FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Agundez, M Cernicharo, J Guelin, M Kahane, C Roueff, E Klos, J Aoiz, FJ Lique, F Marcelino, N Goicoechea, JR Garcia, MG Gottlieb, CA McCarthy, MC Thaddeus, P AF Agundez, M. Cernicharo, J. Guelin, M. Kahane, C. Roueff, E. Klos, J. Aoiz, F. J. Lique, F. Marcelino, N. Goicoechea, J. R. Garcia, M. Gonzalez Gottlieb, C. A. McCarthy, M. C. Thaddeus, P. TI Astronomical identification of CN-, the smallest observed molecular anion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; molecular processes; stars: AGB and post-AGB; circumstellar matter; stars: individual: IRC+10216 ID INTERSTELLAR; IRC+10216; CLOUDS; C6H; C4H; C8H AB We present the first astronomical detection of a diatomic negative ion, the cyanide anion CN-, and quantum mechanical calculations of the excitation of this anion by means of collisions with para-H-2. The anion CN- is identified by observing the J = 2-1 and J = 3-2 rotational transitions in the C-star envelope IRC + 10216 with the IRAM30-m telescope. The U-shaped line profiles indicate that CN-, like the large anion C6H-, is formed in the outer regions of the envelope. Chemical and excitation model calculations suggest that this species forms from the reaction of large carbon anions with N atoms, rather than from the radiative attachment of an electron to CN, as is the case for large molecular anions. The unexpectedly high abundance derived for CN-, 0.25% relative to CN, indicates that its detection in other astronomical sources is likely. A parallel search for the small anion C2H- remains inconclusive, despite the previous tentative identification of the J = 1-0 rotational transition. The abundance of C2H- in IRC + 10216 is found to be vanishingly small, < 0.0014% relative to C2H. C1 [Agundez, M.; Roueff, E.] LUTH, Observ Paris Meudon, F-92190 Meudon, France. [Cernicharo, J.; Marcelino, N.; Goicoechea, J. R.] CSIC INTA, Dept Astrofis, Ctr Astrobiol, Madrid 28850, Spain. [Guelin, M.] Inst Radioastron Millimetr, F-38406 St Martin Dheres, France. [Kahane, C.] Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. [Klos, J.] Univ Maryland, Dept Chem & Biochem, College Pk, MD 20742 USA. [Aoiz, F. J.] Univ Complutense, Dept Quim Fis, Fac Quim, E-28040 Madrid, Spain. [Lique, F.] Univ Havre, CNRS, LOMC FRE 3102, F-76058 Le Havre, France. [Garcia, M. Gonzalez] Inst Radioastron Milimetr, Granada 18012, Spain. [Gottlieb, C. A.; McCarthy, M. C.; Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Agundez, M (reprint author), LUTH, Observ Paris Meudon, F-92190 Meudon, France. EM marcelino.agundez@obspm.fr RI Klos, Jacek/A-6457-2008; LIQUE, Francois/B-9626-2011; Aoiz, F. Javier/G-8240-2015; Agundez, Marcelino/I-5369-2012; OI Klos, Jacek/0000-0002-7407-303X; LIQUE, Francois/0000-0002-0664-2536; Aoiz, F. Javier/0000-0001-5718-5905; Agundez, Marcelino/0000-0003-3248-3564; McCarthy, Michael/0000-0001-9142-0008 FU European Community [235753]; Spanish MICINN [2010 CSD2009-00038, AYA2009-07304, CTQ2008-02578-BQU]; U.S. National Science Foundation [CHE-0848110] FX We acknowledge R. Chamberlin and T. G. Phillips for their kind help during a previous search of the CN^- J = 3-2 transition with the Caltech Submillimeter Observatory (CSO). We are also grateful to the astronomers that helped with the observations during the 2009 winter HERA pool at the IRAM30-m telescope, among them F. S. Tabatabaei, E. De Beck, G. Bano, and J. Rodon. M. A. is supported by a Marie Curie Intra-European Individual Fellowship within the European Community 7th Framework Programme under grant agreement n^o 235753. J. R. G. is supported by a Ramon y Cajal research contract from the Spanish MICINN and co-financed by the European Social Fund. J. K. acknowledges the partial financial supports from the University Complutense of Madrid/Grupo Santander under the program of Movilidad de Investigadores Extranjeros and from the U.S. National Science Foundation under Grant No. CHE-0848110 to M. H. Alexander. This project has been partly financed by the Spanish MICINN grants Consolider-Ingenio 2010 CSD2009-00038, AYA2009-07304, and CTQ2008-02578-BQU. NR 29 TC 98 Z9 98 U1 4 U2 26 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 JUL PY 2010 VL 517 AR L2 DI 10.1051/0004-6361/201015186 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400002 ER PT J AU Bitsakis, T Charmandaris, V Le Floc'h, E Diaz-Santos, T Slater, SK Xilouris, E Haynes, MP AF Bitsakis, T. Charmandaris, V. Le Floc'h, E. Diaz-Santos, T. Slater, S. K. Xilouris, E. Haynes, M. P. TI A mid-IR study of Hickson compact groups I. Probing the effects of environment in galaxy interactions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE infrared: galaxies; galaxies: evolution; galaxies: interactions; galaxies: peculiar ID SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMING GALAXIES; INFRARED PROPERTIES; STEPHANS QUINTET; NEARBY GALAXIES; MOLECULAR GAS; ISOCAM DATA; DUST AB Hickson compact groups (HCGs) are among the densest galaxy environments of the local universe. To examine the effects of the environment on the infrared properties of these systems, we present an analysis of Spitzer and ISO mid-infrared imaging, as well as of deep ground-based near-infrared imaging of 14 HCGs containing a total of 69 galaxies. Based on mid-infrared color diagnostics we identify the galaxies that appear to host an active nucleus, while using a suite of templates, and fit the complete infrared spectral energy distribution for each group member. We compare our estimates of galaxy mass, star formation rate, total infrared luminosities, and specific star formation rates (sSFR) for our HCG sample to samples of isolated galaxies and interacting pairs and find that overall there is no discernible difference among them. However, HCGs that can be considered as dynamically "old" host late-type galaxies with a slightly lower sSFR than the one found in dynamically "young" groups. This could be attributed to multiple past interactions among the galaxies in old groups, that have led to the build up of their stellar mass. It is also consistent with our prediction of the presence of diffuse cold dust in the intergalactic medium of 9 of the dynamically "old" groups. C1 [Bitsakis, T.; Charmandaris, V.; Diaz-Santos, T.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, V.; Diaz-Santos, T.] IESL Fdn Res & Technol Hellas, Iraklion 71110, Greece. [Charmandaris, V.] Observ Paris, F-75014 Paris, France. [Le Floc'h, E.] Univ Paris Diderot, CNRS, Lab AIM, CEA,DSM,DAPNIA,Serv Astrophys, F-91191 Gif Sur Yvette, France. [Slater, S. K.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Dept Phys, Cambridge, MA 02138 USA. [Xilouris, E.] Natl Observ Athens, Inst Astron & Astrophys, Athens 15236, Greece. [Haynes, M. P.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. RP Bitsakis, T (reprint author), Univ Crete, Dept Phys, Iraklion 71003, Greece. EM bitsakis@physics.uoc.gr RI Charmandaris, Vassilis/A-7196-2008; Diaz-Santos, Tanio/B-4875-2011; Xilouris, Emmanuel/K-9459-2013; Bitsakis, Theodoros/O-2766-2013 OI Charmandaris, Vassilis/0000-0002-2688-1956; Bitsakis, Theodoros/0000-0001-5787-8242 FU EU ToK [39965, FP7-REGPOT 206469] FX We would like to thank E. da Cunha, D. Elbaz and G. Magdis for useful discussions, an anonymous referee for the detailed comments that improved this paper. T.B., V.C., and T.D.S., would like to acknoledge partial support from the EU ToK grant 39965 and FP7-REGPOT 206469. NR 54 TC 18 Z9 18 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 JUL PY 2010 VL 517 AR A75 DI 10.1051/0004-6361/201014102 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400085 ER PT J AU Busquet, G Palau, A Estalella, R Girart, JM Sanchez-Monge, A Viti, S Ho, PTP Zhang, Q AF Busquet, G. Palau, A. Estalella, R. Girart, J. M. Sanchez-Monge, A. Viti, S. Ho, P. T. P. Zhang, Q. TI The NH2D/NH3 ratio toward pre-protostellar cores around the UCH II region in IRAS 20293+3952 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; ISM: individual objects: IRAS 20293+3952; ISM: clouds; ISM: molecules ID HIGH-SPATIAL-RESOLUTION; MASS STAR-FORMATION; DEUTERIUM FRACTIONATION; DEUTERATED AMMONIA; MOLECULAR CLOUDS; STELLAR OBJECTS; ENVIRONMENT; DEPLETION AB Context. The deuterium fractionation, D-frac, has been proposed as an evolutionary indicator in pre-protostellar and protostellar cores of low-mass star- forming regions. Aims. We investigate D-frac, with high angular resolution, in the cluster environment surrounding the UCH II region IRAS 20293+3952. Methods. We performed high angular resolution observations with the IRAM Plateau de Bure Interferometer (PdBI) of the ortho-NH(2)D1(11)-1(01) line at 85.926 GHz and compared them with previously reported VLA NH3 data. Results. We detected strong NH2D emission toward the pre-protostellar cores identified in NH3 and dust emission, all located in the vicinity of the UCH II region IRAS 20293+3952. We found high values of D-frac similar or equal to 0.1-0.8 in all the pre-protostellar cores and low values, D-frac < 0.1, associated with young stellar objects. Conclusions. The high values of D-frac in pre-protostellar cores could be indicative of evolution, although outflow interactions and UV radiation could also play a role. C1 [Busquet, G.; Estalella, R.; Sanchez-Monge, A.] Univ Barcelona, Dept Astron & Meteorol IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. [Palau, A.; Girart, J. M.] CSIC IEEC, Inst Ciencies Espai, Fac Ciencies, Bellaterra 08193, Spain. [Viti, S.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Ho, P. T. P.; Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ho, P. T. P.] Acad Sinica Inst Astron & Astrophys, Taipei, Taiwan. RP Busquet, G (reprint author), Univ Barcelona, Dept Astron & Meteorol IEEC UB, Inst Ciencies Cosmos, E-08028 Barcelona, Spain. EM gbusquet@am.ub.es RI Girart, Josep/O-1638-2014 OI Girart, Josep/0000-0002-3829-5591 FU Spanish MEC [AYA2005-08523-C03]; MICINN, FEDER [AYA2008-06189-C03]; JAE-Doc CSIC FX We thank the anonymous referee for his/her useful comments and suggestions. We acknowledge the IRAM staff for their support during the data reduction. G. B., A. P., R. E., J.M.G., and A.S.-M. are supported by the Spanish MEC grant AYA2005-08523-C03 and the MICINN grant AYA2008-06189-C03 (co-funded with FEDER funds). A. P. is supported by a JAE-Doc CSIC fellowship co-funded with the European Social Fund. NR 20 TC 21 Z9 21 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 JUL PY 2010 VL 517 AR L6 DI 10.1051/0004-6361/201014866 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400006 ER PT J AU Democles, J Pratt, GW Pierini, D Arnaud, M Zibett, S D'Onghia, E AF Democles, J. Pratt, G. W. Pierini, D. Arnaud, M. Zibett, S. D'Onghia, E. TI Testing adiabatic contraction of dark matter in fossil group candidates SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: galaxies: clusters; galaxies: clusters: intracluster medium; galaxies: groups: general; dark matter ID INITIAL MASS FUNCTION; X-RAY-CLUSTERS; SURFACE-BRIGHTNESS PROFILES; RELAXED GALAXY CLUSTERS; TO-LIGHT RATIO; XMM-NEWTON; DENSITY PROFILE; REPRESENTATIVE SAMPLE; TEMPERATURE PROFILES; LUMINOSITY FUNCTION AB We present deep XMM-Newton observations and ESO WFI optical imaging of two X-ray-selected fossil group candidates, RXC J0216.7-4749 and RXC J2315.7-0222. Using the X-ray data, we derive total mass profiles under the hydrostatic equilibrium assumption. The central regions of RXC J0216.7-4749 are found to be dominated by an X-ray bright AGN, and although we derive a mass profile, uncertainties are large and the constraints are significantly weakened due to the presence of the central source. The total mass profile of RXC J2315.7-0222 is of high quality, being measured in fifteen bins from [0.075-0.75] R(500) and containing three data points interior to 30 kpc, allowing comprehensive investigation of its properties. We investigate several mass models based on the standard NFW profile or on the Sersic-like model recently suggested by high-resolution N-body simulations. We find that the addition of a stellar component due to the presence of the central galaxy is necessary for a good analytical model fit. In all mass profile models fitted, the mass concentration is not especially high compared to non-fossil systems. In addition, the modification of the dark matter halo by adiabatic contraction slightly improves the fit. However, our result depends critically on the choice of IMF used to convert galaxy luminosity to mass, which leads to a degeneracy between the central slope of the dark matter profile and the normalisation of the stellar component. While we argue on the basis of the range of M(*)/L(R) ratios that lower M(*)/L(R) ratios are preferred on physical grounds and that adiabatic contraction has thus operated in this system, better theoretical and observational convergence on this problem is needed to make further progess. C1 [Democles, J.] CEA Saclay, CNRS, CEA DSM, IRFU Serv Phys Particules, F-91191 Gif Sur Yvette, France. [Pratt, G. W.; Arnaud, M.] Univ Paris Diderot, CEA Saclay, CNRS,CEA DSM, IRFU Serv Phys Particules,Lab AIM, F-91191 Gif Sur Yvette, France. [Pierini, D.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Zibett, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [D'Onghia, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Democles, J (reprint author), CEA Saclay, CNRS, CEA DSM, IRFU Serv Phys Particules, Bat 141, F-91191 Gif Sur Yvette, France. EM jessica.democles@cea.fr FU ESA Member States; USA (NASA); IRAF at the National Optical Astronomy Observatories (NOAO) in Tucson, Arizona FX We thank R. Piffaretti for useful discussions, J. Thomas for help with deprojection of the stellar luminosity profile, H. Bohringer for help with the initial target selection, and the referee for a useful report. The present 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). IRAF is the Image Reduction and Analysis Facility, a general purpose software system for the reduction and analysis of astronomical data. IRAF is written and supported by the IRAF programming group at the National Optical Astronomy Observatories (NOAO) in Tucson, Arizona. NOAO is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under cooperative agreement with the National Science Foundation. NR 74 TC 11 Z9 11 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 JUL PY 2010 VL 517 AR A52 DI 10.1051/0004-6361/201014328 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400062 ER PT J AU Lewis, F Russell, DM Jonker, PG Linares, M Tudose, V Roche, P Clark, JS Torres, MAP Maitra, D Bassa, CG Steeghs, D Patruno, A Migliari, S Wijnands, R Nelemans, G Kewley, LJ Stroud, VE Modjaz, M Bloom, JS Blake, CH Starr, D AF Lewis, F. Russell, D. M. Jonker, P. G. Linares, M. Tudose, V. Roche, P. Clark, J. S. Torres, M. A. P. Maitra, D. Bassa, C. G. Steeghs, D. Patruno, A. Migliari, S. Wijnands, R. Nelemans, G. Kewley, L. J. Stroud, V. E. Modjaz, M. Bloom, J. S. Blake, C. H. Starr, D. TI The double-peaked 2008 outburst of the accreting milli-second X-ray pulsar, IGR J00291+5934 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE pulsars: general; X-rays: binaries; stars: neutron; accretion, accretion disks ID MILLISECOND PULSAR; OPTICAL COUNTERPART; SAX J1808.4-3658; XTE J1118+480; BLACK-HOLES; BINARY; RADIO; JETS; DISC; MASS AB Context. In August 2008, the accreting milli-second X-ray pulsar (AMXP), IGR J00291+5934, underwent an outburst lasting similar to 100 days, the first since its discovery in 2004. Aims. We present data from the 2008 double-peaked outburst of IGR J00291+5934 from Faulkes Telescope North, the Isaac Newton Telescope, the Keck Telescope, PAIRITEL, the Westerbork Synthesis Radio Telescope and the Swift, XMM-Newton and RXTE X-ray missions. We study the outburst's evolution at various wavelengths, allowing us to probe accretion physics in this AMXP. Methods. We study the light curve morphology, presenting the first radio-X-ray spectral energy Distributions (SEDs) for this source and the most detailed UV-IR SEDs for any outbursting AMXP. We show simple models that attempt to identify the emission mechanisms responsible for the SEDs. We analyse short-timescale optical variability, and compare a medium resolution optical spectrum with those from 2004. Results. The outburst morphology is unusual for an AMXP, comprising two peaks, the second containing a "plateau" of similar to 10 days at maximum brightness within 30 days of the initial activity. This has implications on duty cycles of short-period X-ray transients. The X-ray spectrum can be fitted by a single, hard power-law. We detect optical variability of similar to 0.05 mag, on timescales of minutes, but find no periodic modulation. In the optical, the SEDs contain a blue component, indicative of an irradiated disc, and a transient near-infrared (NIR) excess. This excess is consistent with a simple model of an optically thick synchrotron jet (as seen in other outbursting AMXPs), however we discuss other potential origins. The optical spectrum shows a double-peaked Ha profile, a diagnostic of an accretion disc, but we do not clearly see other lines (e.g. He I, II) that were reported in 2004. Conclusions. Optical/IR observations of AMXPs appear to be excellent for studying the evolution of both the outer accretion disc and the inner jet, and may eventually provide us with tight constraints to model disc-jet coupling in accreting neutron stars. C1 [Lewis, F.; Roche, P.; Stroud, V. E.] Cardiff Univ, Sch Phys & Astron, Faulkes Telescope Project, Cardiff CF24 3AA, S Glam, Wales. [Lewis, F.; Roche, P.; Clark, J. S.; Stroud, V. E.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Lewis, F.; Roche, P.; Stroud, V. E.] Univ Glamorgan, Div Earth Space & Environm, Pontypridd CF37 1DL, M Glam, Wales. [Russell, D. M.; Linares, M.; Maitra, D.; Patruno, A.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Jonker, P. G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Torres, M. A. P.; Steeghs, D.; Blake, C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, P. G.; Nelemans, G.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 ED Nijmegen, Netherlands. [Linares, M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Tudose, V.] Netherlands Inst Radio Astron, NL-7991 PD Dwingeloo, Netherlands. [Tudose, V.] Acad Romana, Astron Inst, RO-040557 Bucharest, Romania. [Tudose, V.] Res Ctr Atom Phys & Astrophys, RO-077125 Bucharest, Romania. [Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bassa, C. G.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Steeghs, D.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Migliari, S.] ESAC, Madrid 28080, Spain. [Kewley, L. J.] Univ Hawaii, Honolulu, HI 96822 USA. [Modjaz, M.; Bloom, J. S.; Starr, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Starr, D.] Global Telescope Project, Las Cumbres Observ, Santa Barbara, CA 93117 USA. RP Lewis, F (reprint author), Cardiff Univ, Sch Phys & Astron, Faulkes Telescope Project, 5 Parade, Cardiff CF24 3AA, S Glam, Wales. EM fraser.lewis@faulkes-telescope.com RI Tudose, Valeriu/F-8976-2010; Nelemans, Gijs/D-3177-2012; Steeghs, Danny/C-5468-2009 OI Nelemans, Gijs/0000-0002-0752-2974; Steeghs, Danny/0000-0003-0771-4746 FU Dill Faulkes Educational Trust; Netherlands Organization for Scientific Research (NWO); Netherlands Foundation for Scientific Research (NWO); Netherlands Organisation for Scientific Research; STFC; Harvard University; University of Virginia FX F.L. would like to acknowledge support from the Dill Faulkes Educational Trust. D.M.R. and A.P. acknowledge support from a Netherlands Organization for Scientific Research (NWO) VENI Fellowship. The Faulkes Telescope Project is an educational and research arm of the Las Cumbres Observatory Global Telescope (LCOGT). RXTE/ASM results are provided by the RXTE/ASM teams at MIT and at the RXTE SOF and GOF at NASA's GSFC. The Westerbork Synthesis Radio Telescope is operated by the ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands Foundation for Scientific Research (NWO). P.G.J. acknowledges support from a VIDI grant from the Netherlands Organisation for Scientific Research. D.S. acknowledges a STFC Advanced Fellowship. The Peters Automated Infrared Imaging Telescope (PAIRITEL) is operated by the Smithsonian Astrophysical Observatory (SAO) and was made possible by a grant from the Harvard University Milton Fund, the camera loan from the University of Virginia, and the continued support of the SAO and UC Berkeley. We thank the staff and students of Paulet High School (Burton-on-Trent, England), The Kingsley School (Leamington Spa, England), Czacki High School (Warsaw, Poland), St. Brigid's School (Denbigh, Wales) and St David's Catholic College (Cardiff, Wales) for contributing to the Faulkes LMXB Observing Program and Schools' Initiative (FLOPSI) and Alison Tripp for scheduling these observations. We thank the anonymous referee for their comments and swift reply. NR 79 TC 10 Z9 10 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2010 VL 517 AR A72 DI 10.1051/0004-6361/201014382 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400082 ER PT J AU Macario, G Venturi, T Brunetti, G Dallacasa, D Giacintucci, S Cassano, R Bardelli, S Athreya, R AF Macario, G. Venturi, T. Brunetti, G. Dallacasa, D. Giacintucci, S. Cassano, R. Bardelli, S. Athreya, R. TI The very steep spectrum radio halo in Abell 697 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE radiation mechanism: non-thermal; galaxies: clusters: general; galaxies: clusters: individual: Abell 697 ID NORTHERN SKY SURVEY; X-RAY-EMISSION; GALAXY CLUSTERS; RELIC CANDIDATES; MAGNETIC-FIELD; LOW-FREQUENCY; COMA CLUSTER; COSMIC-RAYS; ELECTRONS; SAMPLE AB Aims. We present a detailed study of the giant radio halo in the galaxy cluster Abell 697 to constrain its origin and connection with the cluster dynamics. Methods. We performed high sensitivity GMRT observations at 325 MHz, which showed that the radio halo is much brighter and larger at this frequency than in previous 610 MHz observations. To derive the integrated spectrum in the frequency range 325 MHz-1.4 GHz, we reanalysed archival VLA data at 1.4 GHz and used proprietary GMRT data at 610 MHz. Results. Our multifrequency analysis shows that the total radio spectrum of the giant radio halo in A697 is very steep, with alpha(1.4GHz)(325MHz) approximate to 1.7-1.8. Owing to energy arguments, a hadronic origin of the halo is disfavoured by this steep spectrum. Very steep spectrum halos in merging clusters are predicted in the case that the emitting electrons are accelerated by turbulence. Observations with upcoming low frequency arrays will be able to test these expectations. C1 [Macario, G.; Venturi, T.; Brunetti, G.; Dallacasa, D.; Giacintucci, S.; Cassano, R.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Macario, G.; Dallacasa, D.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Giacintucci, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bardelli, S.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Athreya, R.] Indian Inst Sci Educ & Res, Pune 411021, Maharashtra, India. RP Macario, G (reprint author), INAF Ist Radioastron, Via Gobetti 101, I-40129 Bologna, Italy. EM tventuri@ira.inaf.it RI Bardelli, Sandro/O-9369-2015; OI Bardelli, Sandro/0000-0002-8900-0298; Brunetti, Gianfranco/0000-0003-4195-8613; Cassano, Rossella/0000-0003-4046-0637; Venturi, Tiziana/0000-0002-8476-6307 FU INAF; ASI [ASI-INAF I/088/06/0]; National Aeronautics and Space Administration FX We thank the staff of the GMRT for their help during the observations. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. This research is partially funded by INAF and ASI through grants PRIN-INAF 2007, PRIN-INAF 2008 and ASI-INAF I/088/06/0. 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 27 Z9 27 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 JUL PY 2010 VL 517 AR A43 DI 10.1051/0004-6361/201014109 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400053 ER PT J AU Maiolino, R Risaliti, G Salvati, M Pietrini, P Torricelli-Ciamponi, G Elvis, M Fabbiano, G Braito, V Reeves, J AF Maiolino, R. Risaliti, G. Salvati, M. Pietrini, P. Torricelli-Ciamponi, G. Elvis, M. Fabbiano, G. Braito, V. Reeves, J. TI "Comets" orbiting a black hole SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: Seyfert; galaxies: nuclei; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; EMISSION-LINE REGIONS; XMM-NEWTON LONG; X-RAY-EMISSION; NGC 1365; NUMERICAL SIMULATIONS; ABSORPTION-LINES; BLOATED STARS; MASS-LOSS; ABSORBER AB We use a long (300 ks), continuous Suzaku X-ray observation of the active nucleus in NGC 1365 to investigate the structure of the circumnuclear broad line region (BLR) clouds through their occultation of the X-ray source. The variations of the absorbing column density and of the covering factor indicate that the clouds surrounding the black hole are far from having a spherical geometry (as sometimes assumed), instead they have a strongly elongated and cometary shape, with a dense head (n similar to 10(11) cm(-3)) and an expanding, dissolving tail. We infer that the cometary tails must be longer than a few times 10(13) cm and their opening angle must be smaller than a few degrees. We suggest that the cometary shape may be a common feature of BLR clouds in general, but which has been difficult to recognize observationally so far. The cometary shape may originate from shocks and hydrodynamical instabilities generated by the supersonic motion of the BLR clouds into the intracloud medium. As a consequence of the mass loss into their tail, we infer that the BLR clouds probably have a lifetime of only a few months, implying that they must be continuously replenished. We also find a large, puzzling discrepancy (two orders of magnitude) between the mass of the BLR inferred from the properties of the absorbing clouds and the mass of the BLR inferred from photoionization models; we discuss the possible solutions to this discrepancy. C1 [Maiolino, R.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Risaliti, G.; Salvati, M.; Torricelli-Ciamponi, G.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.; Elvis, M.; Fabbiano, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pietrini, P.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. [Braito, V.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Braito, V.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Reeves, J.] Keele Univ, Sch Phys & Geog Sci, Astrophys Grp, Keele ST5 5BG, Staffs, England. RP Maiolino, R (reprint author), Osserv Astron Roma, INAF, Via Frascati 33, I-00040 Monte Porzio Catone, Italy. EM maiolino@oa-roma.inaf.it RI XRAY, SUZAKU/A-1808-2009; OI Risaliti, Guido/0000-0002-3556-977X; Braito, Valentina/0000-0002-2629-4989 FU INAF; ASI FX We are grateful to A. Marconi and to C. Perola for useful discussions. This work was partially supported by INAF and by ASI. NR 49 TC 58 Z9 58 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2010 VL 517 AR A47 DI 10.1051/0004-6361/200913985 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400057 ER PT J AU Parenti, S Reale, F Reeves, KK AF Parenti, S. Reale, F. Reeves, K. K. TI Post-flare evolution of AR 10923 with Hinode/XRT SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: activity; Sun: flares; Sun: corona; Sun: X-rays, gamma rays ID CORONAL ACTIVE-REGION; RAY TELESCOPE; SOLAR-FLARES; EMISSION AB Context. Flares are dynamic events which involve rapid changes in coronal magnetic topology end energy release. Even if they may be localized phenomena, the magnetic disturbance at their origin may propagate and be effective in a larger part of the active region. Aims. We investigate the temporal evolution of a flaring active region with respect to the loops morphology, the temperature, and emission measure distributions. Methods. We consider Hinode/XRT data of a the 2006 November 12th C1.1 flare. We inspect the evolution of the morphology of the flaring region also with the aid of TRACE data. XRT filter ratios are used to derive temperature and emission measure maps and evolution. Results. The analyzed flare includes several brightenings. We identify a coherent sequence of tangled and relaxed loop structures before, during, and after the brightenings. Although the thermal information is incomplete because of pixel saturation at the flare peak, thermal maps show fine, evolving spatial structuring. Temperature and emission measure variations show up in great detail, and we are able to detect a secondary heating of larger loops close to the proper flaring region. Finally we estimate the amount of energy released in these flaring loops during the flare decay. C1 [Parenti, S.] Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. [Parenti, S.] Royal Observ Belgium, B-1180 Brussels, Belgium. [Reale, F.] Univ Palermo 1, Dip Sci Fis & Astron, I-90134 Palermo, Italy. [Reale, F.] Osservatorio Astron Palermo GS Vaiana, INAF, I-90134 Palermo, Italy. [Reeves, K. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Parenti, S (reprint author), Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. EM s.parenti@oma.be RI Reeves, Katharine/P-9163-2014; OI Reale, Fabio/0000-0002-1820-4824 FU Belgian Federal Science Policy Office; Italian Ministero dell'Universita e Ricerca; Agenzia Spaziale Italiana (ASI) [I/015/07/0, I/023/09/0]; NASA [NNM07AB07C] FX S. P. acknowledges the support from the Belgian Federal Science Policy Office through the ESA-PRODEX programme. F. R. acknowledges support from Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale Italiana (ASI), contracts I/015/07/0 and I/023/09/0. K. K. R. is supported by NASA contract NNM07AB07C to SAO. The authors acknowledge the anonymous referee for the useful suggestions on the manuscript. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). NR 16 TC 5 Z9 5 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2010 VL 517 AR A41 DI 10.1051/0004-6361/200913697 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400051 ER PT J AU Puga, E Marin-Franch, A Najarro, F Lenorzer, A Herrero, A Pulido, JAA Chavarria, LA Bik, A Figer, D Alegria, SR AF Puga, E. Marin-Franch, A. Najarro, F. Lenorzer, A. Herrero, A. Acosta Pulido, J. A. Chavarria, L. A. Bik, A. Figer, D. Ramirez Alegria, S. TI Near-infrared spectroscopy in NGC 7538 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: early-type; stars: formation; stars: pre-main sequence; infrared: stars ID YOUNG STELLAR OBJECTS; STAR-FORMING REGION; H-II REGIONS; MAIN-SEQUENCE EVOLUTION; K-BAND SPECTROSCOPY; HII-REGIONS; INTERSTELLAR EXTINCTION; MOLECULAR CLOUD; MILKY-WAY; NGC-7538 AB Aims. The characterisation of the stellar population in young high-mass star-forming regions allows fundamental cluster properties like distance and age to be constrained. These are essential when using high-mass clusters as probes for conducting Galactic studies. Methods. NGC 7538 is a star-forming region with an embedded stellar population unearthed only in the near-infrared (NIR). We present the first near-infrared spectro-photometric study of the candidate high-mass stellar content in NGC 7538. We obtained H and K spectra of 21 sources with both the multi-object and long-slit modes of LIRIS at the WHT, and complement these data with subarcsecond JHK(s) photometry of the region using the imaging mode of the same instrument. Results. We find a wide variety of objects within the studied stellar population of NGC 7538. Our results discriminate between a stellar population associated to the H II region, but not contained within its extent, and several pockets of more recent star formation. We report the detection of CO bandhead emission toward several sources, as well as other features indicative of a young stellar nature. We infer a spectro-photometric distance of 2.7 +/- 0.5 kpc, an age spread in the range 0.5-2.2 Myr and a total mass similar to 1.7 x 10(3) M(circle dot) for the older population. C1 [Puga, E.; Najarro, F.] CSIC, INTA, Ctr Astrobiol, Madrid 28850, Spain. [Marin-Franch, A.; Lenorzer, A.; Herrero, A.; Acosta Pulido, J. A.; Ramirez Alegria, S.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Chavarria, L. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bik, A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Figer, D.] Rochester Inst Technol, Rochester, NY 14623 USA. RP Puga, E (reprint author), CSIC, INTA, Ctr Astrobiol, Ctra Torrejon Ajalvir Km 4, Madrid 28850, Spain. EM elena@damir.iem.csic.es RI Najarro, Francisco/G-7288-2015 OI Najarro, Francisco/0000-0002-9124-0039 FU Spanish MICINN [CSD2006-00070]; National Aeronautics and Space Administration; National Science Foundation; [AYA2007-67456-C02/AYA2008-06166-C03] FX E.P is funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc). This work has been partly supported by grants AYA2007-67456-C02/AYA2008-06166-C03.; This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 46 TC 7 Z9 7 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 JUL PY 2010 VL 517 AR A2 DI 10.1051/0004-6361/200913294 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400012 ER PT J AU Sanna, A Moscadelli, L Cesaroni, R Tarchi, A Furuya, RS Goddi, C AF Sanna, A. Moscadelli, L. Cesaroni, R. Tarchi, A. Furuya, R. S. Goddi, C. TI VLBI study of maser kinematics in high-mass star-forming regions II. G23.01-0.41 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE masers; techniques: high angular resolution; ISM: kinematics and dynamics; stars: individual: G23.01-0.41; stars: formation ID LONGITUDE RANGE 3-DEGREES; YOUNG STELLAR OBJECTS; GHZ METHANOL MASERS; LINE OH MASERS; H2O MASERS; ANGULAR RESOLUTION; MAGNETIC-FIELDS; EMISSION; 60-DEGREES; SAMPLE AB Aims. We performed a detailed study of maser and radio continuum emission toward the high-mass star-forming region G23.01-0.41. This study aims at improving our knowledge of the high-mass star-forming process by comparing the gas kinematics near a newly born young stellar object (YSO), analyzed through high spatial resolution maser data, with the large-scale environment of its native hot molecular core (HMC), identified in previous interferometric observations of thermal continuum and molecular lines. Methods. Using the VLBA and the EVN arrays, we conducted phase-referenced observations of the three most powerful maser species in G23.01-0.41: H(2)O at 22.2 GHz (4 epochs), CH(3)OH at 6.7 GHz (3 epochs), and OH at 1.665 GHz (1 epoch). In addition, we performed high-resolution (>= 0 ''.1), high-sensitivity (<0.1 mJy) VLA observations of the radio continuum emission from the HMC at 1.3 and 3.6 cm. Results. We have detected H(2)O, CH(3)OH, and OH maser emission clustered within 2000 AU from the center of a flattened HMC, oriented SE-NW, from which emerges a massive (12)CO outflow, elongated NE-SW, extended up to the pc-scale. Although the three maser species show a clearly different spatial and velocity distribution and sample distinct environments around the massive YSO, the spatial symmetry and velocity field of each maser specie can be explained in terms of expansion from a common center, which possibly denotes the position of the YSO driving the maser motion. Water masers trace both a fast shock (up to 50 km s(-1)) closer to the YSO, powered by a wide-angle wind, and a slower (20 km s(-1)) bipolar jet, at the base of the large-scale outflow. Because the compact free-free emission is found offset from the putative location of the YSO along a direction consistent with that of the maser jet axis, we interpret the radio continuum in terms of a thermal jet. The velocity field of methanol masers can be explained in terms of a composition of slow (4 km s(-1) in amplitude) motions of radial expansion and rotation about an axis approximately parallel to the maser jet. Finally, the distribution of line-of-sight velocities of the hydroxyl masers suggests that they can trace gas less dense (n(H2) <= 10(6) cm(-3)) and more distant from the YSO than that traced by the water and methanol masers, which is expanding toward the observer. A few pairs of OH masers, with different circular polarization, are well aligned in position on the sky and we interpret them as Zeeman pairs. From Zeeman splitting, the derived typical values of the magnetic field are of a few mG. C1 [Sanna, A.] Univ Cagliari, Dipartimento Fis, I-09042 Cagliari, Italy. [Sanna, A.; Tarchi, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, CA, Italy. [Moscadelli, L.; Cesaroni, R.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Furuya, R. S.] Natl Astron Observ Japan, Hilo, HI 96720 USA. [Goddi, C.] European So Observ, D-85748 Garching, Germany. [Goddi, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sanna, A (reprint author), Univ Cagliari, Dipartimento Fis, SP Monserrato Sestu Km 0-7, I-09042 Cagliari, Italy. EM asanna@ca.astro.it OI Tarchi, Andrea/0000-0001-8540-3500; Moscadelli, Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103 FU Ministry of Education, Culture, Sports, Science and Technology of Japan [20740113] FX This work is partially supported by a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science and Technology of Japan (No. 20740113). NR 44 TC 29 Z9 29 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 JUL PY 2010 VL 517 AR A78 DI 10.1051/0004-6361/201014234 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400088 ER PT J AU Sanna, A Moscadelli, L Cesaroni, R Tarchi, A Furuya, RS Goddi, C AF Sanna, A. Moscadelli, L. Cesaroni, R. Tarchi, A. Furuya, R. S. Goddi, C. TI VLBI study of maser kinematics in high-mass star-forming regions SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE masers; techniques: high angular resolution; ISM: kinematics and dynamics; stars: formation; stars: individual: IRAS 18182-1433; stars: individual: G16.59-0.05 ID YOUNG STELLAR OBJECTS; GHZ METHANOL MASERS; PROTOSTELLAR OBJECTS; H2O MASERS; PROPER MOTIONS; OH MASERS; CIRCUMSTELLAR ENVIRONMENTS; TRIGONOMETRIC PARALLAXES; MOLECULAR OUTFLOWS; DUST CONTINUUM AB Aims. To study the high-mass star-forming process, we started a large project to unveil the gas kinematics close to young stellar objects (YSOs) through the Very Long Baseline Interferometry (VLBI) of maser associations. By comparing the high spatial resolution maser data that traces the inner kinematics of the (proto)stellar cocoon with interferometric thermal data that traces the large-scale environment of the hot molecular core (HMC) harboring the (proto) stars, we can investigate the nature and identify the sources of large-scale motions. The present paper focuses on the high-mass star-forming region G16.59-0.05. Methods. Using the VLBA and the EVN arrays, we conducted phase-referenced observations of the three most powerful maser species in G16.59-0.05: H(2)O at 22.2 GHz (4 epochs), CH(3)OH at 6.7 GHz (3 epochs), and OH at 1.665 GHz (1 epoch). In addition, we performed high-resolution (>= 0 ''.1), high-sensitivity (<0.1 mJy) VLA observations of the radio continuum emission from the star-forming region at 1.3 and 3.6 cm. Results. This is the first work to report accurate measurements of the relative proper motions of the 6.7 GHz CH(3)OH masers. The different spatial and 3-D velocity distributions clearly indicate that the 22 GHz water and 6.7 GHz methanol masers trace different kinematic environments. The bipolar distribution of 6.7 GHz maser line-of-sight velocities and the regular pattern of observed proper motions suggest that these masers are tracing rotation around a central mass of about 35 M(circle dot). The flattened spatial distribution of the 6.7 GHz masers, oriented NW-SE, suggests that they can originate in a disk/toroid rotating around the massive YSO that drives the (12)CO (2-1) outflow, oriented NE-SW, observed on an arcsec scale. The extended, radio continuum source observed close to the 6.7 GHz masers could be excited by a wide-angle wind emitted from the YSO associated with the methanol masers, and such a wind has proven to be energetic enough to drive the NE-SW (12)CO (2-1) outflow. The H(2)O masers are distributed across a region offset about 0 ''.5 to the NW of the CH(3)OH masers, in the same area as where the emission of high-density molecular tracers, typical of HMCs, was detected. We postulate that a distinct YSO, possibly in an earlier evolutionary phase than what excites the methanol masers, is responsible for the excitation of the water masers and the HMC molecular lines. C1 [Sanna, A.] Univ Cagliari, Dipartimento Fis, I-09042 Cagliari, Italy. [Sanna, A.; Tarchi, A.] Osservatorio Astron Cagliari, INAF, I-09012 Capoterra, CA, Italy. [Moscadelli, L.; Cesaroni, R.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Furuya, R. S.] Natl Astron Observ Japan, Hilo, HI 96720 USA. [Goddi, C.] European So Observ, D-85748 Garching, Germany. [Goddi, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Sanna, A (reprint author), Univ Cagliari, Dipartimento Fis, SP Monserrato Setsu Km 0-7, I-09042 Cagliari, Italy. EM asanna@ca.astro.it OI Moscadelli, Luca/0000-0002-8517-8881; Cesaroni, Riccardo/0000-0002-2430-5103 FU Ministry of Education, Culture, Sports, Science and Technology of Japan [20740113] FX This work is partially supported by a Grant-in-Aid from the Ministry of Education, Culture, Sports, Science and Technology of Japan (No. 20740113). NR 55 TC 27 Z9 27 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 JUL PY 2010 VL 517 AR A71 DI 10.1051/0004-6361/201014233 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 638WR UT WOS:000280929400081 ER PT J AU Hirano, N Ho, PPT Liu, SY Shang, H Lee, CF Bourke, TL AF Hirano, Naomi Ho, Paul P. T. Liu, Sheng-Yuan Shang, Hsien Lee, Chin-Fei Bourke, Tyler L. TI EXTREME ACTIVE MOLECULAR JETS IN L1448C SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (L1448C); ISM: jets and outflows; ISM: molecules; shock waves; stars: formation ID LOW-MASS PROTOSTARS; SPITZER C2D SURVEY; SIO LINE EMISSION; HIGH-VELOCITY SIO; YOUNG STARS; PROTOSTELLAR JET; SUBMILLIMETER ARRAY; BIPOLAR OUTFLOWS; NUMERICAL SIMULATIONS; INTERSTELLAR CLOUDS AB The protostellar jet driven by L1448C was observed in the SiO J = 8-7 and CO J = 3-2 lines, and 350 GHz dust continuum at similar to 1 '' resolution with the Submillimeter Array. A narrow jet from the northern source L1448C(N) was observed in the SiO and the high-velocity CO. The jet consists of a chain of emission knots with an inter-knot spacing of similar to 2 '' (500 AU) and a semi-periodic velocity variation. These knots are likely to be the internal bow shocks in the jet beam that were formed due to the periodic variation of the ejection velocity with a period of similar to 15-20 yr. The innermost pairs of knots, which are significant in the SiO map but barely seen in the CO, are located at similar to 1 '' ( 250 AU) from the central source, L1448C(N). Since the dynamical timescale for the innermost pair is only similar to 10 yr, SiO may have been formed in the protostellar wind through the gas-phase reaction, or formed on the dust grain and directly released into the gas phase by means of shocks. It is found that the jet is extremely active with a mechanical luminosity of similar to 7L(circle dot), which is comparable to the bolometric luminosity of the central source (7.5L(circle dot)). The mass accretion rate onto the protostar derived from the mass-loss rate is similar to 10(-5) M(circle dot) yr(-1). Such a high mass accretion rate suggests that the mass and the age of the central star are 0.03-0.09 M(circle dot) and (4-12)x10(3) yr, respectively, implying that the central star is in the very early stage of protostellar evolution. The low-velocity CO emission delineates two V-shaped shells with a common apex at L1448C(N). The kinematics of these shells are reproduced by the model of a wide-opening angle wind. The co-existence of the highly collimated jets and the wide-opening angle shells can be explained by the "unified X-wind model" in which highly collimated jet components correspond to the on-axis density enhancement of the wide-opening angle wind. The CO J = 3-2 map also revealed the second outflow driven by the southern source L1448C(S) located at similar to 8 ''.3 (2000 AU) from L1448C(N). Although L1448C(S) is brighter than L1448C(N) in the mid-IR bands, the momentum flux of the outflow from L1448C(S) is 2 or 3 orders of magnitude smaller than that of the L1448C(N) outflow. It is likely that the evolution of L1448C(S) has been strongly affected by the powerful outflow from L1448C(N). C1 [Hirano, Naomi; Ho, Paul P. T.; Liu, Sheng-Yuan; Shang, Hsien; Lee, Chin-Fei] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Ho, Paul P. T.; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hirano, N (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. EM hirano@asiaa.sinica.edu.tw FU NSC [96-2112-M-001-023] FX We thank all the SMA staff in Hawaii, Cambridge, and Taipei for their enthusiastic help during these observations. We also thank the anonymous referee for many helpful comments and suggestions. N.H. thanks M. Machida and S. Inutsuka for fruitful discussion. N.H. is supported by NSC grant 96-2112-M-001-023. NR 69 TC 44 Z9 44 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2010 VL 717 IS 1 BP 58 EP 73 DI 10.1088/0004-637X/717/1/58 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610YV UT WOS:000278777900004 ER PT J AU Zappacosta, L Nicastro, F Maiolino, R Tagliaferri, G Buote, DA Fang, T Humphrey, PJ Gastaldello, F AF Zappacosta, L. Nicastro, F. Maiolino, R. Tagliaferri, G. Buote, D. A. Fang, T. Humphrey, P. J. Gastaldello, F. TI STUDYING THE WHIM CONTENT OF LARGE-SCALE STRUCTURES ALONG THE LINE OF SIGHT TO H 2356-309 SO ASTROPHYSICAL JOURNAL LA English DT Article DE intergalactic medium; large-scale structure of universe ID HOT INTERGALACTIC MEDIUM; X-RAY-ABSORPTION; MISSING BARYONS; SCULPTOR WALL; DATA RELEASE; LOCAL GROUP; XMM-NEWTON; GALAXIES; FILAMENT; EMISSION AB We make use of a 500 ks Chandra HRC-S/LETG spectrum of the blazar H 2356-309, combined with a lower signal-to-noise ratio (S/N; 100 ks) pilot LETG spectrum of the same target, to search for the presence of warm-hot absorbing gas associated with two large-scale structures (LSSs) crossed by this sight line and to constrain its physical state and geometry. Strong (log N(O VII) >= 10(16) cm(-2)) O VII K alpha absorption associated with a third LSS crossed by this line of sight (the Sculptor Wall (SW)), at z = 0.03, has already been detected in a previous work. Here, we focus on two additional prominent filamentary LSSs along the same line of sight, one at z = 0.062 (the Pisces-Cetus Supercluster (PCS)) and another at z = 0.128 (the "Farther Sculptor Wall" (FSW)). The combined LETG spectrum has an S/N of similar to 11.6-12.6 per resolution element in the 20-25 angstrom and an average 3 sigma sensitivity to intervening O VII K alpha absorption line equivalent widths (EWs) of EW(O VII) greater than or similar to 14 m angstrom in the available redshift range (z < 0.165). No statistically significant (i.e., >= 3 sigma) individual absorption is detected from any of the strong He-or H-like transitions of C, O, and Ne (the most abundant metals in gas with solar-like composition) at the redshifts of the PCS and FSW structures and down to the EW thresholds mentioned above. However, we are still able to constrain the physical and geometrical parameters of the putative absorbing gas associated with these structures, by performing a joint spectral fit of various marginal detections and upper limits of the strongest expected lines with our self-consistent hybrid-ionization WHIM spectral model. At the redshift of the PCS, we identify a warm phase with log T = 5.35(-0.13)(+0.07) K and log N(H) = (19.1 +/- 0.2) cm(-2) possibly co-existing with a much hotter and statistically less significant phase with log T = 6.9(-0.8)(+0.1) K and log N(H) = 20.1(-1.7)(+0.3) cm(-2) (1 sigma errors). These two separate physical phases are identified through, and mainly constrained by, C V K alpha (warm phase) and O VIII K alpha (hot phase) absorption, with single line significances of 1.5 sigma each. For the second LSS, at z similar or equal to 0.128, only one hot component is hinted in the data, through O VIII K alpha (1.6 sigma) and Ne IX K alpha (1.2 sigma). For this system, we estimate log T = 6.6(-0.2)(+0.1) K and log N(H) = 19.8(-0.8)(+0.4) cm(-2). Our column density and temperature constraints on the warm-hot gaseous content of these two LSSs, combined with the measurements obtained for the hot gas permeating the SW, allow us to estimate the cumulative number density per unit redshifts of O VII WHIM absorbers at three different EW thresholds of 0.4 m angstrom, 7 m angstrom, and 25.8 m angstrom. This is consistent with expectations only at the very low end of EW thresholds, but exceeds predictions at 7 m angstrom and 25.8 m angstrom (by more than 2 sigma). We also estimate the cosmological mass density of the WHIM based on the four absorbers we tentatively detect along this line of sight, obtaining Omega(WHIM)(b) = (0.021(-0.018)(+0.031))(Z/Z(circle dot))(-1), consistent with the cosmological mass density of the intergalactic "missing baryons" only if we assume high metallicities (Z similar to Z(circle dot)). C1 [Zappacosta, L.; Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zappacosta, L.] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy. [Zappacosta, L.; Nicastro, F.; Maiolino, R.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Nicastro, F.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Tagliaferri, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Buote, D. A.; Fang, T.; Humphrey, P. J.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Gastaldello, F.] INAF IASF, I-20133 Milan, Italy. RP Zappacosta, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lzappacosta@cfa.harvard.edu RI Gastaldello, Fabio/N-4226-2015; OI Gastaldello, Fabio/0000-0002-9112-0184; Nicastro, Fabrizio/0000-0002-6896-1364; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU LTSA [NNG04GD49G]; ASI-AAE [I/088/06/0]; INAF; EU [FP7-REGPOT-2007-1, 206469]; National Aeronautics and Space Administration FX F.N. and L.Z. acknowledge support from the LTSA grant NNG04GD49G and the ASI-AAE grant I/088/06/0. L.Z. acknowledges support from an INAF-OATs fellowship granted on "Basic Research" funds. F.N. acknowledges support from FP7-REGPOT-2007-1 EU grant No. 206469.; 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 38 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2010 VL 717 IS 1 BP 74 EP 84 DI 10.1088/0004-637X/717/1/74 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610YV UT WOS:000278777900005 ER PT J AU Civano, F Elvis, M Lanzuisi, G Jahnke, K Zamorani, G Blecha, L Bongiorno, A Brusa, M Comastri, A Hao, H Leauthaud, A Loeb, A Mainieri, V Piconcelli, E Salvato, M Scoville, N Trump, J Vignali, C Aldcroft, T Bolzonella, M Bressert, E Finoguenov, A Fruscione, A Koekemoer, AM Cappelluti, N Fiore, F Giodini, S Gilli, R Impey, CD Lilly, SJ Lusso, E Puccetti, S Silverman, JD Aussel, H Capak, P Frayer, D Le Floch, E McCracken, HJ Sanders, DB Schiminovich, D Taniguchi, Y AF Civano, F. Elvis, M. Lanzuisi, G. Jahnke, K. Zamorani, G. Blecha, L. Bongiorno, A. Brusa, M. Comastri, A. Hao, H. Leauthaud, A. Loeb, A. Mainieri, V. Piconcelli, E. Salvato, M. Scoville, N. Trump, J. Vignali, C. Aldcroft, T. Bolzonella, M. Bressert, E. Finoguenov, A. Fruscione, A. Koekemoer, A. M. Cappelluti, N. Fiore, F. Giodini, S. Gilli, R. Impey, C. D. Lilly, S. J. Lusso, E. Puccetti, S. Silverman, J. D. Aussel, H. Capak, P. Frayer, D. Le Floch, E. McCracken, H. J. Sanders, D. B. Schiminovich, D. Taniguchi, Y. TI A RUNAWAY BLACK HOLE IN COSMOS: GRAVITATIONAL WAVE OR SLINGSHOT RECOIL? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: formation; galaxies: interactions; galaxies: nuclei; quasars: absorption lines ID ACTIVE GALACTIC NUCLEI; BROAD ABSORPTION-LINE; WIDE-FIELD SURVEY; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; EVOLUTION SURVEY COSMOS; QUASI-STELLAR OBJECTS; DOUBLE-PEAKED EMITTER; X-RAY-SPECTRA; PHOTON BUBBLES AB We present a detailed study of a peculiar source detected in the COSMOS survey at z = 0.359. Source CXOC J100043.1+020637, also known as CID-42, has two compact optical sources embedded in the same galaxy. The distance between the two, measured in the HST/ACS image, is 0 ''.495 +/- 0 ''.005 that, at the redshift of the source, corresponds to a projected separation of 2.46 +/- 0.02 kpc. A large (similar to 1200 km s(-1)) velocity offset between the narrow and broad components of H beta has been measured in three different optical spectra from the VLT/VIMOS and Magellan/IMACS instruments. CID-42 is also the only X-ray source in COSMOS, having in its X-ray spectra a strong redshifted broad absorption iron line and an iron emission line, drawing an inverted P-Cygni profile. The Chandra and XMM-Newton data show that the absorption line is variable in energy by Delta E = 500 eV over four years and that the absorber has to be highly ionized in order not to leave a signature in the soft X-ray spectrum. That these features-the morphology, the velocity offset, and the inverted P-Cygni profile-occur in the same source is unlikely to be a coincidence. We envisage two possible explanations, both exceptional, for this system: (1) a gravitational wave (GW) recoiling black hole (BH), caught 1-10 Myr after merging; or (2) a Type 1/Type 2 system in the same galaxy where the Type 1 is recoiling due to the slingshot effect produced by a triple BH system. The first possibility gives us a candidate GW recoiling BH with both spectroscopic and imaging signatures. In the second case, the X-ray absorption line can be explained as a BAL-like outflow from the foreground nucleus (a Type 2 AGN) at the rearer one (a Type 1 AGN), which illuminates the otherwise undetectable wind, giving us the first opportunity to show that fast winds are present in obscured active galactic nuclei (AGNs), and possibly universal in AGNs. C1 [Civano, F.; Elvis, M.; Lanzuisi, G.; Hao, H.; Aldcroft, T.; Bressert, E.; Fruscione, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lanzuisi, G.] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy. [Jahnke, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Zamorani, G.; Comastri, A.; Bolzonella, M.; Gilli, R.; Lusso, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Blecha, L.; Loeb, A.] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Bongiorno, A.; Brusa, M.; Finoguenov, A.; Cappelluti, N.; Giodini, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Leauthaud, A.] Univ Calif Berkeley, LBNL, Berkeley, CA 94720 USA. [Leauthaud, A.] Univ Calif Berkeley, BCCP, Berkeley, CA 94720 USA. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Piconcelli, E.; Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Salvato, M.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA. [Trump, J.; Impey, C. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Vignali, C.; Lusso, E.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Finoguenov, A.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Lilly, S. J.; Silverman, J. D.] Swiss Fed Inst Technol ETH Honggerberg, Inst Astron, CH-8093 Zurich, Switzerland. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Aussel, H.] Univ Paris 07, CNRS, AIM Unite Mixte Rech CEA, UMR 158, Paris, France. [Le Floch, E.; Sanders, D. B.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [McCracken, H. J.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Schiminovich, D.] Columbia Univ, Dept Astron, New York, NY 10027 USA. [Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. 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; Bolzonella, Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Bressert, Eli/0000-0002-6564-6182; Jahnke, Knud/0000-0003-3804-2137; Vignali, Cristian/0000-0002-8853-9611; Lanzuisi, Giorgio/0000-0001-9094-0984; Bolzonella, Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Cappelluti, Nico/0000-0002-1697-186X; piconcelli, enrico/0000-0001-9095-2782; Bongiorno, Angela/0000-0002-0101-6624; Puccetti, Simonetta/0000-0002-2734-7835; Zamorani, Giovanni/0000-0002-2318-301X; Koekemoer, Anton/0000-0002-6610-2048; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157 FU NASA [GO7-8136A, NAS8-39073]; German Science Foundation (DFG) [JA 1114/3-1]; ASI/INAF In Italy [I/023/05/0, I/024/05/0, I/088/06]; PRIN/MUR [2006-02-5203]; Bundesministerium fur Bildung und Forschung/Deutsches Zentrum fur Luft und Raumfahrt In Germany; Max Planck Society FX F. C. thanks E. Costantini, T. J. Cox, M. Dotti, L. Hernquist, and A. Sesana for useful discussion. The authors thank Chien Y. Peng for useful discussions about GALFIT. The authors thank the anonymous referee, whose critical analysis helped improve this paper, making it more interesting. This work was supported in part by NASA Chandra grant number GO7-8136A (F. C., M. E., and A. F.), NASA contract NAS8-39073 (Chandra X-ray Center). K. J. acknowledges support from the Emmy Noether Programme of the German Science Foundation (DFG) through grant number JA 1114/3-1. In Italy, this work is supported by ASI/INAF contracts I/023/05/0, I/024/05/0, and I/088/06, and by PRIN/MUR grant 2006-02-5203. In Germany, this project is supported by the Bundesministerium fur Bildung und Forschung/Deutsches Zentrum fur Luft und Raumfahrt and the Max Planck Society. NR 135 TC 60 Z9 60 U1 2 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 1 PY 2010 VL 717 IS 1 BP 209 EP 222 DI 10.1088/0004-637X/717/1/209 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610YV UT WOS:000278777900017 ER PT J AU Castro, D Slane, P AF Castro, Daniel Slane, Patrick TI FERMI LARGE AREA TELESCOPE OBSERVATIONS OF SUPERNOVA REMNANTS INTERACTING WITH MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: ISM; ISM: individual objects (G349.7+0.2, CTB 37A, 3C 391, G8.7-0.1); ISM: supernova remnants ID GAMMA-RAY EMISSION; GALACTIC COSMIC-RAYS; MHZ MASER EMISSION; HIGH-ENERGY; SHOCK ACCELERATION; RX J1713.7-3946; INNER GALAXY; 3C 391; ABSORPTION-MEASUREMENTS; NONTHERMAL EMISSION AB We report the detection of gamma-ray emission coincident with four supernova remnants (SNRs) using data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. G349.7+0.2, CTB 37A, 3C 391, and G8.7-0.1 are SNRs known to be interacting with molecular clouds, as evidenced by observations of hydroxyl (OH) maser emission at 1720 MHz in their directions. SNR shocks are expected to be sites of cosmic-ray acceleration, and clouds of dense material can provide effective targets for production of gamma-rays from pi(0) decay. The observations reveal unresolved sources in the direction of G349.7+0.2, CTB 37A, and 3C 391, and a possibly extended source coincident with G8.7-0.1, all with significance levels greater than 10 sigma. C1 [Castro, Daniel; Slane, Patrick] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Castro, Daniel] Univ Simon Bolivar, Dept Fis, Caracas 1080A, Venezuela. RP Castro, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS 8-03060]; Fermi [NNX09AT68G] FX The authors thank Yasunobu Uchiyama and Stefan Funk for their careful reviewof thiswork, and Don Ellison, Keith Bechtol, Joshua Lande, Andrei Bykov, Luke Drury, and Felix Aharonian for helpful discussions. This work was partially funded by NASA contract NAS 8-03060 and Fermi grant NNX09AT68G. P.O.S. acknowledges the KITP in Santa Barbara, where work on this project was begun while participating in a KITP program. NR 74 TC 72 Z9 72 U1 0 U2 1 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 1 PY 2010 VL 717 IS 1 BP 372 EP 378 DI 10.1088/0004-637X/717/1/372 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610YV UT WOS:000278777900033 ER PT J AU Espaillat, C D'Alessio, P Hernandez, J Nagel, E Luhman, KL Watson, DM Calvet, N Muzerolle, J McClure, M AF Espaillat, C. D'Alessio, P. Hernandez, J. Nagel, E. Luhman, K. L. Watson, D. M. Calvet, N. Muzerolle, J. McClure, M. TI UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; circumstellar matter; protoplanetary disks; stars: formation; stars: pre-main sequence ID T-TAURI STARS; MAIN-SEQUENCE EVOLUTION; INFRARED TELESCOPE FACILITY; SPITZER-SPACE-TELESCOPE; AURIGA MOLECULAR CLOUD; HERBIG AE/BE STARS; PROTOPLANETARY DISKS; TRANSITIONAL DISKS; ACCRETION DISKS; CIRCUMSTELLAR DISKS AB In the past few years, several disks with inner holes that are relatively empty of small dust grains have been detected and are known as transitional disks. Recently, Spitzer has identified a new class of "pre-transitional disks" with gaps based on near-infrared photometry and mid-infrared spectra; these objects have an optically thick inner disk separated from an optically thick outer disk by an optically thin disk gap. A near-infrared spectrum provided the first confirmation of a gap in the pre-transitional disk of LkCa 15 by verifying that the near-infrared excess emission in this object was due to an optically thick inner disk. Here, we investigate the difference between the nature of the inner regions of transitional and pre-transitional disks using the same veiling-based technique to extract the near-infrared excess emission above the stellar photosphere. However, in this work we use detailed disk models to fit the excess continua as opposed to the simple blackbody fits previously used. We show that the near-infrared excess emission of the previously identified pre-transitional disks of LkCa 15 and UX Tau A in the Taurus cloud as well as the newly identified pre-transitional disk of ROX 44 in Ophiuchus can be fit with an inner disk wall located at the dust destruction radius. We also present detailed modeling of the broadband spectral energy distributions of these objects, taking into account the effect of shadowing by the inner disk on the outer disk, but considering the finite size of the star, unlike other recent treatments. The near-infrared excess continua of these three pre-transitional disks, which can be explained by optically thick inner disks, are significantly different from that of the transitional disks of GM Aur, whose near-infrared excess continuum can be reproduced by emission from sub-micron-sized optically thin dust, and DM Tau, whose near-infrared spectrum is consistent with a disk hole that is relatively free of small dust. The structure of pre-transitional disks may be a sign of young planets forming in these disks and future studies of pre-transitional disks will provide constraints to aid in theoretical modeling of planet formation. C1 [Espaillat, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [D'Alessio, P.] