26. Observations were made with the Very Energetic Radiation Imaging Telescope Array System during 2010 March 19-26 at relatively large zenith angles due to the position of V407 Cyg. An improved reconstruction technique for large zenith angle observations is presented and used to analyze the data. We do not detect V407 Cygni and place a differential upper limit on the flux at 1.6 TeV of 2.3 x 10(-12) erg cm(-2) s(-1) (at the 95% confidence level). When considered jointly with data from Fermi-LAT, this result places limits on the acceleration of very high energy particles in the nova. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; McCann, A.; Ragan, K.; Staszak, D.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Majumdar, P.; Ong, R. A.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Bouvier, A.; Furniss, A.; 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.; Lee, K.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Collins-Hughes, E.; Khassen, Y.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Connolly, M. P.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Decerprit, G.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.; Telezhinsky, I.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Karlsson, N.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Finnegan, G.; Godambe, S.; Kieda, D.; Nunez, P. D.; Smith, A. W.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.; Vivier, M.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Humensky, T. B.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Perkins, J. S.] NASA, CRESST, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Astroparticle Phys Lab, GSFC, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ, Dept Phys & Astron, Barnard Coll, New York, NY 10027 USA. EM daniel-d-gall@uiowa.edu; kazuma-tsurusaki@uiowa.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; 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; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; STFC in the UK FX We thank Pierre Jean of the Fermi-LAT team for providing the contour data from the Fermi-LAT results and useful discussion. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution; by NSERC in Canada, by Science Foundation Ireland (SFI 10/RFP/AST2748); and by STFC in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. NR 36 TC 13 Z9 13 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 JUL 20 PY 2012 VL 754 IS 1 AR 77 DI 10.1088/0004-637X/754/1/77 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800077 ER PT J AU Kharb, P O'Dea, CP Tilak, A Baum, SA Haynes, E Noel-Storr, J Fallon, C Christiansen, K AF Kharb, P. O'Dea, C. P. Tilak, A. Baum, S. A. Haynes, E. Noel-Storr, J. Fallon, C. Christiansen, K. TI VLBA AND CHANDRA OBSERVATIONS OF JETS IN FRI RADIO GALAXIES: CONSTRAINTS ON JET EVOLUTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; polarization; radio continuum: galaxies; techniques: interferometric; X-rays: individuals (UGC00408, UGC08433) ID ACTIVE GALACTIC NUCLEI; XMM-NEWTON OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; PARSEC-SCALE JETS; BASE-LINE ARRAY; ROTATION MEASURES; COMPLETE SAMPLE; X-RAY; SCHWARZSCHILD RADII; MAGNETIC-FIELDS AB We present here the results from new Very Long Baseline Array (VLBA) observations at 1.6 and 5 GHz of 19 galaxies of a complete sample of 21 Uppasala General Catalog (UGC) Fanaroff-Riley type I (FRI) radio galaxies. New Chandra data of two sources, viz., UGC 00408 and UGC 08433, are combined with the Chandra archival data of 13 sources. The 5 GHz observations of 10 "core-jet" sources are polarization-sensitive, while the 1.6 GHz observations constitute second-epoch total intensity observations of nine "core-only" sources. Polarized emission is detected in the jets of seven sources at 5 GHz, but the cores are essentially unpolarized, except in M87. Polarization is detected at the jet edges in several sources, and the inferred magnetic field is primarily aligned with the jet direction. This could be indicative of magnetic field "shearing" due to jet-medium interaction, or the presence of helical magnetic fields. The jet peak intensity I-nu falls with distance d from the core, following the relation, I-nu proportional to d(a), where a is typically similar to -1.5. Assuming that adiabatic expansion losses are primarily responsible for the jet intensity "dimming," two limiting cases are considered: (1) the jet has a constant speed on parsec scales and is expanding gradually such that the jet radius r proportional to d(0.4); this expansion is, however, unobservable in the laterally unresolved jets at 5 GHz, and (2) the jet is cylindrical and is accelerating on parsec scales. Accelerating parsec-scale jets are consistent with the phenomenon of "magnetic driving" in Poynting-flux-dominated jets. While slow jet expansion as predicted by case (1) is indeed observed in a few sources from the literature that are resolved laterally, on scales of tens or hundreds of parsecs, case (2) cannot be ruled out in the present data, provided the jets become conical on scales larger than those probed by VLBA. Chandra observations of 15 UGC FRIs detect X-ray jets in 9 of them. The high frequency of occurrence of X-ray jets in this complete sample suggests that they are a signature of a ubiquitous process in FRI jets. It appears that the FRI jets start out relativistically on parsec scales but decelerate on kiloparsec scales, with the X-ray emission revealing the sites of bulk deceleration and particle reacceleration. C1 [Kharb, P.; O'Dea, C. P.] RIT, Dept Phys, Rochester, NY 14623 USA. [O'Dea, C. P.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tilak, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Baum, S. A.] RIT, Ctr Imaging Sci, Rochester, NY 14623 USA. [Baum, S. A.; Haynes, E.; Noel-Storr, J.; Fallon, C.; Christiansen, K.] Radcliffe Inst Adv Study, Cambridge, MA 02138 USA. RP Kharb, P (reprint author), RIT, Dept Phys, 54 Lomb Mem Dr, Rochester, NY 14623 USA. FU Radcliffe Institute for Advanced Study at Harvard University FX We thank the referee for comments which have led to considerable improvement of this paper. We thank Robert Laing, Alexander Tchekhovskoy, Masanori Nakamura, and Grant Tremblay for making valuable suggestions which have further improved this work. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work is supported in part by the Radcliffe Institute for Advanced Study at Harvard University. NR 69 TC 7 Z9 7 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 JUL 20 PY 2012 VL 754 IS 1 AR 1 DI 10.1088/0004-637X/754/1/1 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800001 ER PT J AU Knutson, HA Lewis, N Fortney, JJ Burrows, A Showman, AP Cowan, NB Agol, E Aigrain, S Charbonneau, D Deming, D Desert, JM Henry, GW Langton, J Laughlin, G AF Knutson, Heather A. Lewis, Nikole Fortney, Jonathan J. Burrows, Adam Showman, Adam P. Cowan, Nicolas B. Agol, Eric Aigrain, Suzanne Charbonneau, David Deming, Drake Desert, Jean-Michel Henry, Gregory W. Langton, Jonathan Laughlin, Gregory TI 3.6 AND 4.5 mu m PHASE CURVES AND EVIDENCE FOR NON-EQUILIBRIUM CHEMISTRY IN THE ATMOSPHERE OF EXTRASOLAR PLANET HD 189733b SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: eclipsing; planetary systems; techniques: photometric ID HUBBLE-SPACE-TELESCOPE; INFRARED-EMISSION-SPECTRUM; TIDALLY LOCKED EXOPLANETS; HOT JUPITER ATMOSPHERES; METAL-RICH ATMOSPHERE; SUPER-EARTH EXOPLANET; UPSILON ANDROMEDAE B; TRANSMISSION SPECTRUM; LIGHT CURVES; SECONDARY ECLIPSE AB We present new, full-orbit observations of the infrared phase variations of the canonical hot Jupiter HD 189733b obtained in the 3.6 and 4.5 mu m bands using the Spitzer Space Telescope. When combined with previous phase curve observations at 8.0 and 24 mu m, these data allow us to characterize the exoplanet's emission spectrum as a function of planetary longitude and to search for local variations in its vertical thermal profile and atmospheric composition. We utilize an improvedmethod for removing the effects of intrapixel sensitivity variations and robustly extracting phase curve signals from these data, and we calculate our best-fit parameters and uncertainties using a wavelet-based Markov Chain Monte Carlo analysis that accounts for the presence of time-correlated noise in our data. We measure a phase curve amplitude of 0.1242% +/- 0.0061% in the 3.6 mu m band and 0.0982% +/- 0.0089% in the 4.5 mu m band, corresponding to brightness temperature contrasts of 503 +/- 21 K and 264 +/- 24 K, respectively. We find that the times of minimum and maximum flux occur several hours earlier than predicted for an atmosphere in radiative equilibrium, consistent with the eastward advection of gas by an equatorial super-rotating jet. The locations of the flux minima in our new data differ from our previous observations at 8 mu m, and