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Hernandez, J.] CIDA, Merida 5101A, Venezuela. [Nagel, E.] Univ Guanajuato, Dept Astron, Guanajuato 36240, Gto, Mexico. [Luhman, K. L.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luhman, K. L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Watson, D. M.] Univ Rochester, Dept Phys & Astron, Rochester, NY 14627 USA. [Calvet, N.; McClure, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Muzerolle, J.] Space Telescope Inst, Baltimore, MD 21218 USA. RP Espaillat, C (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM cespaillat@cfa.harvard.edu; p.dalessio@crya.unam.mx; jesush@cida.ve; erick@astro.ugto.mx; kluhman@astro.psu.edu; dmw@pas.rochester.edu; ncalvet@umich.edu; muzerol@stsci.edu; melisma@umich.edu OI McClure, Melissa/0000-0003-1878-327X FU National Science Foundation [0901947, AST-0544588]; PAPIIT-DGAPA UNAM; Conacyt; NASA [NNX08AH94G]; National Aeronautics and Space Administration, Science Mission Directorate [NNX08AE38A] FX We thank the referee for useful comments. We thank Cesar Briceno and Scott Kenyon for kindly providing the FAST spectra used in this paper. We also thank Perry Berlind for performing the FAST observations. We thank Sean Andrews and David Wilner for useful discussions. The near-infrared spectra used in this paper were obtained using SpeX at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. C.E. was supported by the National Science Foundation under Award No. 0901947. P. D. acknowledges a grant from PAPIIT-DGAPA UNAM. E.N. thanks a postdoctoral fellowship from Conacyt. K.L. was supported by grant AST-0544588 from the National Science Foundation. N.C. acknowledges support from NASA Origins Grant NNX08AH94G. NR 108 TC 130 Z9 130 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 JUL 1 PY 2010 VL 717 IS 1 BP 441 EP 457 DI 10.1088/0004-637X/717/1/441 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610YV UT WOS:000278777900039 ER PT J AU Hong, SA Rosenberg, JL Ashby, MLN Salzer, JJ AF Hong, Sukbum A. Rosenberg, Jessica L. Ashby, Matthew L. N. Salzer, John J. TI INFRARED PROPERTIES OF A COMPLETE SAMPLE OF STAR-FORMING DWARF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: fundamental parameters; galaxies: ISM; infrared: galaxies ID SPITZER-SPACE-TELESCOPE; INTERNATIONAL SPECTROSCOPIC SURVEY; LUMINOSITY-METALLICITY RELATIONS; DIGITAL SKY SURVEY; ARRAY CAMERA IRAC; WIDE-FIELD SURVEY; METAL ABUNDANCES; KISS GALAXIES; IRREGULAR GALAXIES; OXYGEN ABUNDANCES AB We present a study of a large, statistically complete sample of star-forming dwarf galaxies using mid-infrared observations from the Spitzer Space Telescope. The relationships between metallicity, star formation rate (SFR), and mid-infrared color in these systems show that the galaxies span a wide range of properties. However, the galaxies do show a deficit of 8.0 mu m polycyclic aromatic hydrocarbon emission as is apparent from the median 8.0 mu m luminosity which is only 0.004 L(8.0)(*) while the median B-band luminosity is 0.05 L(B)(*). Despite many of the galaxies being 8.0 mu m deficient, there is about a factor of 4 more extremely red galaxies in the [3.6]-[8.0] color than for a sample of normal galaxies with similar optical colors. We show correlations between the [3.6]-[8.0] color and luminosity, metallicity, and to a lesser extent SFRs that were not evident in the original, smaller sample studied previously. The luminosity-metallicity relation has a flatter slope for dwarf galaxies as has been indicated by previous work. We also show a relationship between the 8.0 mu m luminosity and the metallicity of the galaxy which is not expected given the competing effects (stellar mass, stellar population age, and the hardness of the radiation field) that influence the 8.0 mu m emission. This larger sample plus a well-defined selection function also allows us to compute the 8.0 mu m luminosity function and compare it with the one for the local galaxy population. Our results show that below 10(9) L(circle dot), nearly all the 8.0 mu m luminosity density of the local universe arises from dwarf galaxies that exhibit strong H alpha emission-i.e., 8.0 mu m and H alpha selection identify similar galaxy populations despite the deficit of 8.0 mu m emission observed in these dwarfs. C1 [Hong, Sukbum A.; Rosenberg, Jessica L.] George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. [Ashby, Matthew L. N.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Salzer, John J.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Hong, SA (reprint author), George Mason Univ, Dept Phys & Astron, Fairfax, VA 22030 USA. EM shongg@gmu.edu; jrosenb4@gmu.edu; mashby@cfa.harvard.edu; slaz@astro.indiana.edu FU NASA [1256790, 1407]; NSF [AST 9553020, AST 00-71114, AST 03-07766] 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 NASA contract 1407. Support for this work was provided by NASA through an IRAC GTO award issued by JPL/Caltech under contract 1256790. J.J.S. gratefully acknowledges support for the KISS project from the NSF through grants AST 9553020, AST 00-71114, and AST 03-07766. This work also made use of data products provided by the SDSS. 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 47 TC 2 Z9 2 U1 0 U2 1 PU 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 1 PY 2010 VL 717 IS 1 BP 503 EP 514 DI 10.1088/0004-637X/717/1/503 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610YV UT WOS:000278777900046 ER PT J AU Evans, IN Primini, FA Glotfelty, KJ Anderson, CS Bonaventura, NR Chen, JC Davis, JE Doe, SM Evans, JD Fabbiano, G Galle, EC Gibbs, DG Grier, JD Hain, RM Hall, DM Harbo, PN He, XQ Houck, JC Karovska, M Kashyap, VL Lauer, J McCollough, ML McDowell, JC Miller, JB Mitschang, AW Morgan, DL Mossman, AE Nichols, JS Nowak, MA Plummer, DA Refsdal, BL Rots, AH Siemiginowska, A Sundheim, BA Tibbetts, MS Van Stone, DW Winkelman, SL Zografou, P AF Evans, Ian N. Primini, Francis A. Glotfelty, Kenny J. Anderson, Craig S. Bonaventura, Nina R. Chen, Judy C. Davis, John E. Doe, Stephen M. Evans, Janet D. Fabbiano, Giuseppina Galle, Elizabeth C. Gibbs, Danny G., II Grier, John D. Hain, Roger M. Hall, Diane M. Harbo, Peter N. He, Xiangqun (Helen) Houck, John C. Karovska, Margarita Kashyap, Vinay L. Lauer, Jennifer McCollough, Michael L. McDowell, Jonathan C. Miller, Joseph B. Mitschang, Arik W. Morgan, Douglas L. Mossman, Amy E. Nichols, Joy S. Nowak, Michael A. Plummer, David A. Refsdal, Brian L. Rots, Arnold H. Siemiginowska, Aneta Sundheim, Beth A. Tibbetts, Michael S. Van Stone, David W. Winkelman, Sherry L. Zografou, Panagoula TI THE CHANDRA SOURCE CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; X-rays: general ID DEEP FIELD-SOUTH; X-RAY SOURCES; MEDIUM-SENSITIVITY SURVEY; CCD IMAGING SPECTROMETER; POINT-SOURCE CATALOGS; MS SOURCE CATALOGS; ALL-SKY SURVEY; MONITORING OBSERVATIONS; ENERGY-SPECTRA; UHURU CATALOG AB The Chandra Source Catalog (CSC) is a general purpose virtual X-ray astrophysics facility that provides access to a carefully selected set of generally useful quantities for individual X-ray sources, and is designed to satisfy the needs of a broad-based group of scientists, including those who may be less familiar with astronomical data analysis in the X-ray regime. The first release of the CSC includes information about 94,676 distinct X-ray sources detected in a subset of public Advanced CCD Imaging Spectrometer imaging observations from roughly the first eight years of the Chandra mission. This release of the catalog includes point and compact sources with observed spatial extents less than or similar to 30 ''. The catalog (1) provides access to the best estimates of the X-ray source properties for detected sources, with good scientific fidelity, and directly supports scientific analysis using the individual source data; (2) facilitates analysis of a wide range of statistical properties for classes of X-ray sources; and (3) provides efficient access to calibrated observational data and ancillary data products for individual X-ray sources, so that users can perform detailed further analysis using existing tools. The catalog includes real X-ray sources detected with flux estimates that are at least 3 times their estimated 1 sigma uncertainties in at least one energy band, while maintaining the number of spurious sources at a level of less than or similar to 1 false source per field for a 100 ks observation. For each detected source, the CSC provides commonly tabulated quantities, including source position, extent, multi-band fluxes, hardness ratios, and variability statistics, derived from the observations in which the source is detected. In addition to these traditional catalog elements, for each X-ray source the CSC includes an extensive set of file-based data products that can be manipulated interactively, including source images, event lists, light curves, and spectra from each observation in which a source is detected. C1 [Evans, Ian N.; Primini, Francis A.; Glotfelty, Kenny J.; Anderson, Craig S.; Bonaventura, Nina R.; Chen, Judy C.; Doe, Stephen M.; Evans, Janet D.; Fabbiano, Giuseppina; Galle, Elizabeth C.; Gibbs, Danny G., II; Grier, John D.; Hain, Roger M.; Harbo, Peter N.; He, Xiangqun (Helen); Karovska, Margarita; Kashyap, Vinay L.; Lauer, Jennifer; McCollough, Michael L.; McDowell, Jonathan C.; Miller, Joseph B.; Mitschang, Arik W.; Morgan, Douglas L.; Mossman, Amy E.; Nichols, Joy S.; Plummer, David A.; Refsdal, Brian L.; Rots, Arnold H.; Siemiginowska, Aneta; Sundheim, Beth A.; Tibbetts, Michael S.; Van Stone, David W.; Winkelman, Sherry L.; Zografou, Panagoula] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Davis, John E.; Houck, John C.; Nowak, Michael A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hall, Diane M.] Northrop Grumman, Cambridge, MA 02138 USA. RP Evans, IN (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM ievans@cfa.harvard.edu OI Rots, Arnold/0000-0003-2377-2356; Houck, John/0000-0002-6761-6796; Primini, Francis/0000-0002-6077-0643 FU Chandra X-ray Center; National Aeronautics and Space Administration through the Chandra X-ray Center FX The authors thank the Chandra Source Catalog project review visiting panel, who endorsed the catalog and proposed several key recommendations that have guided the development of the catalog. We acknowledge the support and guidance of the Chandra X-ray Center director, Harvey Tananbaum, and manager, Roger Brissenden.; Support for development of the Chandra Source Catalog is provided by the National Aeronautics and Space Administration through the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics and Space Administration under contract NAS 8-03060. NR 100 TC 165 Z9 165 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 JUL PY 2010 VL 189 IS 1 BP 37 EP 82 DI 10.1088/0067-0049/189/1/37 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 619AW UT WOS:000279400100003 ER PT J AU Horton, BM Holberton, RL AF Horton, Brent M. Holberton, Rebecca L. TI MORPH-SPECIFIC VARIATION IN BASELINE CORTICOSTERONE AND THE ADRENOCORTICAL RESPONSE IN BREEDING WHITE-THROATED SPARROWS (ZONOTRICHIA ALBICOLLIS) SO AUK LA English DT Article DE adrenocortical response; baseline corticosterone; parental care; stress; White-throated Sparrow; Zonotrichia albicollis ID LIFE-HISTORY STAGE; STRESS-RESPONSE; TRADE-OFFS; REPRODUCTIVE SUCCESS; SEASONAL-CHANGES; INDIVIDUAL RISK; PIED FLYCATCHER; HOUSE SPARROW; MODULATION; BEHAVIOR AB The adrenocortical response to perturbation varies considerably within and across avian species during breeding. Among the factors hypothesized to influence this variation is the degree of parental care expressed by an individual. To increase our understanding of the relationship between parental care and the adrenocortical response, we examined corticosterone secretion in the polymorphic White-throated Sparrow (Zonotrichia albicollis) during three breeding stages: prelaying, incubation, and nestling. In addition, we reevaluated previously described morph differences in parental behavior. Tan-striped males provisioned nestlings at higher rates than white-striped males, which is consistent with earlier findings. However, in contrast to previous studies, provisioning rates were similar between female morphs and higher than those exhibited by either male morph. We found that, in males, the more parental morph (tan-striped) expressed a reduced adrenocortical response during the nestling stage, but the less parental morph (white-striped) did not. Females of both morphs exhibited similar and reduced adrenocortical responses during parental stages. In addition, we observed morph differences in baseline corticosterone during the nestling stage: less parental birds (white-striped males) had higher baseline corticosterone levels than more parental birds (females and tan-striped males). These findings support the hypothesis that modulation of baseline corticosterone and the adrenocortical response during breeding is a function of the degree of parental care expressed by an individual. By influencing how parents balance self-maintenance and parental care on a daily basis, or in the face of perturbation, baseline corticosterone and the adrenocortical response may play a role in the alternative reproductive strategies of White-throated Sparrow morphs. Received 23 July 2009, accepted 9 March 2010. C1 [Horton, Brent M.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20003 USA. [Holberton, Rebecca L.] Univ Maine, Lab Avian Biol, Sch Biol & Ecol, Orono, ME 04469 USA. RP Horton, BM (reprint author), Natl Zool Pk, Smithsonian Migratory Bird Ctr, 3001 Connecticut Ave NW MRC 5503, Washington, DC 20003 USA. EM hortonb@si.edu FU Frank M. Chapman Memorial Fund; American Ornithologists' Union; Society for Integrative and Comparative Biology; Sandpiper Technologies; University of Maine's Association of Graduate Students; University of Maine's NSF [DGE-0231642]; University of Maine [A2002-04-05]; Maine Agricultural and Forest Experiment Station FX This research was funded by the Frank M. Chapman Memorial Fund, American Ornithologists' Union, Society for Integrative and Comparative Biology, Sandpiper Technologies, and the University of Maine's Association of Graduate Students (funds to B.M.H.). Additional support was provided by the Maine Agricultural and Forest Experiment Station (funds to R.L.H.). Stipends were provided to B.M.H. by the University of Maine's NSF GK-12 Teaching Fellows Program (DGE-0231642 to S. Brawley et al.) and a University of Maine Graduate Research Assistantship. All research was conducted at the Penobscot Experimental Forest, comanaged by the University of Maine and the U.S. Forest Service. The methods used in this study were approved by the University of Maine's Institutional Animal Care and Use Committee (protocol no. A2002-04-05) and were conducted under appropriate state and federal banding and scientific collection permits (to R.L.H.). Field assistance was provided by M. Bougie, K. Gensel, R. Graves, C. Howell, J. Johnston, J. Kelly, I. Liu, D. McLoughlin, H. McNutt, and H. Murray. Helpful comments on earlier versions of the manuscript were provided by F. Angelier, T. B. Ryder, and two anonymous reviewers. B.M.H. thanks his Ph.D. committee (R. Holberton, A. Dufty Jr., W. Glanz, W. Halteman, and P. Marra) for their guidance. NR 61 TC 12 Z9 12 U1 3 U2 15 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 JUL PY 2010 VL 127 IS 3 BP 540 EP 548 DI 10.1525/auk.2010.09096 PG 9 WC Ornithology SC Zoology GA 637ZM UT WOS:000280858300008 ER PT J AU Ramirez, SR Roubik, DW Skov, C Pierce, NE AF Ramirez, Santiago R. Roubik, David W. Skov, Charlotte Pierce, Naomi E. TI Phylogeny, diversification patterns and historical biogeography of euglossine orchid bees (Hymenoptera: Apidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Review DE Aglae; Amazon; Andes; DTT plots; Eulaema; Miocene; Oligocene; penalized likelihood; relaxed molecular clocks ID DIVERGENCE TIMES; SPECIES HYMENOPTERA; DOMINICAN AMBER; TAXONOMIC NOTES; EVOLUTION; FRAGRANCES; BIOLOGY; FOREST; ANDES; MORPHOLOGY AB The orchid bees constitute a clade of prominent insect pollinators distributed throughout the Neotropical region. Males of all species collect fragrances from natural sources, including flowers, decaying vegetation and fungi, and store them in specialized leg pockets to later expose during courtship display. In addition, orchid bees provide pollination services to a diverse array of Neotropical angiosperms when foraging for food and nesting materials. However, despite their ecological importance, little is known about the evolutionary history of orchid bees. Here, we present a comprehensive molecular phylogenetic analysis based on similar to 4.0 kb of DNA from four loci [cytochrome oxidase (CO1), elongation factor 1-alpha (EF1-alpha), arginine kinase (ArgK) and RNA polymerase II (Pol-II)] across the entire tribe Euglossini, including all five genera, eight subgenera and 126 of the approximately 200 known species. We investigated lineage diversification using fossil-calibrated molecular clocks and the evolution of morphological traits using disparity-through-time plots. In addition, we inferred past biogeographical events by implementing model-based likelihood methods. Our dataset supports a new view on generic relationships and indicates that the cleptoparasitic genus Exaerete is sister to the remaining orchid bee genera. Our divergence time estimates indicate that extant orchid bee lineages shared a most recent common ancestor at 27-42 Mya. In addition, our analysis of morphology shows that tongue length and body size experienced rapid disparity bursts that coincide with the origin of diverse genera (Euglossa and Eufriesea). Finally, our analysis of historical biogeography indicates that early diversification episodes shared a history on both sides of Mesoamerica, where orchid bees dispersed across the Caribbean, and through a Panamanian connection, thus reinforcing the hypothesis that recent geological events (e.g. the formation of the isthmus of Panama) contributed to the diversification of the rich Neotropical biota. (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 100, 552-572. C1 [Ramirez, Santiago R.; Pierce, Naomi E.] Harvard Univ, Museum Comparat Zool, Cambridge, MA 02138 USA. [Roubik, David W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Roubik, David W.] Unit 0948, APO, AA 34002 USA. [Skov, Charlotte] Rungsted Gymnasium, DK-2960 Rungsted Kyst, Denmark. RP Ramirez, SR (reprint author), Univ Calif Berkeley, 137 Mulford Hall,3114, Berkeley, CA 94720 USA. EM sramirez@post.harvard.edu RI Ramirez, Santiago/B-4948-2012 FU National Science Foundation [NSF-DDIG DEB-0608409, NSF DEB-0447242]; Department of Organismic and Evolutionary Biology (Harvard); Putnam Fund; Goelet Fund; David Rockefeller Center for Latin American Studies (Harvard); Society of Systematic Biologists; Fondo Colombia Biodiversa (FAAE); Danish Research Agency; Fulbright Commission; Organization for Tropical Studies (Emily Foster grant); University of Florida FX We thank numerous individuals and their respective institutions who provided invaluable assistance in the acquisition of specimens used in this study. We are particularly indebted to T. Arias, R. Ayala, J. Bermudez, S. Cappellari, T. Eltz, C. Garofalo, J. Gonzalez, A. Link, M. Lehnert, M. Lopez-Uribe, D. McKenna, C. Moreau, J. Neita, L. Packer, A. Parra, H. T. Quental, H. Ramirez, C. Rasmussen, D. Romo, A. Roncancio, T. Samper and C. Yurrita. Funding was provided to SRR and NEP by the National Science Foundation (NSF-DDIG DEB-0608409 and NSF DEB-0447242), and to SRR by the Department of Organismic and Evolutionary Biology (Harvard), the Putnam Fund and Goelet Fund (MCZ, Harvard), the David Rockefeller Center for Latin American Studies (Harvard), the Society of Systematic Biologists Awards for Graduate Student Research, and the Fondo Colombia Biodiversa (FAAE). CS received support from the Danish Research Agency, the Fulbright Commission, the Organization for Tropical Studies (Emily Foster grant), and the University of Florida. Samples were collected (and exported) under permit no. 550 from Colombia (Ministerio del Medio Ambiente), GGVS-309-2003 from Costa Rica (Ministerio de Recursos Naturales, Energia y Minas), AABSX1404311 from Mexico (SEMARNAT) and 005141 from Peru (AG-INRENA). We thank C. Hernandez for assistance with morphometric data. Beth Pringle, Benjamin Bembe, Thomas Eltz and two anonymous reviewers provided useful comments on earlier versions of the manuscript. NR 108 TC 53 Z9 55 U1 1 U2 60 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4066 EI 1095-8312 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD JUL PY 2010 VL 100 IS 3 BP 552 EP 572 PG 21 WC Evolutionary Biology SC Evolutionary Biology GA 619BH UT WOS:000279401800007 ER PT J AU Laurance, SGW Andrade, A Laurance, WF AF Laurance, Susan G. W. Andrade, Ana Laurance, William F. TI Unanticipated Effects of Stand Dynamism on Amazonian Tree Diversity SO BIOTROPICA LA English DT Article DE Amazon; Brazil; forest dynamics; rain forest trees; species richness; tree turnover rates ID TROPICAL RAIN-FORESTS; SPECIES RICHNESS; GLOBAL PATTERNS; DISTURBANCE; COMMUNITIES; TURNOVER; FRAGMENTATION; RECRUITMENT; DENSITY; MANAUS AB We assessed a general hypothesis of tropical tree diversity that predicts that species richness will be positively correlated with stand dynamism. Our analysis was based one of the largest and longest-running datasets on Amazonian trees (>= 10 cm diameter at breast height), with data collected over a 23-yr period within 66 1 ha plots spanning a large (1000 km2) landscape. Within these plots, maximum tree-species richness (329 species/ha) and Fisher's alpha values (227.5) were among the highest ever recorded. Contrary to the diversity-dynamism concept, tree species richness in our landscape was significantly and negatively associated with stand dynamism (measured as the mean rate of annual tree turnover). Because of this unexpected finding, we critically re-evaluated the relationship between stand dynamism and tree diversity across the Amazon basin and the tropics as a whole. With the inclusion of additional data we found that the relationship between stand dynamism and tree diversity becomes non-significant at larger spatial scales. C1 [Laurance, Susan G. W.; Laurance, William F.] James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. [Laurance, Susan G. W.; Laurance, William F.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Andrade, Ana] Natl Inst Amazonian Res INPA, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. RP Laurance, SGW (reprint author), James Cook Univ, Sch Marine & Trop Biol, Cairns, Qld 4878, Australia. EM susan.laurance@jcu.edu.au RI Laurance, Susan/G-6021-2011; Laurance, William/B-2709-2012 OI Laurance, Susan/0000-0002-2831-2933; FU U.S. National Science Foundation; Mellon Foundation; Blue Moon Fund; Marisla Foundation; Conservation, Food and Health Foundation; Smithsonian Institution FX We thank J. Rankin-Merona and the many botanists who assisted with plant identifications, and K. Harms, E. Leigh, M. Pena-Claros, N. Pitman, R. Valenica, and an anonymous referee for useful comments. The U.S. National Science Foundation, Mellon Foundation, Blue Moon Fund, Marisla Foundation, Conservation, Food and Health Foundation, and Smithsonian Institution provided support. This is publication number 542 in the BDFFP technical series. NR 41 TC 7 Z9 7 U1 0 U2 11 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUL PY 2010 VL 42 IS 4 BP 429 EP 434 DI 10.1111/j.1744-7429.2009.00611.x PG 6 WC Ecology SC Environmental Sciences & Ecology GA 619OG UT WOS:000279438900006 ER PT J AU Richardson, DJ Moser, WE Hammond, CI Shevchenko, AC Lazo-Wasem, E AF Richardson, Dennis J. Moser, William E. Hammond, Charlotte I. Shevchenko, Alexis C. Lazo-Wasem, Eric TI New Geographic Distribution Records and Host Specificity of Placobdella ali (Hirudinida: Glossiphoniidae) SO COMPARATIVE PARASITOLOGY LA English DT Article DE Placobdella ali; Glossiphoniidae; American snapping turtle; red-eared slider; southern painted turtle; Chelydra sperpentina; Chrysemys picta; Trachemys scripta elegans; Chrysemys dorsalis AB Placobdella ali Huges and Siddall, 2007 has not been reported since its original description based on 3 specimens from Silver Mine Lake in Orange County, New York. The finding of 3 populations of P. ali in Connecticut along with further collection of this species from its type locality facilitated an investigation of host use by this leech, molecular characterization of the species, and observations on its natural history. Placobdella ali commonly occurred on substrate in Silver Mine Lake in Orange County, New York, and Clark's Pond and North Farms Reservoir in New Haven County, Connecticut. A single specimen was found in Lake Wintergreen in New Haven County, Connecticut. Placobdella was represented by individuals of a light-colored form and a melanic or dark-colored form. Sequences of 2 mitochondrial genes, CO-I and ND-I, were virtually identical among individuals from Connecticut and New York populations, as well as between the 2 color morphs. Placobdella ali was collected from 10 of 15 (66.7%) American snapping turtles (Chelydra serpentina) in North Farms Reservoir. This observation in conjunction with the absence of P. ali on 55 eastern painted turtles (Chrysemys picta) suggests a fairly high degree of host specificity. Two species of exotic turtles, 3 red-eared sliders (Trachemys scripta elegans), and a single southern painted turtle (Chrysemys dorsalis), which is a state record for Connecticut, indicate the potential of introduction of exotic turtles as a vehicle for the introduction of exotic leeches. One of the 3 (33.3%) red-eared sliders was infested with a single individual of P. ali. C1 [Richardson, Dennis J.; Hammond, Charlotte I.; Shevchenko, Alexis C.] Quinnipiac Univ, Sch Biol Sci, Hamden, CT 06518 USA. [Moser, William E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. [Richardson, Dennis J.; Lazo-Wasem, Eric] Yale Univ, Peabody Museum Nat Hist, Div Invertebrate Zool, New Haven, CT 06520 USA. RP Richardson, DJ (reprint author), Quinnipiac Univ, Sch Biol Sci, 275 Mt Carmel Ave, Hamden, CT 06518 USA. EM Dennis.Richardson@quinnipiac.edu; moserw@si.edu; Charlotte.Hammond@quinnipiac.edu; eric.lazo-wasem@yale.edu FU Helminthological Society of Washington and Comparative Parasitology; Department of Biological Sciences; Schools of Arts and Sciences and Health Sciences at Quinnipiac University, Hamden, Connecticut FX Tamara J. Cook, managing editor, is acknowledged for assuming full editorial duties and discretion pertaining to this manuscript, thereby enabling Dennis J. Richardson to support the Helminthological Society of Washington and Comparative Parasitology. Kristen M. DeCesare and Kristen E. Richardson, Quinnipiac University, assisted in the field. Lourdes M. Rojas, Division of Invertebrate Zoology, Peabody Museum of Natural History, Yale University, provided valuable assistance in specimen management. The New York State Office of Parks, Recreation, and Historic Preservation provided permission to collect in Silver Mine Lake, and the State of Connecticut, Department of Environmental Protection, provided permission to collect leeches and trap turtles in Connecticut. Laurie Fortin, Wildlife Division, Connecticut Department of Environmental Protection provided assistance in placement of exotic turtles. Funding for this project was provided in part by the Department of Biological Sciences and Schools of Arts and Sciences and Health Sciences at Quinnipiac University, Hamden, Connecticut. NR 11 TC 19 Z9 21 U1 0 U2 7 PU HELMINTHOLOGICAL SOC WASHINGTON PI LAWRENCE PA C/O ALLEN PRESS INC, 1041 NEW HAMPSHIRE ST, ACCT# 141866, LAWRENCE, KS 66044 USA SN 1525-2647 J9 COMP PARASITOL JI Comp. Parasitol. PD JUL PY 2010 VL 77 IS 2 BP 202 EP 206 PG 5 WC Parasitology; Zoology SC Parasitology; Zoology GA 641NA UT WOS:000281132800011 ER PT J AU Hoos, PM Whitman Miller, A Ruiz, GM Vrijenhoek, RC Geller, JB AF Hoos, Phillip M. Whitman Miller, A. Ruiz, Gregory M. Vrijenhoek, Robert C. Geller, Jonathan B. TI Genetic and historical evidence disagree on likely sources of the Atlantic amethyst gem clam Gemma gemma (Totten, 1834) in California SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Gemma gemma; genetic variation; invasion source; marine biological invasion; oyster associate; phylogeography ID MITOCHONDRIAL-DNA; POPULATION BOTTLENECK; SPECIES INVASIONS; NEW-ZEALAND; DIVERSITY; COMMUNITY; INTRODUCTIONS; AMPLIFICATION; CONSEQUENCES; NUCLEAR AB Aim Historical information about source populations of invasive species is often limited; therefore, genetic analyses are used. We compared inference about source populations from historical and genetic data for the oyster-associated clam, Gemma gemma that invaded California from the USA Atlantic coast. Location Mid-Atlantic (North Carolina, Maryland), Northeastern (New Jersey, New York, Massachusetts) and the California coasts (Elkhorn Slough, San Francisco Bay, Bolinas Lagoon, Tomales Bay, Bodega Harbor). Methods The documented history of transplantation of Eastern oysters to California was reviewed. Cytochrome c oxidase subunit I (COI) sequences from recent and archived clams were examined in a haplotype network. We used AMOVA to detect geographic genetic structure and a permutation test for significant reductions in diversity. Results Chesapeake Bay oysters were transplanted to New York prior to shipment to San Francisco Bay and from there to peripheral bays. Gemma in the Northeastern and Mid-Atlantic regions were genetically differentiated. In California, populations in Bodega Harbor and Tomales Bay were genetically similar to those in the Mid-Atlantic area while clams in San Francisco Bay, Elkhorn Slough and Bolinas Lagoon resembled populations in the Northeastern region. In California, genetic variation was not highest in San Francisco Bay despite greater magnitude of oyster plantings. Haplotypes varied over time in native and introduced populations. Main Conclusions Historical records and inferences from genetics agree that both Northeastern and Mid-Atlantic regions were sources for Gemma in California. Only complex genetic hypotheses reconcile the strong segregation of haplotypes in California to the historical evidence of mixing in their proximate source (New York). These hypotheses include sorting of mixtures of haplotypes or selection in non-native areas. Haplotype turnover in San Francisco and Massachusetts samples over time suggests that the sorting hypothesis is plausible. We suggest, however, that Gemma was introduced independently and recently to Tomales Bay and Bodega Harbor. C1 [Hoos, Phillip M.; Geller, Jonathan B.] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Whitman Miller, A.; Ruiz, Gregory M.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Vrijenhoek, Robert C.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. RP Geller, JB (reprint author), Moss Landing Marine Labs, Pob 450, Moss Landing, CA 95039 USA. EM geller@mlml.calstate.edu OI Ruiz, Gregory/0000-0003-2499-441X NR 42 TC 20 Z9 22 U1 3 U2 22 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD JUL PY 2010 VL 16 IS 4 BP 582 EP 592 DI 10.1111/j.1472-4642.2010.00672.x PG 11 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 609HF UT WOS:000278646000007 ER PT J AU Schnitzer, SA Carson, WP AF Schnitzer, Stefan A. Carson, Walter P. TI Lianas suppress tree regeneration and diversity in treefall gaps SO ECOLOGY LETTERS LA English DT Letter DE Barro Colorado Nature Monument; diversity maintenance; gap-phase regeneration; lianas; Panama; treefall gaps; tropical forests ID BELOW-GROUND COMPETITION; TROPICAL MOIST FOREST; RAIN-FOREST; PHASE REGENERATION; SPECIES-DIVERSITY; SEEDLING ESTABLISHMENT; ABOVEGROUND BIOMASS; LIGHT ENVIRONMENTS; AMAZONIAN FOREST; COSTA-RICA AB P>Treefall gaps are hypothesized to maintain diversity by creating resource-rich, heterogeneous habitats necessary for species coexistence. This hypothesis, however, is not supported empirically for shade-tolerant trees, the dominant plant group in tropical forests. The failure of gaps to maintain shade-tolerant trees remains puzzling, and the hypothesis implicated to date is dispersal limitation. In central Panama, we tested an alternative 'biotic interference' hypothesis: that competition between growth forms (lianas vs. trees) constrains shade-tolerant tree recruitment, survival and diversity in gaps. We experimentally removed lianas from eight gaps and monitored them for 8 years, while also monitoring nine un-manipulated control gaps. Removing lianas increased tree growth, recruitment and richness by 55, 46 and 65%, respectively. Lianas were particularly harmful to shade-tolerant species, but not pioneers. Our findings demonstrate that competition between plant growth forms constrains diversity in a species-rich tropical forest. Because lianas are abundant in many tropical systems, our findings may apply broadly. C1 [Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. [Carson, Walter P.] Univ Pittsburgh, Dept Biol Sci, Pittsburgh, PA 15260 USA. RP Schnitzer, SA (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM Schnitzer@uwm.edu RI Carson, Walter/A-2569-2013; OI Schnitzer, Stefan/0000-0002-2715-9455 NR 52 TC 82 Z9 90 U1 7 U2 51 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD JUL PY 2010 VL 13 IS 7 BP 849 EP 857 DI 10.1111/j.1461-0248.2010.01480.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 611FU UT WOS:000278798100008 PM 20482581 ER PT J AU Launius, RD AF Launius, Roger D. TI writing the history of space's extreme environment SO ENVIRONMENTAL HISTORY LA English DT Editorial Material C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Launius, RD (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 17 TC 1 Z9 1 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1084-5453 EI 1930-8892 J9 ENVIRON HIST-US JI Environ. Hist. PD JUL PY 2010 VL 15 IS 3 BP 526 EP 532 DI 10.1093/envhis/emq053 PG 7 WC Environmental Studies; History SC Environmental Sciences & Ecology; History GA 807AT UT WOS:000293863300011 ER PT J AU Yi, CX Ricciuto, D Li, R Wolbeck, J Xu, XY Nilsson, M Aires, L Albertson, JD Ammann, C Arain, MA de Araujo, AC Aubinet, M Aurela, M Barcza, Z Barr, A Berbigier, P Beringer, J Bernhofer, C Black, AT Bolstad, PV Bosveld, FC Broadmeadow, MSJ Buchmann, N Burns, SP Cellier, P Chen, JM Chen, JQ Ciais, P Clement, R Cook, BD Curtis, PS Dail, DB Dellwik, E Delpierre, N Desai, AR Dore, S Dragoni, D Drake, BG Dufrene, E Dunn, A Elbers, J Eugster, W Falk, M Feigenwinter, C Flanagan, LB Foken, T Frank, J Fuhrer, J Gianelle, D Goldstein, A Goulden, M Granier, A Grunwald, T Gu, L Guo, HQ Hammerle, A Han, SJ Hanan, NP Haszpra, L Heinesch, B Helfter, C Hendriks, D Hutley, LB Ibrom, A Jacobs, C Johansson, T Jongen, M Katul, G Kiely, G Klumpp, K Knohl, A Kolb, T Kutsch, WL Lafleur, P Laurila, T Leuning, R Lindroth, A Liu, HP Loubet, B Manca, G Marek, M Margolis, HA Martin, TA Massman, WJ Matamala, R Matteucci, G McCaughey, H Merbold, L Meyers, T Migliavacca, M Miglietta, F Misson, L Moelder, M Moncrieff, J Monson, RK Montagnani, L Montes-Helu, M Moors, E Moureaux, C Mukelabai, MM Munger, JW Myklebust, M Nagy, Z Noormets, A Oechel, W Oren, R Pallardy, SG Kyaw, TPU Pereira, JS Pilegaard, K Pinter, K Pio, C Pita, G Powell, TL Rambal, S Randerson, JT von Randow, C Rebmann, C Rinne, J Rossi, F Roulet, N Ryel, RJ Sagerfors, J Saigusa, N Sanz, MJ Mugnozza, GS Schmid, HP Seufert, G Siqueira, M Soussana, JF Starr, G Sutton, MA Tenhunen, J Tuba, Z Tuovinen, JP Valentini, R Vogel, CS Wang, JX Wang, SQ Wang, WG Welp, LR Wen, XF Wharton, S Wilkinson, M Williams, CA Wohlfahrt, G Yamamoto, S Yu, GR Zampedri, R Zhao, B Zhao, XQ AF Yi, Chuixiang Ricciuto, Daniel Li, Runze Wolbeck, John Xu, Xiyan Nilsson, Mats Aires, Luis Albertson, John D. Ammann, Christof Arain, M. Altaf de Araujo, Alessandro C. Aubinet, Marc Aurela, Mika Barcza, Zoltan Barr, Alan Berbigier, Paul Beringer, Jason Bernhofer, Christian Black, Andrew T. Bolstad, Paul V. Bosveld, Fred C. Broadmeadow, Mark S. J. Buchmann, Nina Burns, Sean P. Cellier, Pierre Chen, Jingming Chen, Jiquan Ciais, Philippe Clement, Robert Cook, Bruce D. Curtis, Peter S. Dail, D. Bryan Dellwik, Ebba Delpierre, Nicolas Desai, Ankur R. Dore, Sabina Dragoni, Danilo Drake, Bert G. Dufrene, Eric Dunn, Allison Elbers, Jan Eugster, Werner Falk, Matthias Feigenwinter, Christian Flanagan, Lawrence B. Foken, Thomas Frank, John Fuhrer, Juerg Gianelle, Damiano Goldstein, Allen Goulden, Mike Granier, Andre Gruenwald, Thomas Gu, Lianhong Guo, Haiqiang Hammerle, Albin Han, Shijie Hanan, Niall P. Haszpra, Laszlo Heinesch, Bernard Helfter, Carole Hendriks, Dimmie Hutley, Lindsay B. Ibrom, Andreas Jacobs, Cor Johansson, Torbjoern Jongen, Marjan Katul, Gabriel Kiely, Gerard Klumpp, Katja Knohl, Alexander Kolb, Thomas Kutsch, Werner L. Lafleur, Peter Laurila, Tuomas Leuning, Ray Lindroth, Anders Liu, Heping Loubet, Benjamin Manca, Giovanni Marek, Michal Margolis, Hank A. Martin, Timothy A. Massman, William J. Matamala, Roser Matteucci, Giorgio McCaughey, Harry Merbold, Lutz Meyers, Tilden Migliavacca, Mirco Miglietta, Franco Misson, Laurent Moelder, Meelis Moncrieff, John Monson, Russell K. Montagnani, Leonardo Montes-Helu, Mario Moors, Eddy Moureaux, Christine Mukelabai, Mukufute M. Munger, J. William Myklebust, May Nagy, Zoltan Noormets, Asko Oechel, Walter Oren, Ram Pallardy, Stephen G. Kyaw, Tha Paw U. Pereira, Joao S. Pilegaard, Kim Pinter, Krisztina Pio, Casimiro Pita, Gabriel Powell, Thomas L. Rambal, Serge Randerson, James T. von Randow, Celso Rebmann, Corinna Rinne, Janne Rossi, Federica Roulet, Nigel Ryel, Ronald J. Sagerfors, Jorgen Saigusa, Nobuko Sanz, Maria Jose Mugnozza, Giuseppe-Scarascia Schmid, Hans Peter Seufert, Guenther Siqueira, Mario Soussana, Jean-Francois Starr, Gregory Sutton, Mark A. Tenhunen, John Tuba, Zoltan Tuovinen, Juha-Pekka Valentini, Riccardo Vogel, Christoph S. Wang, Jingxin Wang, Shaoqiang Wang, Weiguo Welp, Lisa R. Wen, Xuefa Wharton, Sonia Wilkinson, Matthew Williams, Christopher A. Wohlfahrt, Georg Yamamoto, Susumu Yu, Guirui Zampedri, Roberto Zhao, Bin Zhao, Xinquan TI Climate control of terrestrial carbon exchange across biomes and continents SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE NEE; climate control; terrestrial carbon sequestration; temperature; dryness; eddy flux; biomes; photosynthesis; respiration; global carbon cycle ID EDDY-COVARIANCE MEASUREMENTS; LONG-TERM; INTERANNUAL VARIABILITY; SPATIAL VARIABILITY; SOIL RESPIRATION; DECIDUOUS FOREST; WATER-VAPOR; FLUXES; DIOXIDE; UNCERTAINTY AB Understanding the relationships between climate and carbon exchange by terrestrial ecosystems is critical to predict future levels of atmospheric carbon dioxide because of the potential accelerating effects of positive climate-carbon cycle feedbacks. However, directly observed relationships between climate and terrestrial CO2 exchange with the atmosphere across biomes and continents are lacking. Here we present data describing the relationships between net ecosystem exchange of carbon (NEE) and climate factors as measured using the eddy covariance method at 125 unique sites in various ecosystems over six continents with a total of 559 site-years. We find that NEE observed at eddy covariance sites is (1) a strong function of mean annual temperature at mid-and high-latitudes, (2) a strong function of dryness at mid-and low-latitudes, and (3) a function of both temperature and dryness around the mid-latitudinal belt (45 degrees N). The sensitivity of NEE to mean annual temperature breaks down at similar to 16 degrees C (a threshold value of mean annual temperature), above which no further increase of CO2 uptake with temperature was observed and dryness influence overrules temperature influence. C1 [Yi, Chuixiang; Wolbeck, John; Xu, Xiyan] CUNY, Sch Earth & Environm Sci, Queens Coll, New York, NY 11367 USA. [Ricciuto, Daniel; Gu, Lianhong] Oak Ridge Natl Lab, Div Environm Sci, Oak Ridge, TN 37831 USA. [Li, Runze] Penn State Univ, Dept Stat, University Pk, PA 16802 USA. [Nilsson, Mats; Sagerfors, Jorgen] Swedish Univ Agr Sci, Dept Forest Ecol, SE-90183 Umea, Sweden. [Albertson, John D.] Duke Univ, Dept Civil & Environm Engn, Durham, NC 27708 USA. [Ammann, Christof; Fuhrer, Juerg] Fed Res Stn Agroscope Reckenholz Tanikon, CH-8046 Zurich, Switzerland. [Arain, M. Altaf] McMaster Univ, Sch Geog & Earth Sci, Hamilton, ON L8S 4K1, Canada. [de Araujo, Alessandro C.] Inst Nacl de Pesquisas da Amazonia, BR-69060 Manaus, Amazonas, Brazil. [Aubinet, Marc; Heinesch, Bernard; Moureaux, Christine] Univ Liege, Unit Biosyst Phys, B-5030 Gembloux, Belgium. [Laurila, Tuomas; Tuovinen, Juha-Pekka] Finnish Meteorol Inst, FI-00101 Helsinki, Finland. [Barcza, Zoltan] Eotvos Lorand Univ, Dept Meteorol, H-1117 Budapest, Hungary. [Barr, Alan] Environm Canada, Div Climate Res, Saskatoon, SK S7N 3H5, Canada. [Berbigier, Paul] EPHYSE, UR1263, INRA, F-33883 Villenave Dornon, France. [Beringer, Jason] Monash Univ, Sch Geog & Environm Sci, Clayton, Vic, Australia. [Bernhofer, Christian] Tech Univ Dresden, Inst Hydrol & Meteorol, D-01737 Tharandt, Germany. [Black, Andrew T.] Univ British Columbia, Vancouver, BC V6T 1Z4, Canada. [Bolstad, Paul V.] Univ Minnesota, St Paul, MN 55108 USA. [Bosveld, Fred C.] Royal Netherlands Meteorol Inst, NL-3730 AE De Bilt, Netherlands. [Broadmeadow, Mark S. J.; Wilkinson, Matthew] Alice Holt Lodge, Forest Res, Farnham GU10 4LH, Surrey, England. [Buchmann, Nina; Eugster, Werner; Knohl, Alexander] Inst Plant Sci, ETH, Zurich, Switzerland. [Burns, Sean P.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Cellier, Pierre; Loubet, Benjamin] UMR INRA INA PG, Environm & Arable Crops Unit, F-78850 Thiverval Grignon, France. [Chen, Jingming] Univ Toronto, Dept Geog, Toronto, ON M5S 3G3, Canada. [Chen, Jiquan] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA. 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[Granier, Andre] Ecol & Ecophysiol Forestier, INRA, UMR 1137, F-54280 Seichamps, France. [Gruenwald, Thomas] Tech Univ Dresden, Inst Hydrol & Meteorol, Dept Meteorol, D-01737 Dresden, Germany. [Guo, Haiqiang; Zhao, Bin] Fudan Univ, Inst Biodivers Sci, Minist Educ Key Lab Biodivers Sci & Ecol Engn, Shanghai 200433, Peoples R China. [Hammerle, Albin; Wohlfahrt, Georg] Univ Innsbruck, Inst Ecol, A-6020 Innsbruck, Austria. [Han, Shijie] Chinese Acad Sci, Inst Appl Ecol, Shenyang 110016, Peoples R China. [Hanan, Niall P.] Colorado State Univ, Nat Resource Ecol Lab, Ft Collins, CO 80523 USA. [Haszpra, Laszlo] Hungarian Meteorol Serv, H-1675 Budapest, Hungary. [Helfter, Carole] Ctr Ecol & Hydrol Edinburgh Bush Estate Penicuik, Penicuik EH26 0QB, Midlothian, Scotland. [Hendriks, Dimmie] Vrije Univ Amsterdam, Dept Hydrol & Geo Environm Sci, NL-1081 HV Amsterdam, Netherlands. [Hutley, Lindsay B.] Charles Darwin Univ, Sch Environm & Life Sci, Darwin, NT 0909, Australia. [Ibrom, Andreas; Pilegaard, Kim] Tech Univ Denmark, Biosyst Div, Riso Natl Lab Sustainable Energy, DK-4000 Roskilde, Denmark. [Johansson, Torbjoern; Lindroth, Anders; Moelder, Meelis] Lund Univ, Geobiosphere Sci Ctr, Phys Geog & Ecosyst Anal, SE-22362 Lund, Sweden. [Jongen, Marjan; Pereira, Joao S.] Univ Tecn Lisboa, Inst Super Agron, P-1349017 Lisbon, Portugal. [Katul, Gabriel] Duke Univ, Sch Environm, Durham, NC 27708 USA. [Kiely, Gerard] Univ Coll Cork, Dept Civil & Environm Engn, Cork, Ireland. [Klumpp, Katja; Soussana, Jean-Francois] Unit Agron, INRA, F-63000 Clermont Ferrand, France. [Klumpp, Katja; Soussana, Jean-Francois] Inst Agrarrelevante Klimaforsch, Johann Heinrich Thunen Inst vTI, D-38116 Braunschweig, Germany. [Lafleur, Peter; Rebmann, Corinna] Trent Univ, Dept Geog, Peterborough, ON K9J 7B8, Canada. [Leuning, Ray; Myklebust, May] CSIRO Marine & Atmospher Res, Canberra, ACT, Australia. [Liu, Heping] Jackson State Univ, Dept Phys Atmospher Sci & Geosci, Jackson, MS 39217 USA. [Manca, Giovanni] Inst Atmospher Pollut Consiglio Nazl Ric, Rende Div, I-87036 Arcavacata Di Rende, Italy. [Marek, Michal] Inst Syst Biol & Ecol, Div Ecosyst Processes Lab Plants Ecol Physiol, Ceske Budejovice 370050, Czech Republic. [Martin, Timothy A.] Univ Florida, Gainesville, FL 32611 USA. [Matamala, Roser] Argonne Natl Lab, Biosci Div, Argonne, IL 60439 USA. [Matteucci, Giorgio] Inst Agroenvironm & Forest Biol, Natl Res Council, I-00015 Monterotondo, RM, Italy. [McCaughey, Harry] Queens Univ, Dept Geog, Kingston, ON K7L 3N6, Canada. [Merbold, Lutz] Max Planck Inst Biogeochem, D-07745 Jena, Germany. [Meyers, Tilden] NOAA ATDD, Oak Ridge, TN 37831 USA. [Migliavacca, Mirco] Univ Milano Bicocca, Remote Sensing Environm Dynam Lab, DISAT, Milan, Italy. [Miglietta, Franco; Rossi, Federica] Ist Biometeorol, CNR, IBIMET, I-50145 Florence, Italy. [Misson, Laurent] CEFE, CNRS, F-34293 Montpellier 5, France. [Monson, Russell K.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80309 USA. [Montagnani, Leonardo] Serv Forestali, Agenzia Ambiente, I-39100 Bolzano, Italy. [Montagnani, Leonardo] Free Univ Bozen Bolzano, Fac Sci & Technol, I-39100 Bolzano, Italy. [Moors, Eddy] Alterra Green World Res, NL-6700 AA Wageningen, Netherlands. [Moureaux, Christine] Univ Liege, Unit Crops Management, B-5030 Gembloux, Belgium. [Mukelabai, Mukufute M.] Zambian Meteorol Dept, Mongu, Zambia. [Munger, J. William] Harvard Univ, Div Engn & Appl Sci, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Nagy, Zoltan; Pinter, Krisztina; Tuba, Zoltan] Agr Univ Godollo, Inst Bot & Ecophysiol, H-2103 Godollo, Hungary. [Noormets, Asko] N Carolina State Univ, Dept Forestry & Environm Resources, Raleigh, NC 27695 USA. [Oechel, Walter] San Diego State Univ, Dept Biol, San Diego, CA 92182 USA. [Oren, Ram; Siqueira, Mario] Duke Univ, Nicholas Sch Environm & Earth Sci, Durham, NC 27708 USA. [Pallardy, Stephen G.] Univ Missouri, Dept Forestry, Columbia, MO 65211 USA. [Pio, Casimiro] Univ Aveiro, Dept Environm, P-3810193 Aveiro, Portugal. [Pio, Casimiro] CESAM, P-3810193 Aveiro, Portugal. [Pita, Gabriel] Inst Super Tecn, Dept Mech Engn, P-1049001 Lisbon, Portugal. [Powell, Thomas L.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Rambal, Serge] UMR5175, CNRS, CEFE, DREAM, Montpellier 5, France. [von Randow, Celso] Natl Inst Space Res, Ctr Earth Syst Sci, BR-12630 Cachoeira Paulista, SP, Brazil. [Rinne, Janne] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland. [Ryel, Ronald J.] Utah State Univ, Dept Wildland Resources, Logan, UT 84322 USA. [Saigusa, Nobuko] Natl Inst Environm Studies, Ctr Global Environm Res, Tsukuba, Ibaraki 3058506, Japan. [Sanz, Maria Jose] Ctr Estud Ambient Mediterraneo, E-46980 Paterna, Spain. [Mugnozza, Giuseppe-Scarascia] Dept Agron Forestry & Land Use, Agr Res Council, I-00184 Rome, Italy. [Schmid, Hans Peter] Atmospher Environm Res Inst Meteorol, Garmisch Partenkirchen, Germany. [Schmid, Hans Peter] Climate Res Forschungszentrum Karlsruhe, Garmisch Partenkirchen, Germany. [Seufert, Guenther] Inst Environm & Sustainabil, Joint Res Ctr European Commiss, I-21020 Ispra, Italy. [Starr, Gregory] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Sutton, Mark A.] Atmospher Sci Ctr Ecol & Hydrol CEH, Penicuik EH26 0QB, Midlothian, Scotland. [Tenhunen, John] Univ Bayreuth, Dept Plant Ecol, D-95440 Bayreuth, Germany. [Valentini, Riccardo] Univ Tuscia, Dept Forest Environm & Resources, I-01100 Viterbo, Italy. [Vogel, Christoph S.] Univ Michigan Biol Stn, Pellston, MI 49769 USA. [Wang, Jingxin] Liaoning Normal Univ, Sch Math, Dalian 116039, Peoples R China. [Wang, Shaoqiang; Wen, Xuefa; Yu, Guirui] Chinese Acad Sci, Inst Geog Sci & Nat Resource Res, Beijing 100101, Peoples R China. [Wang, Weiguo] NOAA, IMSG Natl Ctr Environm Predict, Camp Springs, MD 20746 USA. [Welp, Lisa R.] Univ Calif, Geosci Res Div, Scripps Inst Oceanog, La Jolla, CA 92093 USA. [Wharton, Sonia] Lawrence Livermore Natl Lab, Atmospher Earth & Energy Div, Livermore, CA 94551 USA. [Williams, Christopher A.] Clark Univ, Grad Degree Program Geog, Worcester, MA 01610 USA. [Yamamoto, Susumu] Okayama Univ, Okayama 7008530, Japan. [Zhao, Xinquan] Chinese Acad Sci, NW Plateau Inst Biol, Xining 810001, Jiangxi, Peoples R China. RP Yi, CX (reprint author), CUNY, Sch Earth & Environm Sci, Queens Coll, New York, NY 11367 USA. RI Flanagan, Lawrence/B-1307-2013; Elbers, Jan/D-9477-2013; von Randow, Celso/B-3335-2009; Pilegaard, Kim/I-7137-2013; Kiely, Gerard/I-8158-2013; Cook, Bruce/M-4828-2013; Yi, Chuixiang/A-1388-2013; Zhao, Bin/I-3651-2013; 于, 贵瑞/C-1768-2014; Knohl, Alexander/F-9453-2014; Barcza, Zoltan/G-3880-2014; Garmisch-Pa, Ifu/H-9902-2014; Li, Runze/C-5444-2013; Goldstein, Allen/A-6857-2011; Feigenwinter, Christian/A-4606-2012; Valentini, Riccardo/D-1226-2010; Ibrom, Andreas/A-9850-2011; Leuning, Ray/A-2793-2008; Pio, Casimiro/A-8135-2008; Hutley, Lindsay/A-7925-2011; Zhao, Bin/E-5349-2010; Schmid, Hans Peter/I-1224-2012; Migliavacca, mirco/C-1260-2011; Moors, Eddy/J-5165-2012; Sutton, Mark/K-2700-2012; Wang, Weiguo/B-4948-2009; Goulden, Michael/B-9934-2008; Buchmann, Nina/E-6095-2011; Noormets, Asko/A-7257-2009; Katul, Gabriel/A-7210-2008; Helfter, Carole/A-1835-2010; Rinne, Janne/A-6302-2008; Oechel, Walter/F-9361-2010; Chen, Jiquan/D-1955-2009; Ryel, Ronald/A-3422-2008; Burns, Sean/A-9352-2008; Eugster, Werner/E-5116-2010; Miglietta, Franco/A-1257-2009; Feigenwinter, Christian/A-6151-2008; Powell, Thomas/F-9877-2016; Ricciuto, Daniel/I-3659-2016; Munger, J/H-4502-2013; Hammerle, Albin/N-4345-2016; Soussana, Jean-Francois/P-2094-2016; Gianelle, Damiano/G-9437-2011; Gu, Lianhong/H-8241-2014; Beringer, Jason/B-8528-2008; Soussana, Jean-Francois/E-2543-2012; Aurela, Mika/L-4724-2014; Lindroth, Anders/N-4697-2014; Wohlfahrt, Georg/D-2409-2009; Marek, Michal V./D-4383-2014; Merbold, Lutz/K-6103-2012; Desai, Ankur/A-5899-2008; Xu, Xiyan/D-2854-2015; Barr, Alan/H-9939-2014; Seufert, Gunther/J-9918-2013; Matteucci, Giorgio/N-3526-2015; Sanz Sanchez, Maria Jose/A-6099-2016; Meyers, Tilden/C-6633-2016; Montagnani, Leonardo/F-1837-2016 OI Aires, Luis Miguel Igreja/0000-0003-2052-6045; Kiely, Gerard/0000-0003-2189-6427; Ibrom, Andreas/0000-0002-1341-921X; Hanan, Niall/0000-0002-9130-5306; Goulden, Michael/0000-0002-9379-3948; Martin, Timothy/0000-0002-7872-4194; Foken, Thomas/0000-0003-4562-9083; Flanagan, Lawrence/0000-0003-1748-0306; Elbers, Jan/0000-0002-0631-3505; von Randow, Celso/0000-0003-1045-4316; Pilegaard, Kim/0000-0002-5169-5717; Cook, Bruce/0000-0002-8528-000X; Zhao, Bin/0000-0002-3530-2469; Knohl, Alexander/0000-0002-7615-8870; Barcza, Zoltan/0000-0002-1278-0636; Li, Runze/0000-0002-0154-2202; Goldstein, Allen/0000-0003-4014-4896; Valentini, Riccardo/0000-0002-6756-5634; Pio, Casimiro/0000-0002-3531-8620; Hutley, Lindsay/0000-0001-5533-9886; Schmid, Hans Peter/0000-0001-9076-4466; Moors, Eddy/0000-0003-2309-2887; Noormets, Asko/0000-0003-2221-2111; Katul, Gabriel/0000-0001-9768-3693; Rinne, Janne/0000-0003-1168-7138; Oechel, Walter/0000-0002-3504-026X; Burns, Sean/0000-0002-6258-1838; Eugster, Werner/0000-0001-6067-0741; Miglietta, Franco/0000-0003-1474-8143; Feigenwinter, Christian/0000-0003-2447-5492; Powell, Thomas/0000-0002-3516-7164; Ricciuto, Daniel/0000-0002-3668-3021; Munger, J/0000-0002-1042-8452; Hammerle, Albin/0000-0003-1963-5906; Soussana, Jean-Francois/0000-0002-1932-6583; Gianelle, Damiano/0000-0001-7697-5793; Gu, Lianhong/0000-0001-5756-8738; Beringer, Jason/0000-0002-4619-8361; Jongen, Marjan/0000-0003-1026-6622; Pita, Gabriel/0000-0002-2225-5309; Arain, M. Altaf/0000-0002-1433-5173; rambal, serge/0000-0001-5869-8382; Pereira, Joao/0000-0002-3658-5587; Lindroth, Anders/0000-0002-7669-784X; Wohlfahrt, Georg/0000-0003-3080-6702; Merbold, Lutz/0000-0003-4974-170X; Desai, Ankur/0000-0002-5226-6041; Xu, Xiyan/0000-0003-2732-1325; Seufert, Gunther/0000-0002-6019-6688; Matteucci, Giorgio/0000-0002-4790-9540; Sanz Sanchez, Maria Jose/0000-0003-0471-3094; Montagnani, Leonardo/0000-0003-2957-9071 FU National Science Foundation [NSF-DEB-0949637]; PSC-CUNY [62787-00 40]; CarboEuropeIP; FAO-GTOS-TCO; iLEAPS; Max Planck Institute for Biogeochemistry; University of Tuscia; US Department of Energy; AmeriFlux; Fluxnet-Canada; ChinaFlux; OzFlux; CarboAfrica; AsiaFlux; Department of Commerce (NOAA); Department of Agriculture (USDA/Forest Service); NASA; European Commission; Canadian Foundation for Climate and Atmospheric Sciences (CFCAS); Natural Sciences and Engineering Research Council (NSERC); BIOCAP Canada (Fluxnet-Canada only); Chinese Academy of Sciences; Ministry of Science and Technology; Australian Research Council; Ministry of Agriculture, Forest and Fisheries (MAFF); Ministry of Industrial Trade and Industry (MITI); Ministry of Education, Science, Sports and Culture (MESSC); Brazilian Ministry of Science and Technology (MCT); LBA FX This work was financially supported in part by the National Science Foundation (NSF-DEB-0949637) and the PSC-CUNY Faculty Research Award (Grant No 62787-00 40). This work was based on the database produced by the La Thuile FLUXNET project, which received financial support of CarboEuropeIP, FAO-GTOS-TCO, iLEAPS, Max Planck Institute for Biogeochemistry, National Science Foundation, University of Tuscia, US Department of Energy. We acknowledge database and technical support from Berkeley Water Center, Lawrence Berkeley National Laboratory, Microsoft Research eScience, Oak Ridge National Laboratory, University of California-Berkeley, University of Virginia. The following regional networks were involved with this work: AmeriFlux, CarboEuropeIP, Fluxnet-Canada, ChinaFlux, OzFlux, CarboAfrica, and AsiaFlux. AmeriFlux, is sponsored by the United States Departments of Energy (Terrestrial Carbon Program, National Institutes of Global Environmental Change (NIGEC), National Institute for Climate Change Research (NICCR)), Department of Commerce (NOAA), and Department of Agriculture (USDA/Forest Service), NASA, and the National Science Foundation. European sites in the NitroEurope, Euroflux and Medeflu projects are supported by the European Commission Directorate General XII Environment, Climate Program and the Program CONSOLIDER-INGENIO 2010 (GRACCIE). Canadian sites are sponsored by the Canadian Foundation for Climate and Atmospheric Sciences (CFCAS), the Natural Sciences and Engineering Research Council (NSERC), and BIOCAP Canada (Fluxnet-Canada only). Chinese sites are supported by the Chinese Academy of Sciences and the Ministry of Science and Technology. Australian sites are supported by the Australian Research Council. The Japanese site is supported by the Ministry of Agriculture, Forest and Fisheries (MAFF), the Ministry of Industrial Trade and Industry (MITI), and Ministry of Education, Science, Sports and Culture (MESSC). The Brazilian site is supported by the Brazilian Ministry of Science and Technology (MCT) and the LBA program. We thank the numerous scientists, students, and technicians responsible for the day-to-day gathering of the flux data, and the agency representatives who fund the respective projects. Without the dedicated efforts of so many individuals, this analysis would be impossible. NR 45 TC 56 Z9 58 U1 5 U2 132 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 1748-9326 J9 ENVIRON RES LETT JI Environ. Res. Lett. PD JUL-SEP PY 2010 VL 5 IS 3 AR 034007 DI 10.1088/1748-9326/5/3/034007 PG 10 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 655TX UT WOS:000282273700008 ER PT J AU Hirsch, BT AF Hirsch, Ben T. TI Tradeoff Between Travel Speed and Olfactory Food Detection in Ring-Tailed Coatis (Nasua nasua) SO ETHOLOGY LA English DT Article ID BROWN CAPUCHIN MONKEYS; INDIVIDUAL SPATIAL CHOICE; CEBUS-APELLA; PIGTAIL MACAQUES; SQUIRREL-MONKEYS; SEARCH IMAGES; ECOLOGICAL CONSEQUENCES; VIGILANCE BEHAVIOR; LIMITED ATTENTION; FORAGING GROUPS AB The distance at which an animal can detect food has important ramifications for foraging behavior. Although some studies have investigated the factors which affect visual food detection, very little is known about what influences olfactory food detection abilities in wild animals. The food discovery behavior of ring-tailed coatis (Nasua nasua) was studied using experimental fruit plots. Coatis primarily used olfaction to detect these new food sources, and visual food discovery appeared plausible in only five of 148 trials. Coatis detected the fruit from longer distances when traveling compared with when foraging for invertebrates in the leaf litter. Travel speed had a negative effect on discovery distance. Coatis traveling slowly detected the fruit plots from further away, which demonstrated a tradeoff between speed and food detection. If this tradeoff is biologically important, slower groups should have visited more fruit trees per day, so data taken during full-day coati group follows were analyzed to determine whether this pattern occurred. Slower moving groups visited more fruit trees than faster groups once confounding factors such as daily travel distance, group identity, group spread, and year were controlled for. These results are consistent with the hypothesis that coatis exhibit a speed-accuracy tradeoff for olfactory food detection. This tradeoff appears to be an important factor influencing the movement ecology of animal groups. C1 Smithsonian Trop Res Inst, Dpo Aa 34002, Panama. RP Hirsch, BT (reprint author), Smithsonian Trop Res Inst, Unit 9100,Box 0948, Dpo Aa 34002, Panama. EM hirschb@si.edu FU NSF [BCS-0314525] FX I would like to thank Yamil Di Blanco, Santiago Escobar, Carolina Ferrari, Mauro Tommone, and Fermino Silva for help and assistance during the course of the field work. I would also like to thank Viviana Munoz for her veterinary assistance. I am particularly grateful to Charles Janson for the immeasurable amount of advice he gave us during all aspects of this project, and letting me borrow several pieces of much needed field equipment. This paper has benefited tremendously thanks to comments on earlier drafts by Charles Janson, Meg Crofoot, Mario Di Bitetti, Matt Gompper, Andreas Koenig, and two anonymous reviewers. I thank the APN for permission to carry out work in Iguazu. This study complied with all institutional, national, and ASAB/ABS guidelines for animal welfare. This study was funded in part by a NSF grant (BCS-0314525). NR 55 TC 16 Z9 16 U1 4 U2 38 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0179-1613 J9 ETHOLOGY JI Ethology PD JUL PY 2010 VL 116 IS 7 BP 671 EP 679 DI 10.1111/j.1439-0310.2010.01783.x PG 9 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 607QE UT WOS:000278520600011 ER PT J AU Olsen, BJ Greenberg, R Liu, IA Felch, JM Walters, JR AF Olsen, Brian J. Greenberg, Russell Liu, Irene A. Felch, Joshua M. Walters, Jeffrey R. TI Interactions between sexual and natural selection on the evolution of a plumage badge SO EVOLUTIONARY ECOLOGY LA English DT Article DE Sexual dimorphism; Dichromatism; Melospiza georgiana nigrescens; Mating system; Speciation; Signals ID FEATHER-DEGRADING BACILLI; SWAMP SPARROW; GEOGRAPHIC-VARIATION; MATE CHOICE; FEMALE; MELANIN; DICHROMATISM; BIRDS; TESTOSTERONE; COLOR AB The evolutionary stability of signals varies due to interactions between sexual and natural selection. A tidal-marsh sparrow, Melospiza georgiana nigrescens, possesses darker pigmentation than an inland-marsh sparrow, M. g. georgiana. Studies of feather-degrading bacteria and convergent evolution among salt-marsh vertebrates suggest this dark coloration is due to environmental selection. Sexually dichromatic swamp sparrow crowns, however, may be additionally under sexual selection. We investigated ties between two plumage patches (rusty cap and black forehead) and two behaviors (male-male aggression and parental care) in the coastal and inland subspecies to test the effect of sexual versus natural selection on badge evolution. Across both subspecies the extent of rusty feathers in the cap patch was correlated positively with parental care and negatively with aggression, and the extent of black feathers in the forehead patch was correlated positively with aggression. Males with larger forehead patches produced more offspring along the coast, while males with larger cap patches did so inland. The date of the first nesting attempt for both subspecies correlated with cap patch extent, suggesting a similar role for female choice. Natural selection likely accounts for darker coastal females. Coastal male head color, however, is darker due to increased selection for larger forehead patches via intrasexual competition, yet it remains largely rusty due to female choice for larger cap patches. Increased sexual dichromatism among coastal plain swamp sparrows thus provides a clear example of the interplay between sexual and natural selection in subspecies divergence. C1 [Olsen, Brian J.] Univ Maine, Sch Biol & Ecol, Orono, ME 04469 USA. [Olsen, Brian J.; Greenberg, Russell] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Olsen, Brian J.; Walters, Jeffrey R.] Virginia Tech, Dept Biol Sci, Blacksburg, VA 24061 USA. [Liu, Irene A.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Felch, Joshua M.] Virginia Tech, Dept Fisheries & Wildlife Sci, Blacksburg, VA 24061 USA. RP Olsen, BJ (reprint author), Univ Maine, Sch Biol & Ecol, 5751 Murray Hall, Orono, ME 04469 USA. EM brian.olsen@maine.edu OI Olsen, Brian/0000-0001-5608-2779 FU Bailey Fund at Virginia Tech; Smithsonian Institution's Abbot Fund; Delaware Division of Fish and Wildlife; Maryland Ornithological Society; Washington Biologists' Field Club; Washington Group of the Explorer's Club; Eastern Bird Banding Association; Virginia Tech's Graduate Research Development Program; Smithsonian Institution FX We would like to thank the Delaware Division of Fish and Wildlife, H. Ternent of Lonaconing, Maryland, USA, the Western Maryland 4-H Education Center, and the Nature Conservancy for access to and use of our study sites. Funding was supplied by grants from the Bailey Fund at Virginia Tech, the Smithsonian Institution's Abbot Fund, the Delaware Division of Fish and Wildlife, the Maryland Ornithological Society, the Washington Biologists' Field Club, the Washington Group of the Explorer's Club, the Eastern Bird Banding Association, Virginia Tech's Graduate Research Development Program, and Smithsonian Institution Graduate and Pre-doctoral Fellowships. Many thanks to K. Kalasz, J. Wang, M. Powell, K. Murabito, J. Kolts, K. Callaway, A. Wessel, J. Adamson, B. Augustine, B. Beas, K. Heyden, and A. Roadman for assistance in the field and lab. Thanks to B. Ballentine for providing audio recordings of M. g. georgiana song. This research complied with state and federal law. Bird capture and handling were conducted under scientific collection permits from the states of Delaware and Maryland and federal banding permit number 22665. Impacts on animal welfare were approved by the Conservation and Research Center Institutional Animal Care and Use Committee of the Smithsonian National Zoological Park under proposal #04-10. NR 55 TC 11 Z9 12 U1 2 U2 48 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0269-7653 EI 1573-8477 J9 EVOL ECOL JI Evol. Ecol. PD JUL PY 2010 VL 24 IS 4 BP 731 EP 748 DI 10.1007/s10682-009-9330-4 PG 18 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 611PX UT WOS:000278833400007 ER PT J AU Munroe, TA Ross, SW AF Munroe, Thomas A. Ross, Steve W. TI Distribution and life history of two diminutive flatfishes, Citharichthys gymnorhinus and C. cornutus (Pleuronectiformes: Paralichthyidae), in the western North Atlantic SO FISHERY BULLETIN LA English DT Article ID STATES CONTINENTAL-SHELF; FISH ASSEMBLAGES; CLIMATE-CHANGE; LARVAL FISH; NEW-ENGLAND; CAROLINA; BOTHIDAE; COMMUNITY; RECORDS; WATERS AB Citharichthys cornutus and C. gymnorhinus, diminutive flatfishes inhabiting continental shelves in the western Atlantic Ocean, are infrequently reported and poorly known. We identified 594 C. cornutus in 56 different field collections (68-287 m; most between 101-200 m) off the eastern United States, Bahamas, and eastern Caribbean Sea. Historical records and recently captured specimens document the northern geographic range of adults on the shelf off New jersey (40 degrees N, 70 degrees W). Citharichthys cornutus measured 17.2-81.3 mm standard length (SL); males (20.0-79.1 mm SL) and females (28.0-81.3 mm SL) attain similar sizes (sex could not be determined for fish < 20 mm SL). Males reach nearly 100% maturity at >= 60 mm SL. The smallest mature females are 41.5 mm SL, and by 55.1 mm SL virtually all are mature. Juveniles are found with adults on the outer shelf. Only 214 C. gymnorhinus were located in 42 different field collections (35-201 m, with 90% between 61 and 120 m) off the east coast of the United States, Bahamas, and eastern Caribbean Sea. Adults are found as far north as the shelf off Cape Hatteras, NC (35 degrees N, 75 degrees W). This diminutive species (to 52.4 mm SL) is among the smallest flatfishes but males (n=131; 20.3-52.4 mm SL) attain a slightly larger maximum size than that of females (n=58; 26.2-48.0 mm SL). Males begin to mature between 29 and 35 mm SL and reach 100% maturity by 35-40 mm SL. Some females are mature at 29 mm SL, and all females > 35.1 mm SL are mature. Overlooked specimens in museum collections and literature enabled us to correct long-standing inaccuracies in northern distributional limits that appear in contemporary literature and electronic data bases for these species. Associated locality-data for these specimens allow for proper evaluation of distributional information for these species in relation to hypotheses regarding shifts in species ranges due to climate change effects. C1 [Munroe, Thomas A.] Smithsonian Inst, Natl Systemat Lab NMFS NEFSC, Washington, DC 20013 USA. [Ross, Steve W.] Univ N Carolina, Ctr Marine Sci, Wilmington, NC 28409 USA. RP Munroe, TA (reprint author), Smithsonian Inst, Natl Systemat Lab NMFS NEFSC, POB 37012,NHB,WC 57,MRC-153, Washington, DC 20013 USA. EM munroet@si.edu FU U.S. Geological Survey; NOAA Office of Ocean Exploration FX We thank the following individuals who provided information or assisted with specimens, data, and information regarding collections or databases in their care: M. Fahay, J. Finan, J. Galbraith, P. Gerdes, A. Harold, K. Hartel, W. Kramer, J.D. Lyons, D. Machowski, J. Moore, K. Murphy, R. Robins, M. A. Rogers, W. Starnes, M. Underwood, R. Worthen, D. Wyanski, and M. Zokan. D. Steere, M. Rosen, S. Dawicki, and C. Struthers assisted with locating library references. J. Brown, D. Walker, and M. Vecchione provided assistance locating nautical charts; M. Rhode, M. Partyka, M. Carlson, and M. Nizinski assisted with figure preparations; S. Raredon provided photographs; A. Quattrini and L. Willis assisted with various aspects of this study. Partial support for recent sampling was provided by the U.S. Geological Survey and NOAA Office of Ocean Exploration (grants to S.W. Ross). Special thanks are extended to the Ecosystems Survey Branch, NMFS, Woods Hole, for providing specimens and data from their long-term synoptic surveys of the continental shelf off the eastern United States. We also extend our appreciation to all those who collected fishes that were used in this study. NR 61 TC 1 Z9 2 U1 1 U2 4 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 JUL PY 2010 VL 108 IS 3 BP 323 EP 345 PG 23 WC Fisheries SC Fisheries GA 624YF UT WOS:000279857500005 ER PT J AU Quiroz, LI Buatois, LA Mangano, MG Jaramillo, CA Santiago, N AF Quiroz, Luis I. Buatois, Luis A. Mangano, M. Gabriela Jaramillo, Carlos A. Santiago, Nubia TI Is the trace fossil Macaronichnus an indicator of temperate to cold waters? Exploring the paradox of its occurrence in tropical coasts SO GEOLOGY LA English DT Article ID OCEAN CIRCULATION; SOUTH-AMERICA; LATE MIOCENE; EXTINCTION; PANAMA; NEOGENE; ICHNOLOGY; PACIFIC; SEAWAY AB The trace fossil Macaronichnus is reported for the first time from low-latitude, tropical settings based on its occurrence in nearshore deposits in the Upper Oligocene-Lower Miocene Naricual Formation and in the Middle to Upper Miocene Urumaco Formation in northern Venezuela. Macaronichnus is an intrastratal trace fossil attributed to the deposit-feeding of worms in high-energy, sandy shallow-marine environments. The majority of its occurrences are from Mesozoic to Cenozoic high-to intermediate-latitude shorelines. The opheliid polychaetes Ophelia limacina and Euzonus mucronata make structures identical to those described from the fossil record in modern intertidal and shallow subtidal sediments of northwestern United States, western Canada, and Japan. Macaronichnus shows a geographical and environmental distribution in the fossil record similar to that of its modern producers and has been proposed as an indicator of high to intermediate latitudes. Accordingly, its presence in the Neogene of Venezuela is highly anomalous and seems to challenge its paleoclimatic value. However, this occurrence may be related to seasonal coastal upwelling of nutrient-rich cold waters. Such oceanographic conditions were prevalent in the northern coast of South America, at least from the Late Oligocene to the Early Pliocene prior to the final closure of the strait of Panama. This study underscores the value of Macaronichnus because its presence in the tropics may indicate upwelling conditions, providing high-resolution information in paleoceanographic reconstructions. C1 [Quiroz, Luis I.; Buatois, Luis A.; Mangano, M. Gabriela] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. [Quiroz, Luis I.; Jaramillo, Carlos A.] Smithsonian Trop Res Inst, Ctr Trop Paleoecol & Archaeol, Balboa, Panama. [Santiago, Nubia] PDVSA, Gerencia Explora, Div Oriente, Puerto La Cruz 6023, Venezuela. RP Quiroz, LI (reprint author), Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 5E2, Canada. FU Smithsonian Tropical Research Institution; Petroleos de Venezuela (PDVSA); Natural Sciences and Engineering Research Council of Canada FX Financial support was provided by the Smithsonian Tropical Research Institution, Petroleos de Venezuela (PDVSA), and Natural Sciences and Engineering Research Council of Canada Discovery Grants (awarded to Buatois and Mangano). We thank Richard Bromley for making available his unpublished paper on Macaronichnus, Koji Seike, George Pemberton, and Orangel Aguilera for valuable comments, and Mikel Linero for information on the modern polychaete fauna of Venezuela. Christopher Fielding and an anonymous reviewer provided useful feedback. NR 49 TC 15 Z9 16 U1 0 U2 2 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD JUL PY 2010 VL 38 IS 7 BP 651 EP 654 DI 10.1130/G30140.1 PG 4 WC Geology SC Geology GA 614WE UT WOS:000279089700019 ER PT J AU Landeiro, VL Hamada, N Godoy, BS Melo, AS AF Landeiro, Victor L. Hamada, Neusa Godoy, Bruno S. Melo, Adriano S. TI Effects of litter patch area on macroinvertebrate assemblage structure and leaf breakdown in Central Amazonian streams SO HYDROBIOLOGIA LA English DT Article DE Aquatic insect; Brazil; Decomposition; Phylloicus; Triplectides; Tropical stream ID PHYLLOICUS SP TRICHOPTERA; TROPICAL STREAMS; NUTRIENT AVAILABILITY; FEEDING PREFERENCES; HEADWATER STREAM; FOOD QUALITY; SHREDDERS; DETRITIVORES; RIVER; TEMPERATE AB Leaf breakdown in streams is affected by several factors, such as leaf characteristics, water chemistry, microbial activity, and abundance of shredders. In turn, shredders may be resource-controlled. We hypothesized that the size of litter patches affects leaf breakdown, because large patches should be stable over time and therefore harbor high densities of shredders. We selected litter patches (area 0.25-10 m(2)) in 10 pools of three first-order streams (Manaus, Brazil). We installed 10 leaf packs of Mabea speciosa (Euphorbiaceae) in each patch, and sampled one after 1 day and three after 5, 19, and 28 days. The leaf packs were quickly colonized by the shredding caddisflies Triplectides and Phylloicus. The leaf breakdown rate (mean k = 0.026 +/- A 0.0015 SE) was high and similar to values reported for other tropical and temperate streams, although much higher than values reported for the adjacent Cerrado biome. Assemblage composition varied over time, but was not related to the size of litter patches. Contrary to our hypothesis, litter patch area did not affect breakdown rates (r (2) = 0.012, P = 0.766) or abundance of shredders after 5, 19, and 28 days (r (2) < 0.243, P > 0.147). We found, however, a positive relationship between the abundance of tropical shredders and leaf breakdown after 19 days (r (2) = 0.572, P = 0.011), suggesting that shredders play an important role in leaf breakdown in these headwater streams. Our study indicates that leaf breakdown rates in tropical streams are variable and can be as high as those of temperate streams. C1 [Landeiro, Victor L.] Inst Nacl de Pesquisas da Amazonia, Programa Posgrad Ecol, BR-69011970 Manaus, Amazonas, Brazil. [Landeiro, Victor L.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Landeiro, Victor L.] Inst Nacl de Pesquisas da Amazonia, Projeto Dinam Biol Fragmentos Florestais, BR-69011970 Manaus, Amazonas, Brazil. [Godoy, Bruno S.] Univ Fed Goias, Programa Posgrad Ecol & Evolucao, Dept Ecol, ICB I, BR-74001970 Goiania, Go, Brazil. [Melo, Adriano S.] Univ Fed Goias, ICB, Dept Ecol, BR-74001970 Goiania, Go, Brazil. RP Landeiro, VL (reprint author), Inst Nacl de Pesquisas da Amazonia, Programa Posgrad Ecol, Av Andre Araujo 2936,CP 478, BR-69011970 Manaus, Amazonas, Brazil. EM vllandeiro@gmail.com RI Melo, Adriano/D-6859-2013; Hamada, Neusa/E-3383-2013; Adapta, Inct/J-8371-2013; Landeiro, Victor/H-2195-2012; Godoy, Bruno/B-4059-2013 OI Landeiro, Victor/0000-0002-9341-6050; Godoy, Bruno/0000-0001-9751-9885 FU INPA/CNPq; CNPq [302482/2008-3, 476304/2007-5] FX We are very grateful to Regina Luizao, who kindly allowed the work to be done at the Km 41 BDFFP reserve. This is publication number 554 in the BDFFP technical series. We are grateful to William. E. Magnusson, David Dudgeon, and Manuel Graca and two anonymous reviewers for comments on early versions of the manuscript. Janet Reid reviewed the English. We also express thanks to Ana Pes for help with Trichoptera identifications. VLL received a PCI-DTI fellowship from INPA/CNPq. NH has been continuously supported by CNPq grants and productivity fellowships. ASM was supported by a research fellowship (proc. 302482/2008-3) and a research grant from CNPq (proc. 476304/2007-5). NR 47 TC 21 Z9 21 U1 2 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0018-8158 J9 HYDROBIOLOGIA JI Hydrobiologia PD JUL PY 2010 VL 649 IS 1 BP 355 EP 363 DI 10.1007/s10750-010-0278-8 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 596XV UT WOS:000277720100031 ER PT J AU Moullet, A Gurwell, MA Lellouch, E Moreno, R AF Moullet, Arielle Gurwell, Mark A. Lellouch, Emmanuel Moreno, Raphael TI Simultaneous mapping of SO2, SO, NaCl in Io's atmosphere with the Submillimeter Array SO ICARUS LA English DT Article DE IO; Radio observations; Atmospheres, Structure ID VOLCANICALLY DRIVEN ATMOSPHERE; GALILEO MISSION; SODIUM-CHLORIDE; PELE PLUME; PHOTOCHEMISTRY; SURFACE; SULFUR; ECLIPSE; SUBLIMATION; IONOSPHERE AB Many of the key properties of Io's atmosphere, such as its spatial distribution, temperature, column density and composition, are still not fully assessed despite decades of extensive observations. The contribution of the possible gas sources to the atmospheric replenishment are then still unclear. This paper presents disk-resolved observations performed with the Submillimeter Array (SMA) at 345 GHz of atmospheric rotational lines of the main atmospheric species SO2, and, for the first time, of the minor species SO and NaCl All these species appear concentrated on the anti-jovian hemisphere, but do not share the same spatial distribution. The obtained maps and line-averaged fluxes are compared to realistic models simulating gas sources including volcanic plume outgassing, SO2 frost sublimation and photolysis. Arguments in favor of each sources are examined and compared to observations, putting constraints on their relative roles for each species. While sublimation clearly appears as the favored major source for SO2, SO2 photolysis may account for most of the production of SO. Using constraints on the volcanic plumes distribution from Galileo results, we find that direct volcanic input can only contribute for a minor fraction of atmospheric SO2, but represent a more significant source for SO atmosphere, and is likely to be the only source for NaCl. Temperature and column densities findings are also presented for SO2, and compare well to previously published observations and atmospheric models. (C) 2010 Elsevier Inc. All rights reserved. C1 [Moullet, Arielle; Gurwell, Mark A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lellouch, Emmanuel; Moreno, Raphael] Observ Paris, LESIA, F-02195 Meudon, France. RP Moullet, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amoullet@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica FX We are grateful for L. Feaga and C. Moore who contributed to the models presented in this paper. We also thank the SMA operators. 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 40 TC 13 Z9 13 U1 2 U2 6 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 JUL PY 2010 VL 208 IS 1 BP 353 EP 365 DI 10.1016/j.icarus.2010.02.009 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 611RJ UT WOS:000278838200029 ER PT J AU Berke, SK AF Berke, Sarah K. TI Ecosystem Engineering in the Marine Realm SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Berke, Sarah K.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. EM skberke@gmail.com NR 0 TC 0 Z9 0 U1 2 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E12 EP E12 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000047 ER PT J AU Dawson, MN Bayha, KM Daglio, LEG Collins, AG AF Dawson, M. N. Bayha, K. M. Daglio, Gomez L. E. Collins, A. G. TI Phylogeny and Ecology of Jellyfish (Scyphozoa) Mass Occurrences SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Dawson, M. N.; Bayha, K. M.; Daglio, Gomez L. E.; Collins, A. G.] Univ Calif Merced, Smithsonian Inst, Merced, CA 95344 USA. EM mdawson@ucmerced.edu NR 0 TC 0 Z9 0 U1 1 U2 8 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E40 EP E40 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000158 ER PT J AU Hammock, J Lemaitre, R Harasewych, MG AF Hammock, J. Lemaitre, R. Harasewych, M. G. TI Antarctic Invertebrates at the Smithsonian: one-stop shopping SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Hammock, J.; Lemaitre, R.; Harasewych, M. G.] Smithsonian Inst, Washington, DC 20560 USA. EM hammockj@si.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E238 EP E238 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297001163 ER PT J AU Lesoway, MP Collin, R AF Lesoway, M. P. Collin, R. TI Particle capture and ingestion abilities in larvae of calyptraeid gastropods with different modes of development SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Lesoway, M. P.; Collin, R.] Smithsonian Trop Res Inst, Panama City, Panama. EM maryna.lesoway@mail.mcgill.ca RI Collin, Rachel/G-2001-2010 NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E259 EP E259 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297001245 ER PT J AU Luque, J Douglass, JK Jaramillo, CA AF Luque, J. Douglass, J. K. Jaramillo, C. A. TI How much have raninid crab eyes changed after 94 m.y. of evolution? SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 Univ Montreal, Dept Sci Biol, Quebec City, PQ, Canada. Smithsonian Trop Res Inst, Panama City, Panama. EM javierluquec@gmail.com NR 0 TC 0 Z9 0 U1 0 U2 1 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E261 EP E261 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297001254 ER PT J AU Marra, PP AF Marra, P. P. TI Seasonal interactions and carry-over effects: understanding the biology of migratory organisms within the context of the annual cycle SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Marra, P. P.] Smithsonian Inst, Washington, DC 20560 USA. EM marrap@si.edu NR 0 TC 0 Z9 0 U1 1 U2 4 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E109 EP E109 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000432 ER PT J AU Mcdonald, KA Grunbaum, D AF Mcdonald, K. A. Grunbaum, D. TI Swimming embryos point to planktonic performance standards for early-developmental motility SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Mcdonald, K. A.; Grunbaum, D.] Univ Washington, Sch Oceanog, Smithsonian Trop Res Inst, Seattle, WA 98195 USA. EM mcdonaldk2@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E113 EP E113 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000449 ER PT J AU Redmond, NE Collins, AG Diaz, MC Thacker, RW AF Redmond, N. E. Collins, A. G. Diaz, M. C. Thacker, R. W. TI Resolving species identities in the Porifera Tree of Life: a comparison of mitochondrial and nuclear barcodes SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. Univ Alabama, Birmingham, AL USA. EM redmondn@si.edu NR 0 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E144 EP E144 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000573 ER PT J AU Ritson-Williams, R Paul, VJ Arnold, SN Steneck, RS AF Ritson-Williams, R. Paul, V. J. Arnold, S. N. Steneck, R. S. TI Do coral larvae choose between species of coralline algae? SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA. Univ Maine, Darling Marine Ctr, Orono, ME 04469 USA. EM williams@si.edu NR 0 TC 0 Z9 0 U1 1 U2 8 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E148 EP E148 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000590 ER PT J AU Schwartz, ML Norenburg, JL AF Schwartz, M. L. Norenburg, J. L. TI Comparative morphology and evolution of pilidiophoran larvae (Nemertea) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Schwartz, M. L.; Norenburg, J. L.] Univ Puget Sound, Smithsonian Inst, Tacoma, WA 98416 USA. EM mschwartz@pugetsound.edu RI Norenburg, Jon/K-3481-2015 OI Norenburg, Jon/0000-0001-7776-1527 NR 0 TC 1 Z9 1 U1 0 U2 0 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E159 EP E159 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000632 ER PT J AU Sofaer, HR Sillett, TS Ghalambor, CK AF Sofaer, H. R. Sillett, T. S. Ghalambor, C. K. TI Offspring growth and functional performance in Orange-crowed Warblers: a comparison between populations that differ in life-history strategies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 [Sofaer, H. R.; Sillett, T. S.; Ghalambor, C. K.] Colorado State Univ, Smithsonian Migratory Bird Ctr, Ft Collins, CO 80523 USA. EM helen@lamar.colostate.edu NR 0 TC 0 Z9 0 U1 0 U2 7 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E165 EP E165 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297000656 ER PT J AU Thacker, RW Bangalore, P Diaz, MC Hill, A Lavrov, D Lopez, J Peterson, K Pomponi, S Redmond, N Collins, AG AF Thacker, R. W. Bangalore, P. Diaz, M. C. Hill, A. Lavrov, D. Lopez, J. Peterson, K. Pomponi, S. Redmond, N. Collins, A. G. TI Integrative approaches for reconstructing the Porifera Tree of Life (PorToL) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 03-07, 2010 CL Seattle, WA SP Soc Integrat & Comparat Biol C1 U Alabama Birmingham, Birmingham, AL USA. Iowa State U, Ames, IA USA. Nova SE U, Ft Lauderdale, FL USA. Florida Atlantic U, Boca Raton, FL 33431 USA. Smithsonian Inst, Washington, DC 20560 USA. EM thacker@uab.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD JUL PY 2010 VL 50 SU 1 BP E303 EP E303 PG 1 WC Zoology SC Zoology GA 630TL UT WOS:000280297001424 ER PT J AU Peters, VE Mordecai, R Carroll, CR Cooper, RJ Greenberg, R AF Peters, Valerie E. Mordecai, Rua Carroll, C. Ronald Cooper, Robert J. Greenberg, Russell TI Bird community response to fruit energy SO JOURNAL OF ANIMAL ECOLOGY LA English DT Article DE agroecology; community stability; fruit energy; fruit-frugivore; multi-season occupancy model; shade-grown coffee ID PAPUA-NEW-GUINEA; COFFEE PLANTATIONS; SPECIES-DIVERSITY; COSTA-RICA; TEMPORAL VARIATION; FRUGIVOROUS BIRDS; EMERGENT ISLAND; SOUTHERN MEXICO; SEED DISPERSAL; TROPICAL TREES AB P>1. The abundance and predictability of food resources have been posited as explanations for the increase of animal species richness in tropical habitats. However, the heterogeneity of natural ecosystems makes it difficult to quantify a response of animal species richness to these qualities of food resources. 2. Fruit-frugivore studies are especially conducive for testing such ecological theories because fruit is conspicuous and easily counted. Fruit-frugivore research in some locations has demonstrated a relationship between animal abundance and fruit resource abundance, both spatially and temporally. These studies, which typically use fruit counts as the variable of fruit abundance, have never documented a response of species richness at the community level. Furthermore, these studies have not taken into account factors influencing the detection of an individual within surveys. 3. Using a combination of nonstandard approaches to fruit-frugivore research, we show a response of bird species richness to fruit resources. First, we use uniform and structurally similar, one-ha shade-grown coffee plots as replicated experimental units to reduce the influence of confounding variables. Secondly, we use multi-season occupancy modelling of a resident omnivorous bird assemblage in order to account for detection probability in our analysis of site occupancy, local immigration and local emigration. Thirdly, we expand our variable of fruit abundance, Fruit Energy Availability (FEA), to include not only fruit counts but also fruit size and fruit quality. 4. We found that a site's average monthly FEA was highly correlated (0 center dot 90) with a site's average bird species richness. In our multi-season occupancy model 92% of the weight of evidence supported a single model that included effects of FEA on initial occupancy, immigration, emigration and detection. 5. These results demonstrate that fruit calories can broadly influence the richness of a neotropical bird community, and that fluctuations of FEA explains much of the site occupancy patterns of component species. This study shows that in depauperate, managed landscapes fruit resource abundance supports more species and fruit constancy allows for higher levels of avian persistence, an important practical concept for conservation planning. C1 [Peters, Valerie E.; Carroll, C. Ronald] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Mordecai, Rua] SE Partners Flight, Cary, NC 27511 USA. [Cooper, Robert J.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. [Greenberg, Russell] Smithsonian Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. RP Peters, VE (reprint author), Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. EM vale@uga.edu FU Earth Watch Institute and Birders Exchange FX We thank the University of Georgia Research Station in San Luis for logistical support. We especially thank the farmers of the San Luis community Finca la Bella for allowing us to use their land to collect data. This work was supported by funding to V. E. P. from the Earth Watch Institute and Birders Exchange. NR 71 TC 14 Z9 15 U1 1 U2 55 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0021-8790 J9 J ANIM ECOL JI J. Anim. Ecol. PD JUL PY 2010 VL 79 IS 4 BP 824 EP 835 DI 10.1111/j.1365-2656.2010.01699.x PG 12 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 606CP UT WOS:000278399300012 PM 20443988 ER PT J AU Charola, AE Centeno, SA Normandin, K AF Charola, A. Elena Centeno, Silvia A. Normandin, Kyle TI The New York Public Library: Protective Treatment for Sugaring Marble SO JOURNAL OF ARCHITECTURAL CONSERVATION LA English DT Article ID EFFICIENCY AB The marble of the New York Public Library was found to be in a fairly good state of conservation except for the more exposed elements, such as quoins and the many delicately carved elements that decorate the building. This paper focuses on the treatment developed for areas that showed significant sugaring. For this purpose, laboratory examinations and analyses were carried out and preliminary tests were made with silicate ester-based consolidants. These, however, did not perform well in test studies and therefore an approach using inorganic materials was developed. The treatment consisted of spray application of an ammonium oxalate solution that reduced the intensive sugaring of the marble. To further protect these eroded surfaces, a shelter coat based on Type S hydrated dolomitic lime was also applied. This method is fully compatible with the marble substrate and follows the overriding principle of minimum intervention, as stated by the Venice Charter. C1 [Charola, A. Elena] World Monuments Fund, Buenos Aires, DF, Argentina. [Charola, A. Elena] Univ Penn, Smithsonian Museum Conservat Inst, Philadelphia, PA 19104 USA. [Charola, A. Elena] Univ Penn, Grad Program Hist Preservat, Philadelphia, PA 19104 USA. [Charola, A. Elena] Catholic Univ Leuven, Raymond Lemaire Int Ctr, Louvain, Belgium. [Centeno, Silvia A.] Metropolitan Museum Art, New York, NY 10028 USA. [Normandin, Kyle] Elstner Associates Inc, New York, NY USA. RP Charola, AE (reprint author), World Monuments Fund, Buenos Aires, DF, Argentina. OI Centeno, Silvia/0000-0002-8496-4426 NR 30 TC 1 Z9 1 U1 0 U2 3 PU DONHEAD PUBL LTD PI DORSET PA LOWER COOMBE, DONHEAD ST MARY, SHAFTESBURY, DORSET, SP7 9LY, ENGLAND SN 1355-6207 J9 J ARCHIT CONSERV JI J. Archit. Conserv. PD JUL PY 2010 VL 16 IS 2 BP 29 EP 44 PG 16 WC Architecture SC Architecture GA 631CS UT WOS:000280324800003 ER PT J AU Schwenk, WS Strong, AM Sillett, TS AF Schwenk, W. Scott Strong, Allan M. Sillett, T. Scott TI Effects of bird predation on arthropod abundance and tree growth across an elevational gradient SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID COMPLEX TERRESTRIAL COMMUNITY; THROATED BLUE WARBLERS; ACER-PENSYLVANICUM L; STRIPED MAPLE; TROPHIC CASCADES; FOREST BIRDS; TOP-DOWN; HERBIVOROUS INSECTS; INSECTIVOROUS BIRDS; FORAGING BEHAVIOR AB Considerable uncertainty surrounds the conditions under which birds can cause trophic cascades. In a three-year experiment, we studied the direct and indirect effects of insectivorous birds on arthropod abundance, herbivory, and growth of striped maple Acer pensylvanicum saplings in a northern hardwood forest of central New Hampshire, USA. We manipulated bird predation by erecting exclosures around saplings and directly manipulated herbivory by removing herbivores. We also examined how climate modifies these interactions by replicating the experiment at three locations along an elevational gradient. Effects of bird predation were variable. Overall, mean arthropod biomass was 20% greater on saplings within bird exclosures than on controls (p < 0.05). The mean biomass of leaf-chewing herbivores, primarily Lepidoptera larvae, was 25% greater within exclosures but not statistically different from controls. To a lesser degree, mean herbivore damage to foliage within exclosures exceeded that of controls but differences were not significant. We also did not detect significant treatment effects on sapling shoot growth. The high understory vegetation density relative to bird abundance, and low rate of herbivory during the study (mean 5% leaf area removed, controls), may have limited the ability of birds to affect sapling growth. Climate effects operated at multiple scales, resulting in a complex interplay of interactions within the food web. Regional synchrony of climatic conditions resulted in annual fluctuations in herbivore abundance and tree growth that were shared across elevations. At the same time, local environmental variation resulted in site differences in the plant, herbivore, and bird communities. These patterns resulted in a mosaic of top-down strengths across time and space, suggesting an overall pattern of limited effects of birds on plant growth, possibly interspersed with hotspots of trophic cascades. C1 [Schwenk, W. Scott; Strong, Allan M.] Univ Vermont, Rubenstein Sch Environm & Nat Resources, Burlington, VT 05405 USA. [Sillett, T. Scott] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Schwenk, WS (reprint author), Univ Vermont, Rubenstein Sch Environm & Nat Resources, Burlington, VT 05405 USA. EM scott.schwenk@uvm.edu FU USDA; Northeastern States Research Cooperative; U.S. National Science Foundation [DEB 0108488, DEB 0423259, DEB 0640823] FX Joanna Hatt, Nicholas Kovacs, Kiryn Lanning, Briita Orwick, and Sarah Wilkins rendered outstanding assistance in the field. Brian Beckage, Tray Biasiolli, Alison Brody, Gabe Colbeck, Therese Donovan, Richard Holmes, Alan Howard, Matt Kemp, Karen Klinger, Rebecca Pfeiffer, Nicholas Roden-house, Paul Schaberg, Kris Tjernell, Ray Webster and Nate Zalik also provided input and assistance. The climate data used in this publication were obtained by scientists of the Hubbard Brook Ecosystem Study; this publication has not been reviewed by those scientists. The HBEF is operated and maintained by the Northeastern Research Station, USDA Forest Service, Newtown Square, Pennsylvania. Financial support was provided by grants from the USDA McIntire-Stennis Program, the Northeastern States Research Cooperative, and the U.S. National Science Foundation (DEB 0108488, DEB 0423259, DEB 0640823). NR 57 TC 15 Z9 15 U1 5 U2 31 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD JUL PY 2010 VL 41 IS 4 BP 367 EP 377 DI 10.1111/j.1600-048X.2009.04963.x PG 11 WC Ornithology SC Zoology GA 623IO UT WOS:000279733000002 ER PT J AU Ingwell, LL Wright, SJ Becklund, KK Hubbell, SP Schnitzer, SA AF Ingwell, Laura L. Joseph Wright, S. Becklund, Kristen K. Hubbell, Stephen P. Schnitzer, Stefan A. TI The impact of lianas on 10 years of tree growth and mortality on Barro Colorado Island, Panama SO JOURNAL OF ECOLOGY LA English DT Article DE Barro Colorado Island; competition; liana dynamics; lianas; Panama; tropical forest ID BELOW-GROUND COMPETITION; RAIN-FOREST TREE; TROPICAL FOREST; SEEDLINGS; REGENERATION; INFESTATION; BOLIVIA; LOADS; LIGHT; GHANA AB P>1. Lianas compete intensely with trees, but few studies have examined long-term effects of liana infestation on tree growth and mortality. We quantified the effects of lianas in tree crowns (n = 2907) and rooted within 2 m of trees (n = 1086) on growth and mortality of 30 tree species from 1995 to 2005 on Barro Colorado Island (BCI), Panama, documented liana infestation in tree crowns in 1996 and 2007 to determine the dynamics of liana infestation, and quantified liana infestation in the crowns of 3231 additional canopy trees (d.b.h. >= 20 cm) in 2007 to compare with the same metric determined by previous studies in 1967 and 1980. 2. Severe liana infestation increased tree mortality: 21% of liana-free trees in 1996 had died by 2007, whereas 42% of trees with more than 75% of the crown infested by lianas in 1996 had died by 2007. 3. Liana infestation of tree crowns significantly reduced tree growth, particularly on sun-exposed trees. The proximity of rooted lianas significantly reduced the growth of shaded trees. 4. Liana infestation was dynamic: 10.9% of trees with severe liana infestation in their crowns in 1996 had shed all of their lianas by 2007 and 5.3% of trees with no lianas in their crown in 1996 had severe liana infestation in 2007. 5. Liana infestation was common: lianas were present in 53% of trees of the 30 focal species. Including lianas rooted within 2 m of the tree increased this percentage to 78%. Using both above- and below-ground measures may provide a better estimate of liana competition than either measure alone. 6. Liana infestation is increasing on BCI. Lianas were present in the crowns of 73.6% of canopy trees (d.b.h. >= 20 cm). Liana canopy infestation was 57% higher than in 1980 and 65% higher than in 1967, which is consistent with reported increases in liana abundance, biomass, and leaf and flower production. 7.Synthesis. We used one of the largest studies ever conducted on lianas to confirm the negative effects of lianas on tree growth and survival over 10 years. Liana infestation of trees was widespread, dynamic and increasing on BCI. C1 [Ingwell, Laura L.; Becklund, Kristen K.; Schnitzer, Stefan A.] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Joseph Wright, S.; Hubbell, Stephen P.; Schnitzer, Stefan A.] Smithsonian Trop Res Inst, Balboa, Panama. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. RP Schnitzer, SA (reprint author), Univ Wisconsin, Dept Biol Sci, POB 413, Milwaukee, WI 53201 USA. EM schnitzer@uwm.edu RI Wright, Stuart/M-3311-2013; OI Wright, Stuart/0000-0003-4260-5676; Schnitzer, Stefan/0000-0002-2715-9455 FU National Science Foundation [DEB-0613666, DEB-0845071, 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, DEB 0453665]; University of Wisconsin-Milwaukee (UWM) Research Growth Initiative; UWM Center for Latin American and Caribbean Studies; UWM Center for International Education; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; John D. and Catherine T. MacArthur Foundation; Mellon Foundation; Celera Foundation FX We thank two anonymous reviewers for helpful comments on this study. This study was made possible, in part, by financial support to S. A. S. from the National Science Foundation (DEB-0613666 and DEB-0845071), the University of Wisconsin-Milwaukee (UWM) Research Growth Initiative, the UWM Center for Latin American and Caribbean Studies and the UWM Center for International Education. NSF DEB 0453665 funded the census of liana infestation in the crowns of canopy trees in five 4-ha plots. 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. The plot project is part of the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. NR 56 TC 84 Z9 88 U1 6 U2 39 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD JUL PY 2010 VL 98 IS 4 BP 879 EP 887 DI 10.1111/j.1365-2745.2010.01676.x PG 9 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 609RO UT WOS:000278675000016 ER PT J AU Cheesman, AW Dunne, EJ Turner, BL Reddy, KR AF Cheesman, Alexander W. Dunne, Ed J. Turner, Benjamin L. Reddy, K. Ramesh TI Soil Phosphorus Forms in Hydrologically Isolated Wetlands and Surrounding Pasture Uplands SO JOURNAL OF ENVIRONMENTAL QUALITY LA English DT Article ID P-31 NMR-SPECTROSCOPY; NUCLEAR-MAGNETIC-RESONANCE; ORGANIC PHOSPHORUS; LAKE OKEECHOBEE; WATER-QUALITY; AGRICULTURAL PHOSPHORUS; SUBTROPICAL PASTURES; NEW-ZEALAND; FLORIDA; EXTRACTION AB Newly created and restored wetlands play an important role in sequestering excess nutrients at the landscape scale In evaluating the long-term efficacy of nutrient management strategies to increase wetland capacity for sequestering P, information is needed on the forms of P found across the upland-wetland transition To assess this, we studied soils (0-10 cm) from four wetlands within cow-calf pastures north of Lake Okeechobee, FL Wetlands contained significantly (P < 0.05) greater concentrations of organic matter (219 g C kg(-1)), total P (371 mg P kg(-1)). and metals (Al, Fe) relative to surrounding pasture When calculated on an aerial basis, wetland surface sods contained significantly greater amounts of total P (236 kg ha(-1)) compared with upland soils (114 kg ha(-1)), which was linked to the concomitant increase in organic matter with increasing hydroperiod The concentration of P forms. determined by extraction with anion exchange membranes, I mol L(-1) HCl, and an alkaline extract (0 25 mol L(-1) NaOH and 50 mmol L(-1) ethylenediaminetetraacetic acid [EDTA]) showed significant differences between uplands and wetlands but did not alter as a proportion of total P Speciation of NaOH-EDTA extracts by solution (31)P nuclear magnetic resonance spectroscopy revealed that organic P was dominated by phosphomonoesters in boils wetland and pasture sods but that myo-inositol hexakisphosphate was not detected in any sample The tight coupling of total C and P in the sandy sods of the region suggests that the successful management of historically isolated wetlands for P sequestration depends on the long-terns accumulation and stabilization of sod organic matter C1 [Cheesman, Alexander W.; Reddy, K. Ramesh] Univ Florida, IFAS, Wetland Biogeochem Lab, Soil & Water Sci Dep, Gainesville, FL 32611 USA. [Dunne, Ed J.] St Johns River Water Management Dist, Div Environm Sci, Dep Water Resources, Palatka, FL 32177 USA. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Cheesman, AW (reprint author), Univ Florida, IFAS, Wetland Biogeochem Lab, Soil & Water Sci Dep, 106 Newell Hall, Gainesville, FL 32611 USA. RI Turner, Benjamin/E-5940-2011; Cheesman, Alexander/H-5918-2013 OI Turner, Benjamin/0000-0002-6585-0722; Cheesman, Alexander/0000-0003-3931-5766 FU University of Florida; Alex Blumenfeld, University of Idaho; USDA-CREES National Research Initiative [2004-35107-14918]; Florida Department of Agriculture and Consumer Services FX We thank Yu Wang, University of Florida, and Alex Blumenfeld, University of Idaho, for analytical support The project was supported by a grant from the USDA-CREES National Research Initiative (No. 2004-35107-14918) and the Florida Department of Agriculture and Consumer Services Four anonymous reviewers provided constructive comments that helped to improve the final manuscript. NR 66 TC 21 Z9 22 U1 0 U2 22 PU AMER SOC AGRONOMY PI MADISON PA 677 S SEGOE RD, MADISON, WI 53711 USA SN 0047-2425 J9 J ENVIRON QUAL JI J. Environ. Qual. PD JUL-AUG PY 2010 VL 39 IS 4 BP 1517 EP 1525 DI 10.2134/jeq2009.0398 PG 9 WC Environmental Sciences SC Environmental Sciences & Ecology GA 620QK UT WOS:000279514200040 PM 20830938 ER PT J AU Smith, CJ Collins, LS Jaramillo, C Quiroz, LI AF Smith, Carly J. Collins, Laurel S. Jaramillo, Carlos Quiroz, Luiz I. TI MARINE PALEOENVIRONMENTS OF MIOCENE-PLIOCENE FORMATIONS OF NORTH-CENTRAL FALCON STATE, VENEZUELA SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID BOCAS-DEL-TORO; BENTHIC FORAMINIFERA; NORTHWESTERN VENEZUELA; WESTERN VENEZUELA; ASSEMBLAGES; BASIN; NEOGENE; PANAMA; CHRONOLOGY; TECTONICS AB Late middle Miocene to middle or late Pliocene benthic foraminifera from north-central Falcon State, northwestern Venezuela, were used in determinations of the marine paleoenvironments of the Urumaco, Codore, Caujarao, La Vela and San Gregorio formations. From 121 collected samples, 31 that included a total of 126 taxa were applied to paleoenvironmental interpretations, and 20 well-preserved foraminiferal samples were analyzed with cluster analysis. In the Urumaco region, the upper middle to upper Miocene Urumaco Formation, which alternates among continental, marginal marine, and marine facies, was predominantly inner shelf, and the taxa and very low diversities suggest highly variable, low-salinity conditions. Foraminifera of the upper Miocene middle Pliocene Chiguaje Member of the overlying Codore Formation indicate a deepening from inner to deeper-middle shelf. The middle to upper Pliocene San Gregorio Formation varies from estuarine in the lower Verge! Member to inner shelf in the overlying Cocuiza Member. In the Coro-La Vela region to the northeast, paleobathymetries are deeper, fluctuating from middle- to outer-neritic depths in the upper Miocene Taratara Member of the Caujarao Formation, and middle-neritic depths in the conformably overlying upper Miocene, basal part of the La Vela Formation. The relatively stable water depths of the Caujarao and lower La Vela formations support deposition on a stable marine platform. Overall, the shallower facies in the west and deeper facies in the east agree with the interpretation of an eastward progression of inversion of the Falcon basin from Miocene to Pliocene time. The middle Miocene Pliocene shelf sequences of Falcon are compared to other formations of Venezuela and Colombia with similar paleoenvironments. C1 [Smith, Carly J.; Collins, Laurel S.] Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Panama. [Quiroz, Luiz I.] Univ Saskatchewan, Dept Geol Sci, Saskatoon, SK S7N 0W0, Canada. RP Collins, LS (reprint author), Florida Int Univ, Dept Earth & Environm, Miami, FL 33199 USA. EM collinsl@fiu.edu FU Smithsonian Tropical Research Institute FX This research was conducted in partial fulfillment of the requirements of a masters thesis by Smith, who thanks her committee members Florentin Maurrasse and Grenville Draper. Orange] Aguilera, Universidad Nacional Experimental Francisco de Miranda in Coro, Venezuela, graciously hosted the project, and the Smithsonian Tropical Research Institute funded our fieldwork. Geological guidance and camaraderie in the field by Sara Moron and Rodolpho Sanchez were greatly appreciated. Reviews by David Scott and Brent Wilson improved the quality of the paper. NR 70 TC 11 Z9 14 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 JUL PY 2010 VL 40 IS 3 BP 266 EP 282 PG 17 WC Paleontology SC Paleontology GA 618UG UT WOS:000279380600006 ER PT J AU Dudar, JC AF Dudar, J. Christopher TI Qualitative and Quantitative Diagnosis of Lethal Cranial Neural Tube Defects from the Fetal and Neonatal Human Skeleton, with a Case Study Involving Taphonomically Altered Remains SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; anencephaly; neural tube defects; fetal skeleton; neonatal skeleton; fetal abandonment; forensic anthropology AB Cranial neural tube defect, or anencephaly, is the absence of normal brain development because of severe developmental defect in the fetus. While the current incidence of human anencephaly ranges between 1 to 5 per 1000 births, and was higher prior to folic acid supplementation, there is no discussion of anencephaly diagnosis in the forensic literature and only one published example from the archeological record. This article presents both qualitative observations of abnormal cranial elements and an osteometric method to quantitatively determine anencephaly from forensic recovery contexts where taphonomic variables may otherwise mask diagnostic characteristics. Evidence is presented for only the second case of anencephaly diagnosed from a burial context, and the first not involving soft tissue mummification. The initial recognition and accurate prediction of anencephaly is a significant contribution to investigators recovering found human fetal remains. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Repatriat Osteol Lab, Washington, DC 20013 USA. RP Dudar, JC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Repatriat Osteol Lab, POB 37012,MRC 138, Washington, DC 20013 USA. NR 22 TC 2 Z9 2 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD JUL PY 2010 VL 55 IS 4 BP 877 EP 883 DI 10.1111/j.1556-4029.2010.01382.x PG 7 WC Medicine, Legal SC Legal Medicine GA 619RQ UT WOS:000279448200004 PM 20384923 ER PT J AU Mishchenko, MI Rothman, LS Menguc, MP Stoop, J AF Mishchenko, Michael I. Rothman, Laurence S. Menguec, M. Pinar Stoop, Jose TI 50 years of JQSRT: Milestone papers SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material ID MOLECULAR SPECTROSCOPIC DATABASE; TIME-INDEPENDENT EQUATION; ABSORPTION CROSS-SECTIONS; SENSING REFERENCE DATA; 231-794 NM RANGE; RADIATIVE-TRANSFER; LIGHT-SCATTERING; NONSPHERICAL PARTICLES; LINE-WIDTHS; APPROXIMATION C1 [Mishchenko, Michael I.] NASA, Goddard Inst Space Studies, New York, NY 10025 USA. [Rothman, Laurence S.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Menguec, M. Pinar] Univ Kentucky, Dept Mech Engn, Lexington, KY 40506 USA. [Stoop, Jose] Elsevier, NL-1043 NX Amsterdam, Netherlands. RP Mishchenko, MI (reprint author), NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mmishchenko@giss.nasa.gov; lrothman@cfa.narvard.edu; menguc@engr.uky.edu; J.Stoop@elsevier.com RI Menguc, Pinar/O-3114-2013; Mishchenko, Michael/D-4426-2012; OI Rothman, Laurence/0000-0002-3837-4847 NR 42 TC 3 Z9 3 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2010 VL 111 IS 11 SI SI BP 1455 EP 1458 DI 10.1016/j.jqsrt.2010.01.037 PG 4 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 617FG UT WOS:000279265700001 ER PT J AU Rothman, LS AF Rothman, Laurence S. TI A story of a seminal line-shape paper SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material DE Line shape; Molecular collisions; Line widths; Pressure broadening; Line shift AB A background of the publication of the seminal paper on line shape by C.J. Tsao and B. Curnutte (C.J. Tsao, B. Curnutte, Line-widths of pressure-broadened spectral lines, JQSRT 2 (1962) pp. 41-91.) is presented. This highly cited paper continues to have a significant impact on research involving molecular collisions. (C) 2010 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 6 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 0022-4073 EI 1879-1352 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2010 VL 111 IS 11 SI SI BP 1461 EP 1462 DI 10.1016/j.jqsrt.2010.01.034 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 617FG UT WOS:000279265700003 ER PT J AU Rothman, LS AF Rothman, Laurence S. TI A note on a pioneering work in quantitative spectroscopy: UV bands of the hydroxyl radical SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material DE Hydroxyl radical; Ultraviolet absorption; UV transition probabilities ID OH AB The publication by G.H. Dieke and H.M. Crosswhite (JQSRT 1962;2:97-199) is a classic paper detailing the spectroscopy of the A(2)Sigma(+)<- X(2)Pi bands of the hydroxyl radical (OH) in the ultraviolet region. It soon became the basis of astrophysical modeling, most subsequent theoretical and laboratory studies of the OH individual line parameters, and a host of other applications. (C) 2010 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 9 TC 0 Z9 0 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2010 VL 111 IS 11 SI SI BP 1514 EP 1515 DI 10.1016/j.jqsrt.2010.02.003 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 617FG UT WOS:000279265700005 ER PT J AU Rothman, LS AF Rothman, Laurence S. TI The evolution and impact of the HITRAN molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material DE HITRAN; Molecular absorption; Atmospheric transmission; Molecular spectroscopy; Spectroscopic database ID EDITION; HAWKS AB This note provides a brief review of the history and impact of the molecular spectroscopic database known as HITRAN (High Resolution Transmission). We reprint one of the articles describing this database (JQSRT 1998; 60: 665-710), although the series of these papers is among the most cited in the geosciences. HITRAN was established over three decades ago in response to the needs of simulating transmission in the terrestrial atmosphere, and it was enabled by new technology. However the applications of HITRAN, and the requirements on the database, have greatly expanded over the intervening years. (C) 2010 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu OI Rothman, Laurence/0000-0002-3837-4847 NR 9 TC 13 Z9 16 U1 0 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2010 VL 111 IS 11 SI SI BP 1565 EP 1567 DI 10.1016/j.jqsrt.2010.01.027 PG 3 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 617FG UT WOS:000279265700011 ER PT J AU Rothman, LS Rinsland, CP Goldman, A Massie, ST Edwards, DP Flaud, JM Perrin, A Camy-Peyret, C Dana, V Mandin, JY Schroeder, J McCann, A Gamache, RR Wattson, RB Yoshino, K Chance, KV Jucks, KW Brown, LR Nemtchinov, V Varanasi, P AF Rothman, L. S. Rinsland, C. P. Goldman, A. Massie, S. T. Edwards, D. P. Flaud, J. -M. Perrin, A. Camy-Peyret, C. Dana, V. Mandin, J. -Y. Schroeder, J. McCann, A. Gamache, R. R. Wattson, R. B. Yoshino, K. Chance, K. V. Jucks, K. W. Brown, L. R. Nemtchinov, V. Varanasi, P. TI THE HITRAN MOLECULAR SPECTROSCOPIC DATABASE AND HAWKS (HITRAN ATMOSPHERIC WORKSTATION): 1996 EDITION (Reprint from J Quant Spectrosc Radiat Transfer, vol 60, pg 665-710, 1998) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Reprint ID ABSORPTION CROSS-SECTIONS; COLLISION-INDUCED ABSORPTION; FAR-INFRARED SPECTRUM; SELF-BROADENING COEFFICIENTS; DIODE-LASER SPECTROSCOPY; SCHUMANN-RUNGE BANDS; NONLOCAL THERMODYNAMIC-EQUILIBRIUM; DIRECT NUMERICAL DIAGONALIZATION; HIGH-RESOLUTION SPECTROSCOPY; COMPLEX REFRACTIVE-INDEXES AB Since its first publication in 1973, the HITRAN molecular spectroscopic database has been recognized as the international standard for providing the necessary fundamental spectroscopic parameters for diverse atmospheric and laboratory transmission and radiance calculations. There have been periodic editions of HITRAN over the past decades as the database has been expanded and improved with respect to the molecular species and spectral range covered, the number of parameters included, and the accuracy of this information. The 1996 edition not only includes the customary line-by-line transition parameters familiar to HITRAN users, but also cross-section data, aerosol indices of refraction, software to filter and manipulate the data, and documentation. This paper describes the data and features that have been added or replaced since the previous edition of HITRAN. We also cite instances of critical data that are forthcoming. Published by Elsevier Science Ltd. C1 [Rothman, L. S.] USAF, Res Lab, VSBM, Hanscom AFB, MA 01731 USA. [Rothman, L. S.; Yoshino, K.; Chance, K. V.; Jucks, K. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rinsland, C. P.] NASA, Div Atmospher Sci, Langley Res Ctr, Hampton, VA 23681 USA. [Goldman, A.] Univ Denver, Dept Phys, Denver, CO 80208 USA. [Massie, S. T.; Edwards, D. P.] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Flaud, J. -M.; Perrin, A.] Univ Paris 11, Photophys Mol Lab, CNRS, F-91405 Orsay, France. [Camy-Peyret, C.; Dana, V.; Mandin, J. -Y.] Univ Paris 06, LPMA, F-75252 Paris 05, France. [Schroeder, J.; McCann, A.] Ontar Corp, N Andover, MA 01845 USA. [Gamache, R. R.] Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. [Wattson, R. B.] Utah State Univ, Stewart Radiance Lab, Bedford, MA 01730 USA. [Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Nemtchinov, V.; Varanasi, P.] SUNY Stony Brook, Stony Brook, NY 11794 USA. RP Rothman, LS (reprint author), USAF, Res Lab, VSBM, 29 Randolph Rd, Hanscom AFB, MA 01731 USA. NR 289 TC 5 Z9 5 U1 3 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUL PY 2010 VL 111 IS 11 SI SI BP 1568 EP 1613 PG 46 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 617FG UT WOS:000279265700012 ER PT J AU Eggert, LS Powell, DM Ballou, JD Malo, AF Turner, A Kumer, J Zimmerman, C Fleischer, RC Maldonado, JE AF Eggert, Lori S. Powell, David M. Ballou, Jonathan D. Malo, Aurelio F. Turner, Allison Kumer, Jack Zimmerman, Carl Fleischer, Robert C. Maldonado, Jesus E. TI Pedigrees and the Study of the Wild Horse Population of Assateague Island National Seashore SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Article DE Assateague Island National Seashore; Equus caballus; fecal DNA; microsatellites; pedigree analysis; wildlife management ID FERAL HORSES; CONSERVATION PROGRAMS; COMPUTER-PROGRAM; GENETIC-MARKERS; EQUUS-CABALLUS; BARRIER-ISLAND; IMMUNOCONTRACEPTION; MANAGEMENT; KINSHIP; IMPACT AB Recently, a number of papers have addressed the use of pedigrees in the study of wild populations, highlighting the value of pedigrees in conservation management. We used pedigrees to study the horses (Equus caballus) of Assateague Island National Seashore, Maryland, USA, one of a small number of free-ranging animal populations that have been the subject of long-term studies. This population grew from 28 in 1968 to 175 in 2001, causing negative impacts on the island ecosystem. To minimize these effects, an immunocontraception program was instituted, and horse numbers are slowly decreasing. However, there is concern that this program may negatively affect the genetic health of the herd. We found that although mitochondrial DNA diversity is low, nuclear diversity is comparable to that of established breeds. Using genetic data, we verified and amended maternal pedigrees that had been primarily based on behavioral data and inferred paternity using genetic data along with National Park Service records of the historic ranges of males. The resulting pedigrees enabled us to examine demography, founder contributions, rates of inbreeding and loss of diversity over recent generations, as well as the level of kinship among horses. We then evaluated the strategy of removing individuals (using nonlethal means) with the highest mean kinship values. Although the removal strategy increased the retained diversity of founders and decreased average kinship between individuals, it disproportionately impacted sizes of the youngest age classes. Our results suggest that a combined strategy of controlled breeding and immunocontraception would be more effective than removing individuals with high mean kinships in preserving the long-term health and viability of the herd. C1 [Eggert, Lori S.; Ballou, Jonathan D.; Malo, Aurelio F.; Fleischer, Robert C.; Maldonado, Jesus E.] Smithsonian Inst, Natl Zool Pk, Natl Museum Nat Hist, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Powell, David M.] Wildlife Conservat Soc Bronx Zoo, Dept Mammal, Bronx, NY 10460 USA. [Turner, Allison; Kumer, Jack; Zimmerman, Carl] Assateague Isl Natl Seashore, Berlin, MD 21811 USA. RP Eggert, LS (reprint author), Univ Missouri, Div Biol Sci, 226 Tucker Hall, Columbia, MO 65211 USA. EM eggertl@missouri.edu RI Malo, Aurelio/D-3973-2011 OI Malo, Aurelio/0000-0002-0846-2096 NR 61 TC 2 Z9 2 U1 1 U2 38 PU WILDLIFE SOC PI BETHESDA PA 5410 GROSVENOR LANE, BETHESDA, MD 20814-2197 USA SN 0022-541X J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD JUL PY 2010 VL 74 IS 5 BP 963 EP 973 DI 10.2193/2009-231 PG 11 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 617OQ UT WOS:000279290700009 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI US Foreign Policy and National Security: Chronology and Index for the 20th Century, vol 2. SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 JUL PY 2010 VL 135 IS 12 BP 108 EP 108 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 621RS UT WOS:000279600600265 ER PT J AU Douglass, JG France, KE Richardson, JP Duffy, JE AF Douglass, James G. France, Kristin E. Richardson, J. Paul Duffy, J. Emmett TI Seasonal and interannual change in a Chesapeake Bay eelgrass community: Insights into biotic and abiotic control of community structure SO LIMNOLOGY AND OCEANOGRAPHY LA English DT Article ID INDIAN RIVER LAGOON; ZOSTERA-MARINA; ECOLOGICAL COMMUNITIES; SEAGRASS ECOSYSTEMS; AQUATIC VEGETATION; CONTINENTAL-SHELF; AMPHIPODS; DYNAMICS; FLORIDA; GROWTH AB We characterized the seasonal and interannual variation in macrophytes, epiphytes, invertebrate herbivores, small demersal predators, and physicochemical characteristics of an eelgrass (Zostera marina) bed in Chesapeake Bay, Virginia, over 10 yr, to explore the relative importance of abiotic and biotic forcing on community composition and abundance. Our hypotheses were (1) physicochemical drivers affect community structure directly, (2) bottom-up trophic control is evidenced by positive covariance among trophic levels, (3) top-down control generates inverse patterns of abundance at adjacent trophic levels, and (4) species diversity among herbivores contributes to temporal stability. Composition and abundance of eelgrass-associated species varied strongly among seasons and years. Much of this variation correlated with temperature and salinity anomalies, and multivariate analysis grouped communities roughly by season, supporting our first hypothesis. Severe seagrass loss during the hot summer of 2005 shifted the community toward a novel composition, but community structure rebounded within a year. Evidence for trophic control was mixed: selected taxa showed patterns consistent with top-down or bottom-up control, but these patterns generally disappeared at the level of whole years and entire trophic levels. Our ability to detect trophic effects may have been limited, however, by consumer movement or changing behavioral responses to resource availability and predation. There was also little evidence that diversity stabilized total herbivore abundance. Although consumer effects on lower levels were inconsistent, the strong physicochemical forcing of community structure supports suggestions that eelgrass communities are highly vulnerable to natural and anthropogenic changes in climate and hydrography. C1 [Douglass, James G.; France, Kristin E.; Richardson, J. Paul; Duffy, J. Emmett] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [Douglass, James G.] Smithsonian Marine Stn, Ft Pierce, FL USA. [France, Kristin E.] Nature Conservancy, Cent & Western New York Chapter, Rochester, NY USA. RP Douglass, JG (reprint author), Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. EM douglassjm@si.edu FU Office of the Chief Economist [95-21184, OCE-0099226, OCE 03-52343, OCE-0623874] FX We thank John Parker, Jennifer Rhode, Kenneth Macdonald, Melanie Harris, Ruben Rios, Jessie Philpot, Mark Fitchett, Lana Lau, Molly Roggero, Amanda Spivak, Aaron Spivak, Susie Herbert, Kiara Smith, Laura Ladwig, Akwasi Cato, Breanna Korsman, Sara Grill, Timothy Montgomery, Lindsey Moore, Noah Yavit, William Tarantino, Martin Marquez, Phillip Mattich, Gabriella Blohm, Lindsey Albertson, Thomas Hill, Rachael Blake, Diana Chin, Matthew Whalen, and others for field and laboratory assistance. We also thank Kenneth Moore, Robert Orth, and the staff of the Chesapeake Bay National Estuarine Research Reserve Program for invaluable help and data sharing during the preparation of this manuscript. Finally, we thank Per-Olav Moksnes and an anonymous reviewer for help with the production of the final manuscript. This work was supported in part by grant numbers Office of the Chief Economist 95-21184, OCE-0099226, OCE 03-52343, and OCE-0623874 to J.E.D. This is Virginia Institute of Marine Science contribution 3070. NR 73 TC 29 Z9 29 U1 6 U2 48 PU AMER SOC LIMNOLOGY OCEANOGRAPHY PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710-4446 USA SN 0024-3590 J9 LIMNOL OCEANOGR JI Limnol. Oceanogr. PD JUL PY 2010 VL 55 IS 4 BP 1499 EP 1520 DI 10.4319/lo.2010.55.4.1499 PG 22 WC Limnology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 673KA UT WOS:000283657000004 ER PT J AU Mayne, RG Sunshine, JM Mcsween, HY Mccoy, TJ Corrigan, CM Gale, A AF Mayne, Rhiannon G. Sunshine, Jessica M. Mcsween, Harry Y. Mccoy, Timothy J. Corrigan, Catherine M. Gale, Allison TI Petrologic insights from the spectra of the unbrecciated eucrites: Implications for Vesta and basaltic asteroids SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MODIFIED GAUSSIAN MODEL; REFLECTANCE SPECTRA; PARENT BODY; MARTIAN METEORITES; PYROXENES; PETROGENESIS; SPACE; DIFFERENTIATION; SPECTROSCOPY; METAMORPHISM AB We investigate the relationship between the petrology and visible-near infrared spectra of the unbrecciated eucrites and synthetic pyroxene-plagioclase mixtures to determine how spectra obtained by the Dawn mission could distinguish between several models that have been suggested for the petrogenesis of Vesta's crust (e.g., partial melting and magma ocean). Here, we study the spectra of petrologically characterized unbrecciated eucrites to establish spectral observables, which can be used to yield mineral abundances and compositions consistent with petrologic observations. No information about plagioclase could be extracted from the eucrite spectra. In contrast, pyroxene dominates the spectra of the eucrites and absorption band modeling provides a good estimate of the relative proportions of low- and high-Ca pyroxene present. Cr is a compatible element in eucrite pyroxene and is enriched in samples from primitive melts. An absorption at 0.6 mu m resulting from Cr3+ in the pyroxene structure can be used to distinguish these primitive eucrites. The spectral differences present among the eucrites may allow Dawn to distinguish between the two main competing models proposed for the petrogenesis of Vesta (magma ocean and partial melting). These models predict different crustal structures and scales of heterogeneity, which can be observed spectrally. The formation of eucrite Allan Hills (ALH) A81001, which is primitive (Cr-rich) and relatively unmetamorphosed, is hard to explain in the magma ocean model. It could only have been formed as a quench crust. If the magma ocean model is correct, then ALHA81001-like material should be abundant on the surface of Vesta and the Vestoids. C1 [Mayne, Rhiannon G.] Texas Christian Univ, Dept Geol, Ft Worth, TX 76109 USA. [Sunshine, Jessica M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mcsween, Harry Y.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Mccoy, Timothy J.; Corrigan, Catherine M.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Gale, Allison] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Mayne, RG (reprint author), Texas Christian Univ, Dept Geol, TCU Box 298830, Ft Worth, TX 76109 USA. EM r.g.mayne@tcu.edu FU PGG [NNX06AH69G]; NASA [NNG06GG36G]; UCLA [2090-S-JB694] FX This work was supported by PGG grant NNX06AH69G to J. M. S. and NASA Cosmochemistry grant NNG06GG36G and UCLA subcontract 2090-S-JB694 for Dawn to H. Y. M. All meteorite spectra were collected at Brown University's KECK/NASA Reflectance Experiment Laboratory (RELAB). Thanks go to M. Darby Dyar for the collection of Mossbauer spectra. NR 60 TC 24 Z9 24 U1 1 U2 6 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 IS 7 BP 1074 EP 1092 DI 10.1111/j.1945-5100.2010.01090.x PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 674CW UT WOS:000283712300006 ER PT J AU Bouvier, A Wadhwa, M Bullock, ES MacPherson, GJ AF Bouvier, A. Wadhwa, M. Bullock, E. S. MacPherson, G. J. TI Pb-Pb DATING OF A CAI FROM THE REDUCED CV3 CHONDRITE VIGARANO SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [Bouvier, A.; Wadhwa, M.] Arizona State Univ, Sch Earth Space & Explorat, Tempe, AZ USA. [Bullock, E. S.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. EM abouvier@asu.edu NR 7 TC 1 Z9 1 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A20 EP A20 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700033 ER PT J AU Bullock, ES Richter, FM Ushikubo, T Kita, NT Davis, AM MacPherson, GJ AF Bullock, E. S. Richter, F. M. Ushikubo, T. Kita, N. T. Davis, A. M. MacPherson, G. J. TI SILICON ISOTOPE FRACTIONATION IN MELILITE WITHIN TYPE B2 CAIS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc ID CRYSTALLIZATION C1 [Bullock, E. S.; MacPherson, G. J.] US Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Richter, F. M.; Davis, A. M.] Univ Wisconsin, Dept Geophys, Chicago, IL 60637 USA. [Ushikubo, T.; Kita, N. T.] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Davis, A. M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. EM BullockE@si.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A26 EP A26 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700045 ER PT J AU Chapman, CR Strom, RG Fassett, CI Prockter, LM Head, JW Solomon, SC Banks, ME Baker, D Merline, WJ AF Chapman, C. R. Strom, R. G. Fassett, C. I. Prockter, L. M. Head, J. W., III Solomon, S. C. Banks, M. E. Baker, D. Merline, W. J. TI CRATERING ON MERCURY: INSIGHTS FROM THE MESSENGER FLYBYS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [Chapman, C. R.; Merline, W. J.] SW Res Inst, Boulder, CO 80302 USA. [Strom, R. G.] Univ Arizona, LPL, Tucson, AZ 85721 USA. [Fassett, C. I.; Head, J. W., III; Baker, D.] Brown Univ, Dept Geol Sci, Providence, RI 02906 USA. [Prockter, L. M.] Johns Hopkins Univ, APL, Laurel, MD 20723 USA. [Solomon, S. C.] Carnegie Inst Washington, DTM, Washington, DC 20015 USA. [Banks, M. E.] NASM, Smithsonian Inst, Washington, DC 20013 USA. EM cchapman@boulder.swri.edu NR 0 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A32 EP A32 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700056 ER PT J AU Corrigan, CM Welzenbach, LC Fries, M Mccoy, TJ Fries, J AF Corrigan, C. M. Welzenbach, L. C. Fries, M. Mccoy, T. J. Fries, J. TI THE RECENT METEORITE FALL IN LORTON, VIRGINIA, USA SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [Corrigan, C. M.; Welzenbach, L. C.; Mccoy, T. J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Fries, M.] NASA, Jet Prop Lab, Pasadena, CA 91109 USA. [Fries, J.] USAF, Weather Agcy, 1st Weather Grp, Offutt AFB, Omaha, NE 68113 USA. EM corriganc@si.edu NR 2 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A39 EP A39 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700069 ER PT J AU Greenwood, JP Itoh, S Sakamoto, N Vicenzi, EP Yurimoto, H AF Greenwood, J. P. Itoh, S. Sakamoto, N. Vicenzi, E. P. Yurimoto, H. TI D/H ZONING IN APATITE OF MARTIAN METEORITES QUE 94201 AND LOS ANGELES: IMPLICATIONS FOR WATER ON MARS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc ID CLUES C1 [Greenwood, J. P.] Wesleyan Univ, Dept E&ES, Middletown, CT 06459 USA. [Itoh, S.; Yurimoto, H.] Hokkaido Univ, Sapporo, Hokkaido 0600810, Japan. [Sakamoto, N.; Yurimoto, H.] Hokkaido Univ, CRIS, Sapporo, Hokkaido 0600810, Japan. [Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. EM jgreenwood@wesleyan.edu NR 4 TC 1 Z9 1 U1 0 U2 4 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A68 EP A68 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700128 ER PT J AU Ivanova, MA Lorenz, CA Krot, AN MacPherson, GJ AF Ivanova, M. A. Lorenz, C. A. Krot, A. N. MacPherson, G. J. TI MINERALOGY AND BULK CHEMISTRY OF CAIs FROM EFREMOVKA AND NWA 3118 CV CHONDRITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc ID RICH INCLUSIONS C1 [Ivanova, M. A.; Lorenz, C. A.] Vernadsky Inst Geochemistry, Moscow 119991, Russia. [Ivanova, M. A.; MacPherson, G. J.] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. [Krot, A. N.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. EM meteorite2000@mail.ru NR 5 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A92 EP A92 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700175 ER PT J AU MacPherson, GJ Nagashima, K Krot, AN Bullock, ES AF MacPherson, G. J. Nagashima, K. Krot, A. N. Bullock, E. S. TI HIGH-PRECISION O-ISOTOPE MEASUREMENTS IN VIGARANO CAIS: SLOPE 0.94, AND COMMON PRESENCE OF O-16-RICH MELILITE AND ANORTHITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc ID ALLENDE C1 [MacPherson, G. J.; Bullock, E. S.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Nagashima, K.; Krot, A. N.] Univ Hawaii Manoa, Inst Geophys & Planetol, Honolulu, HI 96822 USA. EM macphers@si.edu NR 5 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A125 EP A125 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700240 ER PT J AU Mayne, RG Rose, T Corrigan, CM Smith, SE AF Mayne, R. G. Rose, T. Corrigan, C. M. Smith, S. E. TI QARABAWI'S CAMEL CHARM: AN EGYPTIAN IRON METEORITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [Mayne, R. G.; Smith, S. E.] Texas Christian Univ, Dept Geol, Ft Worth, TX 76129 USA. [Mayne, R. G.; Rose, T.; Corrigan, C. M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A130 EP A130 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700250 ER PT J AU McCoy, TJ AF McCoy, T. J. TI A NEW VIEW OF ASTEROID PARTIAL DIFFERENTIATION: A LEGACY OF BRIAN MASON'S WORK ON ANTARCTIC METEORITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [McCoy, T. J.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 6 TC 0 Z9 0 U1 0 U2 1 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A132 EP A132 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700254 ER PT J AU Mccoy, TJ AF Mccoy, T. J. TI asiihkiwi neehi kiisikwi: A MULTI-GENERATIONAL, CULTURALLY-EMBEDDED EARTH AND SKY CURRICULUM FOR THE MYAAMIAKI SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [Mccoy, T. J.] Natl Museum Nat Hist, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. NR 2 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A133 EP A133 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700255 ER PT J AU Stockstill-Cahill, KR McCoy, TJ AF Stockstill-Cahill, K. R. McCoy, T. J. TI PETROLOGIC MODELING OF CHONDRITIC PARENT MELTS: IMPLICATIONS FOR MESSENGER SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc ID MERCURY C1 [Stockstill-Cahill, K. R.; McCoy, T. J.] NMNH, Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM cahillk@si.edu NR 9 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A197 EP A197 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700382 ER PT J AU Welzenbach, LC Corrigan, CM AF Welzenbach, L. C. Corrigan, C. M. TI BEYOND THE EXHIBIT: OUTREACH ACTIVITIES OF THE SMITHSONIAN'S METEORITE COLLECTION SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 73rd Annual Meeting of the Meteoritical-Society CY JUL 26-30, 2010 CL New York, NY SP Meteorit Soc C1 [Welzenbach, L. C.; Corrigan, C. M.] Smithsonian Inst, Washington, DC 20560 USA. EM welzenbl@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD JUL PY 2010 VL 45 SU S BP A214 EP A214 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 633DC UT WOS:000280478700415 ER PT J AU Shefferson, RP Cowden, CC Mccormick, MK Yukawa, T Ogura-Tsujita, Y Hashimoto, T AF Shefferson, Richard P. Cowden, Charles C. Mccormick, Melissa K. Yukawa, Tomohisa Ogura-Tsujita, Yuki Hashimoto, Toshimasa TI Evolution of host breadth in broad interactions: mycorrhizal specificity in East Asian and North American rattlesnake plantains (Goodyera spp.) and their fungal hosts SO MOLECULAR ECOLOGY LA English DT Article DE Ceratobasidiaceae; Ceratobasidium; mycorrhiza; parasitic fungi; specificity ID LADYS SLIPPER ORCHIDS; TROPICAL ORCHIDS; GREEN ORCHID; DIVERSITY; REPENS; CARBON; COMMUNITIES; IDENTIFICATION; ADAPTATION; MOVEMENT AB Host breadth is often assumed to have no evolutionary significance in broad interactions because of the lack of cophylogenetic patterns between interacting species. Nonetheless, the breadth and suite of hosts utilized by one species may have adaptive value, particularly if it underlies a common ecological niche among hosts. Here, we present a preliminary assessment of the evolution of mycorrhizal specificity in 12 closely related orchid species (genera Goodyera and Hetaeria) using DNA-based methods. We mapped specificity onto a plant phylogeny that we estimated to infer the evolutionary history of the mycorrhiza from the plant perspective, and hypothesized that phylogeny would explain a significant portion of the variance in specificity of plants on their host fungi. Sampled plants overwhelmingly associated with genus Ceratobasidium, but also occasionally with some ascomycetes. Ancestral mycorrhizal specificity was narrow in the orchids, and broadened rarely as Goodyera speciated. Statistical tests of phylogenetic inertia suggested some support for specificity varying with increasing phylogenetic distance, though only when the phylogenetic distance between suites of fungi interacting with each plant taxon were taken into account. These patterns suggest a role for phylogenetic conservatism in maintaining suits of fungal hosts among plants. We stress the evolutionary importance of host breadth in these organisms, and suggest that even generalists are likely to be constrained evolutionarily to maintaining associations with their symbionts. C1 [Shefferson, Richard P.; Cowden, Charles C.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Mccormick, Melissa K.] Smithsonian Environm Res Ctr, Plant Ecol Lab, Edgewater, MD 21037 USA. [Hashimoto, Toshimasa] Nippon Steel Kankyo Engn Corp, Chiba 2920, Japan. [Yukawa, Tomohisa; Ogura-Tsujita, Yuki] Natl Museum Sci, Tsukuba Bot Garden, Tsukuba, Ibaraki 3050005, Japan. RP Shefferson, RP (reprint author), Univ Georgia, Odum Sch Ecol, 140 E Green St, Athens, GA 30602 USA. EM dormancy@gmail.com NR 62 TC 25 Z9 26 U1 0 U2 23 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 JUL PY 2010 VL 19 IS 14 BP 3008 EP 3017 DI 10.1111/j.1365-294X.2010.04693.x PG 10 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 623OF UT WOS:000279751000015 PM 20584135 ER PT J AU Miura, O Torchin, ME Bermingham, E AF Miura, Osamu Torchin, Mark E. Bermingham, Eldredge TI Molecular phylogenetics reveals differential divergence of coastal snails separated by the Isthmus of Panama SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cerithidea; Cerithium; Isthmus of Panama; Molecular evolution; Geminate species; Diversification ID MITOCHONDRIAL-DNA; SEA-URCHINS; GAMETIC INCOMPATIBILITY; MAXIMUM-LIKELIHOOD; ATLANTIC; INVASION; ECHINOMETRA; CALIBRATION; SPECIATION; EVOLUTION AB We used 20 species of coastal marine snails in the genus Cerithidea and Cerithium collected along the Pacific and Atlantic coasts of Central America to investigate the role of the rise of the Isthmus of Panama in the speciation of this group. Of particular interest was the identification of geminate species pairs presumably established by the disruption of gene flow across the isthmian barrier. Hypotheses of phylogenetic relationships were based on approximately 2.4 Kb of the mitochondrial cytochrome oxidase c subunit I gene, 16S ribosomal RNA gene and the nuclear 28S ribosomal gene. We identified four putative geminate species pairs out of the 20 species evaluated, but the level of sequence divergence among the pairs differed more than two-fold. A geminate pair, in which both species live in the high intertidal of mangrove habitats, exhibited less sequence divergence compared to other pairs occupying lower intertidal and subtidal habitats. Mangrove dwelling species were probably the last to be separated by the final closure of the Central American Seaway, and thus their divergence times correspond most accurately to the completion of the Isthmus. (C) 2010 Elsevier Inc. All rights reserved. C1 [Miura, Osamu; Torchin, Mark E.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Miura, Osamu] Kyoto Univ, Grad Sch Global Environm Studies, Sakyo Ku, Kyoto 6068501, Japan. RP Miura, O (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM miurao@si.edu FU STRI; Smithsonian Marine Science Network; Japan Society for the Promotion of Science FX We thank Y. Kam, S. Jagadeeshan, E. Mendoza, E. Ochoa, A. Jaramillo, V. Frankel, E. Siu-Estrada and N. Aleman for their field assistance. We are especially indebted to C. Schloder for invaluable field, laboratory and logistical assistance. We are also grateful to R. Hechinger, E. Toth, N. Smith and A. Terrero for providing us with additional specimens. We thank D. Jacobs, O. Puebla, O. Sanjur and two anonymous reviewers for providing useful comments on the manuscript. We thank the crew of the R.V. Urraca and the staff of the STRI's Naos Island Laboratories, Bocas del Toro marine station, Galeta marine station, Smithsonian Marine Station at Fort Pierce and Carrie Bow Cay Marine Laboratory. Support was provided by STRI and a Smithsonian Marine Science Network Postdoctoral Fellowship (to O.M.) and a STRI Hoch fellowship (to O.M.) and Japan Society for the Promotion of Science (Grant-in-Aid for JSPS Fellows to O.M.). NR 44 TC 24 Z9 26 U1 1 U2 20 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 JUL PY 2010 VL 56 IS 1 BP 40 EP 48 DI 10.1016/j.ympev.2010.04.012 PG 9 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 608MX UT WOS:000278589500004 PM 20399869 ER PT J AU Alva-Campbell, Y Floeter, SR Robertson, DR Bellwood, DR Bernardi, G AF Alva-Campbell, Yvette Floeter, Sergio R. Robertson, D. Ross Bellwood, David R. Bernardi, Giacomo TI Molecular phylogenetics and evolution of Holacanthus angelfishes (Pomacanthidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Holacanthus; Angelfishes; Geminate species; Pomacanthus; Pygoplites ID REEF FISH; RECENT INVASION; INDO-PACIFIC; SPECIATION; ATLANTIC; BIOGEOGRAPHY; PISCES AB The angelfish genus Holacanthus includes seven species in the tropical Eastern Pacific and Atlantic. In this study we performed an analysis on all species, the closely related regal angelfish, and the Cortez angelfish, using four mitochondrial and one nuclear marker. Our results support a monophyletic Holacanthus. The Indo-Pacific regal angelfish, Pygoplytes diacanthus, was found to be the closest relative to Holacanthus. We found a split into two clades with divergences that were consistent with the rise of the Isthmus of Panama. An internally calibrated molecular clock thus placed the origin of Holacanthus to similar to 10.2-7.6 million years ago. (C) 2010 Elsevier Inc. All rights reserved. C1 [Alva-Campbell, Yvette; Bernardi, Giacomo] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95060 USA. [Floeter, Sergio R.] Univ Fed Santa Catarina, Dept Ecol & Zool, BR-88010970 Florianopolis, SC, Brazil. [Robertson, D. Ross] Smithsonian Trop Res Inst, Balboa, Panama. [Bellwood, David R.] James Cook Univ, Australian Res Council Ctr Excellence Coral Reef, Townsville, Qld 4811, Australia. [Bellwood, David R.] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. RP Bernardi, G (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, 100 Shaffer Rd, Santa Cruz, CA 95060 USA. EM bernardi@biology.ucsc.edu RI Bernardi, Giacomo/F-6346-2011; Floeter, Sergio/B-1438-2012 OI Bernardi, Giacomo/0000-0002-8249-4678; NR 32 TC 8 Z9 10 U1 2 U2 20 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 JUL PY 2010 VL 56 IS 1 BP 456 EP 461 DI 10.1016/j.ympev.2010.02.014 PG 6 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 608MX UT WOS:000278589500041 PM 20171293 ER PT J AU McDonald, I van Loon, JT Dupree, AK Boyer, ML AF McDonald, I. van Loon, J. Th. Dupree, A. K. Boyer, M. L. TI Discovery of long-period variable stars in the very metal-poor globular cluster M15 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: AGB and post-AGB; stars: late-type; stars: Population II; stars: variables: general; stars: winds, outflows; globular clusters: individual: M15 ID RED GIANT STARS; COLOR-MAGNITUDE DIAGRAMS; MASS-LOSS; OMEGA-CENTAURI; CHROMOSPHERIC ACTIVITY; INTRACLUSTER MEDIUM; DYNAMICAL DISTANCE; DUST PRODUCTION; SPECTRAL ATLAS; FIELD GIANTS AB We present a search for long-period variable (LPV) stars among giant branch stars in M15 which, at [Fe/H] similar to -2.3, is one of the most metal-poor Galactic globular clusters. We use multicolour optical photometry from the 0.6-m Keele Thornton and 2-m Liverpool Telescopes. Variability of delta V similar to 0.15 mag is detected in K757 and K825 over unusually long time-scales of nearly a year, making them the most metal-poor LPVs found in a Galactic globular cluster. K825 is placed on the long secondary period sequence, identified for metal-rich LPVs, though no primary period is detectable. We discuss this variability in the context of dust production and stellar evolution at low metallicity, using additional spectra from the 6.5-m Magellan (Las Campanas) telescope. A lack of dust production, despite the presence of gaseous mass loss raises questions about the production of dust and the intracluster medium of this cluster. C1 [McDonald, I.; van Loon, J. Th.] Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England. [McDonald, I.] Univ Manchester, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Boyer, M. L.] STScI, Baltimore, MD 21218 USA. RP McDonald, I (reprint author), Keele Univ, Lennard Jones Labs, Astrophys Grp, Keele ST5 5BG, Staffs, England. EM mcdonald@jb.man.ac.uk FU Particle Physics and Astronomy Research Council (PPARC); Science and Technology Facilities Council (STFC); UK Science and Technology Facilities Council FX IM was supported by a Particle Physics and Astronomy Research Council (PPARC) and a Science and Technology Facilities Council (STFC) studentship for the initial stages of this work. This paper includes data gathered with the 6.5-m Magellan Telescopes located at Las Campanas Observatory, Chile, the LT, operated on the island of La Palma by John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrophysica de Canarias with financial support from the UK Science and Technology Facilities Council and the KT operated by and located at Keele University, with dedicated support from local volunteers. NR 63 TC 9 Z9 9 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2010 VL 405 IS 3 BP 1711 EP 1722 DI 10.1111/j.1365-2966.2010.16603.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613ZB UT WOS:000279022900018 ER PT J AU Slatyer, TR Finkbeiner, DP AF Slatyer, Tracy R. Finkbeiner, Douglas P. TI A statistical test of emission from unresolved point sources SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; gamma-rays: diffuse background ID X-RAY BINARIES; ACTIVE GALACTIC NUCLEI; ENERGY COSMIC-RAYS; LUMINOSITY FUNCTION; INDICATOR; CENTAURUS; GALAXIES AB We describe a simple test of the spatial uniformity of an ensemble of discrete events. Given an estimate for the point-source luminosity function and an instrumental point spread function, a robust upper bound on the fractional point-source contribution to a diffuse signal can be found. We verify with Monte Carlo tests that the statistic has advantages over the two-point correlation function for this purpose, and derive analytic estimates of the statistic's mean and variance as a function of the point-source contribution. As a case study, we apply this statistic to recent gamma-ray data from the Fermi Large Area Telescope, and demonstrate that at energies above 10 GeV the contribution of unresolved point sources to the diffuse emission is small in the region relevant for study of the WMAP Haze. C1 [Slatyer, Tracy R.; Finkbeiner, Douglas P.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Slatyer, Tracy R.; Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Slatyer, TR (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM tslatyer@fas.harvard.edu FU American Australian Association FX We wish to acknowledge helpful conversations with Marc Davis, Josh Grindlay, Igor Moskalenko, Jim Peebles and Pat Slane. We thank the anonymous referee for helpful comments. TRS is supported by a Sir Keith Murdoch Fellowship from the American Australian Association. NR 19 TC 4 Z9 4 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2010 VL 405 IS 3 BP 1777 EP 1786 DI 10.1111/j.1365-2966.2010.16550.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613ZB UT WOS:000279022900023 ER PT J AU Posselt, B Schreyer, K Perna, R Sommer, MW Klein, B Slane, P AF Posselt, B. Schreyer, K. Perna, R. Sommer, M. W. Klein, B. Slane, P. TI Submillimetre observations of RX J1856.5-3754 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: individual: RX J1856.5-3754; circumstellar matter ID ISOLATED NEUTRON-STARS; MILLISECOND PULSARS; PLANETARY SYSTEM; PROPELLER REGIME; MAGNETIC-FIELDS; FALLBACK DISKS; XMM-NEWTON; DUST; ACCRETION; NEARBY AB We report on submillimetre bolometer observations of the isolated neutron star RXJ1856.5-3754 using the Large Apex Bolometer Camera bolometer array on the Atacama Pathfinder Experiment telescope. No cold dust continuum emission peak at the position of RXJ1856.5-3754 was detected. The 3 sigma flux density upper limit of 5mJy translates into a cold dust mass limit of a few earth masses. We use the new submillimetre limit, together with a previously obtained H-band limit, to constrain the presence of a gaseous, circumpulsar disc. Adopting a simple irradiated disc model, we obtain a mass accretion limit of. M less than or similar to 10(14) g s(-1) and a maximum outer disc radius of similar to 10(14) cm. By examining the projected proper motion of RXJ1856.5-3754, we speculate about a possible encounter of the neutron star with a dense fragment of the CrA molecular cloud a few thousand years ago. C1 [Posselt, B.; Slane, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Schreyer, K.] Inst Astrophys, D-07745 Jena, Germany. [Schreyer, K.] Univ Sternwarte Jena, D-07745 Jena, Germany. [Perna, R.] Univ Colorado, UCB 440, Boulder, CO 80309 USA. [Sommer, M. W.] Argelander Inst Astron, D-53121 Bonn, Germany. [Klein, B.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Posselt, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bposselt@cfa.harvard.edu OI Posselt, Bettina/0000-0003-2317-9747 FU Deutsche Akademie der Naturforscher Leopoldina (Halle, Germany) [BMBF-LPD 9901/8-170] FX We thank Axel Weiss for kindly providing calibration and opacity tables for the LABOCA observations, as well as E. Dwek and R. Smith for enlightening discussion about X-ray-radiated dust. BP acknowledges the support by the Deutsche Akademie der Naturforscher Leopoldina (Halle, Germany) under grant BMBF-LPD 9901/8-170. NR 55 TC 3 Z9 3 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2010 VL 405 IS 3 BP 1840 EP 1844 DI 10.1111/j.1365-2966.2010.16557.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613ZB UT WOS:000279022900029 ER PT J AU Munoz, JA Trac, H Loeb, A AF Munoz, Joseph A. Trac, Hy Loeb, Abraham TI Galaxy statistics in pencil-beam surveys at high redshifts SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: abundances; galaxies: high-redshift; cosmology: observations; cosmology: theory; early Universe; large-scale structure of Universe ID LY-ALPHA EMITTERS; TO 7-10 GALAXIES; COSMIC REIONIZATION; LUMINOSITY FUNCTION; GLOBULAR-CLUSTERS; POWER-SPECTRUM; MILKY-WAY; IMPRINT; FIELD; POPULATION AB Surveys of faint galaxies at high redshifts often result in a 'pencil- beam' geometry that is much longer along the line of sight than across the sky. We explore the effects of this geometry on the abundance and clustering of Lyman-break galaxies (LBGs) and Lyman alpha emitters (LAEs) in current and future surveys based on cosmological N-body simulations which adequately describe the non-linear growth of structure on small scales and compare to linear theory. We find that the probability distribution of the LBG abundance is skewed towards low values since the narrow transverse dimension of the survey is more likely to probe underdense regions. Over a range that spans 1-2 orders of magnitude in galaxy luminosities, the variance in the number of objects differs from the commonly used analytic prediction and is not dominated by Poisson noise. Additionally, non-linear bias on small scales results in a 1D power spectrum of LAEs using a James Webb Space Telescope field of view that is relatively flat, markedly different from the expectation of linear perturbation theory. We discuss how these results may affect attempts to measure the UV background at high redshifts, estimate the relationship between halo mass and galaxy luminosity, and probe re-ionization by measuring the power-modulating effect of ionized regions. C1 [Munoz, Joseph A.; Trac, Hy; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Munoz, JA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 10, Cambridge, MA 02138 USA. EM jamunoz@cfa.harvard.edu RI Munoz, Joseph/A-3336-2013; Trac, Hy/N-8838-2014 OI Munoz, Joseph/0000-0003-1588-1296; Trac, Hy/0000-0001-6778-3861 FU Institute for Theory and Computation Fellowship; NASA [NNX08AL43G]; Harvard University FX We would like to thank Mark Dijkstra for useful discussions. HT is supported by an Institute for Theory and Computation Fellowship. This research was also supported in part by NASA grants NNX08AL43G and LA, and by Harvard University funds. NR 40 TC 6 Z9 6 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL 1 PY 2010 VL 405 IS 3 BP 2001 EP 2008 DI 10.1111/j.1365-2966.2010.16591.x PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613ZB UT WOS:000279022900045 ER PT J AU Langley, JA Megonigal, JP AF Langley, J. Adam Megonigal, J. Patrick TI Ecosystem response to elevated CO2 levels limited by nitrogen-induced plant species shift SO NATURE LA English DT Article ID ATMOSPHERIC CARBON-DIOXIDE; SOIL NUTRIENT; CLIMATE; CYCLE; METAANALYSIS; COMPETITION; LIMITATION; DEPOSITION; FEEDBACKS; DIVERSITY AB Terrestrial ecosystems gain carbon through photosynthesis and lose it mostly in the form of carbon dioxide (CO2). The extent to which the biosphere can act as a buffer against rising atmospheric CO2 concentration in global climate change projections remains uncertain at the present stage(1-4). Biogeochemical theory predicts that soil nitrogen (N) scarcity may limit natural ecosystem response to elevated CO2 concentration, diminishing the CO2-fertilization effect on terrestrial plant productivity in unmanaged ecosystems(3-7). Recent models have incorporated such carbon-nitrogen interactions and suggest that anthropogenic N sources could help sustain the future CO2-fertilization effect(8,9). However, conclusive demonstration that added N enhances plant productivity in response to CO2-fertilization in natural ecosystems remains elusive. Here we manipulated atmospheric CO2 concentration and soil N availability in a herbaceous brackish wetland where plant community composition is dominated by a C-3 sedge and C-4 grasses, and is capable of responding rapidly to environmental change(10). We found that N addition enhanced the CO2-stimulation of plant productivity in the first year of a multi-year experiment, indicating N-limitation of the CO2 response. But we also found that N addition strongly promotes the encroachment of C-4 plant species that respond less strongly to elevated CO2 concentrations. Overall, we found that the observed shift in the plant community composition ultimately suppresses the CO2-stimulation of plant productivity by the third and fourth years. Although extensive research has shown that global change factors such as elevated CO2 concentrations and N pollution affect plant species differently(11-13), and that they may drive plant community changes(14-17), we demonstrate that plant community shifts can act as a feedback effect that alters the whole ecosystem response to elevated CO2 concentrations. Moreover, we suggest that trade-offs between the abilities of plant taxa to respond positively to different perturbations may constrain natural ecosystem response to global change. C1 [Langley, J. Adam; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Langley, J. Adam] Villanova Univ, Dept Biol, Villanova, PA 19084 USA. RP Langley, JA (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM langleya@si.edu FU USGS [06ERAG0011]; US Department of Energy [DE-FG02-97ER62458]; US Department of Energy's Office of Science (BER) through the Coastal Center of the National Institute of Climate Change Research at Tulane University; Smithsonian Institution FX We acknowledge the support of D. Cahoon, our primary US Geological Survey collaborator, who co-developed the experimental design of this study. We thank J. Duls, J. Keller, M. Sigrist, G. Peresta, B. Drake, E. Sage, A. Martin, D. McKinley, N. Mudd and K. White for the construction and maintenance of the field site at the Smithsonian Climate Change Facility. We appreciate comments from S. Chapman, A. Classen, J. Hines, B. Hungate, T. Mozdzer, A. Sutton-Grier and D. Whigham. The field study was supported by the USGS Global Change Research Program (cooperative agreement 06ERAG0011), the US Department of Energy (grant DE-FG02-97ER62458), the US Department of Energy's Office of Science (BER) through the Coastal Center of the National Institute of Climate Change Research at Tulane University, and the Smithsonian Institution. NR 30 TC 95 Z9 101 U1 21 U2 193 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 1 PY 2010 VL 466 IS 7302 BP 96 EP 99 DI 10.1038/nature09176 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 618HW UT WOS:000279343800041 PM 20596018 ER PT J AU Smith, PA Wilson, S AF Smith, Paul A. Wilson, Scott TI Intraseasonal patterns in shorebird nest survival are related to nest age and defence behaviour SO OECOLOGIA LA English DT Article DE Nest survival; Nest defence; Nest abundance; Predation; Nest age ID DAILY ENERGY-EXPENDITURE; CALIDRIDINE SANDPIPERS; WILLOW PTARMIGAN; SPACING-OUT; PREDATION; INCUBATION; DENSITY; TIME; SCHEDULE; HABITAT AB Nest survival may vary throughout the breeding season for many bird species, and the nature of this temporal variation can reveal the links between birds, their predators, and other components of the ecosystem. We used program Mark to model patterns in nest survival within the breeding season for shorebirds nesting on arctic tundra. From 2000 to 2007, we monitored 521 nests of five shorebird species and found strong evidence for variation in nest survival within a nesting season. Daily nest survival was lowest in the mid-season in 5 of 8 years, but the timing and magnitude of the lows varied. We found no evidence that this quadratic time effect was driven by seasonal changes in weather or the abundance of predators. Contrary to our prediction, the risk of predation was not greatest when the number of active shorebird nests was highest. Although nest abundance reached a maximum near the middle of the breeding season, a daily index of shorebird nest activity was not supported as a predictor of nest survival in the models. Predators' access to other diet items, in addition to shorebird nests, may instead determine the temporal patterns of nest predation. Nest survival also displayed a positive, linear relationship with nest age; however, this effect was most pronounced among species with biparental incubation. Among biparental species, parents defended older nests with greater intensity. We did not detect a similar relationship among uniparental species, and conclude that the stronger relationship between nest age and both nest defence and nest survival for biparental species reflects that their nest defence is more effective. C1 [Wilson, Scott] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Smith, Paul A.] Carleton Univ, Dept Biol, Ottawa, ON K1S 5B6, Canada. RP Smith, PA (reprint author), Canadian Wildlife Serv, Natl Wildlife Res Ctr, 1125 Colonel Dr, Ottawa, ON K1A 0H3, Canada. EM Paulallen.smith@ec.gc.ca FU Environment Canada FX We thank H. Grant Gilchrist and Mark R. Forbes for assistance with study design, and are indebted to the many field assistants responsible for finding and monitoring nests. Field work was funded by Environment Canada, and logistical support provided by the Polar Continental Shelf Project. Two anonymous reviewers provided helpful comments on the manuscript. All research described was approved through permits from the Canadian Wildlife Service, the Territory of Nunavut and the Kivalliq Inuit Association. NR 65 TC 26 Z9 26 U1 1 U2 31 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 EI 1432-1939 J9 OECOLOGIA JI Oecologia PD JUL PY 2010 VL 163 IS 3 BP 613 EP 624 DI 10.1007/s00442-010-1644-y PG 12 WC Ecology SC Environmental Sciences & Ecology GA 611RI UT WOS:000278838000007 PM 20446092 ER PT J AU Wang, SW AF Wang, Sonam Wangyel TI Estimating population densities and biomass of ungulates in the temperate ecosystem of Bhutan SO ORYX LA English DT Article DE Bhutan; biomass; density; leopard; Panthera pardus; Panthera tigris; tiger; ungulates ID BARDIA-WILDLIFE-RESERVE; WANGCHUCK NATIONAL-PARK; TIGERS PANTHERA-TIGRIS; TROPICAL FORESTS; PREY ABUNDANCE; ECOLOGICAL SURVEY; DECIDUOUS FOREST; SOUTHERN INDIA; SELECTION; CARNIVORES AB In this study I estimate population densities and biomass of the major prey species of tiger Panthera tigris, leopard Panthera pardus and dhole Cuon alpinus in Bhutan's temperate ecosystem and recommend measures for reducing crop damage whilst simultaneously protecting ungulate populations. Thirty-two transects totalling 849 km were walked to estimate densities and biomass of ungulates and primates in Bhutan's Jigme Singye Wangchuck National Park during 2005-2006. Adequate detections (>40 sightings) for analysis using Distance were obtained for wild pig Sus scrofa (n=54), muntjac Munticus muntjac (n=102) and sambar Cervus unicolor (n=48). Because of similarity in morphology and habitat use, density of serow Capricornis sumatraensis was estimated using the detection probability for sambar. Detections for langur Trachypithecus geei and macaque Macca mulatta were combined (n=39) to estimate primate density. Mean estimated densities were 3.68 wild pig, 2.17 muntjac, 1.19 sambar, 2.37 primates and 0.36 serow km(-2). The three primary prey species of large predators, wild pig, sambar and muntjac, provided a biomass of 379 kg km(-2), which could support up to 1.2 tigers per 100 km(2). However, the presence of other sympatric carnivores competing for prey in the same area suggests that the actual number of tigers that could be supported is lower. Livestock (density, 6.0 km(-2); biomass, 615 kg km(-2)) apparently supplement prey availability. Ungulate density in the study area is generally low compared to other areas in the Indian sub-continent, and this may be due to conflicts with farmers, excessive grazing of livestock in the forest and the rugged terrain. C1 [Wang, Sonam Wangyel] Minist Agr, Dept Forests, Nat Conservat Div, Thimphu, Bhutan. [Wang, Sonam Wangyel] Univ Oxford, WildCRU, London, England. [Wang, Sonam Wangyel] Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. RP Wang, SW (reprint author), Minist Agr, Dept Forests, Nat Conservat Div, Thimphu, Bhutan. EM wangsonam@gmail.com FU NFWF; Whitley Fund for Nature and Disney Conservation FX I would like to thank my field assistants (Kinzang Lham, Kuenzang Dorji, Kesang Wangchuk, Sonam Dorji, K. B. Gurung, Jigme Wangchuk, Karma and Ngawang Tenzin) for their hard work, and Drs James P. Lassoie, Paul Curtis, Milo E. Richmond, Ullas Karanth, A.J.T. Johnsingh and Koustubh Sharma for reviewing this article. I greatly appreciate the financial support of Save the Tiger Fund/NFWF, Whitley Fund for Nature and Disney Conservation. NR 46 TC 3 Z9 3 U1 1 U2 27 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0030-6053 J9 ORYX JI Oryx PD JUL PY 2010 VL 44 IS 3 BP 376 EP 382 DI 10.1017/S0030605310000487 PG 7 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 645MD UT WOS:000281461600019 ER PT J AU Cairns, SD AF Cairns, Stephen D. TI Review of Octocorallia (Cnidaria: Anthozoa) from Hawai'i and Adjacent Seamounts. Part 3: Genera Thouarella, Plumarella, Callogorgia, Fanellia, and Parastenella SO PACIFIC SCIENCE LA English DT Review ID GRAY; COELENTERATA; GORGONACEA AB Ten species of Hawaiian primnoids are described and/or discussed, completing the review of the 28 primnoids known from the Hawaiian Islands. This family constitutes 29% of the Hawaiian octocoral fauna. Callogorgia ameruana is synonymized with C. gilberti, resulting in a disjunct distribution in the Pacific and Northwest Atlantic. Two new species are described (Plumarella circumoperculum Cairns and Parastenella bayeri Cairns), and two (Callogorgia gilberti and C robusta) are reported for the first time since their original descriptions over a century ago. Keys are provided for the Hawaiian prinmoid genera and all species of the genus Parastenella; comparative tables are provided for the Hawaiian Callogorgia and Pane Ilia. A distinctive nematocyst pad is described for the genus Pm-astern! Highly modified polyps caused by copepod parasites are described for two species. Callogorgia gilberti and Thouarella bilgendorfi. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163,POB 37012, Washington, DC 20560 USA. FU NOAA-OE [NA0OAR4600108, NA04OAR4600071] FX Collections of the Pisces 5 submersible funded by NOAA-OE research grants NA0OAR4600108 and NA04OAR4600071 to Amy Baco Taylor Manuscript accepted 2 September 2009 NR 46 TC 7 Z9 9 U1 1 U2 5 PU UNIV HAWAII PRESS PI HONOLULU PA 2840 KOLOWALU ST, HONOLULU, HI 96822 USA SN 0030-8870 J9 PAC SCI JI Pac. Sci. PD JUL PY 2010 VL 64 IS 3 BP 413 EP 440 DI 10.2984/64.3.413 PG 28 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 620DZ UT WOS:000279480500006 ER PT J AU Hearty, PJ Olson, SL AF Hearty, Paul J. Olson, Storrs L. TI Geochronology, biostratigraphy, and changing shell morphology in the land snail subgenus Poecilozonites during the Quaternary of Bermuda SO PALAEOGEOGRAPHY PALAEOCLIMATOLOGY PALAEOECOLOGY LA English DT Article DE Bermuda; Land snails; Poecilozonites; Punctuated equilibria; Amino acid geochronology; Biostratigraphy; Morphometrics; Anagenesis ID SEA-LEVEL HISTORY; LAST INTERGLACIAL PERIOD; AMINO-ACID RACEMIZATION; LATE PLEISTOCENE; U-SERIES; STRATIGRAPHY; BAHAMAS; HIGHSTAND; ISLANDS; MARINE AB Shells from over 280 collections representing all known forms of subgenus Poecilozonites (Zonitidae) from Bermuda have been ranked in stratigraphic order and relative-age aminostratigraphy. The samples were first grouped by their source lithostratigraphic unit, with additional refinements being made based on the epimerization ratio D-alloisoleucine/L-isoleucine or A/I from nearly 400 representative individual shells of each of the forms. A plot of A/I frequency defines several modes or "aminozones". The aminozones correlate strongly with defined lithostratigraphy, with some minor variation resulting from less optimally preserved shells. The succession of land snails is ranked over chronological range from the middle and early Pleistocene, with greatest resolution since 500 ka. This >500 ka age-range and density of sampling is among the most extensive for any organism on an oceanic island. Morphological analysis of Poecilozonites demonstrates oscillation and repetition of morphotypes over multiple sea-level cycles. Shells from the small island(s) that formed during interglacial times are generally small and show little variation in form. During glacial periods. when Bermuda reached maximal size, shells are much larger. Extreme variation in shell size and shape occurs at interglacial-glacial transitions in as little as 2-4 ka. Because the subgenus has been endemic to Bermuda for at least ca. 1000 ka, such dramatic and rapid shifts in shell morphology cannot be the result of recolonization from outside sources. An intact and undisturbed 130-ka-long biostratigraphic record of Poecilozonites is contained in a single, vertical 2 m-thick talus accumulation in Admirals Cave that has been dated at high resolution by three independent techniques. The bio- and chronostratigraphy show that snails were very large at the close of glacial stage marine isotope stage (MIS) 6, small during interglacial MIS 5, re-evolved identical large size during the last glaciation (MIS 4-2), and changed abruptly to the small paedomorphic modern form at the onset of the Holocene (MIS 2-1) about 10-12 ka ago. When assessed with care, shells of Poecilozonites may be used as guide fossils for rapid field identification of lithostratigraphic units in surface deposits and as chronological indicators in cave and fissure fills when used in combination with vertebrate remains. (C) 2010 Elsevier B.V. All rights reserved. C1 [Hearty, Paul J.] Univ N Carolina, Dept Environm Studies, Wilmington, NC 28403 USA. [Olson, Storrs L.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Hearty, PJ (reprint author), Univ N Carolina, Dept Environm Studies, Wilmington, NC 28403 USA. EM heartyp@uncw.edu NR 55 TC 10 Z9 10 U1 0 U2 4 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 JUL 1 PY 2010 VL 293 IS 1-2 BP 9 EP 29 DI 10.1016/j.palaeo.2010.04.026 PG 21 WC Geography, Physical; Geosciences, Multidisciplinary; Paleontology SC Physical Geography; Geology; Paleontology GA 626ZJ UT WOS:000280007000002 ER PT J AU Butt, Y AF Butt, Yousaf TI Cosmic rays' origins unclear SO PHYSICS TODAY LA English DT Letter C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Butt, Y (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM ybutt2002@yahoo.com NR 3 TC 0 Z9 0 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0031-9228 J9 PHYS TODAY JI Phys. Today PD JUL PY 2010 VL 63 IS 7 BP 8 EP 8 PG 1 WC Physics, Multidisciplinary SC Physics GA 621RD UT WOS:000279599000001 ER PT J AU Clark, CJ Dudley, R AF Clark, Christopher James Dudley, Robert TI Hovering and Forward Flight Energetics in Anna's and Allen's Hummingbirds SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID OXYGEN-CONSUMPTION; INSECT FLIGHT; AVIAN FLIGHT; BIRD FLIGHT; POWER REQUIREMENTS; WIND-TUNNEL; METABOLISM; AERODYNAMICS; PERFORMANCE; MECHANICS AB Aerodynamic theory predicts that the mechanical costs of flight are lowest at intermediate flight speeds; metabolic costs of flight should trend similarly if muscle efficiency is constant. We measured metabolic rates for nine Anna's hummingbirds (Calypte anna) and two male Allen's hummingbirds (Selasphorus sasin) feeding during flight from a free-standing mask over a range of airspeeds. Ten of 11 birds exhibited higher metabolic costs during hovering than during flight at intermediate airspeeds, whereas one individual exhibited comparable costs at hovering and during forward flight up to speeds of similar to 7 m s(-1). Flight costs of all hummingbirds increased at higher airspeeds. Relative to Anna's hummingbirds, Allen's hummingbirds exhibited deeper minima in the power curve, possibly due to higher wing loadings and greater associated costs of induced drag. Although feeding at a mask in an airstream may reduce body drag and, thus, the contributions of parasite power to overall metabolic expenditure, these results suggest that hummingbird power curves are characterized by energetic minima at intermediate speeds relative to hovering costs. C1 [Clark, Christopher James; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Clark, CJ (reprint author), Yale Univ, Peabody Museum Nat Hist, POB 208106, New Haven, CT 06520 USA. EM christopher.clark@yale.edu NR 38 TC 22 Z9 23 U1 3 U2 29 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD JUL-AUG PY 2010 VL 83 IS 4 BP 654 EP 662 DI 10.1086/653477 PG 9 WC Physiology; Zoology SC Physiology; Zoology GA 611BI UT WOS:000278785100009 PM 20455711 ER PT J AU Vernooy, R Haribabu, E Muller, MR Vogel, JH Hebert, PDN Schindel, DE Shimura, J Singer, GAC AF Vernooy, Ronnie Haribabu, Ejnavarzala Muller, Manuel Ruiz Vogel, Joseph Henry Hebert, Paul D. N. Schindel, David E. Shimura, Junko Singer, Gregory A. C. TI Barcoding Life to Conserve Biological Diversity: Beyond the Taxonomic Imperative SO PLOS BIOLOGY LA English DT Editorial Material C1 [Vernooy, Ronnie] Int Dev Res Ctr, Agr & Environm Program Area, Ottawa, ON, Canada. [Haribabu, Ejnavarzala] Univ Hyderabad, Dept Sociol, Hyderabad 500134, Andhra Pradesh, India. [Muller, Manuel Ruiz] Peruvian Soc Environm Law SPDA, Int Affairs & Biodivers Program, Lima, Peru. [Vogel, Joseph Henry] Univ Puerto Rico, Dept Econ, Rio Piedras, PR USA. [Hebert, Paul D. N.; Singer, Gregory A. C.] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Schindel, David E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Shimura, Junko] Secretariat Convent Biol Divers, Montreal, PQ, Canada. RP Vernooy, R (reprint author), Int Dev Res Ctr, Agr & Environm Program Area, Ottawa, ON, Canada. EM rvernooy@idrc.ca RI Hebert, Paul/C-4161-2013 OI Hebert, Paul/0000-0002-3081-6700 NR 10 TC 27 Z9 31 U1 1 U2 17 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1544-9173 J9 PLOS BIOL JI PLoS. Biol. PD JUL PY 2010 VL 8 IS 7 AR e1000417 DI 10.1371/journal.pbio.1000417 PG 5 WC Biochemistry & Molecular Biology; Biology SC Biochemistry & Molecular Biology; Life Sciences & Biomedicine - Other Topics GA 634CM UT WOS:000280557100005 PM 20644709 ER PT J AU Sengupta, B Stemmler, M Laughlin, SB Niven, JE AF Sengupta, Biswa Stemmler, Martin Laughlin, Simon B. Niven, Jeremy E. TI Action Potential Energy Efficiency Varies Among Neuron Types in Vertebrates and Invertebrates SO PLOS COMPUTATIONAL BIOLOGY LA English DT Article ID SODIUM-CALCIUM EXCHANGE; NETWORK MODEL; K+ CHANNEL; BRAIN; INACTIVATION; AXON; EVOLUTION; DENSITY; CELLS AB The initiation and propagation of action potentials (APs) places high demands on the energetic resources of neural tissue. Each AP forces ATP-driven ion pumps to work harder to restore the ionic concentration gradients, thus consuming more energy. Here, we ask whether the ionic currents underlying the AP can be predicted theoretically from the principle of minimum energy consumption. A long-held supposition that APs are energetically wasteful, based on theoretical analysis of the squid giant axon AP, has recently been overturned by studies that measured the currents contributing to the AP in several mammalian neurons. In the single compartment models studied here, AP energy consumption varies greatly among vertebrate and invertebrate neurons, with several mammalian neuron models using close to the capacitive minimum of energy needed. Strikingly, energy consumption can increase by more than ten-fold simply by changing the overlap of the Na(+) and K(+) currents during the AP without changing the APs shape. As a consequence, the height and width of the AP are poor predictors of energy consumption. In the Hodgkin-Huxley model of the squid axon, optimizing the kinetics or number of Na(+) and K(+) channels can whittle down the number of ATP molecules needed for each AP by a factor of four. In contrast to the squid AP, the temporal profile of the currents underlying APs of some mammalian neurons are nearly perfectly matched to the optimized properties of ionic conductances so as to minimize the ATP cost. C1 [Sengupta, Biswa; Laughlin, Simon B.; Niven, Jeremy E.] Univ Cambridge, Dept Zool, Neural Circuit Design Grp, Cambridge, England. [Sengupta, Biswa; Stemmler, Martin] LMU Munchen, BCCN Munich, Martinsried, Germany. [Niven, Jeremy E.] Smithsonian Trop Res Inst, Panama City, Panama. RP Sengupta, B (reprint author), Univ Cambridge, Dept Zool, Neural Circuit Design Grp, Cambridge, England. EM jen22@hermes.cam.ac.uk RI Niven, Jeremy/A-5883-2011; Sengupta, Biswa/N-9674-2014; OI Sengupta, Biswa/0000-0002-1377-6583; Laughlin, Simon/0000-0003-4659-6543 FU BBSRC; GlaxoSmithKline; BMBF; Royal Society; Frank Levinson Family Foundation FX This study was supported by the BBSRC (BS, SBL), GlaxoSmithKline (BS), BMBF (MS), the Royal Society (JEN) and the Frank Levinson Family Foundation to the STRI Laboratory of Behavior and Evolutionary Neurobiology (JEN). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 41 TC 87 Z9 87 U1 0 U2 37 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1553-734X J9 PLOS COMPUT BIOL JI PLoS Comput. Biol. PD JUL PY 2010 VL 6 IS 7 AR e1000840 DI 10.1371/journal.pcbi.1000840 PG 16 WC Biochemical Research Methods; Mathematical & Computational Biology SC Biochemistry & Molecular Biology; Mathematical & Computational Biology GA 633TG UT WOS:000280528300009 PM 20617202 ER PT J AU Smith, DR AF Smith, David R. TI FIVE NEW SPECIES OF ACORDULECERA SAY (HYMENOPTERA: PERGIDAE) FROM ARIZONA AND CALIFORNIA, THE FIRST RECORDS OF THE FAMILY FROM SOUTHWESTERN UNITED STATES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE sawflies; Symphyta; Nearctic AB Five new species of Acordulecera Say are described from the southwestern United States: Acordulecera sonoita, A. grisselli, and A. whittelli from southern Arizona, and A. algodones and A. kimseyi from southern California. These are the first records for the family Pergidae from Arizona and California. A key is given for the currently recognized North American and Mexican species. 