we present new evidence indicating that the flux minimum observed in the 8 mu m is likely caused by an overshooting effect in the 8 mu m array. We obtain improved estimates for HD 189733b's dayside planet-star flux ratio of 0.1466% +/- 0.0040% in the 3.6 mu m band and 0.1787% +/- 0.0038% in the 4.5 mu m band, corresponding to brightness temperatures of 1328 +/- 11 K and 1192 +/- 9 K, respectively; these are the most accurate secondary eclipse depths obtained to date for an extrasolar planet. We compare our new dayside and nightside spectra for HD 189733b to the predictions of one-dimensional radiative transfer models from Burrows et al. and conclude that fits to this planet's dayside spectrum provide a reasonably accurate estimate of the amount of energy transported to the night side. Our 3.6 and 4.5 mu m phase curves are generally in good agreement with the predictions of general circulation models for this planet from Showman et al., although we require either excess drag or slower rotation rates in order to match the locations of the measured maxima and minima in the 4.5, 8.0, and 24 mu m bands. We find that HD 189733b's 4.5 mu m nightside flux is 3.3 sigma smaller than predicted by these models, which assume that the chemistry is in local thermal equilibrium. We conclude that this discrepancy is best explained by vertical mixing, which should lead to an excess of CO and correspondingly enhanced 4.5 mu m absorption in this region. This result is consistent with our constraints on the planet's transmission spectrum, which also suggest excess absorption in the 4.5 mu m band at the day-night terminator. C1 [Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Lewis, Nikole; Showman, Adam P.] Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. [Lewis, Nikole; Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Cowan, Nicolas B.] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Aigrain, Suzanne] Univ Oxford, Dept Phys, Subdept Astrophys, Oxford OX1 3RH, England. [Charbonneau, David; Desert, Jean-Michel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Henry, Gregory W.] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. RP Knutson, HA (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM hknutson@caltech.edu RI Agol, Eric/B-8775-2013 OI Agol, Eric/0000-0002-0802-9145 FU NASA through JPL/Caltech; Miller Institute for Basic Research in Science FX We thank Josh Carter for his assistance in implementing a wavelet MCMC analysis for these data. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. H. A. K. was supported in part by a fellowship from the Miller Institute for Basic Research in Science. NR 95 TC 118 Z9 120 U1 3 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 JUL 20 PY 2012 VL 754 IS 1 AR 22 DI 10.1088/0004-637X/754/1/22 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800022 ER PT J AU Krick, JE Glaccum, WJ Carey, SJ Lowrance, PJ Surace, JA Ingalls, JG Hora, JL Reach, WT AF Krick, Jessica E. Glaccum, William J. Carey, Sean J. Lowrance, Patrick J. Surace, Jason A. Ingalls, James G. Hora, Joseph L. Reach, William T. TI A SPITZER/IRAC MEASURE OF THE ZODIACAL LIGHT SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; infrared: diffuse background; interplanetary medium ID BACKGROUND EXPERIMENT SEARCH; THERMAL EMISSION; SPACE-TELESCOPE; DUST CLOUD; COBE; DIRBE; MISSION; DESIGN; MODEL AB The dominant non-instrumental background source for space-based infrared observatories is the zodiacal light (ZL). We present Spitzer Infrared Array Camera (IRAC) measurements of the ZL at 3.6, 4.5, 5.8, and 8.0 mu m, taken as part of the instrument calibrations. We measure the changing surface brightness levels in approximately weekly IRAC observations near the north ecliptic pole over a period of roughly 8.5 years. This long time baseline is crucial for measuring the annual sinusoidal variation in the signal levels due to the tilt of the dust disk with respect to the ecliptic, which is the true signal of the ZL. This is compared to both Cosmic Background Explorer Diffuse Infrared Background Experiment data and a ZL model based thereon. Our data show a few-percent discrepancy from the Kelsall et al. model including a potential warping of the interplanetary dust disk and a previously detected overdensity in the dust cloud directly behind the Earth in its orbit. Accurate knowledge of the ZL is important for both extragalactic and Galactic astronomy including measurements of the cosmic infrared background, absolute measures of extended sources, and comparison to extrasolar interplanetary dust models. IRAC data can be used to further inform and test future ZL models. C1 [Krick, Jessica E.; Glaccum, William J.; Carey, Sean J.; Lowrance, Patrick J.; Surace, Jason A.; Ingalls, James G.] CALTECH, Jet Prop Lab, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Hora, Joseph L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reach, William T.] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. RP Krick, JE (reprint author), CALTECH, Jet Prop Lab, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM jkrick@caltech.edu OI Hora, Joseph/0000-0002-5599-4650; Reach, William/0000-0001-8362-4094 FU National Aeronautics and Space Administration; National Science Foundation FX We thank the anonymous referee for useful suggestions on the manuscript. This research has made use of data from the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work was based on observations obtained with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 16 TC 7 Z9 7 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2012 VL 754 IS 1 AR 53 DI 10.1088/0004-637X/754/1/53 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800053 ER PT J AU Parenti, S Schmieder, B Heinzel, P Golub, L AF Parenti, S. Schmieder, B. Heinzel, P. Golub, L. TI ON THE NATURE OF PROMINENCE EMISSION OBSERVED BY SDO/AIA SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: atmosphere; Sun: corona; Sun: filaments, prominences; Sun: UV radiation ID EUV-FILAMENT; ATOMIC DATABASE; CORONAL LOOPS; QUIET-SUN; H-ALPHA; SOHO/SUMER; ANGSTROM; PLASMA; LINES; TRACE AB The prominence-corona transition region (PCTR) plays a key role in the thermal and pressure equilibrium of solar prominences. Our knowledge of this interface is limited and several major issues remain open, including the thermal structure and, in particular, the maximum temperature of the detectable plasma. The high signal-to-noise ratio of images obtained by the Atmospheric Imaging Assembly (AIA) on NASA's Solar Dynamics Observatory clearly shows that prominences are often seen in emission in the 171 and 131 bands. We investigate the temperature sensitivity of these AIA bands for prominence observations, in order to infer the temperature content in an effort to explain the emission. Using the CHIANTI atomic database and previously determined prominence differential emission measure distributions, we build synthetic spectra to establish the main emission-line contributors in the AIA bands. We find that the Fe IX line always dominates the 171 band, even in the absence of plasma at >10(6) K temperatures, while the 131 band is dominated by Fe VIII. We conclude that the PCTR has sufficient plasma emitting at >4 x 10(5) K to be detected by AIA. C1 [Parenti, S.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Schmieder, B.] Observ Paris, LESIA, F-92195 Meudon, France. [Heinzel, P.] Acad Sci Czech Republic, Inst Astron, CS-25165 Ondrejov, Czech Republic. [Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Parenti, S (reprint author), Royal Observ Belgium, B-1180 Brussels, Belgium. EM s.parenti@oma.be RI Heinzel, Petr/G-9014-2014 FU Belgian Federal Science Policy Office through the ESA-PRODEX program; Grant Agency of the Czech Republic [P209/12/1652, P209/10/1706]; Lockheed Martin; International Space Science Institute, Bern, Switzerland FX S.P. acknowledges the support from the Belgian Federal Science Policy Office through the ESA-PRODEX program. P.H. was partially supported by the grants P209/12/1652 and P209/10/1706 of the Grant Agency of the Czech Republic. L.G. was supported for this work by a contract from Lockheed Martin to SAO. S.P., B.S., and P.H. acknowledge support from the International Space Science Institute, Bern, Switzerland to the International Team on Solar Prominence Formation and Equilibrium: New Data, New Models. CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA), and the University of Cambridge (UK). The AIA data are provided courtesy of NASA/SDO and the AIA science team. The authors acknowledge the referee comments which have improved the clarity of this paper. NR 30 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 JUL 20 PY 2012 VL 754 IS 1 AR 66 DI 10.1088/0004-637X/754/1/66 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800066 ER PT J AU Savage, SL Holman, G