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 37912,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov FU U.S. Bureau of Land Management [BAA033001/BAA06044] FX I express thanks to E. E. Grissell (Sonoita, AZ) and L. S. Kimsey (University of California, Davis) for providing specimens. For allowing collections, I thank Linda Kennedy (Director, National Audubon Society, Appleton-Whittell Research Ranch, Elgin, AZ). The work on the Algodones Dunes area in California was funded by the U.S. Bureau of Land Management under an Assistance Agreement, BAA033001/BAA06044 issued under the umbrella Cooperative Agreement for the Californian Cooperative Ecosystems Unit (CESU). Michele Touchet (Systematic Entomology Laboratory, USDA, Washington, D.C.), helped with the photographs. I thank the following for review of the manuscript: N. M. Schiff (U.S. Forest Service, Stoneville, MS) and J. Prena and T. J. Henry (Systematic Entomology Laboratory, USDA, Washington, D.C.). NR 8 TC 3 Z9 3 U1 0 U2 0 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 JUL PY 2010 VL 112 IS 3 BP 410 EP 422 DI 10.4289/0013-8797.112.3.410 PG 13 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800004 ER PT J AU Smith, DR AF Smith, David R. TI THE WOODWASP GENUS ERIOTREMEX (HYMENOPTERA: SIRICIDAE), A REVIEW AND A NEW SPECIES FROM MALAYSIA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Review DE southeastern Asia; Indonesia; Papua New Guinea; wood borers ID RECORD; JAPAN AB Eriotremex magnificus, n. sp., from Malaysia is described and illustrated. Current information, including some new distributional records, is given for the other 12 species currently placed in the genus, and a revised key to species is provided. 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 dave.smith@ars.usda.gov NR 26 TC 1 Z9 1 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2010 VL 112 IS 3 BP 423 EP 438 DI 10.4289/0013-8797.112.3.423 PG 16 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800005 ER PT J AU Smith, DR Goulet, H Sikes, DS AF Smith, David R. Goulet, Henri Sikes, Derek S. TI A NEW PSEUDODINEURA KONOW (HYMENOPTERA: TENTHREDINIDAE) FROM KASATOCHI ISLAND, ALASKA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Nematinae; leafminer; Anemone AB Pseudodineura kasatochi Smith, n. sp., is described from Kasatochi Island, Alaska. This is the first record of a species of Pseudodineura from Alaska. The specimen was collected prior to a volcanic eruption in August 2008 that nearly destroyed all life on the island. It is separated from other Palearctic and Nearctic species of the genus. C1 [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Goulet, Henri] Agr & Agri Food Canada, Ottawa, ON K1A 0C6, Canada. [Sikes, Derek S.] Univ Alaska Museum, Fairbanks, AK 99775 USA. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; henri.goulet@agr.gc.ca; dssikes@alaska.edu FU U. S. Fish and Wildlife Service; Alaska EPSCoR NSF [EPS-0701898]; National Science Foundation [DBI-0847904]; State of Alaska FX Stephen S. Talbot, U. S. Fish and Wildlife Service, Anchorage, AK, provided information on the presence of Anemone on the island. Michele Touchet, Systematic Entomology Laboratory, Washington, DC, helped with the photographs. We also thank Vernon Byrd and Jeff Williams of the U. S. Fish and Wildlife Service, for their help in obtaining funding and transportation aboard the USFWS' vessel the M/V Tiglax. Kelly May, Mary Wyatt, specimen preparators, and volunteers in the University of Alaska Museum, are thanked for their efforts. Additional support is acknowledged from Alaska EPSCoR NSF award #EPS-0701898, National Science Foundation BRC award #DBI-0847904, and the State of Alaska. We appreciate reviews by the following: S. M. Blank, Senckenberg Deutsches Entomologisches Institut, Muncheberg, Germany, and D. A. Nick le and T. J. Henry, Systematic Entomology Laboratory, USDA, Beltsville, MD, and Washington, DC, respectively. NR 14 TC 1 Z9 1 U1 0 U2 0 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 JUL PY 2010 VL 112 IS 3 BP 439 EP 443 DI 10.4289/0013-8797.112.3.439 PG 5 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800006 ER PT J AU Smith, DR Sanchez-Martinez, G Ordaz-Silva, S AF Smith, David R. Sanchez-Martinez, Guillermo Ordaz-Silva, Salvador TI A NEW MONOCTENUS (HYMENOPTERA: DIPRIONIDAE) DAMAGING JUNIPERUS FLACCIDA (CUPRESSACEAE) IN SAN LUIS POTOSI, MEXICO SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE sawfly; juniper; Utah; Arizona; Durango; Guatemala ID SAWFLIES AB Monoctenus sanchezi Smith, n. sp., is described. It was found damaging Juniperus flaccida Schlechtendal (Cupressaceae) in San Luis Potosi, Mexico. This is the second Mexican species of the genus. A review of Monoctenus from southwestern United States, Mexico, and Central America is presented, with M. sadadus Smith a new country record for the United States and new records of the genus for Utah and as far south as Guatemala. C1 [Smith, David R.] ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Sanchez-Martinez, Guillermo] INIFAP Campo Expt Pabellon, Pabellon De Artega 20660, Aguascalientes, Mexico. [Ordaz-Silva, Salvador] Com Estatal Sanidad Vegetal SLP, Tamuin 79200, SLP, Mexico. [Ordaz-Silva, Salvador] Secretaria Desarrollo Agropecuario & Recursos Hid, San Luis Potosi 78380, Mexico. RP Smith, DR (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Natl Museum Nat Hist,Smithsonian Inst, POB 37012,MRC 168, Washington, DC 20013 USA. EM dave.smith@ars.usda.gov; sanchezm.guillermo@inifap.gob.mx NR 12 TC 3 Z9 3 U1 0 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2010 VL 112 IS 3 BP 444 EP 450 DI 10.4289/0013-8797.112.3.444 PG 7 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800007 ER PT J AU Solis, MA AF Solis, M. Alma TI NORTH AMERICAN HERPETOGRAMMA LEDERER, 1863 (LEPIDOPTERA: CRAMBIDAE: SPILOMELINAE): TYPE SPECIMENS AND IDENTITY OF SPECIES IN THE UNITED STATES AND CANADA SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE checklist; lectotypes; pests; southern beet webworm; tropical sod webworm AB Type specimens or the type series of 27 North American Herpetogramma species names were located, mostly in European museums, verified, and dissected. Acharana descripta (Warren) is designated as a new synonym of Herpetogramma phaeopteralis (Guenee). Fifteen lectotypes and 14 paralectotypes are designated where it was deemed necessary to fix and stabilize the current concept of the name. A checklist and a key to nine North American species are provided with photographs of the adults. C1 ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Solis, MA (reprint author), ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, POB 37012,E-517,MRC 168, Washington, DC 20013 USA. EM alma.solis@ars.usda.gov NR 25 TC 4 Z9 4 U1 1 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 JUL PY 2010 VL 112 IS 3 BP 451 EP 463 DI 10.4289/0013-8797.112.3.451 PG 13 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800008 ER PT J AU Henry, TJ Hevel, GF Chordas, SW AF Henry, Thomas J. Hevel, Gary F. Chordas, Stephen W., III TI Additional Records of the Little-Known Corixidea major (Heteroptera: Schizopteridae) from Arkansas and Oklahoma SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Editorial Material C1 [Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. [Chordas, Stephen W., III] Ohio State Univ, Ctr Life Sci, Columbus, OH 43210 USA. RP Henry, TJ (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. EM thomas.henry@ars.usda.gov; hevelg@si.edu; chordas.2@osu.edu NR 10 TC 1 Z9 1 U1 1 U2 2 PU ENTOMOL SOC WASHINGTON PI WASHINGTON PA SMITHSONIAN INSTITUTION DEPT ENTOMOLOGY, WASHINGTON, DC 20560 USA SN 0013-8797 J9 P ENTOMOL SOC WASH JI Proc. Entomol. Soc. Wash. PD JUL PY 2010 VL 112 IS 3 BP 475 EP 477 DI 10.4289/0013-8797-112.3.475 PG 3 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800011 ER PT J AU Myers, J Mathis, WN AF Myers, Janet Mathis, Wayne N. TI Hollis (Holly) Barton Williams 1951-2009 OBITUARY SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Biographical-Item C1 [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. EM mathisw@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 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 JUL PY 2010 VL 112 IS 3 BP 481 EP 482 DI 10.4289/0013-8797-112.3.481 PG 2 WC Entomology SC Entomology GA 652IJ UT WOS:000281996800012 ER PT J AU Apai, D Lagerstrom, J Reid, IN Levay, KL Fraser, E Nota, A Henneken, E AF Apai, Daniel Lagerstrom, Jill Reid, Iain Neill Levay, Karen L. Fraser, Elizabeth Nota, Antonella Henneken, Edwin TI Lessons from a High-Impact Observatory: The Hubble Space Telescope's Science Productivity between 1998 and 2008 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID DEEP FIELD; SPECTROGRAPH; CAMERA AB Almost two decades of continuous operation of the versatile and productive Hubble Space Telescope (HST) provide uniquely well-documented, robust statistics to study the scientific impact of a major astronomical observatory. We compiled a detailed database of refereed articles that use HST data for analysis and show it to be > 95% complete. This HST Publication Database is publicly available and searchable: it contains more than 8700 articles, cited more than 300,000 times in the literature. By cross-linking this data set with our extensive proposal database and NASA's ADS service, we are able to trace the evolution of ideas from the proposal stage through the observations and publication steps to the final impact on the astronomical literature. Here we present a detailed study of HST's performance, including the temporal evolution of the publication rate, the citation statistics, the relative contributions from different program types, the time allocation strategy, and the relative contributions of the HST instruments. We also discuss the properties of typical and very highly-cited articles. By analyzing this complete and well-characterized database, we identify five key features that contribute to the productivity and high impact of the observatory: (1) the time allocation policies; (2) the well-characterized HST archive; (3) the breadth of science projects ranging from the solar system to cosmology; (4) the Director's Discretionary time allocations; (5) the large international user community and its involvement in the observatory's functions. In addition, we find the following general characteristics. Following its launch, HST's productivity has been steadily increasing; 8 yr after launch, HST reached equilibrium between the incoming data volume and the number of published articles that are based on those data. The overall productivity, however, is still steadily increasing due to the increasing number of archival articles. We find that small programs produce more citations per orbit than large programs, but only large programs have the potential to lead to very high-impact articles and data sets with lasting legacy value. We find that while typical HST articles receive the largest number of citations 2-3 yr after publication and exhibit a subsequent decline, the most-cited articles show a qualitatively different citation history. Together these results provide a detailed picture of HST's science productivity and identify key characteristics that contribute to making HST a high-impact observatory. C1 [Apai, Daniel; Levay, Karen L.] Space Telescope Sci Inst, Sci Programs, CSC, Baltimore, MD 21218 USA. [Nota, Antonella] Space Telescope Sci Inst, European Space Agcy, Baltimore, MD 21218 USA. [Henneken, Edwin] Harvard Smithsonian Ctr Astrophys, SAO NASA Astrophys Data Syst, Cambridge, MA 02138 USA. RP Apai, D (reprint author), Space Telescope Sci Inst, Sci Programs, CSC, 3700 San Martin Dr, Baltimore, MD 21218 USA. RI Henneken, Edwin/F-9475-2010; OI Henneken, Edwin/0000-0003-4264-2450 NR 20 TC 8 Z9 8 U1 0 U2 1 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUL PY 2010 VL 122 IS 893 BP 808 EP 826 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 615DM UT WOS:000279112700007 ER PT J AU Kersey, DC Wildt, DE Brown, JL Snyder, RJ Huang, Y Monfort, SL AF Kersey, David C. Wildt, David E. Brown, Janine L. Snyder, Rebecca J. Huang, Yan Monfort, Steven L. TI Unique biphasic progestagen profile in parturient and non-parturient giant pandas (Ailuropoda melanoleuca) as determined by faecal hormone monitoring SO REPRODUCTION LA English DT Article ID BEAR URSUS-AMERICANUS; MINK MUSTELA-VISON; DELAYED IMPLANTATION; BLACK BEARS; PROGESTERONE CONCENTRATIONS; CHRYSOCYON-BRACHYURUS; LUTEINIZING-HORMONE; STEROID METABOLITES; SERUM PROGESTERONE; EMBRYONIC DIAPAUSE AB The luteal phase of the giant panda has been exclusively assessed by studying urinary hormone patterns in a very few individuals. To better understand hormonal dynamics of protracted progestagen excretion in this endangered species, we monitored hormonal metabolites in the fibrous faeces of multiple females in the USA and China. Giant pandas that were anoestrual during the breeding season excreted baseline progestagen throughout the year. In contrast, there were two distinctive periods when progestagen excretion increased in females that experienced behavioural oestrus, the first being modest, lasting for 61-122 days, and likely reflecting presumptive ovulation. This increase was far surpassed by a secondary rise in progestagen excretion associated with a rejuvenated luteal capacity or hormone production from an extra-gonadal source. The duration of this 'secondary' rise in progestagen excretion averaged similar to 45 days and terminated in a decline to baseline coincident with parturition or the end of a non-parturient luteal interval. Data revealed that, even with a complex, biphasic progestagen profile, the longitudinal patterns produced by giant pandas were relatively consistent among animals and across years within individuals. However, progestagen excretion patterns throughout this period could not be used to discriminate among non-pregnant, pregnant or pseudopregnant states. Reproduction (2010) 140 183-193 C1 [Kersey, David C.; Wildt, David E.; Brown, Janine L.; Monfort, Steven L.] Ctr Species Survival, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Snyder, Rebecca J.] Zoo Atlanta, Atlanta, GA 30315 USA. [Huang, Yan] Wolong Nat Reserve, China Conservat & Res Ctr Giant Panda, Wenchuan 623006, Sichuan, Peoples R China. RP Kersey, DC (reprint author), Western Univ Hlth Sci, Coll Vet Med, Pomona, CA 91766 USA. EM dkersey@westernu.edu FU National Zoo FX This study was funded by Friends of the National Zoo. NR 67 TC 15 Z9 16 U1 0 U2 7 PU BIOSCIENTIFICA LTD PI BRISTOL PA EURO HOUSE, 22 APEX COURT WOODLANDS, BRADLEY STOKE, BRISTOL BS32 4JT, ENGLAND SN 1470-1626 J9 REPRODUCTION JI Reproduction PD JUL PY 2010 VL 140 IS 1 BP 183 EP 193 DI 10.1530/REP-10-0003 PG 11 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 616XN UT WOS:000279244900019 PM 20406954 ER PT J AU Broun, E AF Broun, Elizabeth TI JEANNE-CLAUDE'S ROLE SO SMITHSONIAN LA English DT Letter C1 Smithsonian Amer Art Museum, Washington, DC USA. RP Broun, E (reprint author), Smithsonian Amer Art Museum, Washington, DC 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 JUL-AUG PY 2010 VL 41 IS 4 SI SI BP 6 EP 6 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 619HY UT WOS:000279421800002 ER PT J AU Clough, GW AF Clough, G. Wayne TI Forward Thinking 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 JUL-AUG PY 2010 VL 41 IS 4 SI SI BP 16 EP 16 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 619HY UT WOS:000279421800007 ER PT J AU Rabenhorst, MC Megonigal, JP Keller, J AF Rabenhorst, Martin C. Megonigal, J. Patrick Keller, Jason TI Synthetic Iron Oxides for Documenting Sulfide in Marsh Pore Water SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID REDUCTION; INDICATOR; SOILS; IRIS AB In estuarine systems, naturally occurring soluble S(2-) is an indicator of anaerobic decomposition by the SO(4)(2-) reduction pathway and can, at high concentrations, be detrimental to plant communities. Depth distributions of soluble S(2-) in marsh pore water are typically measured using either equilibrium dialysis samplers (peepers) or pore water extractors (sippers). The former technique provides concentrations equilibrated over one or more weeks at centimeter-scale resolution, while the latter allows rapid sampling and analysis but with a coarser vertical resolution (5-10 cm). We report on a novel technology for documenting marsh pore water S(2-) concentrations based on reactive synthetic Fe oxides and image analysis, which allows rapid sampling but still captures small-scale spatial resolution. During the last few years, this new technology associated with synthetic Fe oxides known as IRIS (Indicator of Reduction In Soils) has been developed to aid in documenting reducing conditions in wetland soils. Our recent work has shown that IRIS technology can be used to document and measure H(2)S levels in marsh soil pore water. The data obtained can provide detailed, quantitative information on S(2-) concentrations with millimeter-scale spatial resolution. C1 [Rabenhorst, Martin C.] Univ Maryland, Dept Environm Sci & Technol, College Pk, MD 20740 USA. [Megonigal, J. Patrick; Keller, Jason] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Keller, Jason] Chapman Univ, Dept Biol Sci, Orange, CA 92866 USA. RP Rabenhorst, MC (reprint author), Univ Maryland, Dept Environm Sci & Technol, 1109 HJ Patterson Hall, College Pk, MD 20740 USA. EM mrabenho@umd.edu NR 16 TC 9 Z9 9 U1 5 U2 11 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD JUL-AUG PY 2010 VL 74 IS 4 BP 1383 EP 1388 DI 10.2136/sssaj2009.0435 PG 6 WC Soil Science SC Agriculture GA 618NW UT WOS:000279363600033 ER PT J AU Redden, KM Herendeen, PS Wurdack, KJ Bruneau, A AF Redden, Karen M. Herendeen, Patrick S. Wurdack, Kenneth J. Bruneau, Anne TI Phylogenetic Relationships of the Northeastern South American Brownea Clade of Tribe Detarieae (Leguminosae: Caesalpinioideae) based on Morphology and Molecular Data SO SYSTEMATIC BOTANY LA English DT Article DE Elizabetha; Heterostemon; ITS; morphology; Paloue; trial ID NUCLEAR RIBOSOMAL DNA; TRANSCRIBED SPACER SEQUENCES; COMPARATIVE FLORAL ONTOGENY; CHLOROPLAST TRNL INTRON; SENNA LEGUMINOSAE; EVOLUTION; GENUS; INCONGRUENCE; TAXA; SUPPRESSION AB The legume subfamily Caesalpinioideae is a paraphyletic grade, within which are nested the monophyletic subfamilies Mimosoideae and Papilionoideae Although higher level relationships within Caesalpimoideae are now better understood, few studies have examined generic and species level relationships A morphological and molecular phylogenehc analysis of selected members of the Brownea clade (Detarieae Caesalpinioideae) is presented here, focusing on relationships within and among the genera Elizabetha, Heterostemon, Paloveopsis, and Paloue Morphological characters (125) and DNA sequence data from the plastid trill., unroll and nuclear ITS were used to reconstruct phlogenenc relationships These results indicate that (1) Heterostemon is monophyletic, (2) the majority of Elizabetha species form a poorly supported, monophyletic group sister to Pillow, and (3) Priloveopsis is nested within Paloue Intergeneric hybridization between species of Palouc and Elizabetha has been identified and traditional generic, species, and intraspecies boundaries are assessed and reevaluated using the results of the combined phylogenetic analysis C1 [Redden, Karen M.; Wurdack, Kenneth J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Herendeen, Patrick S.] Chicago Bot Garden, Glencoe, IL 60022 USA. [Bruneau, Anne] Univ Montreal, Inst Rech Biol Vegetale, Montreal, PQ H1X 2B2, Canada. [Bruneau, Anne] Univ Montreal, Dept Sci Biol, Montreal, PQ H1X 2B2, Canada. RP Redden, KM (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166,POB 37012, Washington, DC 20013 USA. FU National Science Foundation [DEB-0408041, DEB-0316375]; Smithsonian Institution's Biodiversity; Natural Sciences and Engineering Research Council of Canada; New York Botanical Garden; Sigma XI-George Washington University chapter FX We thank numerous collaborators for their Ideas, discussions, expertise and observations, in particular, Gwilym Lewis, Bente Klitgaard, Hannah Banks, Vicki Funk, Carol Kelloff, and Tom Hollowell We thank the two anonymous reviewers and the editors for their constructive comments on an earlier version of this manuscript We thank the herbaria that provided access to collections and facilitated loans, especially BM, F, K, MO, NY, P. U, US, and WAG We also thank the governments, agencies, and universities of Guyana and Venezuela for facilitating the field work in those countries K Redden would like to thank her Amerindian guides and counterparts who spent months in the field, especially Claudius Perry, Dave Singh, and Paul Ben)amin This work was supported by the National Science Foundation (Dissertation Improvement Grant DEB-0408041, and DEB-0316375), Smithsonian Institution's Biodiversity of the Guianas Program, the Natural Sciences and Engineering Research Council of Canada (grant to AB), New York Botanical Garden (Rupert Barneby Award, to KR for 2004), and Sigma XI-George Washington University chapter This is contribution number 152 in the Smithsonian's Biological Diversity of the Guiana Shield Program publication series NR 70 TC 5 Z9 5 U1 2 U2 9 PU AMER SOC PLANT TAXONOMISTS PI LARAMIE PA UNIV WYOMING, DEPT BOTANY 3165, 1000 E UNIVERSITY AVE, LARAMIE, WY 82071 USA SN 0363-6445 EI 1548-2324 J9 SYST BOT JI Syst. Bot. PD JUL-SEP PY 2010 VL 35 IS 3 BP 524 EP 533 PG 10 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 647MS UT WOS:000281623200008 ER PT J AU Ceruzzi, PE AF Ceruzzi, Paul E. TI When Dreams Become Real SO TECHNOLOGY AND CULTURE LA English DT Editorial Material C1 Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Ceruzzi, PE (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2010 VL 51 IS 3 BP 675 EP 679 PG 5 WC History & Philosophy Of Science SC History & Philosophy of Science GA 640YG UT WOS:000281089600006 ER PT J AU Ghazoul, J Butler, RA Mateo-Vega, J Koh, LP AF Ghazoul, Jaboury Butler, Rhett A. Mateo-Vega, Javier Koh, Lian Pin TI REDD: a reckoning of environment and development implications SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Article ID BRAZILIAN AMAZONIA; AVOIDED DEFORESTATION; BIODIVERSITY; CONSERVATION; EMISSIONS; FORESTS; MALARIA; THREATS AB Reducing Emissions from Deforestation (REDD) aims to curb carbon emissions from deforestation by financially compensating forest owners. However, compensation based on the opportunity costs of REDD might underestimate true costs by failing to account for downstream economic values of current land uses, including employment and wealth generated by processing and service industries. A comprehensive analysis of REDD impacts should also include sociopolitical impacts. REDD might exclude people from forest land, causing demographic shifts, and the declining tax revenues from commodity production and associated industries might be a disincentive to government investment in forested regions to the detriment of forest communities and regional development. We argue for the need to recognize and appropriately compensate the full range of economic, social and political net costs of REDD. C1 [Ghazoul, Jaboury; Koh, Lian Pin] ETH, Inst Terr Ecosyst, CH-8092 Zurich, Switzerland. [Butler, Rhett A.] Mongabay Com, Menlo Pk, CA 94026 USA. [Mateo-Vega, Javier] Yale Univ, Yale Sch Forestry & Environm Studies, Environm Leadership & Training Initiat, New Haven, CT 06511 USA. [Mateo-Vega, Javier] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Ghazoul, J (reprint author), ETH, Inst Terr Ecosyst, CHN G 73-1,Univ Str 16, CH-8092 Zurich, Switzerland. EM jaboury.ghazoul@env.ethz.ch RI Koh, Lian Pin/A-5794-2010 OI Koh, Lian Pin/0000-0001-8152-3871 NR 41 TC 80 Z9 82 U1 4 U2 45 PU ELSEVIER SCIENCE LONDON PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 0169-5347 J9 TRENDS ECOL EVOL JI Trends Ecol. Evol. PD JUL PY 2010 VL 25 IS 7 BP 396 EP 402 DI 10.1016/j.tree.2010.03.005 PG 7 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 620WI UT WOS:000279531700005 PM 20417579 ER PT J AU Benjamin, SP AF Benjamin, Suresh P. TI Revision and cladistic analysis of the jumping spider genus Onomastus (Araneae: Salticidae) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE biodiversity; climate change; hotspots; India; South-East Asia; Sri Lanka AB The jumping spider genus Onomastus Simon, 1900 is revised. Four new species: Onomastus indra sp. nov., Onomastus kaharian sp. nov., Onomastus pethiyagodai sp. nov., and Onomastus rattotensis sp. nov. are described. Parsimony analysis of 26 morphological characters supported the monophyly of Onomastus. Lyssomanes is sister to Onomastus. Onomastus separates into two clades: the widespread South-East Asia clade and the South Asia clade. The South Asia clade is restricted to the Sri Lanka Western Ghats biodiversity hotspot. Species of the South Asia clade appear to be spot endemics, highly in danger of extinction because of habitat loss and climate change. Male palps are complex and species-specific, suggesting rapid divergent evolution. (C) 2010 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 159, 711-745. doi: 10.1111/j.1096-3642.2009.00580.x C1 [Benjamin, Suresh P.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Benjamin, SP (reprint author), Inst Fundamental Studies, Hantana Rd, Kandy, Sri Lanka. EM suresh.benjamin@gmail.com FU Smithsonian Institution FX This study was supported by a Smithsonian Institution postdoctoral fellowship and my personal funds. I am indebted to Christa L. Deeleman-Reinhold and E. J. van Nieukerken (RMNH) for kindly providing a substantial part of the specimens examined in this study. Thanks to Christine Rollard and Elise-Anne Leguin (MNHN) for providing E. Simon's types, to Jonathan Coddington and Dana De Roche (USNM) for providing access to additional material, to Dr Akio Tanikawa for providing specimens of O. kanoi, to Janet Beccaloni (BMNH) for providing the type of O. complexipalpis, to Charles Grisworld (CAS) for providing me with an undescribed species of Onomastus from India, and to Mr A. H. Sumanasena (Department of Wild Life Conservation, Colombo) for providing a research permit to collect in Sri Lanka. I want to express my gratitude to my brother Donald Benjamin and my student Ziyard Jaleel (Open University of Sri Lanka) and Sudath V. Nanayakkara for accompanying me during fieldwork in Sri Lanka. NR 27 TC 8 Z9 11 U1 0 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD JUL PY 2010 VL 159 IS 3 BP 711 EP 745 DI 10.1111/j.1096-3642.2009.00580.x PG 35 WC Zoology SC Zoology GA 627RE UT WOS:000280058500004 ER PT J AU Velazco, PM Gardner, AL Patterson, BD AF Velazco, Paul M. Gardner, Alfred L. Patterson, Bruce D. TI Systematics of the Platyrrhinus helleri species complex (Chiroptera: Phyllostomidae), with descriptions of two new species SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Neotropics; bats; geometric morphometrics; molecular; morphology ID GEOMETRIC MORPHOMETRICS; SHAPE; PHYLOGENETICS; BATS AB Platyrrhinus is a diverse genus of small to large phyllostomid bats characterized by a comparatively narrow uropatagium thickly fringed with hair, a white dorsal stripe, comparatively large inner upper incisors that are convergent at the tips, and three upper and three lower molars. Eighteen species are currently recognized, the majority occurring in the Andes. Molecular, morphological, and morphometric analyses of specimens formerly identified as Platyrrhinus helleri support recognition of Platyrrhinus incarum as a separate species and reveal the presence of two species from western and northern South America that we describe herein as new (Platyrrhinus angustirostris sp. nov. from eastern Colombia and Ecuador, north-eastern Peru, and Venezuela and Platyrrhinus fusciventris sp. nov. from Guyana, Suriname, French Guiana, Trinidad and Tobago, northern Brazil, eastern Ecuador, and southern Venezuela). These two new species are sister taxa and, in turn, sister to Platyrrhinus incarum. (C) 2010 The Linnean Society of London, Zoological journal of the Linnean Society, 2010, 159, 785-812. doi: 10.1111/j.1096-3642.2009.00610.x C1 [Velazco, Paul M.; Patterson, Bruce D.] Field Museum Nat Hist, Dept Zool, Chicago, IL 60605 USA. [Velazco, Paul M.] Univ Illinois, Dept Biol Sci, Chicago, IL 60607 USA. [Gardner, Alfred L.] Smithsonian Inst, USGS Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, MRC 111, Washington, DC 20013 USA. RP Velazco, PM (reprint author), Amer Museum Nat Hist, Dept Mammal, Cent Pk W & 79th St, New York, NY 10024 USA. EM pvelazco@amnh.org OI Patterson, Bruce D./0000-0002-2249-7260 FU Pritzker Foundation; American Society of Mammalogists; Ellen Thorne Smith Fund; Barbara E. Brown Fund for Mammal Research; Lester Armour Graduate Fellowship; Smithsonian Institution; Ernest Mayr Travel Grant in Animal Systematics; University of Illinois at Chicago FX This study was part of P. M. V.'s dissertation submitted to the University of Illinois at Chicago as partial fulfilment of his doctoral degree. P. M. V. thanks committee members M. Ashley, H. F. Howe, R. Mason-Gamer, R. H. Ree, and B. D. Patterson. The following curators and collection staff graciously provided access to specimens and tissues under their care: Nancy B. Simmons, Julie Feinstein (the Ambrose Monell Cryo Collection at the AMNH); Daphne M. Hills and Paula Jenkins (BMNH); Gustavo A. B. da Fonseca, Raquel Texeira de Moura, Valeria C. Tavares, Yuri Leite, and Leonora Pires Costa (DZ-UFMG); Bill Stanley and John Phelps (FMNH); J. Enrique Castillo (IAvH-M); Yaneth Munoz-Saba (ICN); Robb T. Brumfield, Donna L. Dittmann (LSUMZ, Collection of Genetic Resources); Judith Chupasko (MCZ); Victor Pacheco (MUSM); James L. Patton, Carla Cicero (MVZ); Judith L. Eger, Burton K. Lim (ROM); Robert J. Baker, Heath J. Garner (TTU, TK); Philip Myers (UMMZ); Linda K. Gordon, James G. Mead (USNM), and Suzanne C. Peurach (USGS-PWRC); Oscar Murillo Garcia (UV); Hendrik Turni and Robert Asher (ZMB). Sequencing was carried out in the Field Museum's Pritzker Laboratory for Molecular Systematics and Evolution, operated with support from the Pritzker Foundation. Photographs of skulls (Figs 6-8) were taken by Cristian Martinez with a Microptics ML Macro XLT digital imaging system. Betty Strack (FMNH) assisted with the scanning electron microscope photography. Valeria C. Tavares provided measurements for some Brazilian specimens. Robert Reynolds and two anonymous reviewers provided valuable comments, suggestions, and additional insights on an earlier version of this manuscript that greatly improved the quality of the final work. All experimental protocols involving mammals were approved by the University of Illinois at Chicago Institutional Animal Care Committee, approval code ACC no. 06-146. Many of the specimens were collected with NSF support (DEB 9870191 to Bruce D. Patterson and colleagues; OISE 0630149 to B. D. P. and P. M. V.). The research was also supported by a Grant-in-Aid of Research from the American Society of Mammalogists, the Ellen Thorne Smith Fund (FMNH), Barbara E. Brown Fund for Mammal Research (FMNH), the Lester Armour Graduate Fellowship (FMNH), the Smithsonian Institution Pre-doctoral Fellowship (USNM), Ernest Mayr Travel Grant in Animal Systematics (MCZ), The Albert R. and Alma Shadle Fellowship in Mammalogy from the American Society of Mammalogists, and the Provost's Award for Graduate Research from the University of Illinois at Chicago. NR 33 TC 20 Z9 30 U1 3 U2 25 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4082 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD JUL PY 2010 VL 159 IS 3 BP 785 EP 812 DI 10.1111/j.1096-3642.2009.00610.x PG 28 WC Zoology SC Zoology GA 627RE UT WOS:000280058500006 ER PT J AU Puerta-Pinero, C Sanchez-Miranda, A Leverkus, A Castro, J AF Puerta-Pinero, C. Sanchez-Miranda, A. Leverkus, A. Castro, J. TI Management of burnt wood after fire affects post-dispersal acorn predation SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Post-fire restoration; Quercus ilex subsp ballota; Salvage logging; Slash management; Sierra Nevada National Park; Spatial analysis ID QUERCUS-ILEX; SEED PREDATION; SPATIAL-DISTRIBUTION; MEDITERRANEAN OAK; SUS-SCROFA; RECRUITMENT; DISPERSAL; PATTERNS; FORESTS; RODENTS AB The management of burnt wood after a fire may affect seed predation by vertebrates due to the change produced in habitat structure We analyze the effect of burnt wood management on post-dispersal seed predation in the Holm oak Three plots were established in a burnt forest, with three treatments per plot (1) non-intervention (NI. all trees left standing). (2) "partial cut plus lopping" (PCL, felling 90% of trees, cutting their main branches, leaving all the biomass in situ). and (3) "salvage logging" (SL, felling the logs for their removal and masticating the woody debris) Acorns were buried to mimic dispersal by jays or rodents two and three years after fire, with two trials per year (7200 monitored acorns), and the predation rate was evaluated until the time of seedling emergence The spatial patterns of acorn predation were assessed by computing a transformed-Ripley's K function and Moran's I correlograms. There was a large spatial and temporal variability in acorn predation, with differences among trials, plots, and replicates within treatments and plots. Overall. PCL showed the lowest predation values (83 0% versus 874 in NI and 88.0 in SL). Predator species (mice versus wild boar) also differed among treatments, wild boar having a negligible effect in PCL. presumably due to the physical barrier of felled logs and branches The results support that. (1) salvage logging offers no advantage against predators and (2) that post-fire burnt wood management alters the guild of acorn predators and may reshape the pattern of seedling establishment (C) 2010 Elsevier B V All rights reserved. C1 [Puerta-Pinero, C.; Sanchez-Miranda, A.; Leverkus, A.; Castro, J.] Univ Granada, Grp Ecol Terr, Dept Ecol, Fac Ciencias, E-18071 Granada, Spain. RP Puerta-Pinero, C (reprint author), Smithsonian Trop Res Inst, Unit 0948, APO, AA 34002 USA. 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 Organism Autonomo de Parques Nacionales [10/2005]; Ministerio de Ciencia e Innovacion (Spanish government) [CGL2008-01671]; University of Granada; Fundacion Caja Madrid FX We thank the Direction of the Natural and National Parks of Sierra Nevada, the Consejeria de Medio Ambiente of Granada (Junta de Andalucia) and the Empresa de Gestion Media Ambiental S.A. (EGMASA) for coordinating and implementing the field treatments, and for all the technical, material, and personal support they have provided. We thank Sara Maranon-Jimenez, Ramon Ruiz Puche and Enrique Perez Sanchez-Canete for field assistance. This study was supported by the project 10/2005 from the Organism Autonomo de Parques Nacionales and project CGL2008-01671 from Ministerio de Ciencia e Innovacion (Spanish government). CPP and AL attained postdoctoral and novel researcher fellowships respectively from the University of Granada. CPP currently has as a research grant from Fundacion Caja Madrid. NR 50 TC 11 Z9 11 U1 1 U2 18 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 EI 1872-7042 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD JUN 30 PY 2010 VL 260 IS 3 BP 345 EP 352 DI 10.1016/j.foreco.2010.04.023 PG 8 WC Forestry SC Forestry GA 621ME UT WOS:000279582100013 ER PT J AU Bastien-Henri, S Park, A Ashton, M Messier, C AF Bastien-Henri, Sara Park, Andrew Ashton, Mark Messier, Christian TI Biomass distribution among tropical tree species grown under differing regional climates SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Biomass distribution; Size effect; Aitchison transformation; Site condition; Panama; Native tree species ID PRECIPITATION GRADIENT; COSTA-RICA; FOREST; ALLOCATION; LIGHT; PANAMA; PATTERNS; SAPLINGS; LEAF; FERTILIZATION AB In the Neotropics, there is a growing interest in establishing plantations of native tree species for commerce, local consumption, and to replant on abandoned agricultural lands Although numerous trial plantations have been established, comparative information on the performance of native trees under different regional environments is generally lacking In this study, we evaluated the accumulation and partitioning of above-ground biomass in 16 native and two exotic tree species growing in replicated species selection trials in Panama under humid and dry regional environments Seven of the 18 species accumulated greater total biomass at the humid site than at the dry site over a two-year period Species-specific biomass partitioning among leaves, branches and trunks was observed. However, a wide range of total biomass found among species (from 1 06 kg for Dipteryx panamensis to 29 84 kg for Acacia mangium at Soberania) justified the used of an Aitchison log ratio transformation to adjust for size When biomass partitioning was adjusted for size, a majority of these differences proved to be a result of the ability of the tree to support biomass components rather than the result of differences in the regional environments at the two sites These findings were confirmed by comparative ANCOVAs on Aitchison-transformed and non-Aitchison-transformed variables. In these comparisons, basal diameter, height and diameter at breast height were robust predictors of biomass for the pooled data from both sites, but Aitchison-transformed variables had little predictive power (C) 2010 Elsevier B V. All rights reserved. C1 [Bastien-Henri, Sara; Messier, Christian] Univ Quebec, Ctr Etud Foret, Dept Sci Biol, Montreal, PQ H3C 3P8, Canada. [Park, Andrew] Univ Winnipeg, Ctr Forest Interdisciplinary Res, Dept Biol, Winnipeg, MB R3B 2E9, Canada. [Ashton, Mark] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. [Ashton, Mark] Smithsonian Trop Res Inst, Native Species Reforestat Project PRORENA, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. RP Bastien-Henri, S (reprint author), Univ Quebec, Ctr Etud Foret, Dept Sci Biol, CP 8888,Succursale Ctr Ville, Montreal, PQ H3C 3P8, Canada. FU Frank Levinson Family Foundation at the Peninsula Community Foundation; Grantham Foundation; School of Forestry and Environmental Studies, Yale University; NSERC; University of Winnipeg FX We are grateful to the management and technical staff of PRORENA for their invaluable assistance in the field, including Norma Cedeno and her team, Emilio Mariscal and his team and Jose Deago. We also want to thank Mark Wishnie and Daisy Dent for scientific advices at the time of field planning Statistical advices provide by Stephane Daigle from Centre d'etude de la Foret (Quebec, Canada) were greatly appreciated. We are also grateful to Ing. Jaime Orozco of Materiales Orozco y Puertas Orozco in Chepo, Republic of Panama for the use of an industrial oven to dry our samples The PRORENA project is jointly managed by the Smithsonian Tropical Research Institute in Panama and the Tropical Resources Institute at Yale University, and financed by The Frank Levinson Family Foundation at the Peninsula Community Foundation, the Grantham Foundation and the School of Forestry and Environmental Studies, Yale University. Funding to Sara Bastien-Henri was provided by NSERC discovery grant to C. Messier and a University of Winnipeg startup grant to A. Park. NR 37 TC 12 Z9 13 U1 1 U2 15 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 JUN 30 PY 2010 VL 260 IS 3 BP 403 EP 410 DI 10.1016/j.foreco.2010.04.035 PG 8 WC Forestry SC Forestry GA 621ME UT WOS:000279582100020 ER PT J AU Baeza, JA Farias, NE Luppi, TA Spivak, ED AF Baeza, J. A. Farias, N. E. Luppi, T. A. Spivak, E. D. TI Refuge size, group living and symbiosis: testing the "resource economic monopolization" hypothesis with the shrimp Betaeus lilianae and description of its partnership with the crab Platyxanthus crenulatus SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Economic monopolization; Group living; Refuge size; Shrimp; Symbiosis ID RHYNCHOCINETES-TYPUS DECAPODA; SNAPPING SHRIMP; SOCIAL MONOGAMY; CLEANER SHRIMP; SEXUAL SELECTION; MATING SYSTEMS; MARINE SHRIMP; SELFISH HERD; CARIDEA; BEHAVIOR AB Theory predicts that refuge size is most relevant in driving the population distribution of marine organisms. Relatively small refuges are expected to harbor single or pairs of conspecifics because defense against intruders is energetically inexpensive. Relatively large shelters should harbor aggregations because guarding behaviors turn energetically expensive. Here, we used the intertidal shrimp Betaeus lilianae to test the hypothesis that species inhabiting large refuges live in aggregations and not solitarily or in pairs. Also, we provided information on the lifestyle of this species, specifically regarding a newly discovered partnership with the crab Platyxanthus crenulatus. In agreement with theoretical expectations. Betaeus lilianae was found living in aggregations in rock pools, characterized by their large size. Shrimp aggregations featured female-biased sex ratios more frequently than expected by chance alone and had no particular complex social structure. There was no effect of pool size and shrimp group size on sex ratio and no significant relationship between the difference in body size of the largest and second largest male and shrimp group size was observed. Relative growth analyses showed that the major claw had positive allometry in males and females but relative claw growth was greater in males. The information above permitted rejecting several alternative hypotheses on the mating system of B. lilianae: it is neither socially monogamous nor features a promiscuous pure-search mating system. Additional studies are needed to reveal the mating behavior of the studied species. Field observations and laboratory experiments demonstrated that B. lilianae associate preferentially with the crab P. crenulatus. Published by Elsevier B.V. C1 [Baeza, J. A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Baeza, J. A.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Baeza, J. A.] Univ Catolica Norte, Fac Ciencias Mar, Dept Biol Marina, Larrondo 1281, Coquimbo, Chile. [Farias, N. E.; Luppi, T. A.; Spivak, E. D.] Univ Nacl Mar del Plata, Fac Ciencias Exactas & Nat, Dept Biol, RA-7600 Mar Del Plata, Argentina. [Farias, N. E.; Luppi, T. A.; Spivak, E. D.] Consejo Nacl Invest Cient & Tecn, Buenos Aires, DF, Argentina. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM baezaa@si.edu OI Baeza, Juan Antonio/0000-0002-2573-6773; Farias, Nahuel Emiliano/0000-0001-5190-370X FU Smithsonian Tropical Research Institute (STRI); Smithsonian Marine Station (SMS); National Geographic Society, USA; Agencia Nacional de Promocion Cientifica Tecnologica [PICT 21757]; CONICET FX JAB is grateful for the support from a Smithsonian Tropical Research Institute (STRI) Postdoctoral Fellowship and a Smithsonian Marine Station (SMS) Postdoctoral Fellowship. The first author thanks the National Geographic Society, USA for funding a research trip to Papua New Guinea and Okinawa, Japan where part of this manuscript was written. This work was partially founded by Agencia Nacional de Promocion Cientifica Tecnologica PICT 21757 granted to EDS. NEF is supported by a CONICET Doctoral Fellowship. This is contribution number 821 of the Smithsonian Marine Station at Fort Pierce. [SS] NR 50 TC 4 Z9 6 U1 3 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 EI 1879-1697 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD JUN 30 PY 2010 VL 389 IS 1-2 BP 85 EP 92 DI 10.1016/j.jembe.2010.03.014 PG 8 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 615AI UT WOS:000279100800011 ER PT J AU Vinogradova, NT Ponte, RM Tamisiea, ME Davis, JL Hill, EM AF Vinogradova, Nadya T. Ponte, Rui M. Tamisiea, Mark E. Davis, James L. Hill, Emma M. TI Effects of self-attraction and loading on annual variations of ocean bottom pressure SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID SEA-LEVEL; GLOBAL OCEAN; MODEL; VARIABILITY AB The impact of self-attraction and loading (SAL) on ocean bottom pressure xi, an effect not previously considered, is analyzed in terms of the mean annual cycle based on decade long estimates of changes in land hydrology, atmospheric pressure, and oceanic circulation. The SAL-related changes in xi occur as a result of deformation of the crust due to loading and self-gravitation of the variable fluid loads. In the absence of SAL, net freshwater input and changes in mean atmospheric pressure over the ocean give rise to a spatially constant xi annual cycle with an amplitude similar to 1-2 cm in equivalent water thickness. Consideration of SAL physics introduces spatial variations that can be significant, particularly around continental boundaries, where the amplitude of deviations can exceed 1 cm. For the spatial variability induced by SAL effects, changes in both land hydrology and atmospheric pressure are important. Effects related to the changing ocean circulation are relatively weaker, apart from a few shallow coastal regions. Comparisons with a few in situ, deep ocean observations indicate that for the most accurate xi estimates, one needs to consider spatially varying SAL-related signals, along with the effects of mean atmospheric pressure and net freshwater input into the oceans. Nevertheless, the most complete estimates, including also effects of ocean circulation, are able to account for only similar to 1/3 of the observed annual variances. Sources of the remaining contribution remain unclear. C1 [Vinogradova, Nadya T.; Ponte, Rui M.] Atmospher & Environm Res Inc, Lexington, MA 02421 USA. [Tamisiea, Mark E.] Natl Oceanog Ctr, Liverpool L3 5DA, Merseyside, England. [Davis, James L.; Hill, Emma M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vinogradova, NT (reprint author), Atmospher & Environm Res Inc, 131 Harwell Ave, Lexington, MA 02421 USA. EM nadya@aer.com RI Hill, Emma/B-7037-2011; Davis, James/D-8766-2013; OI Hill, Emma/0000-0003-0231-5818; Davis, James/0000-0003-3057-477X; Ponte, Rui/0000-0001-7206-6461 FU NASA [NNX07AM77G, NNX08AJ79G]; National Oceanographic Partnership Program; Natural Environment Research Council FX The authors are grateful to Patrick Heimbach for making ECCO model output available. The work was supported in part by NASA grants NNX07AM77G and NNX08AJ79G. Additional support was provided by the National Oceanographic Partnership Program through its sponsorship of the ECCO project and by the Natural Environment Research Council's Oceans 2025 Program. Useful interactions in the course of this work with many ECCO colleagues are gratefully acknowledged. The authors also thank two anonymous reviewers for commenting on the manuscript. NR 23 TC 9 Z9 9 U1 2 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD JUN 29 PY 2010 VL 115 AR C06025 DI 10.1029/2009JC005783 PG 10 WC Oceanography SC Oceanography GA 620UA UT WOS:000279524600003 ER PT J AU Janzen, DH Hallwachs, W Burns, JM AF Janzen, Daniel H. Hallwachs, Winnie Burns, John M. TI A tropical horde of counterfeit predator eyes SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material ID MIMICS; SYRPHIDAE; PATTERN C1 [Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Burns, John M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20013 USA. RP Janzen, DH (reprint author), Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. EM djanzen@sas.upenn.edu NR 24 TC 52 Z9 55 U1 4 U2 36 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 JUN 29 PY 2010 VL 107 IS 26 BP 11659 EP 11665 DI 10.1073/pnas.0912122107 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 618DT UT WOS:000279332300004 PM 20547863 ER PT J AU Vrinceanu, D Sadeghpour, HR AF Vrinceanu, D. Sadeghpour, H. R. TI Spin polarization transfer in ground and metastable helium atom collisions SO NEW JOURNAL OF PHYSICS LA English DT Article ID HE-HE COLLISIONS; IONIZATION; SPECTRUM; XE-129; GAS AB Cross sections and rate constants for total elastic, diffusion and transfer of metastability for collisions between He(1(1)S)-He(2(3)S) and He(1(1)S)-He(2(3)P) atoms over a wide range of energies and temperatures are presented. The rate constant for spin metastability excitation in He(1(1)S)-He(2(3)P) collision is several orders of magnitude larger than that for He(1(1)S)-He(2(3)S) collision at cold temperatures, due to attractive (3)Pi(g) potential interaction. C1 [Vrinceanu, D.] Texas So Univ, Dept Phys, Houston, TX 77004 USA. [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Vrinceanu, D (reprint author), Texas So Univ, Dept Phys, Houston, TX 77004 USA. EM vrinceanud@tsu.edu FU NSF; Texas Southern University FX This work was supported by NSF through a grant to ITAMP and by Texas Southern University Research Seed Grant 2009. NR 42 TC 1 Z9 1 U1 2 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 1367-2630 J9 NEW J PHYS JI New J. Phys. PD JUN 28 PY 2010 VL 12 AR 065039 DI 10.1088/1367-2630/12/6/065039 PG 9 WC Physics, Multidisciplinary SC Physics GA 625ET UT WOS:000279878000026 ER PT J AU Schultze, M Fiess, M Karpowicz, N Gagnon, J Korbman, M Hofstetter, M Neppl, S Cavalieri, AL Komninos, Y Mercouris, T Nicolaides, CA Pazourek, R Nagele, S Feist, J Burgdorfer, J Azzeer, AM Ernstorfer, R Kienberger, R Kleineberg, U Goulielmakis, E Krausz, F Yakovlev, VS AF Schultze, M. Fiess, M. Karpowicz, N. Gagnon, J. Korbman, M. Hofstetter, M. Neppl, S. Cavalieri, A. L. Komninos, Y. Mercouris, Th. Nicolaides, C. A. Pazourek, R. Nagele, S. Feist, J. Burgdoerfer, J. Azzeer, A. M. Ernstorfer, R. Kienberger, R. Kleineberg, U. Goulielmakis, E. Krausz, F. Yakovlev, V. S. TI Delay in Photoemission SO SCIENCE LA English DT Article ID STREAKING MEASUREMENTS; ATTOSECOND PULSES; TIME-DELAY; ELECTRON; DYNAMICS; OPTICS; SCALE AB Photoemission from atoms is assumed to occur instantly in response to incident radiation and provides the basis for setting the zero of time in clocking atomic-scale electron motion. We used attosecond metrology to reveal a delay of 21 +/- 5 attoseconds in the emission of electrons liberated from the 2p orbitals of neon atoms with respect to those released from the 2s orbital by the same 100-electron volt light pulse. Small differences in the timing of photoemission from different quantum states provide a probe for modeling many-electron dynamics. Theoretical models refined with the help of attosecond timing metrology may provide insight into electron correlations and allow the setting of the zero of time in atomic-scale chronoscopy with a precision of a few attoseconds. C1 [Schultze, M.; Gagnon, J.; Hofstetter, M.; Krausz, F.; Yakovlev, V. S.] Univ Munich, Dept Phys, D-85748 Garching, Germany. [Schultze, M.; Fiess, M.; Karpowicz, N.; Gagnon, J.; Korbman, M.; Cavalieri, A. L.; Kienberger, R.; Kleineberg, U.; Goulielmakis, E.; Krausz, F.; Yakovlev, V. S.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Neppl, S.; Ernstorfer, R.; Kienberger, R.] Tech Univ Munich, Dept Phys, D-85748 Garching, Germany. [Komninos, Y.; Mercouris, Th.; Nicolaides, C. A.] Natl Hellen Res Fdn, Inst Theoret & Phys Chem, GR-11635 Athens, Greece. [Pazourek, R.; Nagele, S.; Feist, J.; Burgdoerfer, J.] Vienna Univ Technol, Inst Theoret Phys, A-1040 Vienna, Austria. [Feist, J.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA. [Azzeer, A. M.] King Saud Univ, Dept Phys & Astron, Riyadh 11451, Saudi Arabia. RP Schultze, M (reprint author), Univ Munich, Dept Phys, Coulombwall 1, D-85748 Garching, Germany. EM Martin.Schultze@mpq.mpg.de; Vladislav.Yakovlev@physik.uni-muenchen.de RI Azzeer, Abdallah/A-4542-2011; Nagele, Stefan/E-6938-2011; Goulielmakis, Eleftherios/F-1693-2011; Ernstorfer, Ralph/D-1590-2009; nhrf, tpci/M-8699-2013; Feist, Johannes/J-7394-2012; Yakovlev, Vladislav/C-4091-2015; OI Azzeer, Abdallah/0000-0001-8334-9256; Nagele, Stefan/0000-0003-1213-0294; Goulielmakis, Eleftherios/0000-0003-3386-0245; Ernstorfer, Ralph/0000-0001-6665-3520; Feist, Johannes/0000-0002-7972-0646; Yakovlev, Vladislav/0000-0002-0648-9375; Gagnon, Justin/0000-0001-9133-9541 FU Max Planck Society; Deutsche Forschungsgemeinschaft Cluster of Excellence: Munich Centre for Advanced Photonics; King Saud University-Max-Planck-Institut fur Quantenoptik collaboration; NSF [TG-PHY090031]; Austrian Science Fund (FWF) [FWF-SFB016]; Marie-Curie Reintegration grant [MERG-CT-2007-208643]; Alexander von Humboldt Foundation; ERC FX Supported by the Max Planck Society and the Deutsche Forschungsgemeinschaft Cluster of Excellence: Munich Centre for Advanced Photonics (www.munich-photonics.de) and the King Saud University-Max-Planck-Institut fur Quantenoptik collaboration. Supported in part by NSF through TeraGrid resources provided by the National Institute for Computational Sciences and Texas Advanced Computing Center under grant TG-PHY090031. R.P., S.N., and J.B. acknowledge support from the Austrian Science Fund (FWF) under grant FWF-SFB016. J.F. acknowledges support by NSF through a grant to ITAMP. E. G. acknowledges a Marie-Curie Reintegration grant (MERG-CT-2007-208643). R. K. acknowledges support from the Sofia Kovalevskaja award of the Alexander von Humboldt Foundation and an ERC starting grant. We thank A. Maquet and R. Taieb for fruitful discussions. NR 32 TC 387 Z9 387 U1 8 U2 101 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 JUN 25 PY 2010 VL 328 IS 5986 BP 1658 EP 1662 DI 10.1126/science.1189401 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 615BY UT WOS:000279107400034 PM 20576884 ER PT J AU Kahn, AS Matsumoto, GI Hirano, YM Collins, AG AF Kahn, Amanda S. Matsumoto, George I. Hirano, Yayoi M. Collins, Allen G. TI Haliclystus californiensis, a "new" species of stauromedusa (Cnidaria: Staurozoa) from the northeast Pacific, with a key to the species of Haliclystus SO ZOOTAXA LA English DT Article DE Haliclystus; Staurozoa; stauromedusa; Cnidaria; H. auricula; H. octoradiatus; H. californiensis; H. tenuis; H. stejnegeri; H. borealis ID PHYLUM-CNIDARIA; RDNA DATA; PHYLOGENY; MEDUSOZOA; EVOLUTION AB We describe Haliclystus californiensis, a new species of stauromedusa from the northeast Pacific. Haliclystus californiensis differs from other species within the genus primarily by its horseshoe-shaped anchors, but also by the presence of prominent glandular pads at the base of its outermost secondary tentacles and by geographic range. It has been found from southern to northern California in coastal waters, 10 to 30 m depth. A single specimen of the species was originally described in an unpublished dissertation; nine additional specimens have been found since that time. We provide an annotated key to the known species of Haliclystus. C1 [Collins, Allen G.] Smithsonian Inst, NMFS, Natl Systemat Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kahn, Amanda S.] Moss Landing Marine Labs, Moss Landing, CA 95039 USA. [Matsumoto, George I.