Reeves, KK Seaton, DB McKenzie, DE Su, Y AF Savage, Sabrina L. Holman, Gordon Reeves, Katharine K. Seaton, Daniel B. McKenzie, David E. Su, Yang TI LOW-ALTITUDE RECONNECTION INFLOW-OUTFLOW OBSERVATIONS DURING A 2010 NOVEMBER 3 SOLAR ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetic reconnection; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: magnetic topology; Sun: UV radiation; Sun: X-rays, gamma rays ID SUPRA-ARCADE DOWNFLOWS; MAGNETIC RECONNECTION; CURRENT SHEET; QUANTITATIVE EXAMINATION; PATCHY RECONNECTION; FLARE PLASMA; MODEL; EJECTION; EMISSIONS; MOTIONS AB For a solar flare occurring on 2010 November 3, we present observations using several SDO/AIA extreme-ultraviolet (EUV) passbands of an erupting flux rope followed by inflows sweeping into a current sheet region. The inflows are soon followed by outflows appearing to originate from near the termination point of the inflowing motion-an observation in line with standard magnetic reconnection models. We measure average inflow plane-of-sky speeds to range from similar to 150 to 690 km s(-1) with the initial, high-temperature inflows being the fastest. Using the inflow speeds and a range of Alfven speeds, we estimate the Alfvenic Mach number which appears to decrease with time. We also provide inflow and outflow times with respect to RHESSI count rates and find that the fast, high-temperature inflows occur simultaneously with a peak in the RHESSI thermal light curve. Five candidate inflow-outflow pairs are identified with no more than a minute delay between detections. The inflow speeds of these pairs are measured to be similar to 10(2) km s(-1) with outflow speeds ranging from similar to 10(2) to 10(3) km s(-1)-indicating acceleration during the reconnection process. The fastest of these outflows are in the form of apparently traveling density enhancements along the legs of the loops rather than the loop apexes themselves. These flows could possibly either be accelerated plasma, shocks, or waves prompted by reconnection. The measurements presented here show an order of magnitude difference between the retraction speeds of the loops and the speed of the density enhancements within the loops-presumably exiting the reconnection site. C1 [Savage, Sabrina L.; Holman, Gordon; Su, Yang] Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Seaton, Daniel B.] Royal Observ Belgium SIDC, B-1180 Brussels, Belgium. [McKenzie, David E.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. [Su, Yang] Graz Univ, Inst Phys, A-8010 Graz, Austria. RP Savage, SL (reprint author), Oak Ridge Associated Univ, NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd,Code 671, Greenbelt, MD 20771 USA. RI Su, Yang/J-5381-2014; Reeves, Katharine/P-9163-2014; OI SEATON, DANIEL/0000-0002-0494-2025 FU NASA HGI; RHESSI; Lockheed-Martin [SP02H1701R, SP02H3901R]; PRODEX [C90345]; PROBA2/SWAP mission; European Commission [218816] FX S. L. Savage is supported by an appointment to the NASA Postdoctoral Program at Goddard Space Flight Center administered by Oak Ridge Associated Universities through a contract with NASA and under the mentorship of G. Holman. G. Holman is supported by a NASA HGI Grant and the RHESSI program. K. K. Reeves is supported under contract SP02H1701R from Lockheed-Martin to SAO. Support for D.B.S.'s contribution to this paper came from PRODEX Grant No. C90345 managed by the European Space Agency in collaboration with the Belgian Federal Science Policy Office (BELSPO) in support of the PROBA2/SWAP mission, and from the European Commission's Seventh Framework Programme (FP7/2007-2013) under the grant agreement no. 218816 (SOTERIA project, www.soteria-space.eu). D. E. McKenzie is supported under contract SP02H3901R from Lockheed-Martin to MSU. The authors thank Dr. Nicholas Murphy for valuable discussions and the anonymous referee for enhancing the manuscript. NR 56 TC 25 Z9 25 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 JUL 20 PY 2012 VL 754 IS 1 AR 13 DI 10.1088/0004-637X/754/1/13 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800013 ER PT J AU Takakuwa, S Saito, M Lim, J Saigo, K Sridharan, TK Patel, NA AF Takakuwa, Shigehisa Saito, Masao Lim, Jeremy Saigo, Kazuya Sridharan, T. K. Patel, Nimesh A. TI A KEPLERIAN CIRCUMBINARY DISK AROUND THE PROTOSTELLAR SYSTEM L1551 NE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (L1551 NE); ISM: molecules; stars: formation ID CIRCUMSTELLAR DUST DISKS; YOUNG STELLAR OBJECTS; STAR-FORMATION; SUBMILLIMETER ARRAY; MAGNETIC BRAKING; PROTOPLANETARY DISK; ENVELOPE STRUCTURE; TAURUS-AURIGA; DARK CLOUD; IRS 5 AB We present Submillimeter Array observations of a Keplerian disk around the Class I protobinary system L1551 NE in 335 GHz continuum emission and submillimeter line emission in (CO)-C-13 (J = 3-2) and (CO)-O-18 (J = 3-2) at a resolution of similar to 120 x 80 AU. The 335 GHz dust-continuum image shows a strong central peak closely coincident with the binary protostars and likely corresponding to circumstellar disks, surrounded by a similar to 600 x 300 AU feature elongated approximately perpendicular to the [Fe II] jet from the southern protostellar component suggestive of a circumbinary disk. The (CO)-C-13 and (CO)-O-18 images confirm that the circumbinary continuum feature is indeed a rotating disk; furthermore, the (CO)-O-18 channel maps can be well modeled by a geometrically thin disk exhibiting Keplerian rotation. We estimate a mass for the circumbinary disk of similar to 0.03-0.12 M-circle dot, compared with an enclosed mass of similar to 0.8 M-circle dot that is dominated by the protobinary system. Compared with several other Class I protostars known to exhibit Keplerian disks, L1551 NE has the lowest bolometric temperature (similar to 91 K), highest envelope mass (similar to 0.39 M-circle dot), and the lowest ratio in stellar mass to envelope + disk + stellar mass (similar to 0.65). L1551 NE may therefore be the youngest protostellar object so far found to exhibit a Keplerian disk. Our observations present firm evidence that Keplerian disks around binary protostellar systems, "Keplerian circumbinary disks," can exist. We speculate that tidal effects from binary companions could transport angular momenta toward the inner edge of the circumbinary disk and create the Keplerian circumbinary disk. C1 [Takakuwa, Shigehisa] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Saito, Masao; Saigo, Kazuya] Natl Inst Nat Sci, Natl Astron Observ Japan, ALMA Project Off, Mitaka, Tokyo 1818588, Japan. [Lim, Jeremy] Univ Hong Kong, Dept Phys, Hong Kong, Hong Kong, Peoples R China. [Sridharan, T. K.; Patel, Nimesh A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Takakuwa, S (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 10617, Taiwan. EM takakuwa@asiaa.sinica.edu.tw FU National Science Council of Taiwan [NSC 99-2112-M-001-009-MY3] FX We are grateful to P. T. P. Ho and N. Ohashi for their fruitful discussions. We thank all the SMA staff supporting this work. S.T. acknowledges a grant from the National Science Council of Taiwan (NSC 99-2112-M-001-009-MY3) in support of this work. NR 63 TC 35 Z9 35 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 JUL 20 PY 2012 VL 754 IS 1 AR 52 DI 10.1088/0004-637X/754/1/52 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800052 ER PT J AU Tanvir, NR Levan, AJ Fruchter, AS Fynbo, JPU Hjorth, J Wiersema, K Bremer, MN Rhoads, J Jakobsson, P O'Brien, PT Stanway, ER Bersier, D Natarajan, P Greiner, J Watson, D Castro-Tirado, AJ Wijers, RAMJ Starling, RLC Misra, K Graham, JF Kouveliotou, C AF Tanvir, N. R. Levan, A. J. Fruchter, A. S. Fynbo, J. P. U. Hjorth, J. Wiersema, K. Bremer, M. N. Rhoads, J. Jakobsson, P. O'Brien, P. T. Stanway, E. R. Bersier, D. Natarajan, P. Greiner, J. Watson, D. Castro-Tirado, A. J. Wijers, R. A. M. J. Starling, R. L. C. Misra, K. Graham, J. F. Kouveliotou, C. TI STAR FORMATION IN THE EARLY UNIVERSE: BEYOND THE TIP OF THE ICEBERG SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: luminosity function, mass function ID GAMMA-RAY-BURST; ULTRA-DEEP-FIELD; HUBBLE-SPACE-TELESCOPE; LYMAN-BREAK GALAXIES; SIMILAR-TO 7; CORE-COLLAPSE SUPERNOVAE; HIGH COLUMN DENSITY; HOST GALAXY; HIGH-REDSHIFT; WFC3/IR OBSERVATIONS AB We present late-time Hubble Space Telescope (HST) imaging of the fields of six Swift gamma-ray bursts (GRBs) lying at 5.0 less than or similar to z less than or similar to 9.5. Our data include very deep observations of the field of the most distant spectroscopically confirmed burst, GRB 090423, at z = 8.2. Using the precise positions afforded by their afterglows, we can place stringent limits on the luminosities of their host galaxies. In one case, that of GRB 060522 at z = 5.11, there is a marginal excess of flux close to the GRB position which may be a detection of a host at a magnitude J(AB) approximate to 28.5. None of the others are significantly detected, meaning that all the hosts lie below L* at their respective redshifts, with star formation rates (SFRs) less than or similar to 4 M-circle dot yr(-1) in all cases. Indeed, stacking the five fields with WFC3-IR data, we conclude a mean SFR < 0.17 M-circle dot yr(-1) per galaxy. These results support the proposition that the bulk of star formation, and hence integrated UV luminosity, at high redshifts arises in galaxies below the detection limits of deep-field observations. Making the reasonable assumption that GRB rate is proportional to UV luminosity at early times allows us to compare our limits with expectations based on galaxy luminosity functions (LFs) derived from the Hubble Ultra-Deep Field and other deep fields. We infer that an LF, which is evolving rapidly toward steeper faint-end slope (alpha) and decreasing characteristic luminosity (L*), as suggested by some other studies, is consistent with our observations, whereas a non-evolving LF shape is ruled out at greater than or similar to 90% confidence. Although it is not yet possible to make stronger statements, in the future, with larger samples and a fuller understanding of the conditions required for GRB production, studies like this hold great potential for probing the nature of star formation, the shape of the galaxy LF, and the supply of ionizing photons in the early universe. C1 [Tanvir, N. R.; Wiersema, K.; O'Brien, P. T.; Starling, R. L. C.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Levan, A. J.; Stanway, E. R.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Fruchter, A. S.; Misra, K.; Graham, J. F.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Fynbo, J. P. U.; Hjorth, J.; Watson, D.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Bremer, M. N.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Rhoads, J.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Jakobsson, P.] Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland. [Bersier, D.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5UX, Merseyside, England. [Natarajan, P.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Natarajan, P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA USA. [Greiner, J.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Castro-Tirado, A. J.] Inst Astrofs Andalucia IAA CSIC, Granada 18008, Spain. [Wijers, R. A. M. J.] Astron Inst Anton Pannekoek, NL-1090 SJ Amsterdam, Netherlands. [Kouveliotou, C.] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. RP Tanvir, NR (reprint author), Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England. EM nrt3@star.le.ac.uk RI Fynbo, Johan/L-8496-2014; Watson, Darach/E-4521-2015; Jakobsson, Pall/L-9950-2015; OI Fynbo, Johan/0000-0002-8149-8298; Watson, Darach/0000-0002-4465-8264; Jakobsson, Pall/0000-0002-9404-5650; Stanway, Elizabeth/0000-0002-8770-809X; Wijers, Ralph/0000-0002-3101-1808; Castro-Tirado, A. J./0000-0003-2999-3563 FU STFC; NASA [NAS 5-26555]; ERC-StG [EGGS-278202]; DNRF FX We acknowledge support from STFC. Based on observations made with the NASA/ESA Hubble Space Telescope (HST), obtained from the data archive at the Space Telescope Institute. STScI is operated by the association of Universities for Research in Astronomy, Inc. under the NASA contract NAS 5-26555. These observations are associated with HST programs GO-10616 (PI: Berger), GO-10926 (PI: Tanvir), GO-11189 (PI: Tanvir), and GO-11734 (PI: Levan).; J.P.U.F. acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. NR 99 TC 64 Z9 64 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2012 VL 754 IS 1 AR 46 DI 10.1088/0004-637X/754/1/46 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 970EV UT WOS:000306111800046 ER PT J AU Kuntner, M Gregoric, M Zhang, SC Kralj-Fiser, S Li, DQ AF Kuntner, Matjaz Gregoric, Matjaz Zhang, Shichang Kralj-Fiser, Simona Li, Daiqin TI Mating Plugs in Polyandrous Giants: Which Sex Produces Them, When, How and Why? SO PLOS ONE LA English DT Article ID ORB-WEB SPIDER; SEXUALLY CANNIBALISTIC SPIDER; SPERM COMPETITION; COPULATORY PLUGS; ARGIOPE-BRUENNICHI; GENITAL MUTILATION; ARANEAE ARANEIDAE; NEPHILID SPIDERS; SPECIES ARANEAE; MALE ADAPTATION AB Background: Males usually produce mating plugs to reduce sperm competition. However, females can conceivably also produce mating plugs in order to prevent unwanted, superfluous and energetically costly matings. In spiders-appropriate models for testing plugging biology hypotheses-mating plugs may consist of male genital parts and/or of amorphous covers consisting of glandular or sperm secretions. In the giant wood spider Nephila pilipes, a highly sexually dimorphic and polygamous species, males are known to produce ineffective embolic plugs through genital damage, but nothing is known about the origin and function of additional conspicuous amorphous plugs (AP) covering female genitals. Methodology: We tested alternative hypotheses of the nature and function of AP in N. pilipes by staging mating trials with varying degrees of polyandry. No APs were ever formed during mating trials, which rules out the possibility of male AP formation. Instead, those females that oviposited produced the AP from a liquid secreted during egg sac formation. Polyandrous females were more likely to lay eggs and to produce the AP, as were those that mated longer and with more total insertions. Our further tests revealed that, in spite of being a side product of egg sac production, AP, when hardened, prevented any subsequent copulation. Conclusions: We conclude that in the giant wood spider (Nephila pilipes), the amorphous mating plugs are not produced by the males, that repeated copulations (most likely polyandrous) are necessary for egg fertilization and AP formation, and that the AP represents a female adaptation to sexual conflict through prevention of unwanted, excessive copulations. Considering the largely unknown origin of amorphous plugs in spiders, we predict that a similar pattern might be detected in other clades, which would help elucidate the evolutionary interplay of various selection pressures responsible for the origin and maintenance of mating plugs. C1 [Kuntner, Matjaz; Gregoric, Matjaz; Kralj-Fiser, Simona] Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, Ljubljana, Slovenia. [Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kuntner, Matjaz; Li, Daiqin] Hubei Univ, Coll Life Sci, Wuhan 430062, Hubei, Peoples R China. [Zhang, Shichang; Li, Daiqin] Natl Univ Singapore, Dept Biol Sci, Singapore 117548, Singapore. RP Kuntner, M (reprint author), Slovenian Acad Sci & Arts, Inst Biol, Ctr Sci Res, 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 of Biodiversity Research Fellowship; Ministry of Education Academic Research Fund [AcRF: R-154-000-435-112]; Humboldt Postdoctoral Fellowship; ARRS Postdoctoral Fellowship [Z1-4194]; Humboldt Return Fellowship FX This research was supported by the Slovenian Research Agency (grant J1-2063) and a Raffles Museum of Biodiversity Research Fellowship to M. Kuntner, by the Ministry of Education Academic Research Fund (AcRF: R-154-000-435-112) to D. Li, and by Humboldt Postdoctoral and Return Fellowships, and an ARRS Postdoctoral Fellowship Z1-4194 to S. Kralj-Fiser. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 9 Z9 9 U1 6 U2 46 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 JUL 19 PY 2012 VL 7 IS 7 AR e40939 DI 10.1371/journal.pone.0040939 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 981GZ UT WOS:000306956300038 PM 22829900 ER PT J AU Irwin, RP Zimbelman, JR AF Irwin, Rossman P., III Zimbelman, James R. TI Morphometry of Great Basin pluvial shore landforms: Implications for paleolake basins on Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID ORBITER LASER ALTIMETER; PAST 250,000 YEARS; SUMMER LAKE; INTERPLANETARY CRUISE; COASTAL GEOMORPHOLOGY; PALEOCLIMATE RECORD; CLIMATE-CHANGE; CRATER LAKES; GUSEV CRATER; OREGON AB Many basins with relict contributing valley networks and outlet valleys in the Martian highlands indicate past flowing and ponded water on the surface. These likely paleolakes motivate an investigation of pluvial shore landforms in the Great Basin region of the western United States, as confident identification of strandlines on Mars would facilitate analyses of its past hydrology and climate. The purpose of this study is to characterize the scale of Late Pleistocene erosional and depositional shore landforms in an endorheic setting, determine the preservation potential of similar forms from multiple epochs in early Martian history, and identify the data products that would be necessary to detect them. We use Differential Global Positioning System field surveys to measure the dimensions and elevations of shore landforms; compare shore platform widths to theoretical maxima; and note the minimum scale of landforms