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Hirano, Yayoi M.] Chiba Univ, Dept Biol, Grad Sch Sci, Inage Ku, Chiba 2638522, Japan. RP Collins, AG (reprint author), Smithsonian Inst, NMFS, Natl Systemat Lab, Natl Museum Nat Hist, MRC-153,POB 37012, Washington, DC 20013 USA. EM akahn@mlml.calstate.edu; mage@mbari.org; yakko@earth.s.chiba-u.ac.jp; collinsa@si.edu RI Collins, Allen/A-7944-2008 OI Collins, Allen/0000-0002-3664-9691 FU US National Science Foundation [0531779] FX We are grateful to G.F. Gwilliam for the considerable amount of work done to describe this species in his dissertation. We also thank the staff of both the National Museum of Natural History, Smithsonian Institution, and the California Academy of Sciences, for loaning specimens. We thank V. and J. Pearse for bringing the specimen that became the holotype to the attention of AGC and allowing him to observe and photograph the animal alive in their basement. Thanks are due to C. Widmer and J. Mariottini of the Monterey Bay Aquarium for collecting a specimen of H. californiensis and graciously allowing us to study it. L. Ivanov provided a crucial Russian translation, without which the dichotomous key would have been incomplete. N.T. Pierce, L. Scheimer, T.S. Burrow, F. Sommer, J. Watanabe, K.W. Demes, T. Suskiewicz, and A. Alifano provided scuba diving and collection assistance. We are grateful to L. Miranda for providing very helpful feedback on an earlier draft. L. Miranda and C. Mills provided valuable feedback that improved an earlier draft. Finally, we thank the Monterey Bay Aquarium Research Institute and Moss Landing Marine Laboratories for use of facilities and resources. AGC acknowledges support from the US National Science Foundation Assembling the Tree of Life grant 0531779 (to AGC, P. Cartwright, and D. Fautin). NR 32 TC 5 Z9 5 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 JUN 25 PY 2010 IS 2518 BP 49 EP 59 PG 11 WC Zoology SC Zoology GA 615MZ UT WOS:000279140700003 ER PT J AU Sane, SP Srygley, RB Dudley, R AF Sane, Sanjay P. Srygley, Robert B. Dudley, Robert TI Antennal regulation of migratory flight in the neotropical moth Urania fulgens SO BIOLOGY LETTERS LA English DT Article DE insect migration; antenna; flight ID INDUCED AIR-FLOW; DRIFT COMPENSATION; FLYING INSECTS; LEPIDOPTERA; BUTTERFLIES; WINDKOMPENSATION; BIENEN; LOCUST AB Migrating insects use their sensory systems to acquire local and global cues about their surroundings. Previous research on tethered insects suggests that, in addition to vision and cephalic bristles, insects use antennal mechano-sensory feedback to maintain their airspeeds. Owing to the large displacements of migratory insects and difficulties inherent in tracking single individuals, the roles of these sensory inputs have never been tested in freely migrating insects. We tracked individual uraniid moths (Urania fulgens) as they migrated diurnally over the Panama Canal, and measured airspeeds and orientation for individuals with either intact or amputated flagella. Consistent with prior observations that antennal input is necessary for flight control, 59 per cent of the experimental moths could not fly after flagella amputation. The remaining fraction (41%) was flight-capable and maintained its prior airspeeds despite severe reduction in antennal input. Thus, maintenance of airspeeds may not involve antennal input alone, and is probably mediated by other modalities. Moths with amputated flagella could not recover their proper migratory orientations, suggesting that antennal integrity is necessary for long-distance navigation. C1 [Sane, Sanjay P.] TIFR, Natl Ctr Biol Sci, Bangalore, Karnataka, India. [Srygley, Robert B.; Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. [Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94710 USA. RP Sane, SP (reprint author), TIFR, Natl Ctr Biol Sci, GKVK Campus, Bangalore, Karnataka, India. EM sane@ncbs.res.in FU Journal of Experimental Biology FX Journal of Experimental Biology funded travel and stay in Panama (S.P.S.) and Smithsonian Tropical Research Institute provided facilities and logistical support. NR 28 TC 11 Z9 13 U1 2 U2 13 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD JUN 23 PY 2010 VL 6 IS 3 BP 406 EP 409 DI 10.1098/rsbl.2009.1073 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 594SU UT WOS:000277559000034 PM 20181558 ER PT J AU de Juan, J Elosegui, P Nettles, M Larsen, TB Davis, JL Hamilton, GS Stearns, LA Andersen, ML Ekstrom, G Ahlstrom, AP Stenseng, L Khan, SA Forsberg, R AF de Juan, Julia Elosegui, Pedro Nettles, Meredith Larsen, Tine B. Davis, James L. Hamilton, Gordon S. Stearns, Leigh A. Andersen, Morten L. Ekstroem, Goeran Ahlstrom, Andreas P. Stenseng, Lars Khan, S. Abbas Forsberg, Rene TI Sudden increase in tidal response linked to calving and acceleration at a large Greenland outlet glacier SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ANTARCTIC ICE STREAM; WEST ANTARCTICA; VELOCITY; SHEET; ISBRAE; SPEED AB Large calving events at Greenland's largest outlet glaciers are associated with glacial earthquakes and near instantaneous increases in glacier flow speed. At some glaciers and ice streams, flow is also modulated in a regular way by ocean tidal forcing at the terminus. At Helheim Glacier, analysis of geodetic data shows decimeter-level periodic position variations in response to tidal forcing. However, we also observe transient increases of more than 100% in the glacier's responsiveness to such tidal forcing following glacial-earthquake calving events. The timing and amplitude of the changes correlate strongly with the step-like increases in glacier speed and longitudinal strain rate associated with glacial earthquakes. The enhanced response to the ocean tides may be explained by a temporary disruption of the subglacial drainage system and a concomitant reduction of the friction at the ice-bedrock interface, and suggests a new means by which geodetic data may be used to infer glacier properties. Citation: de Juan, J., et al. (2010), Sudden increase in tidal response linked to calving and acceleration at a large Greenland outlet glacier, Geophys. Res. Lett., 37, L12501, doi: 10.1029/2010GL043289. C1 [de Juan, Julia; Elosegui, Pedro] CSIC IEEC, Inst Space Sci, E-08034 Barcelona, Spain. [Nettles, Meredith; Ekstroem, Goeran] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Larsen, Tine B.; Andersen, Morten L.; Ahlstrom, Andreas P.] Geol Survey Denmark & Greenland, DK-1350 Copenhagen, Denmark. [Davis, James L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hamilton, Gordon S.] Univ Maine, Climate Change Inst, Orono, ME 04469 USA. [Stearns, Leigh A.] Univ Kansas, Dept Geol, Lawrence, KS 66045 USA. [Andersen, Morten L.] Univ Copenhagen, Niels Bohr Inst, Ctr Ice & Climate, DK-2100 Copenhagen, Denmark. [Stenseng, Lars; Khan, S. Abbas; Forsberg, Rene] Natl Space Inst, DTU Space, DK-2100 Copenhagen, Denmark. RP de Juan, J (reprint author), CSIC IEEC, Inst Space Sci, E Nexus 201,Gran Capita 2, E-08034 Barcelona, Spain. EM dejuan@ice.csic.es RI Hamilton, Gordon/G-1679-2011; Nettles, Meredith/A-8638-2012; Ekstrom, Goran/C-9771-2012; Andersen, Morten/E-5509-2012; Davis, James/D-8766-2013; Ahlstrom, Andreas Peter/E-5257-2014; Khan, Shfaqat/B-2664-2012; OI Ekstrom, Goran/0000-0001-6410-275X; Davis, James/0000-0003-3057-477X; Ahlstrom, Andreas Peter/0000-0001-8235-8070; Khan, Shfaqat Abbas/0000-0002-2689-8563 FU Spanish Ministry of Science and Innovation (MICINN); Gary Comer Science and Education Foundation; U.S. National Science Foundation; Danish Commission for Scientific Research in Greenland (KVUG); Geological Survey of Denmark and Greenland (GEUS); Geocenter Copenhagen; Danish National Space Center; NASA; CSIC FX This work was supported by the Spanish Ministry of Science and Innovation (MICINN), the Gary Comer Science and Education Foundation, the U.S. National Science Foundation, the Danish Commission for Scientific Research in Greenland (KVUG), the Geological Survey of Denmark and Greenland (GEUS), Geocenter Copenhagen, the Danish National Space Center, and NASA. JdJ acknowledges edges a CSIC pre-doctoral fellowship. GPS equipment and technical support were provided by UNAVCO, Inc. We thank S. Anandakrishnan and an anonymous reviewer, whose comments helped improve the manuscript. NR 32 TC 18 Z9 18 U1 2 U2 22 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD JUN 23 PY 2010 VL 37 AR L12501 DI 10.1029/2010GL043289 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 617UP UT WOS:000279307700003 ER PT J AU Soria, R Hau, GKT Graham, AW Kong, AKH Kuin, NPM Li, IH Liu, JF Wu, KW AF Soria, Roberto Hau, George K. T. Graham, Alister W. Kong, Albert K. H. Kuin, N. Paul M. Li, I-Hui Liu, Ji-Feng Wu, Kinwah TI Discovery of an optical counterpart to the hyperluminous X-ray source in ESO 243-49 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE black hole physics; galaxies: individual: ESO 243-49; ultraviolet: galaxies; X-rays: binaries ID MASS BLACK-HOLE; OLD STELLAR POPULATIONS; ACTIVE GALACTIC NUCLEI; DENSE STAR-CLUSTERS; CHANDRA DEEP SURVEY; GLOBULAR-CLUSTERS; VIRGO CLUSTER; GALAXIES; CATALOG; MODELS AB The existence of black holes of masses similar to 10(2)-10(5)M(circle dot) has important implications for the formation and evolution of star clusters and supermassive black holes. One of the strongest candidates to date is the hyperluminous X-ray source (HLX1), possibly located in the S0- a galaxy ESO 243-49, but the lack of an identifiable optical counterpart had hampered its interpretation. Using the Magellan telescope, we have discovered an unresolved optical source with R = 23.80 +/- 0.25 mag and V = 24.5 +/- 0.3 mag within HLX1's positional error circle. This implies an average X-ray/optical flux ratio similar to 500. Taking the same distance as ESO 243-49, we obtain an intrinsic brightness M(R) = -11.0 +/- 0.3 mag, comparable to that of a massive globular cluster. Alternatively, the optical source is consistent with a main-sequence M star in the Galactic halo (for example an M4.4 star at approximate to 2.5 kpc). We also examined the properties of ESO 243-49 by combining Swift/Ultraviolet/Optical Telescope (UVOT) observations with stellar population modelling. We found that the overall emission is dominated by a similar to 5-Gyr-old stellar population, but the UV emission at approximate to 2000 angstrom is mostly due to ongoing star formation at a rate of similar to 0.03M(circle dot) yr(-1). The UV emission is more intense (at least a 9 sigma enhancement above the mean) north-east of the nucleus, in the same quadrant as HLX1. With the combined optical and X-ray measurements, we put constraints on the nature of HLX1. We rule out a foreground star and a background AGN. Two alternative scenarios are still viable. HLX1 could be an accreting intermediate mass black hole in a star cluster, which may itself be the stripped nucleus of a dwarf galaxy that passed through ESO 243-49, an event which might have caused the current episode of star formation. Or, it could be a neutron star in the Galactic halo, accreting from an M4-M5 donor star. C1 [Soria, Roberto; Kuin, N. Paul M.; Wu, Kinwah] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Hau, George K. T.; Graham, Alister W.; Li, I-Hui] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Kong, Albert K. H.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Liu, Ji-Feng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kong, Albert K. H.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. RP Soria, R (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM roberto.soria@mssl.ucl.ac.uk RI Graham, Alister/G-1217-2013 OI Graham, Alister/0000-0002-6496-9414 FU Tsing Hua University (Taiwan); University of Sydney FX We thank Mark Cropper, Rosanne di Stefano, Sean Farrell, Jeanette Gladstone, Craig Heinke, Erik Hooverstein, Pavel Kroupa, Tom Maccarone, Greg Sivakoff, Lee Spitler and Doug Swartz for discussions. We thank the referee for a detailed review and comments. RS acknowledges hospitality and financial assistance at Tsing Hua University (Taiwan), and hospitality at the University of Sydney, during part of this work. NR 50 TC 40 Z9 40 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 21 PY 2010 VL 405 IS 2 BP 870 EP 876 DI 10.1111/j.1365-2966.2010.16517.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 609SQ UT WOS:000278677800011 ER PT J AU Hirose, E Kawabe, K Sigg, D Adhikari, R Saulson, PR AF Hirose, Eiichi Kawabe, Keita Sigg, Daniel Adhikari, Rana Saulson, Peter R. TI Angular instability due to radiation pressure in the LIGO gravitational-wave detector SO APPLIED OPTICS LA English DT Article ID RESONANT OPTICAL INTERFEROMETERS; ALIGNMENT; PRINCIPLES AB We observed the effect of radiation pressure on the angular sensing and control system of the Laser Interferometer Gravitational-Wave Observatory (LIGO) interferometer's core optics at LIGO Hanford Observatory. This is the first measurement of this effect in a complete gravitational-wave interferometer. Only one of the two angular modes survives with feedback control, because the other mode is suppressed when the control gain is sufficiently large. We developed a mathematical model to understand the physics of the system. This model matches well with the dynamics that we observe. (C) 2010 Optical Society of America C1 [Kawabe, Keita; Sigg, Daniel] Hanford Observ, Laser Interferometer Gravitat Wave Observ LIGO, Richland, WA 99354 USA. [Adhikari, Rana] CALTECH, LIGO Lab, Pasadena, CA 91125 USA. [Hirose, Eiichi; Saulson, Peter R.] Syracuse Univ, Dept Phys, Syracuse, NY 13244 USA. RP Hirose, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 50, Cambridge, MA 02138 USA. EM eiich.hirose@gmail.com RI Kawabe, Keita/G-9840-2011; Sigg, Daniel/I-4308-2015 OI Sigg, Daniel/0000-0003-4606-6526 FU National Science Foundation (NSF) [PHY-0600259, PHY-0107417] FX We are grateful to Sam Waldman for useful discussions. This research was supported in part by the National Science Foundation (NSF) under grant PHY-0600259. LIGO was constructed by the California Institute of Technology and the Massachusetts Institute of Technology with funding from the NSF and operates under cooperative agreement PHY-0107417. This article has LIGO document number LIGO-P0900086. NR 24 TC 8 Z9 8 U1 1 U2 4 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD JUN 20 PY 2010 VL 49 IS 18 BP 3474 EP 3484 DI 10.1364/AO.49.003474 PG 11 WC Optics SC Optics GA 612ZV UT WOS:000278946300006 PM 20563200 ER PT J AU Ballard, S Christiansen, JL Charbonneau, D Deming, D Holman, MJ Fabrycky, D A'Hearn, MF Wellnitz, DD Barry, RK Kuchner, MJ Livengood, TA Hewagama, T Sunshine, JM Hampton, DL Lisse, CM Seager, S Veverka, JF AF Ballard, Sarah Christiansen, Jessie L. Charbonneau, David Deming, Drake Holman, Matthew J. Fabrycky, Daniel A'Hearn, Michael F. Wellnitz, Dennis D. Barry, Richard K. Kuchner, Marc J. Livengood, Timothy A. Hewagama, Tilak Sunshine, Jessica M. Hampton, Don L. Lisse, Carey M. Seager, Sara Veverka, Joseph F. TI A SEARCH FOR ADDITIONAL PLANETS IN THE NASA EPOXI OBSERVATIONS OF THE EXOPLANET SYSTEM GJ 436 SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; stars: individual (GJ 436); techniques: image processing; techniques: photometric ID SPACE-BASED PHOTOMETRY; TRANSIT LIGHT-CURVE; NEPTUNE-MASS PLANET; EARTH ORBITING GJ-436; DEEP IMPACT MISSION; M-DWARF GJ-436; EXTRASOLAR PLANETS; HOT NEPTUNE; TERRESTRIAL PLANETS; TIDAL EVOLUTION AB We present time series photometry of the M dwarf transiting exoplanet system GJ 436 obtained with the Extrasolar Planet Observation and Characterization (EPOCh) component of the NASA EPOXI mission. We conduct a search of the high-precision time series for additional planets around GJ 436, which could be revealed either directly through their photometric transits or indirectly through the variations these second planets induce on the transits of the previously known planet. In the case of GJ 436, the presence of a second planet is perhaps indicated by the residual orbital eccentricity of the known hot Neptune companion. We find no candidate transits with significance higher than our detection limit. From Monte Carlo tests of the time series, we rule out transiting planets larger than 1.5R interior to GJ 436b with 95% confidence and larger than 1.25.R(circle plus) with 80% confidence. Assuming coplanarity of additional planets with the orbit of GJ 436b, we cannot expect that putative planets with orbital periods longer than about 3.4 days will transit. However, if such a planet were to transit, we would rule out planets larger than 2.0R(circle plus) with orbital periods less than 8.5 days with 95% confidence. We also place dynamical constraints on additional bodies in the GJ 436 system, independent of radial velocity measurements. Our analysis should serve as a useful guide for similar analyses of transiting exoplanets for which radial velocity measurements are not available, such as those discovered by the Kepler mission. From the lack of observed secular perturbations, we set upper limits on the mass of a second planet as small as 10M(circle plus) in coplanar orbits and 1M(circle plus) in non-coplanar orbits close to GJ 436b. We present refined estimates of the system parameters for GJ 436. We find P = 2.64389579 +/- 0.00000080 d, R(star) = 0.437 +/- 0.016 R(circle dot), and R(p) = 3.880 +/- 0.147R(circle dot). We also report a sinusoidal modulation in the GJ 436 light curve that we attribute to star spots. This signal is best fit by a period of 9.01 days, although the duration of the EPOCh observations may not have been long enough to resolve the full rotation period of the star. C1 [Ballard, Sarah; Christiansen, Jessie L.; Charbonneau, David; Holman, Matthew J.; Fabrycky, Daniel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Deming, Drake; Barry, Richard K.; Kuchner, Marc J.; Livengood, Timothy A.; Hewagama, Tilak] Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [A'Hearn, Michael F.; Wellnitz, Dennis D.; Hewagama, Tilak; Sunshine, Jessica M.] Univ Maryland, College Pk, MD 20742 USA. [Hampton, Don L.] Univ Alaska Fairbanks, Fairbanks, AK 99775 USA. [Lisse, Carey M.] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. [Seager, Sara] MIT, Cambridge, MA 02159 USA. [Veverka, Joseph F.] Cornell Univ, Dept Space Sci, Ithaca, NY 14853 USA. RP Ballard, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sballard@cfa.harvard.edu RI Wellnitz, Dennis/B-4080-2012; Hewagama, T/C-8488-2012; Livengood, Timothy/C-8512-2012; Kuchner, Marc/E-2288-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Charbonneau, David/0000-0002-9003-484X; Fabrycky, Daniel/0000-0003-3750-0183 FU National Aeronautics and Space Administration [NNX08AB64A, NNX08AD05A]; Michelson Fellowship; National Aeronautics and Space Administration FX Support for this work was provided by the EPOXI Project of the National Aeronautics and Space Administration's Discovery Program via funding to the Goddard Space Flight Center, to Harvard University viaCo-operative Agreement NNX08AB64A, and to the Smithsonian Astrophysical Observatory via Cooperative Agreement NNX08AD05A.; D.F. gratefully acknowledges support from the Michelson Fellowship, supported by the National Aeronautics and Space Administration and administered by the Michelson Science Center. NR 63 TC 32 Z9 33 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2010 VL 716 IS 2 BP 1047 EP 1059 DI 10.1088/0004-637X/716/2/1047 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606WH UT WOS:000278459000012 ER PT J AU Plagge, T Benson, BA Ade, PAR Aird, KA Bleem, LE Carlstrom, JE Chang, CL Cho, HM Crawford, TM Crites, AT de Haan, T Dobbs, MA George, EM Hall, NR Halverson, NW Holder, GP Holzapfel, WL Hrubes, JD Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Marrone, D McMahon, JJ Mehl, J Meyer, SS Mohr, JJ Montroy, TE Padin, S Pryke, C Reichardt, CL Ruhl, JE Schaffer, KK Shaw, L Shirokoff, E Spieler, HG Stalder, B Staniszewski, Z Stark, AA Vanderlinde, K Vieira, JD Williamson, R Zahn, O AF Plagge, T. Benson, B. A. Ade, P. A. R. Aird, K. 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. George, E. M. Hall, N. R. Halverson, N. W. Holder, G. P. Holzapfel, W. L. Hrubes, J. D. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Marrone, D. McMahon, J. J. Mehl, J. Meyer, S. S. Mohr, J. J. Montroy, T. E. Padin, S. Pryke, C. Reichardt, C. L. Ruhl, J. E. Schaffer, K. K. Shaw, L. Shirokoff, E. Spieler, H. G. Stalder, B. Staniszewski, Z. Stark, A. A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. TI SUNYAEV-ZEL'DOVICH CLUSTER PROFILES MEASURED WITH THE SOUTH POLE TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; galaxies: clusters: intracluster medium ID RELAXED GALAXY CLUSTERS; X-RAY; SCALING RELATIONS; XMM-NEWTON; TEMPERATURE PROFILES; INTRACLUSTER MEDIUM; DARK-MATTER; MASS; SAMPLE; GAS AB We present Sunyaev-Zel'dovich (SZ) measurements of 15 massive X-ray-selected galaxy clusters obtained with the South Pole Telescope (SPT). The SZ cluster signals are measured at 150 GHz, and concurrent 220 GHz data are used to reduce astrophysical contamination. Radial profiles are computed using a technique that takes into account the effects of the beams and filtering. In several clusters, significant SZ decrements are detected out to a substantial fraction of the virial radius. The profiles are fit to the beta-model and to a generalized Navarro-Frenk-White (NFW) pressure profile, and are scaled and stacked to probe their average behavior. We find model parameters that are consistent with previous studies: beta = 0.86 and r(core)/r(500) = 0.20 for the beta-model, and (alpha(n), beta(n), gamma(n), c(500)) = (1.0, 5.5, 0.5, 1.0) for the generalized NFW model. Both models fit the SPT data comparably well, and both are consistent with the average SZ profile out to beyond r(500). The integrated Compton-y parameter Y(SZ) is computed for each cluster using both model-dependent and model-independent techniques, and the results are compared to X-ray estimates of cluster parameters. We find that Y(SZ) scales with Y(X) and gas mass with low scatter. Since these observables have been found to scale with total mass, our results point to a tight mass-observable relation for the SPT cluster survey. C1 [Plagge, T.; Cho, H. -M.; George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Keisler, R.; Leitch, E. M.; Marrone, D.; McMahon, J. J.; Meyer, S. S.; Padin, S.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Ade, P. A. R.] Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, S Glam, Wales. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Pryke, C.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.; Keisler, R.; McMahon, J. J.; Meyer, S. S.; Pryke, C.; Schaffer, K. K.; Vieira, J. D.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Pryke, C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [de Haan, T.; Dobbs, M. A.; Holder, G. P.; Shaw, L.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Hall, N. R.; Knox, L.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, VP62, Dept Space Sci, Huntsville, AL 35812 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Lab, Div Phys, Berkeley, CA 94720 USA. [Marrone, D.] Natl Radio Astron Observ, Charlottesville, VA 22903 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, Cleveland, OH 44106 USA. [Montroy, T. E.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. RP Plagge, T (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM tplagge@bolo.berkeley.edu 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 FU National Science Foundation [ANT-0638937, ANT-0130612]; NSF Physics Frontier Center [PHY-0114422] 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 EngineeringResearch Council of Canada, the Quebec Fonds de recherche sur la nature et les technologies, and the Canadian Institute for Advanced Research. The following individuals acknowledge additional support: B. A. B. and K. K. S. from a KICP Fellowship; J.J.M. from a Fermi Fellowship; Z.S. from a GAAN Fellowship; A. T. L. from the Miller Institute for Basic Research in Science, University of California, Berkeley; and N.W.H. from an Alfred P. Sloan Research Fellowship. NR 60 TC 83 Z9 83 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2010 VL 716 IS 2 BP 1118 EP 1135 DI 10.1088/0004-637X/716/2/1118 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606WH UT WOS:000278459000018 ER PT J AU Laycock, S Zezas, A Hong, J Drake, JJ Antoniou, V AF Laycock, Silas Zezas, Andreas Hong, Jaesub Drake, Jeremy J. Antoniou, Valsamo TI EXPLORING THE SMALL MAGELLANIC CLOUD TO THE FAINTEST X-RAY FLUXES: SOURCE CATALOG, TIMING, AND SPECTRAL ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Magellanic Clouds; stars: emission-line, Be; stars: neutron; X-rays: binaries ID CHANDRA MULTIWAVELENGTH PROJECT; XMM-NEWTON OBSERVATIONS; BINARY PULSARS; GALACTIC-CENTER; RADIO PULSARS; SMC REGION; LONG; EMISSION; NUMBER; PERIOD AB We present the results of a pair of 100 ks Chandra observations in the Small Magellanic Cloud (SMC) to survey high-mass X-ray binaries (HMXBs), stars, and low-mass X-ray binaries (LMXBs)/cataclysmic variables down to L-x = 4.3 x 10(32) erg s(-1). The two SMC Deep Fields (DFs) are located in the most active star-forming region of the bar, with Deep Field-1 positioned at the most pulsar-rich location identified from previous surveys. Two new pulsars were discovered in the outburst: CXOU J004929.7-731058 (P = 892 s), CXOU J005252.2-721715 (P = 326 s), and three new HMXB candidates were identified. Of the 15 Be-pulsars now known in the field, 13 were detected, with pulsations seen in 9 of them. Ephemerides demonstrate that 6 of the 10 pulsars known to exhibit regular outbursts were seen outside their periastron phase, and quiescent X-ray emission at L-X = 10(33)-10(34) erg s(-1) is shown to be common. Comparison with ROSAT, ASCA, and XMM-Newton catalogs resulted in positive identification of several previously ambiguous sources. Bright optical counterparts exist for 40 of the X-ray sources, of which 33 are consistent with early-type stars (M-V < -2, B-V < 0.2), and are the subject of a companion paper. The results point to an underlying HMXB population density up to double that of active systems. The full catalog of 394 point sources is presented along with detailed analyses of timing and spectral properties. C1 [Laycock, Silas] Gemini Observ, Hilo, HI 96720 USA. [Zezas, Andreas; Hong, Jaesub; Drake, Jeremy J.; Antoniou, Valsamo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zezas, Andreas; Antoniou, Valsamo] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Zezas, Andreas] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Greece. RP Laycock, S (reprint author), Gemini Observ, 670 N Aohoku Pl, Hilo, HI 96720 USA. RI Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 NR 65 TC 15 Z9 15 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2010 VL 716 IS 2 BP 1217 EP 1240 DI 10.1088/0004-637X/716/2/1217 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606WH UT WOS:000278459000025 ER PT J AU Keto, E Rybicki, G AF Keto, Eric Rybicki, George TI MODELING MOLECULAR HYPERFINE LINE EMISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; radiative transfer ID RADIO-ASTRONOMICAL SPECTROSCOPY; MULTILEVEL RADIATIVE-TRANSFER; LAMBDA ITERATION METHOD; STARLESS CORES; COLLISIONAL EXCITATION; N2H+; TRANSITIONS; CONTINUUM; CLOUDS; CS AB In this paper, we discuss two approximate methods previously suggested for modeling hyperfine spectral line emission for molecules whose collisional transition rates between hyperfine levels are unknown. Hyperfine structure is seen in the rotational spectra of many commonly observed molecules such as HCN, HNC, NH(3), N(2)H(+), and C(17)O. The intensities of these spectral lines can be modeled by numerical techniques such as Lambda-iteration that alternately solve the equations of statistical equilibrium and the equation of radiative transfer. However, these calculations require knowledge of both the radiative and collisional rates for all transitions. For most commonly observed radio frequency spectral lines, only the net collisional rates between rotational levels are known. For such cases, two approximate methods have been suggested. The first method, hyperfine statistical equilibrium, distributes the hyperfine level populations according to their statistical weight, but allows the population of the rotational states to depart from local thermal equilibrium (LTE). The second method, the proportional method, approximates the collision rates between the hyperfine levels as fractions of the net rotational rates apportioned according to the statistical degeneracy of the final hyperfine levels. The second method is able to model non-LTE hyperfine emission. We compare simulations of N(2)H(+) hyperfine lines made with approximate and more exact rates and find that satisfactory results are obtained. C1 [Keto, Eric; Rybicki, George] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Keto, E (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 22 TC 26 Z9 26 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2010 VL 716 IS 2 BP 1315 EP 1322 DI 10.1088/0004-637X/716/2/1315 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606WH UT WOS:000278459000032 ER PT J AU Forbrich, J Tappe, A Robitaille, T Muench, AA Teixeira, PS Lada, EA Stolte, A Lada, CJ AF Forbrich, Jan Tappe, Achim Robitaille, Thomas Muench, August A. Teixeira, Paula S. Lada, Elizabeth A. Stolte, Andrea Lada, Charles J. TI DISENTANGLING PROTOSTELLAR EVOLUTIONARY STAGES IN CLUSTERED ENVIRONMENTS USING SPITZER-IRS SPECTRA AND COMPREHENSIVE SPECTRAL ENERGY DISTRIBUTION MODELING SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; open clusters and associations: individual (NGC 2264, IC 348) ID YOUNG STELLAR OBJECTS; EFFECTIVE COLLISION STRENGTHS; 2-DIMENSIONAL RADIATIVE-TRANSFER; ELECTRON-IMPACT EXCITATION; INITIAL MASS FUNCTION; STAR-FORMING REGIONS; NGC 2264; INFRARED SPECTROGRAPH; INTERSTELLAR EXTINCTION; PROTOPLANETARY DISKS AB When studying the evolutionary stages of protostars that form in clusters, the role of any intracluster medium cannot be neglected. High foreground extinction can lead to situations where young stellar objects (YSOs) appear to be in earlier evolutionary stages than they actually are, particularly when using simple criteria like spectral indices. To address this issue, we have assembled detailed spectral energy distribution characterizations of a sample of 56 Spitzer-identified candidate YSOs in the clusters NGC 2264 and IC 348. For these, we use spectra obtained with the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope and ancillary multi-wavelength photometry. The primary aim is twofold: (1) to discuss the role of spectral features, particularly those due to ices and silicates, in determining a YSO's evolutionary stage, and (2) to perform comprehensive modeling of SEDs enhanced by the IRS data. The SEDs consist of ancillary optical-to-submillimeter multi-wavelength data as well as an accurate description of the 9.7 mu m silicate feature and of the mid-infrared continuum derived from line-free parts of the IRS spectra. We find that using this approach, we can distinguish genuine protostars in the cluster from T Tauri stars masquerading as protostars due to external foreground extinction. Our results underline the importance of photometric data in the far-infrared/submillimeter wavelength range, at sufficiently high angular resolution to more accurately classify cluster members. Such observations are becoming possible now with the advent of the Herschel Space Observatory. C1 [Forbrich, Jan; Tappe, Achim; Robitaille, Thomas; Muench, August A.; Lada, Charles J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teixeira, Paula S.] European So Observ, D-85748 Garching, Germany. [Lada, Elizabeth A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Stolte, Andrea] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. RP Forbrich, J (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Teixeira, Paula Stella/O-2289-2013; OI Teixeira, Paula Stella/0000-0002-3665-5784; Muench, August/0000-0003-0666-6367; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [1288815] FX We thank Grace Wolf-Chase, for providing us with files of her submillimeter data of NGC 2264, as well as the referee, Dan Watson, whose constructive comments led to improvements of this paper. This project is based, in a large 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 award no. 1288815 issued by JPL/Caltech. NR 56 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2010 VL 716 IS 2 BP 1453 EP 1477 DI 10.1088/0004-637X/716/2/1453 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606WH UT WOS:000278459000046 ER PT J AU Papovich, C Momcheva, I Willmer, CNA Finkelstein, KD Finkelstein, SL Tran, KV Brodwin, M Dunlop, JS Farrah, D Khan, SA Lotz, J McCarthy, P McLure, RJ Rieke, M Rudnick, G Sivanandam, S Pacaud, F Pierre, M AF Papovich, C. Momcheva, I. Willmer, C. N. A. Finkelstein, K. D. Finkelstein, S. L. Tran, K. -V. Brodwin, M. Dunlop, J. S. Farrah, D. Khan, S. A. Lotz, J. McCarthy, P. McLure, R. J. Rieke, M. Rudnick, G. Sivanandam, S. Pacaud, F. Pierre, M. TI A SPITZER-SELECTED GALAXY CLUSTER AT z=1.62 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (ClG 0218.3-0510); galaxies: evolution; large-scale structure of universe ID COLOR-MAGNITUDE RELATION; INFRARED ARRAY CAMERA; IRAC SHALLOW SURVEY; X-RAY-CLUSTERS; RED-SEQUENCE; SPACE-TELESCOPE; HIGH-REDSHIFT; DISTANT CLUSTERS; SPECTROSCOPIC CONFIRMATION; LUMINOSITY FUNCTION AB We report the discovery of a galaxy cluster at z = 1.62 located in the Spitzer Wide-Area Infrared Extragalactic survey XMM-LSS field. This structure was selected solely as an overdensity of galaxies with red Spitzer/Infrared Array Camera colors, satisfying ([3.6] - [4.5]) AB > -0.1 mag. Photometric redshifts derived from the Subaru XMM Deep Survey (BV iz bands), the UKIRT Infrared Deep Survey-Ultra-Deep Survey (UKIDSS-UDS, JK bands), and from the Spitzer Public UDS survey (3.6-8.0 mu m) show that this cluster corresponds to a surface density of galaxies at z approximate to 1.6 that is >20 sigma above the mean at this redshift. We obtained optical spectroscopic observations of galaxies in the cluster region using IMACS on the Magellan telescope. We measured redshifts for seven galaxies in the range z = 1.62-1.63 within 2.8 arcmin (<1.4 Mpc) of the astrometric center of the cluster. A posteriori analysis of the XMM data in this field reveal a weak (4 sigma) detection in the [0.5-2 keV] band compatible with the expected thermal emission from such a cluster. The color-magnitude diagram of the galaxies in this cluster shows a prominent red sequence, dominated by a population of red galaxies with (z - J) > 1.7 mag. The photometric-redshift probability distributions for the red galaxies are strongly peaked at z = 1.62, coincident with the spectroscopically confirmed galaxies. The rest-frame (U - B) color and scatter of galaxies on the red sequence are consistent with a mean luminosity-weighted age of 1.2 +/- 0.1 Gyr, yielding a formation redshift (z(f)) over bar = 2.35 +/- 0.10, and corresponding to the last significant star formation period in these galaxies. C1 [Papovich, C.; Finkelstein, K. D.; Finkelstein, S. L.; Tran, K. -V.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. [Papovich, C.; Finkelstein, K. D.; Finkelstein, S. L.; Tran, K. -V.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Momcheva, I.; McCarthy, P.] Carnegie Inst Sci, Pasadena, CA 91101 USA. [Willmer, C. N. A.; Rieke, M.; Sivanandam, S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Brodwin, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dunlop, J. S.; McLure, R. J.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh, Midlothian, Scotland. [Farrah, D.] Univ Sussex, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Khan, S. A.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Khan, S. A.] Shanghai Normal Univ, Shanghai Key Lab Astrophys, Shanghai 200234, Peoples R China. [Lotz, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Rudnick, G.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Pacaud, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Pierre, M.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. RP Papovich, C (reprint author), Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA. EM papovich@physics.tamu.edu NR 85 TC 155 Z9 155 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2010 VL 716 IS 2 BP 1503 EP 1513 DI 10.1088/0004-637X/716/2/1503 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606WH UT WOS:000278459000049 ER PT J AU Antoniou, V Zezas, A Hatzidimitriou, D Kalogera, V AF Antoniou, V. Zezas, A. Hatzidimitriou, D. Kalogera, V. TI STAR FORMATION HISTORY AND X-RAY BINARY POPULATIONS: THE CASE OF THE SMALL MAGELLANIC CLOUD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Magellanic Clouds; pulsars: general; stars: early-type; stars: emission-line, Be; stars: formation; X-rays: binaries ID CATALOG; METALLICITY; VELOCITIES; SMC; CLUSTERS; PULSARS; FIELD AB Using Chandra, XMM-Newton, and optical photometric catalogs we study the young X-ray binary (XRB) populations of the Small Magellanic Cloud. We find that the Be/X-ray binaries (Be-XRBs) are observed in regions with star formation rate bursts similar to 25-60 Myr ago. The similarity of this age with the age of maximum occurrence of the Be phenomenon (similar to 40 Myr) indicates that the presence of a circumstellar decretion disk plays a significant role in the number of observed XRBs in the 10-100 Myr age range. We also find that regions with strong but more recent star formation (e. g., the Wing) are deficient in Be-XRBs. By correlating the number of observed Be-XRBs with the formation rate of their parent populations, we measure a Be-XRB production rate of similar to 1 system per 3 x 10(-3) M(circle dot) yr(-1). Finally, we use the strong localization of the Be-XRB systems in order to set limits on the kicks imparted on the neutron star during the supernova explosion. C1 [Antoniou, V.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Antoniou, V.; Zezas, A.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. [Antoniou, V.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Zezas, A.; Hatzidimitriou, D.] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Crete, Greece. [Hatzidimitriou, D.] Univ Athens, Dept Phys, Sect Astrophys Astron & Mech, GR-15784 Athens, Greece. [Kalogera, V.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. RP Antoniou, V (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM vantoniou@head.cfa.harvard.edu RI Hatzidimitriou, Despina/A-3732-2015; Zezas, Andreas/C-7543-2011; Antoniou, Vallia/E-3837-2013 OI Zezas, Andreas/0000-0001-8952-676X; Antoniou, Vallia/0000-0001-7539-1593 FU NASA LTSA [NAG5-13056, G02-3117X, NNX08AB68G, NNG06GE68G, NNX10AH47G]; [206469] FX We thank Ewan O'Sullivan for helping with the XMM-Newton data analysis, and the anonymous referee for comments which improved this Letter. This work was supported by NASA LTSA grant NAG5-13056, NASA grants G02-3117X, NNX08AB68G, NNG06GE68G, NNX10AH47G, and FP7 grant 206469 (ASTROSPACE). NR 37 TC 32 Z9 32 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 JUN 20 PY 2010 VL 716 IS 2 BP L140 EP L145 DI 10.1088/2041-8205/716/2/L140 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608NW UT WOS:000278592000010 ER PT J AU Pacciani, L Vittorini, V Tavani, M Fiocchi, MT Vercellone, S D'Ammando, F Sakamoto, T Pian, E Raiteri, CM Villata, M Sasada, M Itoh, R Yamanaka, M Uemura, M Striani, E Fugazza, D Tiengo, A Krimm, HA Stroh, MC Falcone, AD Curran, PA Sadun, AC Lahteenmaki, A Tornikoski, M Aller, HD Aller, MF Lin, CS Larionov, VM Leto, P Takalo, LO Berdyugin, A Gurwell, MA Bulgarelli, A Chen, AW Donnarumma, I Giuliani, A Longo, F Pucella, G Argan, A Barbiellini, G Caraveo, P Cattaneo, PW Costa, E De Paris, G Del Monte, E Di Cocco, G Evangelista, Y Ferrari, A Feroci, M Fiorini, M Fuschino, F Galli, M Gianotti, F Labanti, C Lapshov, I Lazzarotto, F Lipari, P Marisaldi, M Mereghetti, S Morelli, E Moretti, E Morselli, A Pellizzoni, A Perotti, F Piano, G Picozza, P Pilia, M Prest, M Rapisarda, M Rappoldi, A Rubini, A Sabatini, S Soffitta, P Trifoglio, M Trois, A Vallazza, E Zanello, D Colafrancesco, S Pittori, C Verrecchia, F Santolamazza, P Lucarelli, F Giommi, P Salotti, L AF Pacciani, L. Vittorini, V. Tavani, M. Fiocchi, M. T. Vercellone, S. D'Ammando, F. Sakamoto, T. Pian, E. Raiteri, C. M. Villata, M. Sasada, M. Itoh, R. Yamanaka, M. Uemura, M. Striani, E. Fugazza, D. Tiengo, A. Krimm, H. A. Stroh, M. C. Falcone, A. D. Curran, P. A. Sadun, A. C. Lahteenmaki, A. Tornikoski, M. Aller, H. D. Aller, M. F. Lin, C. S. Larionov, V. M. Leto, P. Takalo, L. O. Berdyugin, A. Gurwell, M. A. Bulgarelli, A. Chen, A. W. Donnarumma, I. Giuliani, A. Longo, F. Pucella, G. Argan, A. Barbiellini, G. Caraveo, P. Cattaneo, P. W. Costa, E. De Paris, G. Del Monte, E. Di Cocco, G. Evangelista, Y. Ferrari, A. Feroci, M. Fiorini, M. Fuschino, F. Galli, M. Gianotti, F. Labanti, C. Lapshov, I. Lazzarotto, F. Lipari, P. Marisaldi, M. Mereghetti, S. Morelli, E. Moretti, E. Morselli, A. Pellizzoni, A. Perotti, F. Piano, G. Picozza, P. Pilia, M. Prest, M. Rapisarda, M. Rappoldi, A. Rubini, A. Sabatini, S. Soffitta, P. Trifoglio, M. Trois, A. Vallazza, E. Zanello, D. Colafrancesco, S. Pittori, C. Verrecchia, F. Santolamazza, P. Lucarelli, F. Giommi, P. Salotti, L. TI THE 2009 DECEMBER GAMMA-RAY FLARE OF 3C 454.3: THE MULTIFREQUENCY CAMPAIGN SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (3C 454.3); quasars: general; radiation mechanisms: non-thermal ID MULTIWAVELENGTH OBSERVATIONS; TIMING EXPLORER; CRAZY-DIAMOND; BLAZAR MODEL; WEBT; TELESCOPE; OUTBURST; CALIBRATION; 3C-454.3; RADIO AB During the month of 2009 December, the blazar 3C 454.3 became the brightest gamma-ray source in the sky, reaching a peak flux F similar to 2000 x 10(-8) photons cm(-2) s(-1) for E > 100 MeV. Starting in 2009 November intensive multifrequency campaigns monitored the 3C 454 gamma-ray outburst. Here, we report on the results of a two-month campaign involving AGILE, INTEGRAL, Swift/XRT, Swift/BAT, and Rossi XTE for the high-energy observations and Swift/UVOT, KANATA, Goddard Robotic Telescope, and REM for the near-IR/optical/UV data. GASP/WEBT provided radio and additional optical data. We detected a long-term active emission phase lasting similar to 1 month at all wavelengths: in the gamma-ray band, peak emission was reached on 2009 December 2-3. Remarkably, this gamma-ray super-flare was not accompanied by correspondingly intense emission in the optical/UV band that reached a level substantially lower than the previous observations in 2007-2008. The lack of strong simultaneous optical brightening during the super-flare and the determination of the broadband spectral evolution severely constrain the theoretical modeling. We find that the pre- and post-flare broadband behavior can be explained by a one-zone model involving synchrotron self-Compton plus external Compton emission from an accretion disk and a broad-line region. However, the spectra of the 2009 December 2-3 super-flare and of the secondary peak emission on 2009 December 9 cannot be satisfactorily modeled by a simple one-zone model. An additional particle component is most likely active during these states. C1 [Pacciani, L.; Vittorini, V.; Tavani, M.; Fiocchi, M. T.; Donnarumma, I.; Argan, A.; Costa, E.; De Paris, G.; Del Monte, E.; Evangelista, Y.; Feroci, M.; Lapshov, I.; Lazzarotto, F.; Piano, G.; Rubini, A.; Sabatini, S.; Soffitta, P.; Trois, A.] INAF IASF Roma, I-00133 Rome, Italy. [Vittorini, V.; Tavani, M.; Striani, E.; Piano, G.; Picozza, P.] Univ Roma Tor Vergata, Dip Fis, I-00133 Rome, Italy. [Vercellone, S.; D'Ammando, F.] INAF IASF Palermo, I-90146 Palermo, Italy. [Sakamoto, T.; Krimm, H. A.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Sakamoto, T.] Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. [Pian, E.] INAF OATS, I-34143 Trieste, Italy. [Pian, E.] SNS, I-56126 Pisa, Italy. [Raiteri, C. M.; Villata, M.] OATO INAF, I-10025 Pino Torinese, To, Italy. [Sasada, M.; Itoh, R.; Yamanaka, M.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. [Yamanaka, M.; Uemura, M.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima 7398526, Japan. [Striani, E.; Morselli, A.; Piano, G.; Picozza, P.] INFN Roma Tor Vergata, I-00133 Rome, Italy. [Fugazza, D.] OAB INAF, I-20121 Milan, Italy. [Tiengo, A.; Chen, A. W.; Giuliani, A.; Caraveo, P.; Fiorini, M.; Mereghetti, S.; Perotti, F.] INAF IASF Milano, I-20133 Milan, Italy. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Stroh, M. C.; Falcone, A. D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Curran, P. A.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Sadun, A. C.] Univ Colorado, Denver, CO 80202 USA. [Lahteenmaki, A.; Tornikoski, M.] Aalto Univ, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Aller, H. D.; Aller, M. F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Lin, C. S.] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Larionov, V. M.] St Petersburg State Univ, Astron Inst, St Petersburg, Russia. [Larionov, V. M.] Pulkovo Observ, St Petersburg, Russia. [Larionov, V. M.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Leto, P.] Osserv Astrofis Catania, INAF, Catania, Italy. [Takalo, L. O.; Berdyugin, A.] Univ Turku, Dept Phys & Astron, Tuorla Observ, FI-21500 Piikkio, Finland. [Gurwell, M. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bulgarelli, A.; Di Cocco, G.; Fuschino, F.; Gianotti, F.; Labanti, C.; Marisaldi, M.; Morelli, E.; Trifoglio, M.] INAF IASF Bologna, I-40129 Bologna, Italy. [Chen, A. W.] CIFS Torino, I-10133 Turin, Italy. [Longo, F.; Barbiellini, G.; Moretti, E.; Vallazza, E.] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy. [Longo, F.; Barbiellini, G.; Moretti, E.; Vallazza, E.] INFN Trieste, I-34127 Trieste, Italy. [Pucella, G.; Rapisarda, M.] ENEA Frascati, I-00044 Rome, Italy. [Ferrari, A.] Univ Turin, Dip Fis, Turin, Italy. [Galli, M.] ENEA Bologna, I-40129 Bologna, Italy. [Lipari, P.; Zanello, D.] INFN Roma La Sapienza, I-00185 Rome, Italy. [Pellizzoni, A.; Pilia, M.] INAF OAC, I-09012 Capoterra, Italy. [Pilia, M.; Prest, M.] Univ Insubria, Dip Fis, I-22100 Como, Italy. [Colafrancesco, S.; Pittori, C.; Verrecchia, F.; Santolamazza, P.; Lucarelli, F.; Giommi, P.] ASI Sci Data Ctr, I-00044 Rome, Italy. [Salotti, L.] Agenzia Spaziale Italiana, I-00198 Rome, Italy. RP Pacciani, L (reprint author), INAF IASF Roma, I-00133 Rome, Italy. EM luigi.pacciani@iasf-roma.inaf.it RI Morselli, Aldo/G-6769-2011; Lazzarotto, Francesco/J-4670-2012; Curran, Peter/B-5293-2013; Larionov, Valeri/H-1349-2013; Lahteenmaki, Anne/L-5987-2013; Trifoglio, Massimo/F-5302-2015; Pittori, Carlotta/C-7710-2016; OI Del Monte, Ettore/0000-0002-3013-6334; trois, alessio/0000-0002-3180-6002; Labanti, Claudio/0000-0002-5086-3619; Feroci, Marco/0000-0002-7617-3421; Soffitta, Paolo/0000-0002-7781-4104; Picozza, Piergiorgio/0000-0002-7986-3321; Villata, Massimo/0000-0003-1743-6946; Fuschino, Fabio/0000-0003-2139-3299; Gianotti, Fulvio/0000-0003-4666-119X; Vercellone, Stefano/0000-0003-1163-1396; Raiteri, Claudia Maria/0000-0003-1784-2784; Sasada, Mahito/0000-0001-5946-9960; MEREGHETTI, SANDRO/0000-0003-3259-7801; Fiocchi, Mariateresa/0000-0001-5697-6019; Tavani, Marco/0000-0003-2893-1459; Lucarelli, Fabrizio/0000-0002-6311-764X; Pian, Elena/0000-0001-8646-4858; Leto, Paolo/0000-0003-4864-2806; Lazzarotto, Francesco/0000-0003-4871-4072; Costa, Enrico/0000-0003-4925-8523; giommi, paolo/0000-0002-2265-5003; Donnarumma, Immacolata/0000-0002-4700-4549; Pellizzoni, Alberto Paolo/0000-0002-4590-0040; Tiengo, Andrea/0000-0002-6038-1090; Sabatini, Sabina/0000-0003-2076-5767; Caraveo, Patrizia/0000-0003-2478-8018; PREST, MICHELA/0000-0003-3161-4454; Verrecchia, Francesco/0000-0003-3455-5082; Marisaldi, Martino/0000-0002-4000-3789; Fiorini, Mauro/0000-0001-8297-1983; Morselli, Aldo/0000-0002-7704-9553; Curran, Peter/0000-0003-3003-4626; Larionov, Valeri/0000-0002-4640-4356; Trifoglio, Massimo/0000-0002-2505-3630; Pittori, Carlotta/0000-0001-6661-9779; Bulgarelli, Andrea/0000-0001-6347-0649; galli, marcello/0000-0002-9135-3228; Pacciani, Luigi/0000-0001-6897-5996 FU Italian Space Agency (ASI) [I/089/06/2, ASI-INAFI/088/06/0]; Italian Institute of Astrophysics (INAF); Italian Institute of Nuclear Physics (INFN); Russian RFBR foundation [09-02-00092]; NSF; NASA; University of Michigan; Smithsonian Institution; Academia Sinica Institute of Astronomy and Astrophysics FX The AGILE Mission is funded by the Italian Space Agency (ASI) with scientific and programmatic participation by the Italian Institute of Astrophysics (INAF) and the Italian Institute of Nuclear Physics (INFN). This investigation was carried out with partial support from the ASI contract no. I/089/06/2. V. L. acknowledges support from Russian RFBR foundation via grant 09-02-00092. The operation of UMRAO is made possible by funding from the NSF, NASA, and the University of Michigan. The Submillimeter Array is funded by the Smithsonian Institution and the Academia Sinica Institute of Astronomy and Astrophysics. The GASP president acknowledges the ASI support through contract ASI-INAFI/088/06/0. NR 38 TC 31 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 JUN 20 PY 2010 VL 716 IS 2 BP L170 EP L175 DI 10.1088/2041-8205/716/2/L170 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608NW UT WOS:000278592000016 ER PT J AU Suarez-Morales, E AF Suarez-Morales, Eduardo TI On the taxonomic status of Monstrilla leucopis Sars (Crustacea: Copepoda: Monstrilloida) from Norway, with comments on the male of M. longiremis Giesbrecht SO ZOOTAXA LA English DT Article DE marine zooplankton; associated copepods; taxonomy; Copepoda; monstrilloids AB Specimens of monstrilloid copepods collected and described in the early 20(th) century by G.O. Sars from the coasts of Norway and deposited in the Sars Collection (University of Oslo) were re-examined. Monstrilla leucopis Sars, 1921 was described based on female and male specimens, but the species was later synonymized with M. conjunctiva Giesbrecht, 1902 by several authors. Females of this species were analyzed and compared with closely related congeners, particularly with M. conjunctiva. This analysis includes the description of previously unknown morphological details following upgraded descriptive standards in this group. Evidence was found to support the notion that the female type specimens from Kvalo, Norway represent a distinct species; thus, M. leucopis is redescribed and reinstated as a valid taxon. Previous tropical records of female M. conjunctiva are questionable, but differences with M. leucopis can be found in body and antennule proportions, the structure of the genital spines and fifth legs, and most probably, their geographical ranges. Furthermore, M. leucopis has a modified thick-walled seta on the endopods of legs 2-4, so far a unique character among monstrilloids. The single male specimen labeled as M. leucopis in the Sars Collection was also examined and it is not the male of this species as depicted by G.O. Sars (1921). It is in fact a male of M. longiremis Giesbrecht, 1893, a species for which a short supplementary description and taxonomic comments are also provided herein. The male of M. leucopis also shares some important characters with that of M. conjunctiva, but also with another male specimen that was questionably assigned to the latter species; this male probably represents an undescribed species. C1 [Suarez-Morales, Eduardo] Colegio Frontera ECOSUR, Unidad Chetumal, Chetmal 77014, Quintana Roo, Mexico. [Suarez-Morales, Eduardo] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Suarez-Morales, E (reprint author), Colegio Frontera ECOSUR, Unidad Chetumal, AP 424, Chetmal 77014, Quintana Roo, Mexico. EM esuarez@ecosur.mx FU Museum of Comparative Zoology, Harvard University FX This survey was enabled by an Ernst Mayr Grant of the Museum of Comparative Zoology, Harvard University, awarded to the author. Dr. Lutz Bachmann and Ase Wilhelmsen, Zoological Museum, University of Oslo, kindly authorized the loan of G.O. Sars's specimens of M. leucopis and provided additional information about this material. Paul Greenhall and Chad Walter of the National Museum of Natural History, Smithsonian Institution, Washington, D. C. helped to process the loan and return of these specimens. The comments from two anonymous reviewers greatly helped to improve a previous version of this contribution. NR 29 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 JUN 18 PY 2010 IS 2510 BP 55 EP 67 PG 13 WC Zoology SC Zoology GA 613EI UT WOS:000278960400003 ER PT J AU Wells, KS Campbell, DB Campbell, BA Carter, LM AF Wells, Kassandra S. Campbell, Donald B. Campbell, Bruce A. Carter, Lynn M. TI Detection of small lunar secondary craters in circular polarization ratio radar images SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID EUROPA; RAYS; MARS AB The identification of small (D < a few kilometers) secondary craters and their global distributions are of critical importance to improving our knowledge of surface ages in the solar system. We investigate a technique by which small, distal secondary craters can be discerned from the surrounding primary population of equivalent size based on asymmetries in their ejecta blankets. The asymmetric ejecta blankets are visible in radar circular polarization ratio (CPR) but not as optical albedo features. Measurements with our new technique reveal 94 secondary craters on the Newton and Newton-A crater floors near the lunar south pole. These regions are not in an obvious optical ray, but the orientation of asymmetric secondary ejecta blankets suggests that they represent an extension of the Tycho crater ray that crosses Clavius crater. Including the secondary craters at Newton and Newton-A skews the terrain age inferred by crater counts. It is reduced by few percentages by their removal, from 3.8 to 3.75 Gyr at Newton-A. Because "hidden rays" like that identified here may also occur beyond the edges of other optically bright lunar crater rays, we assess the effect that similar but hypothetical populations would have on lunar terrains of various ages. The average secondary crater density measured at 1 km diameter is equivalent to the crater density at 1 km on a 3.4 Gyr surface [Neukum et al., 2001]. Younger surfaces (i.e., younger crater ejecta blankets) would be dominated by secondary craters below 1 km if superposed by a hidden ray. C1 [Wells, Kassandra S.; Campbell, Donald B.] Cornell Univ, Dept Astron & Space Sci, Ithaca, NY 14853 USA. [Campbell, Bruce A.; Carter, Lynn M.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Wells, KS (reprint author), Cornell Univ, Dept Astron & Space Sci, 514 Space Sci Bldg, Ithaca, NY 14853 USA. EM kassiew@astro.cornell.edu RI Carter, Lynn/D-2937-2012 NR 22 TC 8 Z9 8 U1 0 U2 4 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 JUN 17 PY 2010 VL 115 AR E06008 DI 10.1029/2009JE003491 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 613PE UT WOS:000278990500001 ER PT J AU Elliot, JL Person, MJ Zuluaga, CA Bosh, AS Adams, ER Brothers, TC Gulbis, AAS Levine, SE Lockhart, M Zangari, AM Babcock, BA DuPre, K Pasachoff, JM Souza, SP Rosing, W Secrest, N Bright, L Dunham, EW Sheppard, SS Kakkala, M Tilleman, T Berger, B Briggs, JW Jacobson, G Valleli, P Volz, B Rapoport, S Hart, R Brucker, M Michel, R Mattingly, A Zambrano-Marin, L Meyer, AW Wolf, J Ryan, EV Ryan, WH Morzinski, K Grigsby, B Brimacombe, J Ragozzine, D Montano, HG Gilmore, A AF Elliot, J. L. Person, M. J. Zuluaga, C. A. Bosh, A. S. Adams, E. R. Brothers, T. C. Gulbis, A. A. S. Levine, S. E. Lockhart, M. Zangari, A. M. Babcock, B. A. DuPre, K. Pasachoff, J. M. Souza, S. P. Rosing, W. Secrest, N. Bright, L. Dunham, E. W. Sheppard, S. S. Kakkala, M. Tilleman, T. Berger, B. Briggs, J. W. Jacobson, G. Valleli, P. Volz, B. Rapoport, S. Hart, R. Brucker, M. Michel, R. Mattingly, A. Zambrano-Marin, L. Meyer, A. W. Wolf, J. Ryan, E. V. Ryan, W. H. Morzinski, K. Grigsby, B. Brimacombe, J. Ragozzine, D. Montano, H. G. Gilmore, A. TI Size and albedo of Kuiper belt object 55636 from a stellar occultation SO NATURE LA English DT Article ID EL61 COLLISIONAL FAMILY; DWARF PLANET HAUMEA; COLOR DIVERSITY; SATELLITES; ATMOSPHERE; MEMBERS AB The Kuiper belt is a collection of small bodies (Kuiper belt objects, KBOs) that lie beyond the orbit of Neptune and which are believed to have formed contemporaneously with the planets. Their small size and great distance make them difficult to study. KBO 55636 (2002 TX(300)) is a member of the water-ice-rich Haumea KBO collisional family(1). The Haumea family are among the most highly reflective objects in the Solar System. Dynamical calculations indicate that the collision that created KBO 55636 occurred at least 1 Gyr ago(2,3). Here we report observations of a multi-chord stellar occultation by KBO 55636, which occurred on 9 October 2009 UT. We find that it has a mean radius of 143 +/- 65 km (assuming a circular solution). Allowing for possible elliptical shapes, we find a geometric albedo of 0.88(0.06)(+0.15) in the V photometric band, which establishes that KBO 55636 is smaller than previously thought and that, like its parent body, it is highly reflective. The dynamical age implies either that KBO 55636 has an active resurfacing mechanism, or that fresh water-ice in the outer Solar System can persist for gigayear timescales. C1 [Elliot, J. L.; Person, M. J.; Zuluaga, C. A.; Bosh, A. S.; Adams, E. R.; Brothers, T. C.; Gulbis, A. A. S.; Levine, S. E.; Lockhart, M.; Zangari, A. M.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Elliot, J. L.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Elliot, J. L.; Bright, L.; Dunham, E. W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gulbis, A. A. S.] So Africa Large Telescope & S African Astron Obse, ZA-8935 Cape Town, South Africa. [Levine, S. E.; Tilleman, T.] USNO, Flagstaff, AZ 86001 USA. [Levine, S. E.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. [Babcock, B. A.] Williams Coll, Dept Phys, Williamstown, MA 01267 USA. [DuPre, K.; Pasachoff, J. M.; Souza, S. P.] Williams Coll, Dept Astron, Williamstown, MA 01267 USA. [Rosing, W.] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Secrest, N.] Univ Hawaii, Hilo, HI 96720 USA. [Sheppard, S. S.] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. [Kakkala, M.] Univ Hawaii, Dept Geol, Leeward Community Coll, Pearl City, HI 96782 USA. [Berger, B.; Briggs, J. W.; Jacobson, G.; Valleli, P.; Volz, B.] Amateur Telescope Makers Boston, Westford, MA 01886 USA. [Briggs, J. W.] Dexter Southfield Sch, Brookline, MA 02145 USA. [Rapoport, S.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Hart, R.] Univ So Queensland, Mt Kent Observ, Toowoomba, Qld 4350, Australia. [Brucker, M.] Univ Nebraska, Dept Phys & Astron, Lincoln, NE 68588 USA. [Michel, R.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Mattingly, A.] IBM Corp, St Leonards, NSW 2065, Australia. [Zambrano-Marin, L.] Univ Texas Brownsville, Texas Southmost Coll, Nompuewenu Observ, Brownsville, TX 78520 USA. [Meyer, A. W.] NASA, Univ Space Res Assoc, SOFIA, Moffett Field, CA 94035 USA. [Wolf, J.] NASA, Deutsch SOFIA Inst, SOFIA, Moffett Field, CA 94035 USA. [Ryan, E. V.; Ryan, W. H.] Magdalena Ridge Observ, Socorro, NM 87801 USA. [Morzinski, K.; Grigsby, B.