that have survived since the Late Noachian and Early Hesperian Epochs on Mars. We find that due to impact gardening and aeolian erosion, Martian highland paleolakes like those in the pluvial Great Basin would likely not have well-preserved shore landforms, unless they were unusually large and formed in the Late Hesperian or later. Individual strandlines are often not equally well expressed around an entire basin, so correlating shore landforms in plan view imaging and using their consistency in elevation as a hypothesis test for paleolakes can be challenging. Detection of younger shore landforms like those examined here would require meter-resolution imaging and topography such as stereo digital elevation models. C1 [Irwin, Rossman P., III; Zimbelman, James R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Irwin, Rossman P., III] Planetary Sci Inst, Tucson, AZ USA. RP Irwin, RP (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315,6th St & Independence Ave SW, Washington, DC 20013 USA. EM irwinr@si.edu FU NASA Mars Fundamental Research Program [NNX07AQ71G]; Mars Data Analysis Program [NNX11AI92G] FX A grant from the NASA Mars Fundamental Research Program (NNX07AQ71G; JRZ, Principal Investigator) funded the field investigation, and the Mars Data Analysis Program (NNX11AI92G, RPI, Principal Investigator) funded analysis of planetary data. We thank Tim Parker, Monica Pondrelli, and Nicolas Mangold for their constructive reviews. Much of this work was completed while RPI was a visiting scientist at NASA Goddard Space Flight Center, Greenbelt, Maryland. NR 79 TC 7 Z9 7 U1 0 U2 16 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 JUL 18 PY 2012 VL 117 AR E07004 DI 10.1029/2012JE004046 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 977YD UT WOS:000306700500001 ER PT J AU Wappler, T Labandeira, CC Rust, J Frankenhauser, H Wilde, V AF Wappler, Torsten Labandeira, Conrad C. Rust, Jes Frankenhaeuser, Herbert Wilde, Volker TI Testing for the Effects and Consequences of Mid Paleogene Climate Change on Insect Herbivory SO PLOS ONE LA English DT Article ID CARBON-DIOXIDE CONCENTRATIONS; TROPICAL RAIN-FORESTS; PLANT DIVERSITY; CENTRAL-EUROPE; ATMOSPHERIC CO2; ECKFELD EIFEL; EOCENE; ASSOCIATIONS; GERMANY; DEFENSE AB Background: The Eocene, a time of fluctuating environmental change and biome evolution, was generally driven by exceptionally warm temperatures. The Messel (47.8 Ma) and Eckfeld (44.3 Ma) deposits offer a rare opportunity to take a census of two, deep-time ecosystems occurring during a greenhouse system. An understanding of the long-term consequences of extreme warming and cooling events during this interval, particularly on angiosperms and insects that dominate terrestrial biodiversity, can provide insights into the biotic consequences of current global climatic warming. Methodology/Principal Findings: We compare insect-feeding damage within two middle Eocene fossil floras, Messel and Eckfeld, in Germany. From these small lake deposits, we studied 16,082 angiosperm leaves and scored each specimen for the presence or absence of 89 distinctive and diagnosable insect damage types (DTs), each of which was allocated to a major functional feeding group, including four varieties of external foliage feeding, piercing- and-sucking, leaf mining, galling, seed predation, and oviposition. Methods used for treatment of presence-absence data included general linear models and standard univariate, bivariate and multivariate statistical techniques. Conclusions/Significance: Our results show an unexpectedly high diversity and level of insect feeding than comparable, penecontemporaneous floras from North and South America. In addition, we found a higher level of herbivory on evergreen, rather than deciduous taxa at Messel. This pattern is explained by a ca. 2.5-fold increase in atmospheric CO2 that overwhelmed evergreen antiherbivore defenses, subsequently lessened during the more ameliorated levels of Eckfeld times. These patterns reveal important, previously undocumented features of plant-host and insect-herbivore diversification during the European mid Eocene. C1 [Wappler, Torsten; Rust, Jes] Univ Bonn, Steinmann Inst, Bonn, Germany. [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20560 USA. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. [Frankenhaeuser, Herbert] Mainz Nat Hist Museum State Collect Nat Hist Rhin, Mainz, Germany. [Wilde, Volker] Senckenberg Forschungsinst, Frankfurt, Germany. [Wilde, Volker] Natl Museum, Frankfurt, Germany. RP Wappler, T (reprint author), Univ Bonn, Steinmann Inst, Bonn, Germany. EM twappler@uni-bonn.de RI Wappler, Torsten/D-4287-2011 OI Wappler, Torsten/0000-0003-1592-0988 FU Deutsche Forschungsgemeinschaft (DFG) DFG [RU 665/4-1, RU 665/4-2] FX Funding was provided from the Deutsche Forschungsgemeinschaft (DFG) DFG project No. RU 665/4-1 and 4-2 (to TW and JR). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 104 TC 19 Z9 19 U1 2 U2 39 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 JUL 18 PY 2012 VL 7 IS 7 AR e40744 DI 10.1371/journal.pone.0040744 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 975YY UT WOS:000306548900042 PM 22815805 ER PT J AU Gowaty, PA Kim, YK Anderson, WW AF Gowaty, Patricia Adair Kim, Yong-Kyu Anderson, Wyatt W. TI No evidence of sexual selection in a repetition of Bateman's classic study of Drosophila melanogaster SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE genetic parentage; monogamy ID PRINCIPLES AB We are unique in reporting a repetition of Bateman [Bateman AJ (1948) Heredity (Edinb) 2:349-368] using his methods of parentage assignment, which linked sex differences in variance of reproductive success and variance in number of mates in small populations of Drosophila melanogaster. Using offspring phenotypes, we inferred who mated with whom and assigned offspring to parents. Like Bateman, we cultured adults expressing dramatic phenotypes, so that each adult was heterozygous-dominant at its unique marker locus but had only wild-type alleles at all other subjects' marker loci. Assuming no viability effects of parental markers on offspring, the frequencies of parental phenotypes in offspring follow Mendelian expectations: one-quarter will be double-mutants who inherit the dominant gene from each parent, the offspring from which Bateman counted the number of mates per breeder; half of the offspring must be single mutants inheriting the dominant gene of one parent and the wild-type allele of the other parent; and one-quarter would inherit neither of their parent's marker mutations. Here we show that inviability of double-mutant offspring biased inferences of mate number and number of offspring on which rest inferences of sex differences in fitness variances. Bateman's method overestimated subjects with zero mates, underestimated subjects with one or more mates, and produced systematically biased estimates of offspring number by sex. Bateman's methodology mismeasured fitness variances that are the key variables of sexual selection. C1 [Gowaty, Patricia Adair] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Univ Calif Los Angeles, Inst Environm, Los Angeles, CA 90095 USA. [Gowaty, Patricia Adair] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. [Kim, Yong-Kyu; Anderson, Wyatt W.] Univ Georgia, Dept Genet, Athens, GA 30602 USA. [Kim, Yong-Kyu] Emory Univ, Dept Biol, Atlanta, GA 30322 USA. RP Gowaty, PA (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM gowaty@eeb.ucla.edu; wyatt@uga.edu FU National Science Foundation [IBN-9631801, IBN-0911606, IOS-1121797] FX We thank Malin Ah-King, Margaret Anderson, Dan Blumstein, John Byers, Sergio Castrezana, Don Dewsbury, Lee C. Drickamer, Brant Faircloth, Mark Friedman, Greg Grether, Thierry Hoquet, Therese Markow, Steve Hubbell, Allen Moore, Sahotra Sarkar, Zuleyma Tang-Martinez, and Judy Stamps for comments and useful discussions; and Kyungsun "Sun" Kim for her work in carrying out the experiments. National Science Foundation Grants IBN-9631801, IBN-0911606, and IOS-1121797 each provided partial support for the study. NR 16 TC 27 Z9 27 U1 3 U2 77 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 JUL 17 PY 2012 VL 109 IS 29 BP 11740 EP 11745 DI 10.1073/pnas.1207851109 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 979RI UT WOS:000306837100054 PM 22689966 ER PT J AU Weigt, LA Baldwin, CC Driskell, A Smith, DG Ormos, A Reyier, EA AF Weigt, Lee A. Baldwin, Carole C. Driskell, Amy Smith, David G. Ormos, Andrea Reyier, Eric A. TI Using DNA Barcoding to Assess Caribbean Reef Fish Biodiversity: Expanding Taxonomic and Geographic Coverage SO PLOS ONE LA English DT Article ID FRESH-WATER FISHES; C-OXIDASE-I; TELEOSTEI GOBIIDAE; IDENTIFICATION; NUCLEOTIDE; PERCIFORMES; EXTRACTION; SPECIATION; DIVERSITY; DIVERGENCE AB This paper represents a DNA barcode data release for 3,400 specimens representing 521 species of fishes from 6 areas across the Caribbean and western central Atlantic regions (FAO Region 31). Merged with our prior published data, the combined efforts result in 3,964 specimens representing 572 species of marine fishes and constitute one of the most comprehensive DNA barcoding "coverages" for a region reported to date. The barcode data are providing new insights into Caribbean shorefish diversity, allowing for more and more accurate DNA-based identifications of larvae, juveniles, and unknown specimens. Examples are given correcting previous work that was erroneous due to database incompleteness. C1 [Weigt, Lee A.; Driskell, Amy; Ormos, Andrea] Smithsonian Inst, Labs Analyt Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Baldwin, Carole C.; Smith, David G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Reyier, Eric A.] Kennedy Space Ctr, IHA Environm Serv, Kennedy Space Ctr, FL USA. RP Weigt, LA (reprint author), Smithsonian Inst, Labs Analyt Biol, Natl Museum Nat Hist, Washington, DC 20560 USA. EM weigtl@si.edu FU Smithsonian Marine Science Network; Smithsonian DNA Barcoding Initiative at L.A.B. FX Funding was provided by the Smithsonian Marine Science Network and the Smithsonian DNA Barcoding Initiative at L.A.B. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 51 TC 27 Z9 30 U1 3 U2 41 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 JUL 17 PY 2012 VL 7 IS 7 AR e41059 DI 10.1371/journal.pone.0041059 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 975JG UT WOS:000306507000059 PM 22815912 ER PT J AU Lemeshko, M Krems, RV Weimer, H AF Lemeshko, Mikhail Krems, Roman V. Weimer, Hendrik TI Nonadiabatic Preparation of Spin Crystals with Ultracold Polar Molecules SO PHYSICAL REVIEW LETTERS LA English DT Article ID ISING-MODEL AB We study the growth dynamics of ordered structures of strongly interacting polar molecules in optical lattices. Using a dipole blockade of microwave excitations, we map the system onto an interacting spin-1/2 model possessing ground states with crystalline order, and describe a way to prepare these states by nonadiabatically driving the transitions between molecular rotational levels. The proposed technique bypasses the need to cross a phase transition and allows for the creation of ordered domains of considerably larger size compared to approaches relying on adiabatic preparation. C1 [Lemeshko, Mikhail; Weimer, Hendrik] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lemeshko, Mikhail; Weimer, Hendrik] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Krems, Roman V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. RP Lemeshko, M (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM mikhail.lemeshko@gmail.com; rkrems@chem.ubc.ca; hweimer@cfa.harvard.edu FU National Science Foundation; German Academic Exchange Service (DAAD) FX We thank Susanne Yelin, Samuel Meek, Nicolas Vanhaecke, and Charles Mathy for insightful discussions. This work was supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory and within the Postdoc Program of the German Academic Exchange Service (DAAD). NR 33 TC 22 Z9 22 U1 1 U2 21 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 JUL 16 PY 2012 VL 109 IS 3 AR 035301 DI 10.1103/PhysRevLett.109.035301 PG 5 WC Physics, Multidisciplinary SC Physics GA 974FY UT WOS:000306417600007 PM 22861865 ER PT J AU Sessa, JA Ivany, LC Schlossnagle, TH Samson, SD Schellenberg, SA AF Sessa, Jocelyn A. Ivany, Linda C. Schlossnagle, Trevor H. Samson, Scott D. Schellenberg, Stephen A. TI The fidelity of oxygen and strontium isotope values from shallow shelf settings: Implications for temperature and age reconstructions SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Mollusc; Sclerochronology; Stable isotopes; Palaeoclimatology; Age reconstruction; Shelf ID GULF COASTAL-PLAIN; EOCENE THERMAL MAXIMUM; EARLY MIDDLE EOCENE; ATLANTIC SURF CLAM; STABLE-ISOTOPE; MOLLUSK SHELLS; SPISULA-SOLIDISSIMA; BIVALVE MOLLUSK; LATE PALEOCENE; NORTH-AMERICA AB The oxygen and strontium isotopic ratios of marine carbonates are widely employed to derive paleotemperature and age, respectively. While open ocean samples are the standard source for these measures, shelf settings can also provide detailed records. However, the implementation of shelf data for these purposes has been hindered by the perception that local environmental conditions (such as freshwater influx) confound regional and global signals. Here, we directly evaluate this concern by assessing the spatial variability in the isotopic composition of biogenic carbonate precipitated along the depositional strike of an inner shelf environment. Data are derived from mollusc shells collected from a stratigraphically restricted, transgressive unit in the early Eocene (similar to 55 Ma) of the US Gulf Coastal Plain (GCP). Lithofacies and fossil assemblages suggest that an estuary was present in the westernmost study region, whereas more typically marine facies predominated elsewhere. Isotopic composition varies predictably with paleoenvironmental setting; shells from the estuary have delta O-18 values and Sr-87/Sr-88 ratios that reflect high freshwater input. Specimens in the eastern GCP, however, from within and between outcrops separated by up to 400 km, all yield similar results. Serial microsampling reveals congruence not only in mean delta O-18 values, but also in winter and summer extremes. Estimated paleotemperatures (mean annual temperature of 26 degrees C) agree well with proxy and model evidence for the early Eocene and the GCP, and 87Sr/88Sr ratios are consistent with the established early Eocene seawater ratio. The fidelity of isotopic values relative to environment indicates that shallow shelf records have much to contribute to studies of ancient climate and ocean chemistry. (c) 2012 Elsevier B.V. All rights reserved. C1 [Sessa, Jocelyn A.; Ivany, Linda C.; Schlossnagle, Trevor H.; Samson, Scott D.] Syracuse Univ, Dept Earth Sci, Syracuse, NY 13244 USA. [Schellenberg, Stephen A.] San Diego State Univ, Dept Geol Sci, San Diego, CA 92182 USA. RP Sessa, JA (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. EM SessaJ@si.edu FU National Science Foundation Grant [EAR-0719645] FX G. Died, J. Nagel-Myers, and A. Molineux are thanked for access to specimens, and E. Fenton for the collection of the Sowashee Creek specimens. We are grateful to B. Sell, A. Satkoski, and T. Dasgupta for help with Sr-isotope sample preparation and analysis, to H. Ford for running some of the minor elemental analyses, to J. Andrew Beard for sampling three specimens for minor elemental analysis, and to J. Post for microdiffractometer assistance. Stable isotope analyses were run by Lora Wingate at the University of Michigan Stable Isotope Laboratory and Gregory Cane at the University of Kansas Keck Paleoenvironmental and Environmental Stable Isotope Laboratory. P. Jardine kindly identified pollen in the Sabinetown samples. We are grateful to E. Grossman for providing the oxygen isotopic values for specimen BSV1 from Kobashi et al. (2001). We thank D. Siegel for helpful discussion and B. Huber and G. Harrington for insightful comments on an earlier version of this. manuscript. E. Grossman and D. Gillikin provided thoughtful reviews that improved this manuscript. This research was supported by National Science Foundation Grant EAR-0719645 to Ivany. NR 117 TC 9 Z9 9 U1 2 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 JUL 15 PY 2012 VL 342 BP 27 EP 39 DI 10.1016/j.palaeo.2012.04.021 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 978GE UT WOS:000306727800003 ER PT J AU Woodman, N Matson, JO McCarthy, TJ Eckerlin, RP Bulmer, W Ordonez-Garza, N AF Woodman, Neal Matson, John O. McCarthy, Timothy J. Eckerlin, Ralph P. Bulmer, Walter Ordonez-Garza, Nicte TI DISTRIBUTIONAL RECORDS OF SHREWS (MAMMALIA, SORICOMORPHA, SORICIDAE) FROM NORTHERN CENTRAL AMERICA WITH THE FIRST RECORD OF SOREX FROM HONDURAS SO ANNALS OF CARNEGIE MUSEUM LA English DT Article DE food habits; Insectivora; parasites; pit fall; reproduction; shrews; trap success ID SMALL-EARED SHREW; FOOD NICHE OVERLAP; GENUS CRYPTOTIS; MONTANE FOREST; MORPHOLOGICAL VARIATION; MOLECULAR SYSTEMATICS; ECOLOGICAL SEPARATION; COSTA-RICA; INSECTIVORA; GUATEMALA AB Short term surveys for small mammals in Guatemala and Honduras during 1992-2009 provided important new records for 12 taxa of shrews from 24 localities. These locality records expand the known geographic distributions for live species and for the genus Sorex Linnaeus, 1758: the geographic range of Cryptotis goodwini Jackson, 1933, now includes the Sierra de las Minas, Guatemala, and several isolated highlands in western Honduras; the known distribution of Cryptotis mayensis (Merriam, 1901) is increased with the first definite modern record for this