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brimacombe, J.] James Cook Univ, Cairns, Qld 4870, Australia. [Ragozzine, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Montano, H. G.] Univ Nacl Autonoma Mexico, Astron Observ, Managua, Nicaragua. [Gilmore, A.] Mt John Univ Observ, Lake Tekapo 7945, New Zealand. RP Elliot, JL (reprint author), MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. EM jle@mit.edu RI Ragozzine, Darin/C-4926-2013; Brucker, Melissa/B-4322-2014; OI Brucker, Melissa/0000-0002-2079-179X; Morzinski, Katie/0000-0002-1384-0063 FU NASA; NSF FX We are grateful to W. M. Grundy for supplying HV magnitudes from his database and for discussions of water-ice surfaces in the outer Solar System; to W. B. McKinnon for discussions of the physical state of water-ice at low temperatures; to E. D. Schmidt for use of the telescope and participating in the observations at Behlen Observatory; to B. Carter for help in obtaining telescope time at Mt Kent, and to L. A. Young for assisting with the McDonald observations. We thank D. Byrne of the Visitor Information Station at the Onizuka Center for International Astronomy on Mauna Kea for use of their equipment and facilitating the observations from their site. J.W. thanks E. Gates of Lick Observatory, and E. Becklin, E. Pfueller, M. Wiedemann and M. Burgdort of SOFIA, for support of his observations. B. Sicardy provided several comments that improved the paper. Occultation research at MIT and Williams College is supported by NASA and NSF. NR 30 TC 42 Z9 42 U1 0 U2 3 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUN 17 PY 2010 VL 465 IS 7300 BP 897 EP 900 DI 10.1038/nature09109 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 611HN UT WOS:000278804500031 PM 20559381 ER PT J AU Woodman, N AF Woodman, Neal TI Two new species of shrews (Soricidae) from the western highlands of Guatemala SO JOURNAL OF MAMMALOGY LA English DT Article DE Central America; Eulipotyphla; Insectivora; new species; Soricinae; Soricomorpha ID FOOD NICHE OVERLAP; SMALL-EARED SHREW; ECOLOGICAL SEPARATION; GENUS CRYPTOTIS; INSECTIVORA; MAMMALIA; MORPHOLOGY AB The broad-clawed shrews (Soricomorpha: Soricidae: Cryptotis) encompass a clade of 5 species Cryptotis alticolus (Merriam), C. goldmani (Merriam), C. goodwini Jackson, C. griseoventris Jackson, and C. peregrinus (Merriam) that is known collectively as the Cryptotis goldmani group and is characterized by broadened forefeet, elongated and broadened fore claws, and broadened humeri. These shrews are distributed in highland regions from central Mexico to Honduras. Two broad-clawed shrews, C. goodwini and C. griseoventris, occur in southern Mexico and Guatemala and are presumed sister species whose primary distinguishing feature is the larger size of C. goodwini. In an investigation of variation within and between these 2 species, I studied characteristics of the postcranial skeleton. Statistical analyses of a variety of character suites indicate that the forelimb morphology in this group exhibits less intraspecific variation and greater interspecific variation than cranio-mandibular morphology, although most skull characters support groupings based on forelimb characters. Together, these characters define 4 distinct groups among the specimens examined. C. griseoventris is restricted to the northern highlands of Chiapas, Mexico, and C. goodwini occurs in the southern highlands of Chiapas and Guatemala. Herein, I describe 2 new species of broad-clawed shrews from the Sierra de los Cuchumatanes, Guatemala. DOI: 10.1644/09-MAMM-A-346.1. C1 Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Woodman, N (reprint author), Smithsonian Inst, US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 25 TC 15 Z9 18 U1 0 U2 1 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 JUN 16 PY 2010 VL 91 IS 3 BP 566 EP 579 DI 10.1644/09-MAMM-A-346.1 PG 14 WC Zoology SC Zoology GA 615JG UT WOS:000279130300004 ER PT J AU Cote, R Juarros, E Kirby, K AF Cote, Robin Juarros, Elizabeth Kirby, Kate TI Formation of ultracold polar molecules in a single quantum state SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATION; HYDROGEN-ATOMS; LITHIUM ATOMS; LIH; CURVES AB We compute the formation rate of a polar molecule, LiH, into the lowest triplet electronic state, a (3)Sigma(+), via population of the intermediate excited electronic state, b(3)Pi, followed by radiative decay. We find large formation rates into the single rovibrational bound state (nu = 0, J = 0) of the a (3)Sigma(+), which can be explained by the unusually large overlap of its wave function with those of the two upper-most bound levels of the b(3)Pi. With conservative parameters, we estimate that over 10(4) molecules/s could be produced in the single rovibrational level of the a (3)Sigma(+) state. We also discuss scattering properties of LiH triplet molecules and their relevance to ultracold chemical reactions. C1 [Cote, Robin; Juarros, Elizabeth] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Kirby, Kate] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Kirby, Kate] Amer Phys Soc, College Pk, MD 20740 USA. RP Cote, R (reprint author), Univ Connecticut, Dept Phys, 2152 Hillside Rd, Storrs, CT 06269 USA. FU Department of Energy, Office of Basic Energy Sciences FX The work of E.J. and R. C. was supported in part by the Department of Energy, Office of Basic Energy Sciences. NR 33 TC 3 Z9 3 U1 1 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUN 16 PY 2010 VL 81 IS 6 AR 060704 DI 10.1103/PhysRevA.81.060704 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 611SX UT WOS:000278844000001 ER PT J AU Park, A van Breugel, M Ashton, MS Wishnie, M Mariscal, E Deago, J Ibarra, D Cedeno, N Hall, JS AF Park, Andrew van Breugel, Michiel Ashton, Mark S. Wishnie, Mark Mariscal, Emilio Deago, Jose Ibarra, Diogenes Cedeno, Norma Hall, Jefferson S. TI Local and regional environmental variation influences the growth of tropical trees in selection trials in the Republic of Panama SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Local environmental variation; Regional climate; Neotropical trees; Regression tree analysis; Panama; Species selection trials ID COSTA-RICA; FOREST TREES; RAIN-FOREST; SPATIAL DISTRIBUTIONS; TOPOGRAPHIC POSITION; PLANTATION FORESTRY; REGRESSION TREES; EDAPHIC FACTORS; DRY TROPICS; REFORESTATION AB Native Neotropical trees are being increasingly planted for restoration purposes and timber production, but we lack species-specific data on growth responses to different regional climates and local environmental variation. We used regression trees and variance components to quantify the effects of within and among-site environmental variation on the basal area (BA) of 21 Neotropical and two exotic tree species at three selection trials in the Republic of Panama. Sites represented distinct regional climates in which annual rainfall varied from 1100 to 2226 mm, with dry seasons of 4.1-6.7 months. Local environmental variables included measures of slope steepness and position, soil texture, soil color, and indicators of soil condition, such as subsoil rockiness. Basal area in 17 species responded primarily to regional differences among sites, and explained between 32% and 72% of species BA. Low BA plots of most species were located in the driest site, while high BA plots were found in the two wetter sites (mean BA difference = 117 +/- 20.6 cm(2)). Local variables also influenced the growth of 12 species, with percent slope, soil texture at 5-10 cm, subsoil rockiness and Munsell value from 20 to 50 cm explaining between 0.2% and 24.5% of within-site variance in BA. For these variables, BA differences across adjacent branches of regression trees ranged from 59 +/- 23.4 cm(2) (subsoil rockiness) to 176 +/- 45.9 cm(2) (Munsell value). Our results support the growing evidence that local as well as regional environmental variation influences tree community composition, growth and survival in mature forests. Furthermore, the heterogeneity of responses to local variables among environmentally sensitive species allowed us to make some preliminary site and species-specific silvicultural recommendations. For site generalists, future research should extend the current trials to multiple sites within each regional climate to separate climatic influences from those of the local environment. (C) 2010 Elsevier B.V. All rights reserved. C1 [Park, Andrew] Univ Winnipeg, Dept Biol, Winnipeg, MB R3B 2E9, Canada. [Park, Andrew] Univ Winnipeg, CFIR, Winnipeg, MB R3B 2E9, Canada. [van Breugel, Michiel; Wishnie, Mark; Mariscal, Emilio; Deago, Jose; Ibarra, Diogenes; Cedeno, Norma; Hall, Jefferson S.] Smithsonian Trop Res Inst, PRORENA, Ancon, Panama. [Ashton, Mark S.] Yale Univ, Sch Forestry & Environm Studies, New Haven, CT 06511 USA. RP Park, A (reprint author), Univ Winnipeg, Dept Biol, 515 Portage Ave, Winnipeg, MB R3B 2E9, Canada. EM a.park@uwinnipeg.ca OI van Breugel, Michiel/0000-0003-2778-7803 FU Frank Levinson Family Foundation; Grantham Foundation; School of Forestry and Environmental Studies, Yale University; NSERC; STRI; University of Winnipeg FX We thank the researchers, staff and students of PRORENA, a joint program of the School of Forestry and Environmental Studies, Yale University, and the Smithsonian Tropical Research Institute's Center for Tropical Forest Science, for designing and setting up this experiment and for collecting tree growth data. Funding to establish and maintain PRORENA is generously provided by The Frank Levinson Family Foundation at the Peninsula Community Foundation, the Grantham Foundation and the School of Forestry and Environmental Studies, Yale University. Andrew Park's research was funded by NSERC, STRI, and a startup grant from the University of Winnipeg. NR 56 TC 19 Z9 20 U1 2 U2 26 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-1127 EI 1872-7042 J9 FOREST ECOL MANAG JI For. Ecol. Manage. PD JUN 15 PY 2010 VL 260 IS 1 BP 12 EP 21 DI 10.1016/j.foreco.2010.03.021 PG 10 WC Forestry SC Forestry GA 614YJ UT WOS:000279095400002 ER PT J AU Simons, KK Harlow, GE Brueckner, HK Goldstein, SL Sorensen, SS Hemming, NG Langmuir, CH AF Simons, Kyla K. Harlow, George E. Brueckner, Hannes K. Goldstein, Steven L. Sorensen, Sorena S. Hemming, N. Gary Langmuir, Charles H. TI Lithium isotopes in Guatemalan and Franciscan HP-LT rocks: Insights into the role of sediment-derived fluids during subduction SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID MOTAGUA FAULT ZONE; PLASMA-MASS SPECTROMETRY; BEARING LAWSONITE ECLOGITE; OCEAN-RIDGE BASALTS; SECTOR ICP-MS; HIGH-PRESSURE; LI-ISOTOPE; PRECISE DETERMINATION; PERIDOTITE XENOLITHS; OROGENIC ECLOGITES AB High-pressure, low-temperature (HP-LT) rocks from a Cretaceous age subduction complex occur as tectonic blocks in serpentinite melange along the Motagua Fault (ME) in central Guatemala. Eclogite and jadeitite among these are characterized by trace element patterns with enrichments in fluid mobile elements, similar to arc lavas. Eclogite is recrystallized from MORB-like altered oceanic crust, presumably at the boundary between the down-going plate and overlying mantle wedge. Eclogite geochemistry, mineralogy and petrography suggest a two step petrogenesis of (1) dehydration during prograde metamorphism at low temperatures (<500 degrees C) followed by (2) partial rehydration/fertilization at even lower T during exhumation. In contrast, Guatemalan jadeitites are crystallized directly from low-T aqueous fluid as veins in serpentinizing mantle during both subduction and exhumation. The overall chemistry and mineralogy of Guatemalan eclogites are similar to those from the Franciscan Complex, California, implying similar P-T-x paths. Li concentrations (<= 90 ppm) in mineral separates and whole rocks (WR) from Guatemalan and Franciscan HP-LT rocks are significantly higher than MORB (4-6 ppm), but similar to HP-LT rocks globally. Li isotopic compositions range from -5 parts per thousand to +5 parts per thousand for Guatemalan HP LT rocks, and -4 parts per thousand to +1 parts per thousand for Franciscan eclogites, overlapping previous findings for other HP LT suites. The combination of Li concentrations greater than MORB, and Li isotopic values lighter than MORB are inconsistent with a simple dehydration model. We prefer a model in which Li systematics in Guatemalan and Franciscan eclogites reflect reequilibration with subduction fluids during exhumation. Roughly 5-10% of the Li in these fluids is derived from sediments. Model results predict that the dehydrated bulk ocean crust is isotopically lighter (delta Li-7 <= +1 +/- 3 parts per thousand) than the depleted mantle (similar to+3.5 +/- 0.5 parts per thousand), while the mantle wedge beneath the arc is the isotopic complement of the bulk crust. A subduction fluid with an AOC-GLOSS composition over the full range of model temperatures (50-600 degrees C) gives an average fluid delta Li-7 (similar to+7 +/- 5 parts per thousand 1 sigma) that is isotopically heavier than the depleted mantle. If the lowest temperature steps are excluded (50-260 degrees C) as too cold to participate in circulation of the mantle wedge, then the average subduction fluid (delta Li-7 = +4 +/- 2.3 parts per thousand 1 sigma, is indistinguishable from depleted mantle. Because of the relatively compatible nature of Li in metamorphic minerals, the most altered part of the crust (uppermost extrusives), may retain a Li isotopic signature(similar to+5 +/- 3 parts per thousand) heavier than the bulk crust. The range of Li isotopic values for OIB, IAB and MORB overlap, making it is difficult to resolve which of these components may contribute to the recycled component in the mantle using delta Li-7 alone. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Simons, Kyla K.; Brueckner, Hannes K.; Goldstein, Steven L.; Hemming, N. Gary] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Simons, Kyla K.; Brueckner, Hannes K.; Goldstein, Steven L.; Hemming, N. Gary] Columbia Univ, Dept Earth & Environm Sci, Palisades, NY 10964 USA. [Harlow, George E.] Amer Museum Nat Hist, Dept Earth & Planetary Sci, New York, NY 10024 USA. [Brueckner, Hannes K.; Hemming, N. Gary] CUNY Queens Coll, Sch Earth & Environm Sci, Flushing, NY 11367 USA. [Sorensen, Sorena S.] Smithsonian Inst, Dept Mineral Sci, Washington, DC USA. [Langmuir, Charles H.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Simons, KK (reprint author), Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, 4600 Rickenbacker Causeway, Miami, FL 33149 USA. EM ksimons@rsmas.miami.edu FU National Science Foundation [EAR 0309832, EAR 039320, EAR 0309116] FX We would like to thank Jinny Sisson, Tatsuki Tsujimori, Sidney Hemming and Jackie Dixon for their insight and editing. We would also like to thank A.E. Ryerson, Horst Marschall, Paul Tomascak, Thomas Zack, Samuel Agostini, Jeff Ryan and an anonymous reviewer for their help and useful comments. Funding for this work was made available by the National Science Foundation (EAR 0309832, EAR 039320 and EAR 0309116). NR 138 TC 25 Z9 28 U1 1 U2 29 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN 15 PY 2010 VL 74 IS 12 BP 3621 EP 3641 DI 10.1016/j.gca.2010.02.033 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 599WU UT WOS:000277945500018 ER PT J AU Aiello, A AF Aiello, Annette TI Adventures Among Ants: A Global Safari with a Cast of Trillions SO LIBRARY JOURNAL LA English DT Book Review C1 [Aiello, Annette] Smithsonian Trop Res Inst, Balboa, Panama. RP Aiello, A (reprint author), Smithsonian Trop Res Inst, Balboa, Panama. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 15 PY 2010 VL 135 IS 11 BP 88 EP 88 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 612KG UT WOS:000278896600261 ER PT J AU Rittenhouse, ST Sadeghpour, HR AF Rittenhouse, Seth T. Sadeghpour, H. R. TI Ultracold Giant Polyatomic Rydberg Molecules: Coherent Control of Molecular Orientation SO PHYSICAL REVIEW LETTERS LA English DT Article ID POLAR-MOLECULES; STATES AB We predict the existence of a class of ultracold giant molecules formed from trapped ultracold Rydberg atoms and polar molecules. The interaction which leads to the formation of such molecules is the anisotropic, long-range charge-dipole interaction. We show that prominent candidate molecules such as deuterated hydroxyl (OD) and KRb should bind to Rydberg rubidium atoms, with energies E(b) similar or equal to 5-25 GHz at distances R similar or equal to 0.1-1 mu m. These molecules form in double wells, mimicking chiral molecules, with each well containing a particular dipole orientation. We prepare a set of correlated dressed electron-dipole eigenstates which are used in an on-resonance Raman scheme to coherently control the molecular dipole orientation. C1 [Rittenhouse, Seth T.; Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Rittenhouse, ST (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM srittenhouse@cfa.harvard.edu; hsadeghpour@cfa.harvard.edu RI Rittenhouse, Seth/E-7688-2011 FU NSF at the Harvard-Smithsonian Center for Astrophysics and Harvard Physics Department FX We are grateful to M. Cavagnero, C. Ticknor, and J. Feist for discussions. This work was funded by a grant from the NSF to ITAMP at the Harvard-Smithsonian Center for Astrophysics and Harvard Physics Department. NR 21 TC 26 Z9 26 U1 0 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUN 15 PY 2010 VL 104 IS 24 AR 243002 DI 10.1103/PhysRevLett.104.243002 PG 4 WC Physics, Multidisciplinary SC Physics GA 610XJ UT WOS:000278773000001 PM 20867298 ER PT J AU Zulliger, DE Lessios, HA AF Zulliger, Deborah E. Lessios, H. A. TI Phylogenetic relationships in the genus Astropecten Gray (Paxillosida: Astropectinidae) on a global scale: molecular evidence for morphological convergence, species-complexes and possible cryptic speciation SO ZOOTAXA LA English DT Article DE global phylogeny; Asteroidea; mitochondrial DNA; echinoderm; marine invertebrates ID MULTIPLE SEQUENCE ALIGNMENT; MISSING DATA; MARINE SPECIATION; INCOMPLETE TAXA; CLUSTAL-X; PHYLOGEOGRAPHY; ECHINODERMATA; SYSTEMATICS; DIVERGENCE; DISPERSAL AB With over 150 described species, Astropecten Gray (Paxillosida: Astropectinidae) is one of the most species-rich genera among sea stars. This diversity is remarkable, because most species of Astropecten have a long-lived planktotrophic larval stage, which would be expected to lead to a low speciation rate. The taxonomy of this genus is complex and not well resolved, and phylogenetic relationships have only been addressed in the beginning of the last century. In order to resolve general taxonomic issues, identify speciation patterns and estimate species diversity within the genus Astropecten, we inferred a molecular phylogeny of 117 specimens of Astropecten belonging to 40 species from around the world using mitochondrial DNA (mtDNA) sequences of 12S rRNA, 16S rRNA and cytochrome oxidase subunit I (COI). We compared the resulting molecular phylogeny to a previously published morphological one by Doderlein and investigated the possibility of morphological convergence in species from different geographic regions. Finally, we also aimed at identifying potentially problematic descriptions and/or signs of cryptic speciation in Astropecten. The global molecular phylogeny exhibited three main clades, each containing specimens of the same geographic region: 1. the Indo-Pacific; 2. the Neotropics; and 3. the eastern Atlantic and Mediterranean. Phylogenetic inferences based on mtDNA indicate that morphological and ecological convergence has taken place in Astropecten, resulting in allopatric non-sister taxa with similar morphologies and habitat preferences. The comparison to Doderlein's morphological phylogeny reveals congruence on the whole but many discrepancies on a local scale, indicating that meaningful morphological characters are not easily identified and categorized in Astropecten. Our results also reveal that A. polyacanthus Muller & Troschel and A. indicus Doderlein are species-complexes; cryptic speciation may have occurred within each of these morphospecies. Furthermore, several variants, previously presumed to be conspecific, exhibit genetic distances large enough to justify recognizing them as separate species. C1 [Zulliger, Deborah E.] Univ Zurich, Zool Museum, CH-8057 Zurich, Switzerland. [Lessios, H. A.] Smithsonian Trop Res Inst, Balboa, Panama. RP Zulliger, DE (reprint author), Univ Zurich, Zool Museum, Winterthurerstr 190, CH-8057 Zurich, Switzerland. EM deborah.zulliger@access.uzh.ch; lessiosh@si.edu FU Smithsonian Tropical Research Institute; Swiss National Science Foundation FX For providing samples and hosting museum visits we thank the following people and institutions: The late C. Ahearn and the Smithsonian National Museum of Natural History, N. Ameziane and the Museum National d'Histoire Naturelle in Paris, the Zoological Museum Amsterdam, G. Borrero and INVEMAR in Colombia, M. Brogger, A. Cabrinovich and the London Natural History Museum, T. Cerveira Borges and the BIOPESCAS team (CCMAR, University of Algarve), the California Academy of Science Collections, R. Collin, J. Collins, T. Danckwart, S. Diliberto, A. Gebruk and the Shirshov Institute, L. Granek, S. Godwin and the Bishop Museum, G. Hendler and the Natural History Museum of Los Angeles County, J. Hoover, M. Huber, M. Komatsu, D. Lane, L. Lovell and the Scripps Institution of Oceanography, C. Luter and the Zoological Museum Berlin, H. Maag, M. Matsubara, P. Morais, C. Nielsen and the Zoological Museum of the University of Copenhagen, G. Pauley and the Florida Museum of Natural History, the Phuket Marine Biological Center, C. Ruckstuhl, H. Sekiguchi, M. Sewell, F. Solis-Marin and the Colleccion National de Equinodermos de la Universidad Nacional Autonoma de Mexico, the collections of the University of South Carolina, Q. Tahera and the Marine reference collection & Resource centre in Karachi, S. Tanner, S. Tassis, M. von Arx, K. Wakabayashi and P. Wirtz. We thank T. Bucher, A. and L. Calderon, S. Sbilordo and S. Tanner for technical and lab assistance. We received valuable advice on data analysis from M. Bernasconi, A. Faucci, A. Hiller-Galvis, R. Sponer and T. Wilson, for which we are very grateful. Further, we would like to thank D. Blake, A. Gale and C. Mah for their help with species identification and general advice and two anonymous reviewers for their useful comments. We are also greatly indebted to the late G. Ribi who helped outlining the project and provided assistance in many ways. This project was partially funded by the Smithsonian Tropical Research Institute and the Swiss National Science Foundation. NR 53 TC 10 Z9 10 U1 1 U2 4 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 14 PY 2010 IS 2504 BP 1 EP 19 PG 19 WC Zoology SC Zoology GA 610DZ UT WOS:000278712600001 ER PT J AU Hart, LB Wells, RS Adams, JD Rotstein, DS Schwacke, LH AF Hart, Leslie Burdett Wells, Randall S. Adams, Jeffrey D. Rotstein, Dave S. Schwacke, Lori H. TI Modeling lacaziosis lesion progression in common bottlenose dolphins Tursiops truncatus using long-term photographic records SO DISEASES OF AQUATIC ORGANISMS LA English DT Article DE Lacaziosis; Lacazia loboi; Bottlenose dolphin; Monomolecular growth model; Skin disease; Sarasota Bay; Lobomycosis ID INDIAN RIVER LAGOON; LOBOS-DISEASE; LOBOMYCOSIS; FLORIDA AB Lacaziosis (lobomycosis) is a skin disease caused by Lacazia loboi, occurring naturally only in humans and dolphins. Attempts to culture the pathogen in vitro have been unsuccessful, and inoculation studies of lacaziosis development in mice have provided only limited, short-term data on the progression and propagation of L. loboi. The present study used photographic data from long-term photo-identification and health assessment projects to model and quantify the progression of lacaziosis lesions in 3 common bottlenose dolphins Tursiops truncatus from Sarasota Bay, Florida, USA. Dorsal fin images throughout each animal's sighting history were examined for lesion growth, and the proportion of lesion coverage in each photograph was estimated using image analysis tools in Adobe Photoshop (R). The progression of lacaziosis lesions and lesion growth rates were modeled using a non-linear monomolecular growth model. As data on lacaziosis development and advancement are limited in humans and laboratory animals, dolphins with a long-term case history of the disease may serve as a good animal model to better understand lacaziosis progression. Furthermore, this study demonstrates the utility of long-term population monitoring data for tracking the progression of a poorly understood disease that is relevant to both dolphin and human health. C1 [Hart, Leslie Burdett; Schwacke, Lori H.] Med Univ S Carolina, Dept Med, Div Biostat & Epidemiol, Charleston, SC 29425 USA. [Wells, Randall S.] Mote Marine Lab, Chicago Zool Soc, Sarasota, FL 34236 USA. [Adams, Jeffrey D.] NOAA, NCCOS Ctr Coastal Environm Hlth & Biomol Res, Charleston, SC 29412 USA. [Rotstein, Dave S.] Univ Corp Atmospher Res, Smithsonian Museum Support Ctr, Suitland, MD 20746 USA. [Schwacke, Lori H.] NOAA, NCCOS Ctr Human Hlth Risk, Charleston, SC 29412 USA. RP Hart, LB (reprint author), Med Univ S Carolina, Dept Med, Div Biostat & Epidemiol, Charleston, SC 29425 USA. EM leslie.burdett@noaa.gov NR 38 TC 7 Z9 7 U1 0 U2 11 PU INTER-RESEARCH PI OLDENDORF LUHE PA NORDBUNTE 23, D-21385 OLDENDORF LUHE, GERMANY SN 0177-5103 J9 DIS AQUAT ORGAN JI Dis. Aquat. Org. PD JUN 11 PY 2010 VL 90 IS 2 BP 105 EP 112 DI 10.3354/dao02224 PG 8 WC Fisheries; Veterinary Sciences SC Fisheries; Veterinary Sciences GA 613KO UT WOS:000278978300003 PM 20662366 ER PT J AU Simionescu, A Werner, N Forman, WR Miller, ED Takei, Y Bohringer, H Churazov, E Nulsen, PEJ AF Simionescu, A. Werner, N. Forman, W. R. Miller, E. D. Takei, Y. Boehringer, H. Churazov, E. Nulsen, P. E. J. TI Metal transport by gas sloshing in M87 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: abundances; cooling flows; galaxies: individual: M87; X-rays: galaxies: clusters ID XMM-NEWTON OBSERVATIONS; ACTIVE GALACTIC NUCLEI; INTRA-CLUSTER MEDIUM; GALAXY CLUSTERS; VIRGO-CLUSTER; COLD FRONTS; INTRACLUSTER MEDIUM; GASEOUS ATMOSPHERE; ELLIPTIC GALAXIES; TEMPERATURE STRUCTURE AB We present the results of an XMM-Newton mosaic covering the central similar to 200 kpc of the nearby Virgo cluster. We focus on a strong surface brightness discontinuity in the outskirts of the brightest cluster galaxy (BCG), M87. Using both XMM-Newton and Suzaku, we derive accurate temperature and metallicity profiles across this feature and show that it is a cold front probably due to sloshing of the Virgo intracluster medium (ICM). It is also associated with a discontinuity in the chemical composition. The gas in the inner, bright region of the front is similar to 40 per cent more abundant in Fe than the gas outside the front, suggesting the important role of sloshing in transporting metals through the ICM. For the first time, we provide a quantitative estimate of the mass of Fe transported by a cold front. This amounts to similar to 6 per cent of the total Fe mass within the radial range affected by sloshing, significantly more than the amount of metals transported by the active galactic nucleus in the same cluster core. The very low Fe abundance of only similar to 0.2 solar immediately outside the cold front at a radius of 90 kpc suggests we are witnessing first-hand the transport of higher metallicity gas into a pristine region, whose abundance is typical of the cluster outskirts. The Mg/Fe and O/Fe abundance ratios remain approximately constant over the entire radial range between the centre of M87 and the faint side of the cold front, which requires the presence of a centrally peaked distribution not only for Fe but also for core-collapse type supernova products. This peak may stem from the star formation triggered as the BCG assembled during the protocluster phase. C1 [Simionescu, A.; Werner, N.] Stanford Univ, KIPAC, Stanford, CA 94305 USA. [Simionescu, A.; Boehringer, H.] MPE, D-85748 Garching, Germany. [Forman, W. R.; Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Takei, Y.] JAXA, ISAS, Sagamihara, Kanagawa 2298510, Japan. [Churazov, E.] MPA, D-85748 Garching, Germany. [Churazov, E.] Space Res Inst IKI, Moscow 117810, Russia. RP Simionescu, A (reprint author), Stanford Univ, KIPAC, 452 Lomita Mall, Stanford, CA 94305 USA. EM asimi@stanford.edu RI Churazov, Eugene/A-7783-2013; XRAY, SUZAKU/A-1808-2009; OI Nulsen, Paul/0000-0003-0297-4493 FU NASA [PF9-00070, PF8-90056, NNX08AZ88G]; Chandra X-ray Center, NASA [NAS8-03060]; USA (NASA); JAXA; NASA; DfG [SPP 1177, TR33]; Dark Universe FX The authors would like to thank J. de Plaa, A. Finoguenov, J. S. Kaastra, E. Roediger, M. Bruggen, C. Jones, A. Baldi and H. Matsumoto for helpful discussion. Support for this work was provided by NASA through Einstein Post-doctoral Fellowship grant numbers PF9-00070 and PF8-90056 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We acknowledge NASA grant NNX08AZ88G. AS is grateful for the hospitality of the Harvard-Smithsonian CfA. 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). The authors thank the Suzaku operation team and Guest Observer Facility, supported by JAXA and NASA. HB acknowledges support by the DfG Schwerpunkt Programm SPP 1177 and the Transregio Program TR33, the Dark Universe. NR 70 TC 33 Z9 33 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 JUN 11 PY 2010 VL 405 IS 1 BP 91 EP 99 DI 10.1111/j.1365-2966.2010.16450.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604YA UT WOS:000278313200029 ER PT J AU Ghisellini, G Della Ceca, R Volonteri, M Ghirlanda, G Tavecchio, F Foschini, L Tagliaferri, G Haardt, F Pareschi, G Grindlay, J AF Ghisellini, G. Della Ceca, R. Volonteri, M. Ghirlanda, G. Tavecchio, F. Foschini, L. Tagliaferri, G. Haardt, F. Pareschi, G. Grindlay, J. TI Chasing the heaviest black holes of jetted active galactic nuclei SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; BL Lacertae objects: general; quasars: general; gamma-rays: theory; X-rays: general ID RADIO-LOUD QUASARS; SLIM ACCRETION DISKS; EXTREME MEV BLAZAR; HIGH-REDSHIFT; OBSERVATIONAL APPEARANCE; FERMI BLAZARS; SKY SURVEY; TELESCOPE; UNIVERSE; GROWTH AB We investigate the physical properties of 10 blazars at redshift greater than 2 detected in the 3-yr all-sky survey performed by the Burst Alert Telescope (BAT) on board the Swift satellite. We find that the jets of these blazars are among the most powerful known. Furthermore, the mass of their central black hole, inferred from the optical-ultraviolet bump, exceeds a few billions of solar masses, with accretion luminosities being a large fraction of the Eddington one. We compare their properties with those of the brightest blazars of the 3-month survey performed by the Large Area Telescope (LAT) on board the Fermi satellite. We find that the BAT blazars have more powerful jets, more luminous accretion discs and larger black hole masses than LAT blazars. These findings can be simply understood on the basis of the blazar sequence, which suggests that the most powerful blazars have a spectral energy distribution with a high-energy peak at MeV (or even sub-MeV) energies. This implies that the most extreme blazars can be found more efficiently in hard X-rays, rather than in the high-energy gamma-ray band. We then discuss the implications of our findings for future missions, such as the New Hard X-ray Mission (NHXM) and especially the Energetic X-ray Imaging Survey Telescope (EXIST) mission which, during its planned 2-yr all-sky survey, is expected to detect thousands of blazars, with a few of them at z greater than or similar to 6. C1 [Ghisellini, G.; Ghirlanda, G.; Tavecchio, F.; Foschini, L.; Tagliaferri, G.; Pareschi, G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Della Ceca, R.] Osserv Astron Brera, INAF, I-20100 Milan, Italy. [Volonteri, M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Haardt, F.] Univ Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy. [Haardt, F.] Ist Nazl Fis Nucl, Sez Milano Bicocca, I-20126 Milan, Italy. [Grindlay, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ghisellini, G (reprint author), Osserv Astron Brera, INAF, Via Bianchi 46, I-23807 Merate, Italy. EM gabriele.ghisellini@brera.inaf.it RI Foschini, Luigi/H-3833-2012; OI Foschini, Luigi/0000-0001-8678-0324; Della Ceca, Roberto/0000-0001-7551-2252; Ghisellini, Gabriele/0000-0002-0037-1974; Pareschi, Giovanni/0000-0003-3967-403X; Tagliaferri, Gianpiero/0000-0003-0121-0723; Ghirlanda, Giancarlo/0000-0001-5876-9259 FU MIUR [2007 COFIN]; ASI [I/088/06/0]; NASA FX We thank the anonymous referee for his/her comments. We thank Andrea Merloni and Marco Ajello for discussions. This work was partly financially supported by a 2007 COFIN-MIUR and an ASI I/088/06/0 grants. This research made use of the NED which is operated by the Jet Propulsion Laboratory, Caltech, under contract with NASA, and the Swift public data made available by the HEASARC archive system. We also thank Neil Gehrels and the Swift team for quickly approving and performing the requested too observations of 1210+330. NR 58 TC 51 Z9 51 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 JUN 11 PY 2010 VL 405 IS 1 BP 387 EP 400 DI 10.1111/j.1365-2966.2010.16449.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604YA UT WOS:000278313200053 ER PT J AU Campbell, MA Evans, CJ Mackey, AD Gieles, M Alves, J Ascenso, J Bastian, N Longmore, AJ AF Campbell, M. A. Evans, C. J. Mackey, A. D. Gieles, M. Alves, J. Ascenso, J. Bastian, N. Longmore, A. J. TI VLT-MAD observations of the core of 30 Doradus SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: adaptive optics; techniques: high angular resolution; open clusters and associations: individual: 30 Doradus; Magellanic Clouds ID LARGE-MAGELLANIC-CLOUD; YOUNG STELLAR CLUSTERS; INITIAL MASS FUNCTION; SURFACE BRIGHTNESS PROFILES; WOLF-RAYET STARS; SPECTRAL CLASSIFICATION; INTERSTELLAR EXTINCTION; FUNDAMENTAL PARAMETERS; INFRARED OBSERVATIONS; INTERMEDIATE-MASS AB We present H- and K(s)-band imaging of three fields at the centre of 30 Doradus (30 Dor) in the Large Magellanic Cloud, obtained as part of the Science Demonstration programme with the Multiconjugate Adaptive optics Demonstrator (MAD) at the Very Large Telescope. Strehl ratios of 15-30 per cent were achieved in the K(s) band, yielding near-infrared images of this dense and complex region at unprecedented angular resolution at these wavelengths. The MAD data are used to construct a near-infrared luminosity profile for R136, the cluster at the core of 30 Dor. Using cluster profiles of the form used by Elson et al., we find the surface brightness can be fit by a relatively shallow power-law function (gamma similar to 1.5-1.7) over the full extent of the MAD data, which extends to a radius of similar to 40 arcsec (similar to 10 pc). We do not see compelling evidence for a break in the luminosity profile as seen in optical data in the literature, arguing that cluster asymmetries are the dominant source, although extinction effects and stars from nearby triggered star formation likely also contribute. These results highlight the need to consider cluster asymmetries and multiple spatial components in interpretation of the luminosity profiles of distant unresolved clusters. We also investigate seven candidate young stellar objects reported by Gruendl & Chu from Spitzer observations, six of which have apparent counterparts in the MAD images. The most interesting of these (053839.24-690552.3) appears related to a striking bow-shock-like feature, orientated away from both R136 and the Wolf-Rayet star Brey 75, at distances of 19.5 and 8 arcsec (4.7 and 1.9 pc in projection), respectively. C1 [Campbell, M. A.; Evans, C. J.; Mackey, A. D.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Evans, C. J.; Longmore, A. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gieles, M.] European So Observ, Santiago 19, Chile. [Alves, J.] Calar Alto Observ, Ctr Astron Hispano Aleman, Almeria 04004, Spain. [Ascenso, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bastian, N.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Campbell, MA (reprint author), Univ Edinburgh, Royal Observ, Inst Astron, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM mac@roe.ac.uk OI Gieles, Mark/0000-0002-9716-1868; Alves, Joao/0000-0002-4355-0921 FU Science and Technology Facilities Council (STFC) FX The data presented here were obtained during the MAD Science Demonstration campaign (package name MADD-SD-EV, ID 96408) and we are indebted to the MAD team of Paola Amico, Enrico Marchetti and Johann Kolb (with particular thanks to Johann for the Strehl maps). MAC acknowledges financial support from the Science and Technology Facilities Council (STFC). We thank the referee, Morten Andersen, and Nolan Walborn and Jesus Maiz Apellaniz for their suggestions and comments which improved this article. We also thank the HAWK-I instrument and commissioning teams for making the 30 Dor frames available and John Pritchard for his advice with those images, Robert Gruendl for correspondence regarding the YSO catalogue, Yazan Al Momany for a fateful conversation over coffee in Santiago and subsequent advice on the individual frames method, and Peter Stetson for making his routines available to us. NR 68 TC 30 Z9 30 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2010 VL 405 IS 1 BP 421 EP 435 DI 10.1111/j.1365-2966.2010.16447.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604YA UT WOS:000278313200055 ER PT J AU Nelemans, G Voss, R Nielsen, MTB Roelofs, G AF Nelemans, Gijs Voss, Rasmus Nielsen, Mikkel T. B. Roelofs, Gijs TI The Type Ib supernova 2010O: an explosion in a Wolf-Rayet X-ray binary? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: close; supernovae: general; X-ray: binaries ID ARP 299; IC-10 X-1; PROGENITOR; COUNTERPART; EVOLUTION; GALAXIES; ARP-299; CHANDRA; 2007ON AB The Type Ib supernova 2010O was recently discovered in the interacting starburst galaxy Arp 299. We present an analysis of two archival Chandra X-ray observations of Arp 299 taken before the explosion and show that there is a transient X-ray source at a position consistent with the supernova. Due to the diffuse emission, the background is difficult to estimate. We estimate the flux of the transient from the difference of the two X-ray images and conclude that the transient can be described by a 0.225-keV blackbody with a luminosity of 2.5 +/- 0.7 x 10(39) erg s(-1) for a distance of 41 Mpc. These properties put the transient in between the Galactic black hole binary XTE J1550-564 and the ultraluminous X-ray binaries NGC 1313 X-1 and X-2. The high level of X-ray variability associated with the active starburst makes it impossible to rule out a chance alignment. If the source is associated with the supernova, it suggests SN 2010O is the explosion of the second star in a Wolf-Rayet X-ray binary, such as Cyg X-3, IC 10 X-1 and NGC 300 X-1. C1 [Nelemans, Gijs; Nielsen, Mikkel T. B.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Voss, Rasmus] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Voss, Rasmus] Tech Univ Munich, D-85748 Garching, Germany. [Roelofs, Gijs] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roelofs, Gijs] Netherlands Bur Econ Policy Anal, NL-2585 JR The Hague, Netherlands. RP Nelemans, G (reprint author), Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands. EM nelemans@astro.ru.nl RI Nelemans, Gijs/D-3177-2012 OI Nelemans, Gijs/0000-0002-0752-2974 FU Netherlands Organisation of Scientific Research; DFG FX We thank Joseph Brimacombe for providing us the fits files of his observations, Peter Jonker for discussions on the properties of black hole binaries and the referee for helpful comments. We thank the Central Bureau for Astronomical Telegrams for providing a list of SNe. This research has made use of data obtained from the Chandra Data Archive and software provided by the Chandra X-ray Center in the application package CIAO. GN and MTBN are supported by the Netherlands Organisation of Scientific Research. This research was supported by the DFG cluster of excellence 'Origin and Structure of the Universe'. NR 32 TC 9 Z9 9 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 11 PY 2010 VL 405 IS 1 BP L71 EP L75 DI 10.1111/j.1745-3933.2010.00861.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 604YA UT WOS:000278313200015 ER PT J AU Bond, NA Ivezic, Z Sesar, B Juric, M Munn, JA Kowalski, A Loebman, S Roskar, R Beers, TC Dalcanton, J Rockosi, CM Yanny, B Newberg, HJ Prieto, CA Wilhelm, R Lee, YS Sivarani, T Majewski, SR Norris, JE Bailer-Jones, CAL Fiorentin, PR Schlegel, D Uomoto, A Lupton, RH Knapp, GR Gunn, JE Covey, KR Smith, JA Miknaitis, G Doi, M Tanaka, M Fukugita, M Kent, S Finkbeiner, D Quinn, TR Hawley, S Anderson, S Kiuchi, F Chen, A Bushong, J Sohi, H Haggard, D Kimball, A McGurk, R Barentine, J Brewington, H Harvanek, M Kleinman, S Krzesinski, J Long, D Nitta, A Snedden, S Lee, B Pier, JR Harris, H Brinkmann, J Schneider, DP AF Bond, Nicholas A. Ivezic, Zeljko Sesar, Branimir Juric, Mario Munn, Jeffrey A. Kowalski, Adam Loebman, Sarah Roskar, Rok Beers, Timothy C. Dalcanton, Julianne Rockosi, Constance M. Yanny, Brian Newberg, Heidi J. Prieto, Carlos Allende Wilhelm, Ron Lee, Young Sun Sivarani, Thirupathi Majewski, Steven R. Norris, John E. Bailer-Jones, Coryn A. L. Fiorentin, Paola Re Schlegel, David Uomoto, Alan Lupton, Robert H. Knapp, Gillian R. Gunn, James E. Covey, Kevin R. Smith, J. Allyn Miknaitis, Gajus Doi, Mamoru Tanaka, Masayuki Fukugita, Masataka Kent, Steve Finkbeiner, Douglas Quinn, Tom R. Hawley, Suzanne Anderson, Scott Kiuchi, Furea Chen, Alex Bushong, James Sohi, Harkirat Haggard, Daryl Kimball, Amy McGurk, Rosalie Barentine, John Brewington, Howard Harvanek, Mike Kleinman, Scott Krzesinski, Jurek Long, Dan Nitta, Atsuko Snedden, Stephanie Lee, Brian Pier, Jeffrey R. Harris, Hugh Brinkmann, Jonathan Schneider, Donald P. TI THE MILKY WAY TOMOGRAPHY WITH SDSS. III. STELLAR KINEMATICS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: disk; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: stellar content; Galaxy: structure; methods: data analysis; stars: statistics ID DIGITAL SKY SURVEY; GENEVA-COPENHAGEN SURVEY; HORIZONTAL-BRANCH STARS; SURVEY DATA RELEASE; SOLAR NEIGHBORHOOD; SPECTROSCOPIC SURVEY; GALACTIC STRUCTURE; CIRCULAR VELOCITY; PROPER MOTIONS; HIPPARCOS DATA AB We study Milky Way kinematics using a sample of 18.8 million main-sequence stars with r < 20 and proper-motion measurements derived from Sloan Digital Sky Survey (SDSS) and POSS astrometry, including similar to 170,000 stars with radial-velocity measurements from the SDSS spectroscopic survey. Distances to stars are determined using a photometric-parallax relation, covering a distance range from similar to 100 pc to 10 kpc over a quarter of the sky at high Galactic latitudes (|b| > 20 degrees). We find that in the region defined by 1 kpc < Z < 5 kpc and 3 kpc < R < 13 kpc, the rotational velocity for disk stars smoothly decreases, and all three components of the velocity dispersion increase, with distance from the Galactic plane. In contrast, the velocity ellipsoid for halo stars is aligned with a spherical coordinate system and appears to be spatially invariant within the probed volume. The velocity distribution of nearby (Z < 1 kpc) K/M stars is complex, and cannot be described by a standard Schwarzschild ellipsoid. For stars in a distance-limited subsample of stars (< 100 pc), we detect a multi-modal velocity distribution consistent with that seen by HIPPARCOS. This strong non-Gaussianity significantly affects the measurements of the velocity-ellipsoid tilt and vertex deviation when using the Schwarzschild approximation. We develop and test a simple descriptive model for the overall kinematic behavior that captures these features over most of the probed volume, and can be used to search for substructure in kinematic and metallicity space. We use this model to predict further improvements in kinematic mapping of the Galaxy expected from Gaia and the Large Synoptic Survey Telescope. C1 [Bond, Nicholas A.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Ivezic, Zeljko; Sesar, Branimir; Kowalski, Adam; Loebman, Sarah; Roskar, Rok; Dalcanton, Julianne; Quinn, Tom R.; Hawley, Suzanne; Anderson, Scott; Kiuchi, Furea; Chen, Alex; Bushong, James; Sohi, Harkirat; Haggard, Daryl; Kimball, Amy; McGurk, Rosalie] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Juric, Mario] Inst Adv Study, Princeton, NJ 08540 USA. [Munn, Jeffrey A.; Pier, Jeffrey R.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86002 USA. [Beers, Timothy C.; Lee, Young Sun; Sivarani, Thirupathi] Michigan State Univ, Joint Inst Nucl Astrophys, E Lansing, MI 48824 USA. [Rockosi, Constance M.] Univ Calif Santa Cruz, Santa Cruz, CA 95060 USA. [Yanny, Brian; Miknaitis, Gajus; Kent, Steve] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA. [Newberg, Heidi J.] Rensselaer Polytech Inst, Dept Phys Appl Phys & Astron, Troy, NY 12180 USA. [Prieto, Carlos Allende] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Prieto, Carlos Allende] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Prieto, Carlos Allende] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Wilhelm, Ron] Texas Tech Univ, Dept Phys, Lubbock, TX 79409 USA. [Sivarani, Thirupathi] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Majewski, Steven R.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Norris, John E.; Harris, Hugh] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Bailer-Jones, Coryn A. L.; Fiorentin, Paola Re] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Fiorentin, Paola Re] Univ Ljubljana, Dept Phys, Ljubljana 1000, Slovenia. [Schlegel, David; Lee, Brian] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. [Uomoto, Alan] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lupton, Robert H.; Knapp, Gillian R.; Gunn, James E.] Princeton Univ Observ, Princeton, NJ 08544 USA. [Covey, Kevin R.; Finkbeiner, Douglas] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Smith, J. Allyn] Austin Peay State Univ, Dept Phys & Astron, Clarksville, TN 37044 USA. [Doi, Mamoru] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Tanaka, Masayuki] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Fukugita, Masataka] Univ Tokyo, Inst Cosm Ray Res, Chiba, Japan. [Barentine, John; Brewington, Howard; Harvanek, Mike; Kleinman, Scott; Krzesinski, Jurek; Long, Dan; Nitta, Atsuko; Snedden, Stephanie; Brinkmann, Jonathan] Apache Point Observ, Sunspot, NM 88349 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Bond, NA (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA. OI McGurk, Rosalie/0000-0003-2064-4105; Re Fiorentin, Paola/0000-0002-4995-0475; Covey, Kevin/0000-0001-6914-7797 FU NSF [AST-615991, AST-0707901, AST-0551161, AST-02-38683, AST-06-07634, AST-0807444, PHY05-51164]; NASA [NAG5-13057, NAG5-13147, NNXO-8AH83G]; Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA) [PHY 08-22648]; U.S. National Science Foundation; Marie Curie Research Training Network ELSA (European Leadership in Space Astrometry) [MRTN-CT-2006-033481]; Fermi Research Alliance, LLC, United States Department of Energy [DE-AC02-07CH11359]; Alfred P. Sloan Foundation; Participating Institutions; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank Vladimir Korchagin for making his code for calculating equilibrium velocity dispersion profile available to us.. 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. J. Dalcanton acknowledges NSF CAREER grant AST-02-38683. D. Schneider acknowledges support by NSF grant AST-06-07634. Allende Prieto acknowledges support by NASA grants NAG5-13057 and NAG5-13147. T. C. Beers, Y.S. Lee, and T. Sivarani acknowledge partial support from PHY 08-22648: Physics Frontier Center/Joint Institute for Nuclear Astrophysics (JINA), awarded by the U.S. National Science Foundation. P. Re Fiorentin acknowledges support through the Marie Curie Research Training Network ELSA (European Leadership in Space Astrometry) under contract MRTN-CT-2006-033481. M. J. acknowledges support by NASA grant NNXO-8AH83G and NSF grant AST-0807444. 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-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 85 TC 94 Z9 95 U1 0 U2 14 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 1 EP 29 DI 10.1088/0004-637X/716/1/1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000001 ER PT J AU Abdo, AA Ackermann, M Agudo, I Ajello, M Aller, HD Aller, MF Angelakis, E Arkharov, AA Axelsson, M Bach, U Baldini, L Ballet, J Barbiellini, G Bastieri, D Baughman, BM Bechtol, K Bellazzini, R Benitez, E Berdyugin, A Berenji, B Blandford, RD Bloom, ED Boettcher, M Bonamente, E Borgland, AW Bregeon, J Brez, A Brigida, M Bruel, P Burnett, TH Burrows, D Buson, S Caliandro, GA Calzoletti, L Cameron, RA Capalbi, M Caraveo, PA Carosati, D Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chaty, S Chekhtman, A Chen, WP Chiang, J Chincarini, G Ciprini, S Claus, R Cohen-Tanugi, J Colafrancesco, S Cominsky, LR Conrad, J Costamante, L Cutini, S D'ammando, F Deitrick, R D'Elia, V Dermer, CD de Angelis, A de Palma, F Digel, SW Donnarumma, I Silva, EDE Drell, PS Dubois, R Dultzin, D Dumora, D Falcone, A Farnier, C Favuzzi, C Fegan, SJ Focke, WB Forne, E Fortin, P Frailis, M Fuhrmann, L Fukazawa, Y Funk, S Fusco, P Gomez, JL Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giommi, P Giordano, F Giuliani, A Glanzman, T Godfrey, G Grenier, IA Gronwall, C Grove, JE Guillemot, L Guiriec, S Gurwell, MA Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Healey, SE Heidt, J Hiriart, D Horan, D Hoversten, EA Hughes, RE Itoh, R Jackson, MS Johannesson, G Johnson, AS Johnson, WN Jorstad, SG Kadler, M Kamae, T Katagiri, H Kataoka, J Kawai, N Kennea, J Kerr, M Kimeridze, G Knodlseder, J Kocian, ML Kopatskaya, EN Koptelova, E Konstantinova, TS Kovalev, YY Kovalev, YA Kurtanidze, OM Kuss, M Lande, J Larionov, VM Latronico, L Leto, P Lindfors, E Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Madejski, GM Makeev, A Marchegiani, P Marscher, AP Marshall, F Max-Moerbeck, W Mazziotta, MN McConville, W McEnery, JE Meurer, C Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nestoras, I Nilsson, K Nizhelsky, NA Nolan, PL Norris, JP Nuss, E Ohsugi, T Ojha, R Omodei, N Orlando, E Ormes, JF Osborne, J Ozaki, M Pacciani, L Padovani, P Pagani, C Page, K Paneque, D Panetta, JH Parent, D Pasanen, M Pavlidou, V Pelassa, V Pepe, M Perri, M Pesce-Rollins, M Piranomonte, S Piron, F Pittori, C Porter, TA Puccetti, S Rahoui, F Raino, S Raiteri, C Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Richards, JL Ritz, S Rochester, LS Rodriguez, AY Romani, RW Ros, JA Roth, M Roustazadeh, P Ryde, F Sadrozinski, HFW Sadun, A Sanchez, D Sander, A Parkinson, PMS Scargle, JD Sellerholm, A Sgro, C Shaw, MS Sigua, LA Siskind, EJ Smith, DA Smith, PD Spandre, G Spinelli, P Starck, JL Stevenson, M Stratta, G Strickman, MS Suson, DJ Tajima, H Takahashi, H Takahashi, T Takalo, LO Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Uchiyama, Y Usher, TL Vasileiou, V Verrecchia, F Vilchez, N Villata, M Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Ylinen, T Zensus, JA Zhekanis, GV Ziegler, M AF Abdo, A. A. Ackermann, M. Agudo, I. Ajello, M. Aller, H. D. Aller, M. F. Angelakis, E. Arkharov, A. A. Axelsson, M. Bach, U. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Baughman, B. M. Bechtol, K. Bellazzini, R. Benitez, E. Berdyugin, A. Berenji, B. Blandford, R. D. Bloom, E. D. Boettcher, M. Bonamente, E. Borgland, A. W. Bregeon, J. Brez, A. Brigida, M. Bruel, P. Burnett, T. H. Burrows, D. Buson, S. Caliandro, G. A. Calzoletti, L. Cameron, R. A. Capalbi, M. Caraveo, P. A. Carosati, D. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe. Charles, E. Chaty, S. Chekhtman, A. Chen, W. P. Chiang, J. Chincarini, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Colafrancesco, S. Cominsky, L. R. Conrad, J. Costamante, L. Cutini, S. D'ammando, F. Deitrick, R. D'Elia, V. Dermer, C. D. de Angelis, A. de Palma, F. Digel, S. W. Donnarumma, I. do Couto e Silva, E. Drell, P. S. Dubois, R. Dultzin, D. Dumora, D. Falcone, A. Farnier, C. Favuzzi, C. Fegan, S. J. Focke, W. B. Forne, E. Fortin, P. Frailis, M. Fuhrmann, L. Fukazawa, Y. Funk, S. Fusco, P. Gomez, J. L. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giommi, P. Giordano, F. Giuliani, A. Glanzman, T. Godfrey, G. Grenier, I. A. Gronwall, C. Grove, J. E. Guillemot, L. Guiriec, S. Gurwell, M. A. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Healey, S. E. Heidt, J. Hiriart, D. Horan, D. Hoversten, E. A. Hughes, R. E. Itoh, R. Jackson, M. S. Johannesson, G. Johnson, A. S. Johnson, W. N. Jorstad, S. G. Kadler, M. Kamae, T. Katagiri, H. Kataoka, J. Kawai, N. Kennea, J. Kerr, M. Kimeridze, G. Knoedlseder, J. Kocian, M. L. Kopatskaya, E. N. Koptelova, E. Konstantinova, T. S. Kovalev, Y. Y. Kovalev, Yu. A. Kurtanidze, O. M. Kuss, M. Lande, J. Larionov, V. M. Latronico, L. Leto, P. Lindfors, E. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Madejski, G. M. Makeev, A. Marchegiani, P. Marscher, A. P. Marshall, F. Max-Moerbeck, W. Mazziotta, M. N. McConville, W. McEnery, J. E. Meurer, C. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nestoras, I. Nilsson, K. Nizhelsky, N. A. Nolan, P. L. Norris, J. P. Nuss, E. Ohsugi, T. Ojha, R. Omodei, N. Orlando, E. Ormes, J. F. Osborne, J. Ozaki, M. Pacciani, L. Padovani, P. Pagani, C. Page, K. Paneque, D. Panetta, J. H. Parent, D. Pasanen, M. Pavlidou, V. Pelassa, V. Pepe, M. Perri, M. Pesce-Rollins, M. Piranomonte, S. Piron, F. Pittori, C. Porter, T. A. Puccetti, S. Rahoui, F. Raino, S. Raiteri, C. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Richards, J. L. Ritz, S. Rochester, L. S. Rodriguez, A. Y. Romani, R. W. Ros, J. A. Roth, M. Roustazadeh, P. Ryde, F. Sadrozinski, H. F. -W. Sadun, A. Sanchez, D. Sander, A. Parkinson, P. M. Saz Scargle, J. D. Sellerholm, A. Sgro, C. Shaw, M. S. Sigua, L. A. Siskind, E. J. Smith, D. A. Smith, P. D. Spandre, G. Spinelli, P. Starck, J. -L. Stevenson, M. Stratta, G. Strickman, M. S. Suson, D. J. Tajima, H. Takahashi, H. Takahashi, T. Takalo, L. O. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Uchiyama, Y. Usher, T. L. Vasileiou, V. Verrecchia, F. Vilchez, N. Villata, M. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Ylinen, T. Zensus, J. A. Zhekanis, G. V. Ziegler, M. TI THE SPECTRAL ENERGY DISTRIBUTION OF FERMI BRIGHT BLAZARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE BL Lacertae objects: general; galaxies: active; gamma rays: galaxies; quasars: general; radiation mechanisms: non-thermal ID BL-LACERTAE OBJECTS; GAMMA-RAY EMISSION; ALL-SKY SURVEY; MICROWAVE BACKGROUND-RADIATION; LOG-PARABOLIC SPECTRA; LARGE-AREA TELESCOPE; MULTIWAVELENGTH OBSERVATIONS; ELECTRON ACCELERATION; PARTICLE-ACCELERATION; LAC OBJECTS AB We have conducted a detailed investigation of the broadband spectral properties of the gamma-ray selected blazars of the Fermi LAT Bright AGN Sample (LBAS). By combining our accurately estimated Fermi gamma-ray spectra with Swift, radio, infra-red, optical, and other hard X-ray/gamma-ray data, collected within 3 months of the LBAS data taking period, we were able to assemble high-quality and quasi-simultaneous spectral energy distributions (SED) for 48 LBAS blazars. The SED of these gamma-ray sources is similar to that of blazars discovered at other wavelengths, clearly showing, in the usual log nu-log nu F-nu representation, the typical broadband spectral signatures normally attributed to a combination of low-energy synchrotron radiation followed by inverse Compton emission of one or more components. We have used these SED to characterize the peak intensity of both the low-and the high-energy components. The results have been used to derive empirical relationships that estimate the position of the two peaks from the broadband colors (i.e., the radio to optical, alpha(ro), and optical to X-ray, alpha(ox), spectral slopes) and from the gamma-ray spectral index. Our data show that the synchrotron peak frequency (nu(S)(peak)) is positioned between 10(12.5) and 10(14.5) Hz in broad-lined flat spectrum radio quasars (FSRQs) and between 10(13) and 10(17) Hz in featureless BL Lacertae objects. We find that the gamma-ray spectral slope is strongly correlated with the synchrotron peak energy and with the X-ray spectral index, as expected at first order in synchrotron-inverse Compton scenarios. However, simple homogeneous, one-zone, synchrotron self-Compton (SSC) models cannot explain most of our SED, especially in the case of FSRQs and low energy peaked (LBL) BL Lacs. More complex models involving external Compton radiation or multiple SSC components are required to reproduce the overall SED and the observed spectral variability. While more than 50% of known radio bright high energy peaked (HBL) BL Lacs are detected in the LBAS sample, only less than 13% of known bright FSRQs and LBL BL Lacs are included. This suggests that the latter sources, as a class, may be much fainter gamma-ray emitters than LBAS blazars, and could in fact radiate close to the expectations of simple SSC models. We categorized all our sources according to a new physical classification scheme based on the generally accepted paradigm for Active Galactic Nuclei and on the results of this SED study. Since the LAT detector is more sensitive to flat spectrum gamma-ray sources, the correlation between nu(S)(peak) and gamma-ray spectral index strongly favors the detection of high energy peaked blazars, thus explaining the Fermi overabundance of this type of sources compared to radio and EGRET samples. This selection effect is similar to that experienced in the soft X-ray band where HBL BL Lacs are the dominant type of blazars. C1 [Abdo, A. A.; Chekhtman, A.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Makeev, A.; Parent, D.; Strickman, M. S.; Wood, K. S.] USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. [Abdo, A. A.] Natl Acad Sci, Natl Res Council, Washington, DC 20001 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Ackermann, M.; Ajello, M.; Bechtol, K.; Berenji, B.; Blandford, R. D.; Bloom, E. D.; Borgland, A. W.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Costamante, L.; Digel, S. W.; do Couto e Silva, E.; Drell, P. S.; Dubois, R.; Focke, W. B.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Healey, S. E.; Johannesson, G.; Johnson, A. S.; Kamae, T.; Kocian, M. L.; Lande, J.; Madejski, G. M.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Omodei, N.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Rochester, L. S.; Romani, R. W.; Shaw, M. S.; Tajima, H.; Tanaka, T.; Thayer, J. B.; Thayer, J. G.; Uchiyama, Y.; Usher, T. L.; Waite, A. P.; Wang, P.] Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. [Agudo, I.; Gomez, J. L.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Aller, H. D.; Aller, M. F.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Angelakis, E.; Bach, U.; Fuhrmann, L.; Guillemot, L.; Kovalev, Y. Y.; Nestoras, I.; Zensus, J. A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Arkharov, A. A.] Pulkovo Observ, St Petersburg 196140, Russia. [Axelsson, M.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Axelsson, M.] Lund Observ, SE-22100 Lund, Sweden. [Axelsson, M.; Conrad, J.; Jackson, M. 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[Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Ritz, S.; Sadrozinski, H. F. -W.; Parkinson, P. M. Saz; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Sadun, A.] Univ Colorado, Dept Phys, Denver, CO 80220 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. [Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden. RP Abdo, AA (reprint author), USN, Res Lab, Div Space Sci, Washington, DC 20375 USA. RI Starck, Jean-Luc/D-9467-2011; Tosti, Gino/E-9976-2013; Larionov, Valeri/H-1349-2013; Kopatskaya, Evgenia/H-4720-2013; Thompson, David/D-2939-2012; Harding, Alice/D-3160-2012; Gehrels, Neil/D-2971-2012; McEnery, Julie/D-6612-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Ozaki, Masanobu/K-1165-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Kurtanidze, Omar/J-6237-2014; Kovalev, Yuri/J-5671-2013; Funk, Stefan/B-7629-2015; Pavlidou, Vasiliki/C-2944-2011; Agudo, Ivan/G-1701-2015; Kovalev, Yuri/N-1053-2015; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Loparco, Francesco/O-8847-2015; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Pittori, Carlotta/C-7710-2016; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Stratta, Maria Giuliana/L-3045-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Verrecchia, Francesco/0000-0003-3455-5082; Raiteri, Claudia Maria/0000-0003-1784-2784; Padovani, Paolo/0000-0002-4707-6841; Puccetti, Simonetta/0000-0002-2734-7835; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Chaty, Sylvain/0000-0002-5769-8601; Pesce-Rollins, Melissa/0000-0003-1790-8018; Axelsson, Magnus/0000-0003-4378-8785; Perri, Matteo/0000-0003-3613-4409; D'Elia, Valerio/0000-0002-7320-5862; Villata, Massimo/0000-0003-1743-6946; Leto, Paolo/0000-0003-4864-2806; giommi, paolo/0000-0002-2265-5003; De Angelis, Alessandro/0000-0002-3288-2517; Donnarumma, Immacolata/0000-0002-4700-4549; Frailis, Marco/0000-0002-7400-2135; Caraveo, Patrizia/0000-0003-2478-8018; Starck, Jean-Luc/0000-0003-2177-7794; Larionov, Valeri/0000-0002-4640-4356; Kopatskaya, Evgenia/0000-0001-9518-337X; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Kovalev, Yuri/0000-0001-9303-3263; Funk, Stefan/0000-0002-2012-0080; Pavlidou, Vasiliki/0000-0002-0870-1368; Agudo, Ivan/0000-0002-3777-6182; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Loparco, Francesco/0000-0002-1173-5673; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Pittori, Carlotta/0000-0001-6661-9779; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Stratta, Maria Giuliana/0000-0003-1055-7980; Torres, Diego/0000-0002-1522-9065; Rando, Riccardo/0000-0001-6992-818X; Sgro', Carmelo/0000-0001-5676-6214; Pacciani, Luigi/0000-0001-6897-5996; Angelakis, Emmanouil/0000-0001-7327-5441; Kadler, Matthias/0000-0001-5606-6154; Cutini, Sara/0000-0002-1271-2924; Berenji, Bijan/0000-0002-4551-772X; Gasparrini, Dario/0000-0002-5064-9495; Tramacere, Andrea/0000-0002-8186-3793; Baldini, Luca/0000-0002-9785-7726 FU Fermi-LAT Collaboration; 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; K. A. Wallenberg Foundation in Sweden; Russian Foundation for Basic Research [01-02-6812, 08-02-00545]; Georgian National Science Foundation [GNSF/ST-08/4-404]; Smithsonian Institution; Academia Sinica. St. Petersburg University; Russian RFBR foundation [09-02-00092] FX The Fermi-LAT Collaboration acknowledges the generous support of a number of agencies and institutes that have supported the Fermi-LAT Collaboration. 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 from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the K. A. Wallenberg Foundation in Sweden. This research is based also on observations with the 100 m telescope of the MPIfR (Max-Planck-Institut fur Radioastronomie) at Effelsberg. RATAN-600 observations are supported in part by the Russian Foundation for Basic Research (projects 01-02-6812 and 08-02-00545). Part of this work was supported by Georgian National Science Foundation grant GNSF/ST-08/4-404 The mid-infrared VISIR results are based on observations carried out at the European Southern Observatory under programmes ID 078.B-0366, 079.B-0448, and 081.B-0404. 