shrew from Guatemala; Cryptotis merriami Choate, 1970, is now known to occur in the Sierra de las Minas and the Sierra del Merendon, Guatemala, as well as the isolated Sierra de Omoa and Montana de La Muralla in Honduras, and its documented elevational range (600-1720 m) is expanded; records of Sorer veraepacis Alston, 1877, expand the known distribution of this species to include the Sierra de Yalijux, Guatemala; and discovery of Sorex salvini Merriam, 1897, at Celaque, Honduras (1825-3110 m), represents a considerable extension of the geographic range of the species, and it is the first record of the genus Sorer from Honduras. In addition, the first record of potential syntopy among C. goodwini, C. merriami, and Cryptotis orophilus (J.A. Allen, 1895), is reported at an elevation of 1430 in in the Sierra de Celaque, Honduras. Information associated with these records contributes substantially to knowledge of habitat use, elevational distributions, reproductive patterns, diet, and parasites of the species encountered. General patterns include the first evidence that Neotropical species of soricids have smaller litters than their temperate congeners. C1 [Woodman, Neal] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Sect Mammals,Carnegie Museum Nat Hist, Washington, DC 20013 USA. [Matson, John O.] San Jose State Univ, Dept Biol Sci, San Jose, CA 95192 USA. [McCarthy, Timothy J.] Carnegie Museum Nat Hist, Sect Mammals, Pittsburgh, PA 15206 USA. [Eckerlin, Ralph P.] No Virginia Community Coll, Div Nat Sci, Natl Museum Nat Hist, Sect Invertebrate Zool, Annandale, VA 22003 USA. [Ordonez-Garza, Nicte] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. RP Woodman, N (reprint author), Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Sect Mammals,Carnegie Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu; johnomatson@gmail.com; reckerlin@nvcc.edu; wbulmer@comcast.net; nicte.ordonez-garza@ttu.edu FU M. Graham Netting Fund; O'Neil Field Research Fund; National Geographic Society [6105-98]; R.K. Mellon North American Mammal Research Institute of the Carnegie Museum of Natural History; U.S. Food and Drug Administration; The Section of Mammals, Carnegie Museum of Natural History; The Department of Biological Sciences, San Jose State University; Northern Virginia Community College Professional Development Fund; The Nature Conservancy; Campmor Inc.; United States Geological Survey FX For various forms of assistance, we thank J. Bucklin, J.A. Campbell, G.A. Cruz D., L. Barahona, E. Fernandez, S.R. Flores R., Fundacion Ecologista, H. Galeano, FUNDAECO, L.L. Hodges, J.A. Ibarra, G. Ibarra U., H. Lanier, S. Midence, J. Monzon S., B. Myton, A. Novack, A.J. Paredes, S.G. Perez C., V. Roth, M. Roth, J.C. Schuster, E.N. Smith, S.P. Thorn, O. Valdez, and J.R. Valdez. E. Cano and J.J. Polisar kindly provided access to specimen records; L. Wilkins assisted information requests. Special thanks to P.D. Jenkins, R. Portela Miguez, D. Hills, and R. Harbord (BMNH) for access to registers, literature, and specimens, and J. Thackary for access to archives in the BMNH Library. Field work was supported by M. Graham Netting Fund; O'Neil Field Research Fund; National Geographic Society (#6105-98 to TJM); the R.K. Mellon North American Mammal Research Institute of the Carnegie Museum of Natural History; U.S. Food and Drug Administration (to RPE); The Section of Mammals, Carnegie Museum of Natural History; The Department of Biological Sciences, San Jose State University (to JOM); Northern Virginia Community College Professional Development Fund (to RPE); The Nature Conservancy; Campmor Inc.; and the United States Geological Survey. We are grateful to the Departamento de Biologia, Universidad Nacional Autonoma de Honduras, Cooperacion Hondurena de Forestales (COHDEFOR; V. Archaga, T. Garcia), and Consejo Nacional de Areas Protegidas, Guatemala (CONAP; O.F. Lara, M. Garcia de Solorzano, F. Herrera, E. Flores), for providing collection permits and other valuable assistance. The Union para Proteger el Bosque Nuboso (UPROBON) graciously granted permission to work in Chelemha Natural Reserve. Robert P. Reynolds and two anonymous reviewers provided helpful comments on previous versions of this 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 80 TC 8 Z9 9 U1 0 U2 7 PU CARNEGIE MUSEUM NATURAL HISTORY PI PITTSBURGH PA 4400 FORBES AVE, PITTSBURGH, PA 15213 USA SN 0097-4463 EI 1943-6300 J9 ANN CARNEGIE MUS JI Ann. Carnegie Mus. PD JUL 15 PY 2012 VL 80 IS 3 BP 207 EP 237 PG 31 WC Paleontology; Zoology SC Paleontology; Zoology GA 983SO UT WOS:000307139200003 ER PT J AU Glaeser, SS Hunt, KE Martin, MS Finnegan, M Brown, JL AF Glaeser, S. S. Hunt, K. E. Martin, M. S. Finnegan, M. Brown, J. L. TI Investigation of individual and group variability in estrous cycle characteristics in female Asian elephants (Elephas maximus) at the Oregon Zoo SO THERIOGENOLOGY LA English DT Article DE Elephant; Reproduction; Estrous cycle; Follicular phase; Luteal phase; Progesterone ID LOXODONTA-AFRICANA ELEPHANTS; LUTEINIZING-HORMONE; OVARIAN-FUNCTION; PROGESTERONE; ENDOCRINOLOGY; MANAGEMENT; CAPTIVITY; BEHAVIOR; BIOLOGY; SERUM AB Evaluating ovarian cycle activity through longitudinal progestagen monitoring is important for optimizing breeding management of captive elephants and understanding impact of life events (births, deaths, and transfers) on reproductive function. This study summarized serum progestagen profiles for eight Asian mainland elephants (Elephas maximus indicus) and one Bornean elephant (E. maximus borneensis) at the Oregon Zoo over a 20-yr interval, and represents the longest longitudinal dataset evaluated to date. Estrous cycle characteristics were more varied than previously reported for this species, with an overall duration of 12 to 19 wk, luteal phase duration of 4 to 15 wk, and follicular phase duration of 2 to 12 wk. In general, there was more cycle variability across than within individual elephants. Compared with other elephants in the group, the Borneo female exhibited consistently longer cycle lengths, higher progestagen concentrations, and greater cycle variability; however, it is not known if this represents a subspecies or an individual difference. Cycle durations did not appear to change over time or with age, and the first pubertal cycle was similar to subsequent cycles. Variability in duration of the follicular phase was greater than that of the luteal phase. In addition, there was a significant negative relationship between luteal and follicular phase durations, suggesting a possible regulatory role of the follicular phase in maintaining a relatively consistent cycle duration within individuals. Overall, we found these elephants to be highly resilient in that major life events (births, deaths, and changes in herd structure) had minimal effect on cycle dynamics over time. In conclusion, the higher range in cycle phase characteristics is likely because of the larger number of elephants studied and longer duration of longitudinal monitoring, and may be more representative of the captive population as a whole. Furthermore, identification of significant interanimal variability suggests that understanding the complexities of herd reproductive characteristics could facilitate development of more effective institution-specific breeding management strategies. (c) 2012 Elsevier Inc. All rights reserved. C1 [Glaeser, S. S.; Hunt, K. E.; Martin, M. S.; Finnegan, M.] Oregon Zoo, Portland, OR 97221 USA. [Brown, J. L.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. RP Glaeser, SS (reprint author), Oregon Zoo, 4001 SW Canyon Rd, Portland, OR 97221 USA. EM sharon.glaeser@oregonzoo.org FU Oregon Zoo FX The existence of this vast dataset is due to the Oregon Zoo elephant handlers, past and present, who consistently collected blood from the entire herd for over 20 yrs (Jeb Barsh, Dimas Dominguez, Pat Flora, Doug Groves, Jay Haight, Roger Henneous, Ray Hopper, David Illig, Mike Keele, Jeremy Kirby, Bob Lee, Fred Marion, Sioux Marion, Phil Prewett, Charlie Rutkowski, Joe Sabastiani, Jim Sanford, Pam Starkey, and April Yoder). We owe the integrity of this dataset to the Oregon Zoo laboratory technicians, past and present (Carrie Hays, Karen Lewis, Camie Meller, Tracy Mott, Anne Schmidt, Nancy Scott, and Barbara Slade). We thank David Hess for his consulting advice and Bruce Shulte for recovering some of the historical data. We appreciate the support and assistance of Oregon Zoo's Mike Keele, Karen Lewis, Jan Mothershed, Luis Rodriguez, David Shepherdson, and Anne Warner. Finally, we owe our gratitude to Michael Schmidt and David Hess, who started blood collection on these elephants at the Oregon Zoo in 1974, and provided the first endocrine description of the reproductive cycle and pregnancy of female Asian elephants [14]. NR 28 TC 9 Z9 10 U1 0 U2 46 PU ELSEVIER SCIENCE INC PI NEW YORK PA 360 PARK AVE SOUTH, NEW YORK, NY 10010-1710 USA SN 0093-691X J9 THERIOGENOLOGY JI Theriogenology PD JUL 15 PY 2012 VL 78 IS 2 BP 285 EP 296 DI 10.1016/j.theriogenology.2012.01.014 PG 12 WC Reproductive Biology; Veterinary Sciences SC Reproductive Biology; Veterinary Sciences GA 969EX UT WOS:000306039600006 PM 22578614 ER PT J AU Mascaro, J Asner, GP Dent, DH DeWalt, SJ Denslow, JS AF Mascaro, Joseph Asner, Gregory P. Dent, Daisy H. DeWalt, Saara J. Denslow, Julie S. TI Scale-dependence of aboveground carbon accumulation in secondary forests of Panama: A test of the intermediate peak hypothesis SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Carbon storage; Carnegie Airborne Observatory; Forest structure; LiDAR; Treefall gaps; Tropical secondary forests ID BARRO-COLORADO ISLAND; TROPICAL RAIN-FOREST; BIOMASS; CHRONOSEQUENCE; DYNAMICS; SUCCESSION; AMAZON; LIDAR; VEGETATION; COLOMBIA AB Accumulation of aboveground carbon is one of the most important services provided by tropical secondary forests a land-cover type that is increasing in importance globally. Carbon accumulates rapidly for the first 20 years of succession, but few studies have considered forests older than 20 years, and the available data do not yield a consistent pattern. Two alternative hypotheses have been proposed: (1) an asymptotic increase, with the highest carbon stocks occurring in the oldest stands, and (2) an intermediate peak, caused by roughly synchronous tree maturity (and thus high carbon stocks) after which time treefall gaps cause carbon stocks to regress. Here we revisited a well-studied tropical moist forest chronosequence in Barro Colorado Nature Monument, Central Panama, consisting of 35, 55, 85, and 115-year-old stands, as well as old-growth stands, to determine whether past evidence for the intermediate peak hypothesis was influenced by the spatial limitations of the field plots used to assess forest structure. We used airborne LiDAR (light detection and ranging) to measure carbon stocks at the scale of the original transects (0.16 ha), in surrounding forest of the same age (up to 20 ha), and at a landscape scale incorporating thousands of hectares not previously measured. We also compared forest structure as measured in three dimensions by LiDAR, considering vertical and horizontal variation in canopy organization, as well as the abundance of treefall gaps. Our results suggested a strong scale-dependence of aboveground carbon accumulation, supporting the intermediate peak hypothesis at the fine scale of the 0.16-ha transects, but an asymptotic model at the landscape scale incorporating thousands of hectares. Further analyses of forest structure suggest that both the limitations of small plots and intrinsic scaling of forest structure and carbon dynamics account for the scale-dependence of aboveground carbon accumulation in this secondary forest matrix. (C) 2012 Elsevier B.V. All rights reserved. C1 [Mascaro, Joseph; Asner, Gregory P.] Carnegie Inst Sci, Dept Global Ecol, Stanford, CA 94305 USA. [Mascaro, Joseph; Dent, Daisy H.] Smithsonian Trop Res Inst, Balboa, Panama. [Dent, Daisy H.] Univ Stirling, Dept Biol & Environm Sci, Stirling FK9 4LA, Scotland. [DeWalt, Saara J.] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Denslow, Julie S.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Denslow, Julie S.] USDA Forest Serv, Inst Pacific Isl Forestry, Hilo, HI USA. RP Mascaro, J (reprint author), Carnegie Inst Sci, Dept Global Ecol, 260 Panama St, Stanford, CA 94305 USA. EM jmascaro@stanford.edu RI Asner, Gregory/G-9268-2013; Dent, Daisy/L-3549-2016 OI Asner, Gregory/0000-0001-7893-6421; Dent, Daisy/0000-0002-1219-7344 FU Gordon and Betty Moore Foundation; John D. and Catherine T. MacArthur Foundation; HSBC Climate Partnership; SENACYT [COL10-052]; National Science Foundation [DEB-92-08031] FX We thank T. Kennedy-Bowdoin, J. Jacobson, D. Knapp, A. Balaji, and the rest of the Carnegie Airborne Observatory team for collecting and processing airborne LiDAR data, and two anonymous reviewers for comments that significantly improved this manuscript. This study was supported by the Gordon and Betty Moore Foundation, the John D. and Catherine T. MacArthur Foundation, the HSBC Climate Partnership, SENACYT (COL10-052 to Daisy Dent) and the National Science Foundation (DEB-92-08031 to Julie Denslow). The Carnegie Airborne Observatory is made possible by the Gordon and Betty Moore Foundation, the Grantham Foundation for the Protection of the Environment, W.M. Keck Foundation, and William Hearst III. NR 46 TC 12 Z9 14 U1 1 U2 36 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 JUL 15 PY 2012 VL 276 BP 62 EP 70 DI 10.1016/j.foreco.2012.03.032 PG 9 WC Forestry SC Forestry GA 964TO UT WOS:000305719800007 ER PT J AU Suleimanov, YV Tscherbul, TV Krems, RV AF Suleimanov, Yu. V. Tscherbul, T. V. Krems, R. V. TI Efficient method for quantum calculations of molecule-molecule scattering properties in a magnetic field SO JOURNAL OF CHEMICAL PHYSICS LA English DT Article ID POLAR-MOLECULES; DIPOLAR COLLISIONS; DIATOMIC MOLECULE; COLD MOLECULES; ATOMS; CHEMISTRY; STATES; BEAMS; GAS AB We show that the cross sections for molecule-molecule collisions in the presence of an external field can be computed efficiently using a total angular momentum basis, defined either in the body-fixed frame or in the space-fixed coordinate system. This method allows for computations with much larger basis sets than previously possible. We present calculations for (NH)-N-15-(NH)-N-15 collisions in a magnetic field. Our results support the conclusion of the previous study that the evaporative cooling of rotationally ground (NH)-N-15 molecules in a magnetic trap has a prospect of success. (C) 2012 American Institute of Physics. [http://dx.doi.org/10.1063/1.4733288] C1 [Suleimanov, Yu. V.] MIT, Dept Chem Engn, Cambridge, MA 02139 USA. [Suleimanov, Yu. V.] Princeton Univ, Dept Mech & Aerosp Engn, Combust Energy Frontier Res Ctr, Princeton, NJ 08544 USA. [Tscherbul, T. V.] Harvard MIT Ctr Ultracold Atoms, Cambridge, MA 02138 USA. [Tscherbul, T. V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Krems, R. V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. RP Suleimanov, YV (reprint author), MIT, Dept Chem Engn, Cambridge, MA 02139 USA. EM ysuleyma@princeton.edu RI Tscherbul, Timur/K-3286-2014 OI Tscherbul, Timur/0000-0001-5689-040X FU Canadian Foundation for Innovation FX We thank Liesbeth Janssen, Jeremy Hutson, and Gerrit Groenenboom for discussions and providing the results of their calculations. Y.V.S. and R.V.K. are grateful for the hospitality of the ITAMP visitor program. The computations were performed using a computer cluster funded by the Canadian Foundation for Innovation. The allocation of computer time on Western Canada Research Grid (WestGrid) is also gratefully acknowledged. NR 73 TC 12 Z9 12 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 J9 J CHEM PHYS JI J. Chem. Phys. PD JUL 14 PY 2012 VL 137 IS 2 AR 024103 DI 10.1063/1.4733288 PG 8 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 973LG UT WOS:000306361000005 PM 22803524 ER PT J AU Alyabyshev, SV Lemeshko, M Krems, RV AF Alyabyshev, Sergey V. Lemeshko, Mikhail Krems, Roman V. TI Sensitive imaging of electromagnetic fields with paramagnetic polar molecules SO PHYSICAL REVIEW A LA English DT Article ID MICROSCOPY; MAGNETOMETRY; RESOLUTION; DIAMOND AB We propose a method for sensitive parallel detection of low-frequency electromagnetic fields based on the fine structure interactions in paramagnetic polar molecules. Compared to the recently implemented scheme employing ultracold Rb-87 atoms by Bohi et al. [Appl. Phys. Lett. 97, 051101 (2010)], the technique based on molecules offers a 100-fold higher sensitivity, the possibility to measure both the electric and magnetic field components, and a probe of a wide range of frequencies from the dc limit to the THz regime. C1 [Alyabyshev, Sergey V.; Krems, Roman V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. [Lemeshko, Mikhail] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lemeshko, Mikhail] Harvard Phys Dept, Cambridge, MA 02138 USA. RP Alyabyshev, SV (reprint author), Univ British Columbia, Dept Chem, 2036 Main Mall, Vancouver, BC V6T 1Z1, Canada. EM salyabyshev@gmail.com; mikhail.lemeshko@gmail.com; rkrems@chem.ubc.ca FU NSERC of Canada; NSF at Harvard University; Smithsonian Astrophysical Observatory FX The work was supported by NSERC of Canada and a NSF grant to ITAMP at Harvard University and the Smithsonian Astrophysical Observatory. NR 32 TC 7 Z9 7 U1 1 U2 17 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL 13 PY 2012 VL 86 IS 1 AR 013409 DI 10.1103/PhysRevA.86.013409 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 974CN UT WOS:000306407500008 ER EF