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. St. Petersburg University team acknowledges support from Russian RFBR foundation via grant 09-02-00092. AZT-24 observations are made within an agreement between Pulkovo, Rome, and Teramo observatories. We acknowledge the use of data and software facilities from the ASDC, managed by the Italian Space Agency (ASI). Part of this work is based on archival data and on bibliographic information obtained from the NASA/IPAC Extragalactic Database (NED) and from the Astrophysics Data System (ADS). NR 103 TC 307 Z9 314 U1 8 U2 32 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 30 EP 70 DI 10.1088/0004-637X/716/1/30 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000002 ER PT J AU Williams, BF Dalcanton, JJ Gilbert, KM Stilp, A Dolphin, A Seth, AC Weisz, D Skillman, E AF Williams, Benjamin F. Dalcanton, Julianne J. Gilbert, Karoline M. Stilp, Adrienne Dolphin, Andrew Seth, Anil C. Weisz, Daniel Skillman, Evan TI THE ADVANCED CAMERA FOR SURVEYS NEARBY GALAXY SURVEY TREASURY. VI. THE ANCIENT STAR-FORMING DISK OF NGC 404 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (NGC 404); galaxies: stellar content ID HUBBLE-SPACE-TELESCOPE; TULLY-FISHER RELATIONS; DIGITAL SKY SURVEY; M81 OUTER DISK; FORMATION HISTORY; S0 GALAXIES; STELLAR POPULATIONS; LUMINOSITY FUNCTION; LENTICULAR GALAXY; FORMATION LAW AB We present HST/WFPC2 observations across the disk of the nearby isolated dwarf S0 galaxy NGC 404, which hosts an extended gas disk. The locations of our fields contain a roughly equal mixture of bulge and disk stars. All of our resolved stellar photometry reaches m(F814W) = 26 (M(F814W) = -1.4), which covers 2.5 mag of the red giant branch and main-sequence stars with ages <300 Myr. Our deepest field reaches m(F814W) = 27.2 (M(F814W) = -0.2), sufficient to resolve the red clump and main-sequence stars with ages <500 Myr. Although we detect trace amounts of star formation at times more recent than 10 Gyr ago for all fields, the proportion of red giant stars to asymptotic giants and main-sequence stars suggests that the disk is dominated by an ancient (>10 Gyr) population. Detailed modeling of the color-magnitude diagram suggests that similar to 70% of the stellar mass in the NGC 404 disk formed by z similar to 2 (10 Gyr ago) and at least similar to 90% formed prior to z similar to 1 (8 Gyr ago). These results indicate that the stellar populations of the NGC 404 disk are on average significantly older than those of other nearby disk galaxies, suggesting that early-and late-type disks may have different long-term evolutionary histories, not simply differences in their recent star formation rates. Comparisons of the spatial distribution of the young stellar mass and FUV emission in Galaxy Evolution Explorer images show that the brightest FUV regions contain the youngest stars, but that some young stars (<160 Myr) lie outside of these regions. FUV luminosity appears to be strongly affected by both age and stellar mass within individual regions. Finally, we use our measurements to infer the relationship between the star formation rate and the gas density of the disk at previous epochs. We find that most of the history of the NGC 404 disk is consistent with star formation that has decreased with the gas density according to the Schmidt law. However, similar to 0.5-1 Gyr ago, the star formation rate was unusually low for the inferred gas density, consistent with the possibility that there was a gas accretion event that reignited star formation similar to 0.5 Gyr ago. Such an event could explain why this S0 galaxy hosts an extended gas disk. C1 [Williams, Benjamin F.; Dalcanton, Julianne J.; Gilbert, Karoline M.; Stilp, Adrienne] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Dolphin, Andrew] Raytheon, Tucson, AZ 85706 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weisz, Daniel; Skillman, Evan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. RP Williams, BF (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM ben@astro.washington.edu; jd@astro.washington.edu; stephanie@astro.washington.edu; roskar@astro.washington.edu; dolphin@raytheon.com; aseth@cfa.harvard.edu; dweisz@astro.umn.edu; skillman@astro.umn.edu FU Space Telescope Science Institute [GO-10915, GO-11719] FX Support for this work was provided by NASA through grants GO-10915 and GO-11719 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 51 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 71 EP 83 DI 10.1088/0004-637X/716/1/71 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000003 ER PT J AU Kilic, M Brown, WR Prieto, CA Kenyon, SJ Panei, JA AF Kilic, Mukremin Brown, Warren R. Allende Prieto, Carlos Kenyon, S. J. Panei, J. A. TI THE DISCOVERY OF BINARY WHITE DWARFS THAT WILL MERGE WITHIN 500 Myr SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: individual (SDSS J082212.57+275307.4, SDSS J084910.13+044528.7, SDSS J105353.89+520031.0, SDSS J143633.29+501026.8); stars: low-mass; white dwarfs ID CORONAE-BOREALIS STARS; HYDROGEN-DEFICIENT CARBON; PERIOD DOUBLE-DEGENERATE; EXTREME HELIUM STARS; DIGITAL SKY SURVEY; X-RAY BINARIES; LOW-MASS; CLOSE BINARIES; SPY PROJECT; GALACTIC DISK AB We present radial velocity observations of four extremely low-mass (0.2M(circle dot)) white dwarfs (WDs). All four stars show peak-to-peak radial velocity variations of 540-710 km s(-1) with 1.0-5.9 hr periods. The optical photometry rules out main-sequence companions. In addition, no millisecond pulsar companions are detected in radio observations. Thus, the invisible companions are most likely WDs. Two of the systems are the shortest period binary WDs yet discovered. Due to the loss of angular momentum through gravitational radiation, three of the systems will merge within 500 Myr. The remaining system will merge within a Hubble time. The mass functions for three of the systems imply companions more massive than 0.46M(circle dot); thus, those are carbon/oxygen core WDs. The unknown inclination angles prohibit a definitive conclusion about the future of these systems. However, the chance of a supernova Ia event is only 1%-5%. These systems are likely to form single R Coronae Borealis stars, providing evidence for a WD + WD merger mechanism for these unusual objects. One of the systems, SDSS J105353.89+520031.0, has a 70% chance of having a low-mass WD companion. This system will probably form a single helium-enriched subdwarf O star. All four WD systems have unusual mass ratios of <0.2-0.8 that may also lead to the formation of AM CVn systems. C1 [Kilic, Mukremin; Brown, Warren R.; Kenyon, S. J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Allende Prieto, Carlos] Univ Coll London, Mullard Space Sci Lab, Holmbury RH5 6NT, Surrey, England. [Panei, J. A.] UNLP, Fac Ciencias Astron & Geofis, La Plata, Buenos Aires, Argentina. [Panei, J. A.] CONICET UNLP, IALP, Inst Astrofis La Plata, La Plata, Buenos Aires, Argentina. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA, Caltech FX Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. We thank M. Agueros, D. Steeghs, T. Marsh, and J. Guillochon for helpful discussions, D. Koester for kindly providing DA WD model spectra, and an anonymous referee for a detailed and constructive report. NR 71 TC 46 Z9 46 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 122 EP 130 DI 10.1088/0004-637X/716/1/122 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000008 ER PT J AU McKee, CF Offner, SSR AF McKee, Christopher F. Offner, Stella S. R. TI THE PROTOSTELLAR MASS FUNCTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE stars: formation; stars: luminosity function, mass function ID YOUNG STELLAR OBJECTS; SELF-SIMILAR COLLAPSE; STAR-FORMATION; DENSE CORES; TURBULENT FRAGMENTATION; GRAVITATIONAL COLLAPSE; COMPETITIVE ACCRETION; LUMINOSITY FUNCTIONS; ISOTHERMAL SPHERES; MOLECULAR CLOUDS AB The protostellar mass function (PMF) is the present-day mass function of the protostars in a region of star formation. It is determined by the initial mass function weighted by the accretion time. The PMF thus depends on the accretion history of protostars and in principle provides a powerful tool for observationally distinguishing different protostellar accretion models. We consider three basic models here: the isothermal sphere model, the turbulent core model, and an approximate representation of the competitive accretion model. We also consider modified versions of these accretion models, in which the accretion rate tapers off linearly in time. Finally, we allow for an overall acceleration in the rate of star formation. At present, it is not possible to directly determine the PMF since protostellar masses are not currently measurable. We carry out an approximate comparison of predicted PMFs with observation by using the theory to infer the conditions in the ambient medium in several star-forming regions. Tapered and accelerating models generally agree better with observed star formation times than models without tapering or acceleration, but uncertainties in the accretion models and in the observations do not allow one to rule out any of the proposed models at present. The PMF is essential for the calculation of the protostellar luminosity function, however, and this enables stronger conclusions to be drawn. C1 [McKee, Christopher F.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [McKee, Christopher F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Offner, Stella S. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP McKee, CF (reprint author), Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. EM cmckee@astro.berkeley.edu; soffner@cfa.harvard.edu FU NSF [AST-0606831, AST-0908553, AST-0901055] FX We thank Steve Stahler for pointing out his previous work on this problem, Neal Evans, Shu-Ichiro Inusuka, and Zhi-Yun Li for useful comments, and Melissa Enoch for clarifying and supplying observational values for the data comparison. This research has been supported by the NSF through grants AST-0606831 (CFM & SSRO), AST-0908553 (CFM), and AST-0901055 (SSRO). NR 52 TC 25 Z9 25 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 167 EP 180 DI 10.1088/0004-637X/716/1/167 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000012 ER PT J AU Johannsen, T Psaltis, D AF Johannsen, Tim Psaltis, Dimitrios TI TESTING THE NO-HAIR THEOREM WITH OBSERVATIONS IN THE ELECTROMAGNETIC SPECTRUM. I. PROPERTIES OF A QUASI-KERR SPACETIME SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; gravitation ID ROTATING NEUTRON-STARS; RELATIVISTIC GRAVITATIONAL COLLAPSE; ARBITRARY MULTIPOLE MOMENTS; SUPERMASSIVE BLACK-HOLE; SAGITTARIUS A-ASTERISK; GALACTIC-CENTER; EVENT-HORIZON; NONSPHERICAL PERTURBATIONS; STELLAR ORBITS; MASSIVE BODY AB According to the no-hair theorem, an astrophysical black hole is uniquely described by only two quantities, the mass and the spin. In this series of papers, we investigate a framework for testing the no-hair theorem with observations of black holes in the electromagnetic spectrum. We formulate our approach in terms of a parametric spacetime which contains a quadrupole moment that is independent of both mass and spin. If the no-hair theorem is correct, then any deviation of the black hole quadrupole moment from its Kerr value has to be zero. We analyze in detail the properties of this quasi-Kerr spacetime that are critical to interpreting observations of black holes and demonstrate their dependence on the spin and quadrupole moment. In particular, we show that the location of the innermost stable circular orbit and the gravitational lensing experienced by photons are affected significantly at even modest deviations of the quadrupole moment from the value predicted by the no-hair theorem. We argue that observations of black hole images, of relativistically broadened iron lines, as well as of thermal X-ray spectra from accreting black holes will lead in the near future to an experimental test of the no-hair theorem. C1 [Johannsen, Tim] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Psaltis, Dimitrios] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Psaltis, Dimitrios] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Johannsen, T (reprint author), Univ Arizona, Dept Phys, 1118 E 4th St, Tucson, AZ 85721 USA. EM timj@physics.arizona.edu; dpsaltis@email.arizona.edu FU NSF [NSF 0746549] FX We thank Avery Broderick, Abraham Loeb, Scott Hughes, Kostas Glampedakis, Emanuele Berti, Nico Yunes, Sarah Vigeland, and Daniel Marrone for helpful discussions. We also thank Sarah Vigeland and Scott Hughes for sharing their paper with us in advance of publication. D. P. thanks the ITC at the Harvard-Smithsonian Center for Astrophysics for their hospitality. This work was supported by the NSF CAREER award NSF 0746549. NR 85 TC 59 Z9 60 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 187 EP 197 DI 10.1088/0004-637X/716/1/187 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000014 ER PT J AU Brusa, M Civano, F Comastri, A Miyaji, T Salvato, M Zamorani, G Cappelluti, N Fiore, F Hasinger, G Mainieri, V Merloni, A Bongiorno, A Capak, P Elvis, M Gilli, R Hao, H Jahnke, K Koekemoer, AM Ilbert, O Le Floc'h, E Lusso, E Mignoli, M Schinnerer, E Silverman, JD Treister, E Trump, JD Vignali, C Zamojski, M Aldcroft, T Aussel, H Bardelli, S Bolzonella, M Cappi, A Caputi, K Contini, T Finoguenov, A Fruscione, A Garilli, B Impey, CD Iovino, A Iwasawa, K Kampczyk, P Kartaltepe, J Kneib, JP Knobel, C Kovac, K Lamareille, F Leborgne, JF Le Brun, V Le Fevre, O Lilly, SJ Maier, C McCracken, HJ Pello, R Peng, YJ Perez-Montero, E de Ravel, L Sanders, D Scodeggio, M Scoville, NZ Tanaka, M Taniguchi, Y Tasca, L de la Torre, S Tresse, L Vergani, D Zucca, E AF Brusa, M. Civano, F. Comastri, A. Miyaji, T. Salvato, M. Zamorani, G. Cappelluti, N. Fiore, F. Hasinger, G. Mainieri, V. Merloni, A. Bongiorno, A. Capak, P. Elvis, M. Gilli, R. Hao, H. Jahnke, K. Koekemoer, A. M. Ilbert, O. Le Floc'h, E. Lusso, E. Mignoli, M. Schinnerer, E. Silverman, J. D. Treister, E. Trump, J. D. Vignali, C. Zamojski, M. Aldcroft, T. Aussel, H. Bardelli, S. Bolzonella, M. Cappi, A. Caputi, K. Contini, T. Finoguenov, A. Fruscione, A. Garilli, B. Impey, C. D. Iovino, A. Iwasawa, K. Kampczyk, P. Kartaltepe, J. Kneib, J. P. Knobel, C. Kovac, K. Lamareille, F. Leborgne, J. -F. Le Brun, V. Le Fevre, O. Lilly, S. J. Maier, C. McCracken, H. J. Pello, R. Peng, Y. -J. Perez-Montero, E. de Ravel, L. Sanders, D. Scodeggio, M. Scoville, N. Z. Tanaka, M. Taniguchi, Y. Tasca, L. de la Torre, S. Tresse, L. Vergani, D. Zucca, E. TI THE XMM-NEWTON WIDE-FIELD SURVEY IN THE COSMOS FIELD (XMM-COSMOS): DEMOGRAPHY AND MULTIWAVELENGTH PROPERTIES OF OBSCURED AND UNOBSCURED LUMINOUS ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; surveys; X-rays: diffuse background; X-rays: galaxies; X-rays: general ID SUPERMASSIVE BLACK-HOLES; X-RAY SOURCES; SPECTRAL ENERGY-DISTRIBUTIONS; BRIGHT SERENDIPITOUS SURVEY; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; ULTRALUMINOUS INFRARED GALAXIES; EVOLUTION SURVEY COSMOS; LYMAN BREAK GALAXIES; POINT-SOURCE CATALOG AB We report the final optical identifications of the medium-depth (similar to 60 ks), contiguous (2 deg(2)) XMM-Newton survey of the COSMOS field. XMM-Newton has detected similar to 1800 X-ray sources down to limiting fluxes of similar to 5 x 10(-16), similar to 3 x 10(-15), and similar to 7 x 10(-15) erg cm(-2) s(-1) in the 0.5-2 keV, 2-10 keV, and 5-10 keV bands, respectively (similar to 1 x 10(-15), similar to 6 x 10(-15), and similar to 1 x 10(-14) erg cm(-2) s(-1), in the three bands, respectively, over 50% of the area). The work is complemented by an extensive collection of multiwavelength data from 24 mu m to UV, available from the COSMOS survey, for each of the X-ray sources, including spectroscopic redshifts for greater than or similar to 50% of the sample, and high-quality photometric redshifts for the rest. The XMM and multiwavelength flux limits are well matched: 1760 (98%) of the X-ray sources have optical counterparts, 1711 (similar to 95%) have IRAC counterparts, and 1394 (similar to 78%) have MIPS 24 mu m detections. Thanks to the redshift completeness (almost 100%) we were able to constrain the high-luminosity tail of the X-ray luminosity function confirming that the peak of the number density of log L(X) > 44.5 active galactic nuclei (AGNs) is at z similar to 2. Spectroscopically identified obscured and unobscured AGNs, as well as normal and star-forming galaxies, present well-defined optical and infrared properties. We devised a robust method to identify a sample of similar to 150 high-redshift (z > 1), obscured AGN candidates for which optical spectroscopy is not available. We were able to determine that the fraction of the obscured AGN population at the highest (L(X) > 10(44) erg s(-1)) X-ray luminosity is similar to 15%-30% when selection effects are taken into account, providing an important observational constraint for X-ray background synthesis. We studied in detail the optical spectrum and the overall spectral energy distribution of a prototypical Type 2 QSO, caught in a stage transitioning from being starburst dominated to AGN dominated, which was possible to isolate only thanks to the combination of X-ray and infrared observations. C1 [Brusa, M.; Cappelluti, N.; Merloni, A.; Bongiorno, A.; Finoguenov, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Civano, F.; Elvis, M.; Hao, H.; Aldcroft, T.; Fruscione, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Comastri, A.; Zamorani, G.; Gilli, R.; Lusso, E.; Mignoli, M.; Vignali, C.; Bardelli, S.; Bolzonella, M.; Cappi, A.; Iwasawa, K.; Vergani, D.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [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. [Salvato, M.; Hasinger, G.] IPP Max Planck Inst Plasma Phys, D-85748 Garching, Germany. [Salvato, M.; Merloni, A.] Excellence Cluster Universe, D-85748 Garching, Germany. [Salvato, M.; Scoville, N. Z.] CALTECH, Pasadena, CA 91125 USA. [Cappelluti, N.] Univ Maryland, Baltimore, MD 21250 USA. [Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Mainieri, V.; Tanaka, M.] European So Observ, D-85748 Garching, Germany. [Capak, P.; Zamojski, M.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Jahnke, K.; Schinnerer, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ilbert, O.] Lab Astrophys Marseille, F-13376 Marseille 12, France. [Le Floc'h, E.] Univ Paris Diderot, CEA Saclay, DAPNIA,Serv Astrophys,CEA DSM CNRS, Lab AIM, F-91191 Gif Sur Yvette, France. [Lusso, E.; Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Silverman, J. D.] Univ Tokyo, IPMU, Chiba 2778568, Japan. [Treister, E.; Kartaltepe, J.; Sanders, D.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Trump, J. D.; Impey, C. D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Aussel, H.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Caputi, K.] Univ Edinburgh, SUPA Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Contini, T.; Lamareille, F.; Leborgne, J. -F.; Pello, R.] Observ Midi Pyrenees, Astrophys Lab, UMR 5572, F-31400 Toulouse, France. [Garilli, B.; Scodeggio, M.; Tasca, L.] INAF IASF Milano, I-20133 Milan, Italy. [Iovino, A.; Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85721 USA. [Kampczyk, P.; Knobel, C.; Kovac, K.; Lilly, S. J.; Maier, C.; Peng, Y. -J.; Perez-Montero, E.] ETH, Dept Phys, CH-8093 Zurich, Switzerland. [Kneib, J. P.; Le Brun, V.; Le Fevre, O.; de Ravel, L.; Tasca, L.; de la Torre, S.; Tresse, L.] Lab Astrophys Marseille, F-13376 Marseille, France. [McCracken, H. J.] LERMA, Observ Paris, F-75014 Paris, France. [Taniguchi, Y.] Ehime Univ, Grad Sch Sci & Engn, Dept Phys, Matsuyama, Ehime 7908577, Japan. RP Brusa, M (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. RI Pello, Roser/G-4754-2010; Le Fevre, Olivier/G-7389-2011; Vignali, Cristian/J-4974-2012; Kneib, Jean-Paul/A-7919-2015; Bardelli, Sandro/O-9369-2015; Cappi, Alberto/O-9391-2015; Zucca, Elena/O-9396-2015; Mignoli, Marco/O-9426-2015; Bolzonella, Micol/O-9495-2015; Comastri, Andrea/O-9543-2015; Gilli, Roberto/P-1110-2015; OI Iovino, Angela/0000-0001-6958-0304; Scodeggio, Marco/0000-0002-2282-5850; Vignali, Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989; Bardelli, Sandro/0000-0002-8900-0298; Cappi, Alberto/0000-0002-9200-7167; Zucca, Elena/0000-0002-5845-8132; Mignoli, Marco/0000-0002-9087-2835; Bolzonella, Micol/0000-0003-3278-4607; Comastri, Andrea/0000-0003-3451-9970; Gilli, Roberto/0000-0001-8121-6177; Bongiorno, Angela/0000-0002-0101-6624; Vergani, Daniela/0000-0003-0898-2216; Jahnke, Knud/0000-0003-3804-2137; Maier, Christian/0000-0001-6405-2182; Koekemoer, Anton/0000-0002-6610-2048; Zamorani, Giovanni/0000-0002-2318-301X; Perez Montero, E/0000-0003-3985-4882; Schinnerer, Eva/0000-0002-3933-7677; Brusa, Marcella/0000-0002-5059-6848; Fiore, Fabrizio/0000-0002-4031-4157; Garilli, Bianca/0000-0001-7455-8750; Cappelluti, Nico/0000-0002-1697-186X FU ESA Member States; USA (NASA); Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR) [FKZ 50 OX 0001]; Max-Planck Society; Heidenhain-Stiftung; Deutsches Zentrum fur Luft-und Raumfahrt [50 OR 0207, 50 OR 0405]; MIUR [2006-02-5203]; ASI-INAF [I/023/05/00, I/088/06]; ASI/COFIS [WP3110, I/026/07/0]; NASA Chandra [GO7-8136A]; CONACyT [83564 DGAPA/PAPIIT IN10209]; NASA [NNX07AT02G, NNX07AV03G, PF8-90055]; Deutsche Forschungsgemeinschaft [HA 1850/28-1]; German Science Foundation DFG 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). In Germany, the XMM-Newton project is supported by the Bundesministerium fur Wirtschaft und Technologie/Deutsches Zentrum fur Luft-und Raumfahrt (BMWI/DLR, FKZ 50 OX 0001), the Max-Planck Society, and the Heidenhain-Stiftung. Part of this work was supported by the Deutsches Zentrum fur Luft-und Raumfahrt, DLR project numbers 50 OR 0207 and 50 OR 0405. In Italy, the XMM-COSMOS project is supported by PRIN/MIUR under grant 2006-02-5203, ASI-INAF grants I/023/05/00, I/088/06 and ASI/COFIS/WP3110, I/026/07/0. This work was supported in part by NASA Chandra grant number GO7-8136A (F. C., M. E., A. F., H. H.). T. M. acknowledges support from CONACyT 83564 DGAPA/PAPIIT IN10209 to IA-UNAM as well as the NASA ADP (NNX07AT02G) grant to UCSD. G. H. and M. S. acknowledge a contribution from the Leibniz Prize of the Deutsche Forschungsgemeinschaft under the grant HA 1850/28-1. N.C. and A. F. were partially supported from a NASA grant NNX07AV03G to UMBC. K.J. is supported by the Emmy Noether-Programme of the German Science Foundation DFG. E. T. is supported by the National Aeronautics and Space Administration through Chandra Postdoctoral Fellowship Award Number PF8-90055. We thank James Aird and Jacobo Ebrero for sending us machine-readable tables of their X-ray luminosity functions, Desika Narayanan for help with his model SEDs, and Ryan Hickox for providing unpublished information about the X-Bootes survey. We gratefully thank Nick Wright for a carefully reading of the manuscript. This work is based in part on observations obtained with MegaPrime/MegaCam, a joint project of Canada-France-Hawaii Telescope (CFHT) and CEA/DAPNIA, at the CFHT, and on data products produced at TERAPIX data center located at the Institut d'Astophysique de Paris. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. We gratefully acknowledge the contribution of the entire COSMOS collaboration; more information on the COSMOS survey is available at http://www.astro.caltech.edu/cosmos. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the SDSS spectral archive. Finally, we thank the anonymous referee for detailed and constructive comments to the first version of this paper. NR 182 TC 177 Z9 179 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 348 EP 369 DI 10.1088/0004-637X/716/1/348 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000025 ER PT J AU Kauffmann, J Pillai, T Shetty, R Myers, PC Goodman, AA AF Kauffmann, J. Pillai, T. Shetty, R. Myers, P. C. Goodman, A. A. TI THE MASS-SIZE RELATION FROM CLOUDS TO CORES. II. SOLAR NEIGHBORHOOD CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; methods: data analysis; stars: formation ID GALACTIC MOLECULAR CLOUDS; FIELD EXTINCTION MAPS; INFRARED-DARK CLOUDS; C2D LEGACY CLOUDS; STAR-FORMATION; STRUCTURAL-ANALYSIS; INITIAL CONDITIONS; PIPE NEBULA; DENSE CORES; PERSEUS AB We measure the mass and size of cloud fragments in several molecular clouds continuously over a wide range of spatial scales (0.05 less than or similar to r/pc less than or similar to 3). Based on the recently developed "dendrogram-technique," this characterizes dense cores as well as the enveloping clouds. "Larson's Third Law" of constant column density, m(r) proportional to r(2), is not well suited to describe the derived mass-size data. Solar neighborhood clouds not forming massive stars (less than or similar to 10 M(circle dot); Pipe Nebula, Taurus, Perseus, and Ophiuchus) obey m(r) <= 870 M(circle dot) (r/pc)(1.33). In contrast to this, clouds forming massive stars (Orion A, G10.15-0.34, G11.11-0.12) do exceed the aforementioned relation. Thus, this limiting mass-size relation may approximate a threshold for the formation of massive stars. Across all clouds, cluster-forming cloud fragments are found to be-at given radius-more massive than fragments devoid of clusters. The cluster-bearing fragments are found to roughly obey a mass-size law m proportional to r(1.27) (where the exponent is highly uncertain in any given cloud, but is certainly smaller than 1.5). C1 [Kauffmann, J.; Shetty, R.; Goodman, A. A.] IIC, Cambridge, MA 02138 USA. [Kauffmann, J.; Pillai, T.; Shetty, R.; Myers, P. C.; Goodman, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kauffmann, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jens.kauffmann@jpl.nasa.gov RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU Harvard Interfaculty Initiative; National Science Foundation [AST-0908159]; JPL/Caltech; NASA FX We are indebted to a careful and thorough anonymous referee, who saved us from making an embarrassing mistake. This project would not have been possible without help from Erik Rosolowsky. His dendrogram analysis code (Rosolowsky et al. 2008) was instrumental for our analysis. Carey et al. (2000), J. Alves (2010, private communication), Enoch et al. (2006), Lombardi et al. (2006), Ridge et al. (2006), Roman-Zuniga et al. (2009), and M. A. Thompson et al. (2010, in preparation) contributed maps to the present study. We are grateful for their help. This work was in part made possible through Harvard Interfaculty Initiative funding to the Harvard Initiative in Innovative Computing (IIC). It is based upon work supported by the National Science Foundation under grant No. AST-0908159, and is based in part on archival data obtained 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 will was provided by an award issued by JPL/Caltech. NR 61 TC 59 Z9 59 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 433 EP 445 DI 10.1088/0004-637X/716/1/433 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000032 ER PT J AU Simon, JD Frebel, A McWilliam, A Kirby, EN Thompson, IB AF Simon, Joshua D. Frebel, Anna McWilliam, Andrew Kirby, Evan N. Thompson, Ian B. TI HIGH-RESOLUTION SPECTROSCOPY OF EXTREMELY METAL-POOR STARS IN THE LEAST EVOLVED GALAXIES: LEO IV SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: dwarf; galaxies: individual (Leo IV); Local Group; stars: abundances ID DWARF SPHEROIDAL GALAXY; NEUTRON-CAPTURE ELEMENTS; MILKY-WAY SATELLITES; ULTRA-FAINT DWARFS; DIGITAL SKY SURVEY; CHEMICAL-COMPOSITION; PHOTOMETRIC SYSTEMS; ABUNDANCE PATTERNS; R-PROCESS; BOOTES I AB We present high-resolution Magellan/MIKE spectroscopy of the brightest star in the ultra-faint dwarf galaxy Leo IV. We measure an iron abundance of [Fe/H] = -3.2, adding to the rapidly growing sample of extremely metal-poor (EMP) stars being identified in Milky Way satellite galaxies. The star is enhanced in the a elements Mg, Ca, and Ti by similar to 0.3 dex, very similar to the typical Milky Way halo abundance pattern. All of the light and iron-peak elements follow the trends established by EMP halo stars, but the neutron-capture elements Ba and Sr are significantly underabundant. These results are quite similar to those found for stars in the ultra-faint dwarfs Ursa Major II, Coma Berenices, Bootes I, and Hercules, suggesting that the chemical evolution of the lowest-luminosity galaxies may be universal. The abundance pattern we observe is consistent with predictions for nucleosynthesis from a Population III supernova explosion. The extremely low metallicity of this star also supports the idea that a significant fraction (similar to 10%) of the stars in the faintest dwarfs have metallicities below [Fe/H] = -3.0. C1 [Simon, Joshua D.; McWilliam, Andrew; Thompson, Ian B.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Frebel, Anna] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kirby, Evan N.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. RP Simon, JD (reprint author), Observ Carnegie Inst Washington, 813 Santa Barbara St, Pasadena, CA 91101 USA. EM jsimon@ociw.edu; afrebel@cfa.harvard.edu; andy@ociw.edu; enk@astro.caltech.edu; ian@ociw.edu OI Kirby, Evan/0000-0001-6196-5162 FU Carnegie Institution of Washington; NASA [HST-HF-01233.01, NAS 5-26555] FX We thank Dan Kelson for assistance with the data reduction, Steve Shectman for observing suggestions, Alexander Heger for extensive help with comparisons to theoretical SN models, and the referee for a helpful report. J.D.S gratefully acknowledges the support of a Vera Rubin Fellowship provided by the Carnegie Institution of Washington, and A.F. that of a Clay Fellowship administered by the Smithsonian Astrophysical Observatory. This work was also supported by NASA through Hubble Fellowship grant HST-HF-01233.01 awarded to E.N.K. by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. This research made use of NASA's Astrophysics Data System Bibliographic Services. NR 44 TC 59 Z9 59 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 446 EP 452 DI 10.1088/0004-637X/716/1/446 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000033 ER PT J AU Lawton, B Gordon, KD Babler, B Block, M Bolatto, AD Bracker, S Carlson, LR Engelbracht, CW Hora, JL Indebetouw, R Madden, SC Meade, M Meixner, M Misselt, K Oey, MS Oliveira, JM Robitaille, T Sewilo, M Shiao, B Vijh, UP Whitney, B AF Lawton, B. Gordon, K. D. Babler, B. Block, M. Bolatto, A. D. Bracker, S. Carlson, L. R. Engelbracht, C. W. Hora, J. L. Indebetouw, R. Madden, S. C. Meade, M. Meixner, M. Misselt, K. Oey, M. S. Oliveira, J. M. Robitaille, T. Sewilo, M. Shiao, B. Vijh, U. P. Whitney, B. TI SPITZER ANALYSIS OF H II REGION COMPLEXES IN THE MAGELLANIC CLOUDS: DETERMINING A SUITABLE MONOCHROMATIC OBSCURED STAR FORMATION INDICATOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: individual (LMC, SMC); galaxies: ISM; H II regions ID MULTIBAND IMAGING PHOTOMETER; SPECTRAL ENERGY-DISTRIBUTION; GALAXY EVOLUTION SAGE; INFRARED ARRAY CAMERA; SPACE-TELESCOPE; LUMINOSITY FUNCTION; ABSOLUTE CALIBRATION; HII-REGIONS; STARBURST GALAXIES; INTERSTELLAR DUST AB H II regions are the birth places of stars, and as such they provide the best measure of current star formation rates (SFRs) in galaxies. The close proximity of the Magellanic Clouds allows us to probe the nature of these star forming regions at small spatial scales. To study the H II regions, we compute the bolometric infrared flux, or total infrared (TIR), by integrating the flux from 8 to 500 mu m. The TIR provides a measure of the obscured star formation because the UV photons from hot young stars are absorbed by dust and re-emitted across the mid-to-far-infrared (IR) spectrum. We aim to determine the monochromatic IR band that most accurately traces the TIR and produces an accurate obscured SFR over large spatial scales. We present the spatial analysis, via aperture/annulus photometry, of 16 Large Magellanic Cloud (LMC) and 16 Small Magellanic Cloud (SMC) H II region complexes using the Spitzer Space Telescope's IRAC (3.6, 4.5, 8 mu m) and MIPS (24, 70, 160 mu m) bands. Ultraviolet rocket data (1500 and 1900 angstrom) and SHASSA H alpha data are also included. All data are convolved to the MIPS 160 mu m resolution (40 arcsec full width at half-maximum), and apertures have a minimum radius of 35 ''. The IRAC, MIPS, UV, and Ha spatial analysis are compared with the spatial analysis of the TIR. We find that nearly all of the LMC and SMC H II region spectral energy distributions (SEDs) peak around 70 mu m at all radii, from similar to 10 to similar to 400 pc from the central ionizing sources. As a result, we find the following: the sizes of H II regions as probed by 70 mu m are approximately equal to the sizes as probed by TIR (approximate to 70 pc in radius); the radial profile of the 70 mu m flux, normalized by TIR, is constant at all radii (70 mu m similar to 0.45 TIR); the 1 sigma standard deviation of the 70 mu m fluxes, normalized by TIR, is a lower fraction of the mean (0.05-0.12 out to similar to 220 pc) than the normalized 8, 24, and 160 mu m normalized fluxes (0.12-0.52); and these results are the same for the LMC and the SMC. From these results, we argue that 70 mu m is the most suitable IR band to use as a monochromatic obscured star formation indicator because it most accurately reproduces the TIR of H II regions in the LMC and SMC and over large spatial scales. We also explore the general trends of the 8, 24, 70, and 160 mu m bands in the LMC and SMC H II region SEDs, radial surface brightness profiles, sizes, and normalized (by TIR) radial flux profiles. We derive an obscured SFR equation that is modified from the literature to use 70 mu m luminosity, SFR (M-circle dot yr(-1)) = 9.7(0.7) x 10(-44)L(70) (ergs s(-1)), which is applicable from 10 to 300 pc distance from the center of an H II region. We include an analysis of the spatial variations around H II regions between the obscured star formation indicators given by the IR and the unobscured star formation indicators given by UV and H alpha. We compute obscured and unobscured SFRs using equations from the literature and examine the spatial variations of the SFRs around H II regions. C1 [Lawton, B.; Gordon, K. D.; Meixner, M.; Sewilo, M.; Shiao, B.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Babler, B.; Bracker, S.; Meade, M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Block, M.; Engelbracht, C. W.; Misselt, K.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bolatto, A. D.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Carlson, L. R.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Hora, J. L.; Robitaille, T.] Harvard Smithsonian, CfA, Cambridge, MA 02138 USA. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Madden, S. C.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Oey, M. S.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Oliveira, J. M.] Univ Keele, Sch Phys & Geog Sci, Lennard Jones Labs, Keele ST5 5BG, Staffs, England. [Vijh, U. P.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. [Whitney, B.] Space Sci Inst, Boulder, CO 80301 USA. RP Lawton, B (reprint author), Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM lawton@stsci.edu; kgordon@stsci.edu OI Babler, Brian/0000-0002-6984-5752; Hora, Joseph/0000-0002-5599-4650; Robitaille, Thomas/0000-0002-8642-1329 FU NASA [1407, 1275598, NAG5-12595] FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under NASA contract 1407. The SAGE-LMC project has been supported by NASA/Spitzer grant 1275598 and Meixner's efforts have had additional support from NASA NAG5-12595. NR 84 TC 29 Z9 29 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 453 EP 473 DI 10.1088/0004-637X/716/1/453 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000034 ER PT J AU Wang, JF Feigelson, ED Townsley, LK Broos, PS Roman-Zuniga, CG Lada, E Garmire, G AF Wang, Junfeng Feigelson, Eric D. Townsley, Leisa K. Broos, Patrick S. Roman-Zuniga, Carlos G. Lada, Elizabeth Garmire, Gordon TI A CHANDRA STUDY OF THE ROSETTE STAR-FORMING COMPLEX. III. THE NGC 2237 CLUSTER AND THE REGION'S STAR FORMATION HISTORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Rosette Nebula); open clusters and associations: individual (NGC 2237 NGC 2244); stars: formation; stars: pre-main sequence; X-rays: stars ID ORION ULTRADEEP PROJECT; YOUNG STELLAR OBJECTS; X-RAY-EMISSION; T-TAURI STARS; INITIAL MASS FUNCTION; GALACTIC HII-REGIONS; HERBIG AE/BE STARS; MOLECULAR CLOUD; OB ASSOCIATIONS; EMBEDDED CLUSTERS AB We present high spatial resolution Chandra X-ray images of the NGC 2237 young stellar cluster on the periphery of the Rosette Nebula. We detect 168 X-ray sources, 80% of which have stellar counterparts in USNO, Two Micron All Sky Survey, and deep FLAMINGOS images. These constitute the first census of the cluster members with 0.2 less than or similar to M less than or similar to 2 M(circle dot). Star locations in near-infrared color-magnitude diagrams indicate a cluster age around 2 Myr with a visual extinction of 1 less than or similar to A(V) less than or similar to 3 at 1.4 kpc, the distance of the Rosette Nebula's main cluster NGC 2244. We derive the K-band luminosity function and the X-ray luminosity function of the cluster, which indicate a population similar to 400-600 stars. The X-ray-selected sample shows a K-excess disk frequency of 13%. The young Class II counterparts are aligned in an arc similar to 3 pc long suggestive of a triggered formation process induced by the O stars in NGC 2244. The diskless Class III sources are more dispersed. Several X-ray emitting stars are located inside the molecular cloud and around gaseous pillars projecting from the cloud. These stars, together with a previously unreported optical outflow originating inside the cloud, indicate that star formation is continuing at a low level and the cluster is still growing. This X-ray view of young stars on the western side of the Rosette Nebula complements our earlier studies of the central cluster NGC 2244 and the embedded clusters on the eastern side of the Nebula. The large-scale distribution of the clusters and molecular material is consistent with a scenario in which the rich central NGC 2244 cluster formed first, and its expanding H II region triggered the formation of the now-unobscured satellite clusters Rosette Molecular Cloud (RMC) XA and NGC 2237. A large swept-up shell material around the H II region is now in a second phase of collect-and-collapse fragmentation, leading to the recent formation of subclusters. Other clusters deeper in the molecular cloud appear unaffected by the Rosette Nebula expansion. C1 [Wang, Junfeng; Feigelson, Eric D.; Townsley, Leisa K.; Broos, Patrick S.; Garmire, Gordon] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Roman-Zuniga, Carlos G.] Ctr Astron Hispano Aleman, Granada 18008, Spain. [Lada, Elizabeth] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Wang, JF (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM juwang@cfa.harvard.edu RI Wang, Junfeng/A-1476-2011; Roman-Zuniga, Carlos/F-6602-2016 OI Roman-Zuniga, Carlos/0000-0001-8600-4798 FU Chandra ACIS Team (G. Garmire: PI) through NASA [NAS8-38252]; NASA [NNX09AC74G, NNG05D66G]; NSF [AST97-31180, AST97-3367, AST02-02976]; Kitt Peak National Observatory FX We thank the anonymous referee for his/her careful reading and comments that significantly improved the clarity of this paper. We thank Travis Rector and Mark Heyer for kindly providing the KPNO MOSAIC images of the Rosette Nebula and the CO emission maps of the Rosette Complex, respectively. This work was supported by the Chandra ACIS Team (G. Garmire: PI) through NASA contract NAS8-38252. E.D.F., P.S.B., and L.K.T. also received support from NASA grant NNX09AC74G. FLAMINGOS was designed and constructed by the IR instrumentation group (PI: R. Elston) at the University of Florida, Department of Astronomy with support from NSF grant AST97-31180 and Kitt Peak National Observatory. The data were collected under the NOAO Survey Program, "Towards a Complete Near-Infrared Spectroscopic Survey of Giant Molecular Clouds" (PI: E. Lada) and supported by NSF grants AST97-3367 and AST02-02976 to the University of Florida. E.A.L. also acknowledges support from NASA LTSA NNG05D66G. This publication makes use of data products from the Two Micron All Sky Survey (a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and NSF), and the SIMBAD database and the VizieR catalog access tool (operated by the CDS). NR 89 TC 17 Z9 17 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 474 EP 489 DI 10.1088/0004-637X/716/1/474 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000035 ER PT J AU Smith, HA Li, AG Li, MP Kohler, M Ashby, MLN Fazio, GG Huang, JS Marengo, M Wang, Z Willner, S Zezas, A Spinoglio, L Wu, YL AF Smith, Howard A. Li, Aigen Li, M. P. Koehler, M. Ashby, M. L. N. Fazio, G. G. Huang, J. -S. Marengo, M. Wang, Z. Willner, S. Zezas, A. Spinoglio, L. Wu, Y. L. TI ANOMALOUS SILICATE DUST EMISSION IN THE TYPE 1 LINER NUCLEUS OF M81 SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: individual (M81); galaxies: nuclei; galaxies: Seyfert; infrared: galaxies ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; SPECTRAL ENERGY-DISTRIBUTIONS; POLYCYCLIC AROMATIC-HYDROCARBONS; HIGH-RESOLUTION SPECTROSCOPY; DIFFUSE INTERSTELLAR-MEDIUM; SPITZER-SPACE-TELESCOPE; PALOMAR-GREEN QUASARS; STAR-FORMING GALAXIES; ULIRG EVOLUTION AB We report the detection and successful modeling of the unusual 9.7 mu m Si-O stretching silicate emission feature in the type 1 (i.e., face-on) LINER nucleus of M81. Using the Infrared Spectrograph (IRS) instrument on Spitzer, we determine the feature in the central 230 pc of M81 to be in strong emission, with a peak at similar to 10.5 mu m. This feature is strikingly different in character from the absorption feature of the galactic interstellar medium, and from the silicate absorption or weak emission features typical of galaxies with active star formation. We successfully model the high signal-to-noise ratio IRS spectra with porous silicate dust using laboratory-acquired mineral spectra. We find that the most probable fit uses micron-sized, porous grains of amorphous silicate and amorphous carbon. In addition to silicate dust, there is weak polycyclic aromatic hydrocarbon (PAH) emission present (particularly at 11.3 mu m, arising from the C-H out-of-plane bending vibration of relatively large PAHs of similar to 500-1000 C atoms) whose character reflects the low-excitation active galactic nucleus environment, with some evidence that small PAHs of similar to 100-200 C atoms (responsible for the 7.7 mu m C-C stretching band) in the immediate vicinity of the nucleus have been preferentially destroyed. Analysis of the infrared fine structure lines confirms the LINER character of the M81 nucleus. Four of the infrared H(2) rotational lines are detected and fit to an excitation temperature of T similar to 800 K. Spectral maps of the central 230 pc in the [Ne II] 12.8 mu m line, the H(2) 17 mu m line, and the 11.3 mu m PAH C-H bending feature reveal arc-or spiral-like structures extending from the core. We also report on epochal photometric and spectroscopic observations of M81, whose nuclear intensity varies in time across the spectrum due to what is thought to be inefficient, sub-Eddington accretion onto its central black hole. We find that, contrary to the implications of earlier photometry, the nucleus has not varied over a period of two years at these infrared wavelengths to a precision of about 1%. C1 [Smith, Howard A.; Ashby, M. L. N.; Fazio, G. G.; Huang, J. -S.; Marengo, M.; Wang, Z.; Willner, S.; Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Li, Aigen; Li, M. P.; Koehler, M.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50010 USA. [Zezas, A.] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Spinoglio, L.] CNR, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. [Wu, Y. L.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91101 USA. RP Smith, HA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hsmith@cfa.harvard.edu; lia@missouri.edu RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Spinoglio, Luigi/0000-0001-8840-1551 FU NASA [NAG5-10654, 1407, 960541]; Spitzer Theory Programs; Herschel Theory Program; NSF [AST 07-07866] FX We thank Ciska Kemper-Markwick for her advice on and assistance with dust modeling, and Achim Tappe for help with CUBISM in general and IRS calibration issues in particular. We thank Nick Devereux for providing the data for the Ha image in Figure 2, and for his helpful comments. We also thank Lei Hao, Ciska Kemper-Markwick, Ralf Siebenmorgen, Henrik Spoon, Eckhard Sturm, Doug Whittet, and Martin Haas for providing us with the observational data of 3C273, GC Sgr A*, IRAS 08572+3915, NGC 3998, Cygni OB2 #12, and 3CR galaxies. We thank the anonymous referee for his/her thoughtful comments, which helped to improve this paper. H.A.S. and M.L.N.A. acknowledge partial support from NASA Grant NAG5-10654. A.L., M.K., and M.P.L. are supported in part by Spitzer Theory Programs, a Herschel Theory Program, and NSF grant AST 07-07866. 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 NASA contract 1407. Support for the IRAC instrument was provided by NASA through Contract Number 960541 issued by JPL. CUBISM is a product of the SSC and the IRS team. NR 105 TC 18 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 JUN 10 PY 2010 VL 716 IS 1 BP 490 EP 503 DI 10.1088/0004-637X/716/1/490 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000036 ER PT J AU Shcherbakov, RV Baganoff, FK AF Shcherbakov, Roman V. Baganoff, Frederick K. TI INFLOW-OUTFLOW MODEL WITH CONDUCTION AND SELF-CONSISTENT FEEDING FOR Sgr A* SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; conduction; Galaxy: center; stars: winds, outflows ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; ACCRETION FLOWS; CENTRAL PARSEC; SAGITTARIUS-A; SPHERICAL ACCRETION; THERMAL CONDUCTION; FARADAY-ROTATION; STELLAR ORBITS; HOT GAS AB We propose a two-temperature radial inflow-outflow model near Sgr A* with self-consistent feeding and conduction. Stellar winds from individual stars are considered to find the rates of mass injection and energy injection. These source terms help to partially eliminate the boundary conditions on the inflow. Electron thermal conduction is crucial for inhibiting the accretion. Energy diffuses out from several gravitational radii, unbinding more gas at several arcseconds and limiting the accretion rate to <1% of Bondi rate. We successfully fit the X-ray surface brightness profile found from the extensive Chandra observations and reveal the X-ray point source in the center. The super-resolution technique allows us to infer the presence and estimate the unabsorbed luminosity L approximate to 4 x 1032 erg s(-1) of the point source. The employed relativistic heat capacity and direct heating of electrons naturally lead to low electron temperature T(e) approximate to 4 x 1010 K near the black hole. Within the same model, we fit 86 GHz optically thick emission and obtain the order of magnitude agreement of Faraday rotation measure, thus achieving a single accretion model suitable at all radii. C1 [Shcherbakov, Roman V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Baganoff, Frederick K.] MIT, Ctr Space Res, Cambridge, MA 02139 USA. RP Shcherbakov, RV (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rshcherbakov@cfa.harvard.edu FU NASA [NNX08AX04H, NNX08AH32G]; Chandra Award [GO9-0101X]; SAO [2834-MIT-SAO-4018]; NSF [AST-0805832] FX The authors are grateful to Ramesh Narayan for fruitful discussions, referee Eliot Quataert, Fu-Guo Xie for encouraging us with the shooting method, Feng Yuan, Jorge Cuadra, and Avi Loeb for useful comments. The work is supported by the NASA grants NNX08AX04H, NNX08AH32G, Chandra Award GO9-0101X, SAO Award 2834-MIT-SAO-4018, and the NSF grant AST-0805832. NR 38 TC 40 Z9 40 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 504 EP 509 DI 10.1088/0004-637X/716/1/504 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000037 ER PT J AU Kozlowski, S Kochanek, CS Stern, D Ashby, MLN Assef, RJ Bock, JJ Borys, C Brand, K Brodwin, M Brown, MJI Cool, R Cooray, A Croft, S Dey, A Eisenhardt, PR Gonzalez, A Gorjian, V Griffith, R Grogin, N Ivison, R Jacob, J Jannuzi, BT Mainzer, A Moustakas, L Rottgering, H Seymour, N Smith, HA Stanford, SA Stauffer, JR Sullivan, IS van Breugel, W Willner, SP Wright, EL AF Kozlowski, Szymon Kochanek, Christopher S. Stern, Daniel Ashby, Matthew L. N. Assef, Roberto J. Bock, J. J. Borys, C. Brand, K. Brodwin, M. Brown, M. J. I. Cool, R. Cooray, A. Croft, S. Dey, Arjun Eisenhardt, P. R. Gonzalez, A. Gorjian, V. Griffith, R. Grogin, N. Ivison, R. Jacob, J. Jannuzi, B. T. Mainzer, A. Moustakas, L. Rottgering, H. Seymour, N. Smith, H. A. Stanford, S. A. Stauffer, J. R. Sullivan, I. S. van Breugel, W. Willner, S. P. Wright, E. L. TI MID-INFRARED VARIABILITY FROM THE SPITZER DEEP WIDE-FIELD SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: active; infrared: galaxies; quasars: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; ARRAY CAMERA IRAC; X-RAY SURVEY; LUMINOSITY FUNCTION; QUASAR VARIABILITY; MAGELLANIC CLOUDS; EDDINGTON RATIOS; HOT DUST; GALAXIES AB We use the multi-epoch, mid-infrared Spitzer Deep Wide-Field Survey to investigate the variability of objects in 8.1 deg(2) of the NOAO Deep Wide Field Survey Bootes field. We perform a Difference Image Analysis of the four available epochs between 2004 and 2008, focusing on the deeper 3.6 and 4.5 mu m bands. Out of 474,179 analyzed sources, 1.1% meet our standard variability selection criteria that the two light curves are strongly correlated (r > 0.8) and that their joint variance (sigma(12)) exceeds that for all sources with the same magnitude by 2 sigma. We then examine the mid-IR colors of the variable sources and match them with X-ray sources from the XBootes survey, radio catalogs, 24 mu m selected active galactic nucleus (AGN) candidates, and spectroscopically identified AGNs from the AGN and Galaxy Evolution Survey (AGES). Based on their mid-IR colors, most of the variable sources are AGNs (76%), with smaller contributions from stars (11%), galaxies (6%), and unclassified objects, although most of the stellar, galaxy, and unclassified sources are false positives. For our standard selection criteria, 11%-12% of the mid-IR counterparts to X-ray sources, 24 mu m AGN candidates, and spectroscopically identified AGNs show variability. The exact fractions depend on both the search depth and the selection criteria. For example,12% of the 1131 known z > 1 AGNs in the field and 14%-17% of the known AGNs with well-measured fluxes in all four Infrared Array Camera bands meet our standard selection criteria. The mid-IR AGN variability can be well described by a single power-law structure function with an index of gamma approximate to 0.5 at both 3.6 and 4.5 mu m, and an amplitude of S-0 similar or equal to 0.1 mag on rest-frame timescales of 2 yr. The variability amplitude is higher for shorter rest-frame wavelengths and lower luminosities. C1 [Kozlowski, Szymon; Kochanek, Christopher S.; Assef, Roberto J.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Kochanek, Christopher S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Stern, Daniel; Eisenhardt, P. R.; Gorjian, V.; Griffith, R.; Jacob, J.; Mainzer, A.; Moustakas, L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ashby, Matthew L. N.; Brodwin, M.; Smith, H. A.; Willner, S. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Stauffer, J. R.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Brand, K.; Grogin, N.; Sullivan, I. S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Brown, M. J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Cool, R.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Cooray, A.] Univ Calif Irvine, Irvine, CA 92697 USA. [Croft, S.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Dey, Arjun; Jannuzi, B. T.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Gonzalez, A.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Ivison, R.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R.] Univ Edinburgh, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Seymour, N.] UCL, Mullard Space Sci Lab, London WC1E 6BT, England. [Stanford, S. A.] Univ Calif Davis, Davis, CA 95616 USA. [van Breugel, W.] Univ Calif, Merced, CA 95344 USA. [Wright, E. L.] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. RP Kozlowski, S (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM simkoz@astronomy.ohio-state.edu RI Kozlowski, Szymon/G-4799-2013; Brown, Michael/B-1181-2015; Ivison, R./G-4450-2011; OI Croft, Steve/0000-0003-4823-129X; Kozlowski, Szymon/0000-0003-4084-880X; Brown, Michael/0000-0002-1207-9137; Ivison, R./0000-0001-5118-1313; Seymour, Nicholas/0000-0003-3506-5536; Moustakas, Leonidas/0000-0003-3030-2360 FU National Aeronautics and Space Administration (NASA) [1310744, 1314516, 1317692]; NSF, National Science Foundation [AST-0708082]; W.M. Keck Foundation FX This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of the Technology under contract with the National Aeronautics and Space Administration (NASA). Support for this work was provided by NASA through award numbers 1310744 (C.S.K. and S.K.), 1314516 (M.L.N.A.), and 1317692 (H.A.S.) issued by JPL/CalTech. C.S.K. and S.K. are also supported by NSF grant AST-0708082. The NDWFS and the research of A.D. and B.T.J. are supported 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. Support for M.B. was provided by the W.M. Keck Foundation. NR 54 TC 21 Z9 21 U1 1 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 JUN 10 PY 2010 VL 716 IS 1 BP 530 EP 543 DI 10.1088/0004-637X/716/1/530 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000040 ER PT J AU Zheng, Z Cen, RY Trac, H Miralda-Escude, J AF Zheng, Zheng Cen, Renyue Trac, Hy Miralda-Escude, Jordi TI RADIATIVE TRANSFER MODELING OF Ly alpha EMITTERS. I. STATISTICS OF SPECTRA AND LUMINOSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: halos; galaxies: high-redshift; galaxies: statistics; intergalactic medium; large-scale structure of universe; line: profiles; radiative transfer; scattering ID LYMAN BREAK GALAXIES; RESONANCE-LINE RADIATION; INITIAL MASS FUNCTION; STAR-FORMATION HISTORY; GUNN-PETERSON TROUGH; LARGE OPTICAL DEPTH; SUBARU DEEP FIELD; EMITTING GALAXIES; HIGH-REDSHIFT; COSMOLOGICAL SIMULATIONS AB We combine a cosmological reionization simulation with box size of 100 h(-1) Mpc on a side and a Monte Carlo Ly alpha radiative transfer code to model Ly alpha Emitters (LAEs) at z similar to 5.7. The model introduces Ly alpha radiative transfer as the single factor for transforming the intrinsic Ly alpha emission properties into the observed ones. Spatial diffusion of Ly alpha photons from radiative transfer results in extended Ly alpha emission and only the central part with high surface brightness can be observed. Because of radiative transfer, the appearance of LAEs depends on density and velocity structures in circumgalactic and intergalactic media as well as the viewing angle, which leads to a broad distribution of apparent (observed) Ly alpha luminosity for a given intrinsic Ly alpha luminosity. Radiative transfer also causes frequency diffusion of Ly alpha photons. The resultant Ly alpha line is asymmetric with a red tail. The peak of the Ly alpha line shifts toward longer wavelength and the shift is anti-correlated with the apparent-to-intrinsic Ly alpha luminosity ratio. The simple radiative transfer model provides a new framework for studying LAEs. It is able to explain an array of observed properties of z similar to 5.7 LAEs in Ouchi et al., producing Ly alpha spectra, morphology, and apparent Ly alpha luminosity function (LF) similar to those seen in observation. The broad distribution of apparent Ly alpha luminosity at fixed UV luminosity provides a natural explanation for the observed UV LF, especially the turnover toward the low luminosity end. The model also reproduces the observed distribution of Ly alpha equivalent width (EW) and explains the deficit of UV bright, high EW sources. Because of the broad distribution of the apparent-to-intrinsic Ly alpha luminosity ratio, the model predicts effective duty cycles and Ly alpha escape fractions for LAEs. C1 [Zheng, Zheng] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Zheng, Zheng] Inst Adv Study, Princeton, NJ 08540 USA. [Cen, Renyue] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Trac, Hy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Miralda-Escude, Jordi] Inst Catalana Recerca & Estudis Avancats, Barcelona, Spain. [Miralda-Escude, Jordi] Univ Barcelona, Inst Ciencies Cosmos, Barcelona, Spain. RP Zheng, Z (reprint author), Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. EM zheng.zheng@yale.edu RI Trac, Hy/N-8838-2014; OI Trac, Hy/0000-0001-6778-3861; Miralda-Escude, Jordi/0000-0002-2316-8370 FU NASA [NNG06GI09G]; Institute for Theory and Computation Fellowship; European Research Council [2006-046435]; Spanish grant [AYA2009-09745]; National Science Foundation FX We are grateful to Masami Ouchi for valuable conversations on various observational aspects of LAEs, for kindly providing the observational data in electronic form, and for helpful comments on an earlier draft. We thank Andrei Mesinger for useful discussions and David Weinberg for helpful comments. Z.Z. thanks Juna Kollmeier and Rashid Sunyaev for useful discussions about Ly alpha radiative transfer. We thank the referee for useful comments. Z.Z. gratefully acknowledges support from the Institute for Advanced Study through a John Bahcall Fellowship at an early stage of this work and support from Yale Center for Astronomy and Astrophysics through a YCAA fellowship. Z.Z. acknowledges the hospitality of the Kavli Institute for Astronomy and Astrophysics at Peking University (KIAA-PKU), where part of the work was done. Z.Z. also thanks Aspen Center for Physics for a stimulating atmosphere and Mark Dijkstra and Paul Shapiro for interesting discussions. J.M. thanks the Institute for Advanced Study for their hospitality. This work is supported in part by NASA grant NNG06GI09G. H. T. is supported by an Institute for Theory and Computation Fellowship. J.M. is supported by the International Reintegration Grant of the European Research Council 2006-046435 and Spanish grant AYA2009-09745. This research was supported in part by the National Science Foundation through TeraGrid resources provided by NASA. The Lya radiative transfer computations were performed at the Princeton Institute for Computational Science and Engineering (PICSciE). Some analyses were conducted at the aurora cluster at the Institute for Advanced Study. NR 103 TC 89 Z9 89 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 574 EP 598 DI 10.1088/0004-637X/716/1/574 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000044 ER PT J AU Li, CT Kubo, DY Wilson, W Lin, KY Chen, MT Ho, PTP Chen, CC Han, CC Oshiro, P Martin-Cocher, P Chang, CH Chang, SH Altamirano, P Jiang, HM Chiueh, TD Lien, CH Wang, HE Wei, RM Yang, CH Peterson, JB Chang, SW Huang, YD Hwang, YJ Kesteven, M Koch, P Liu, GC Nishioka, H Umetsu, K Wei, TS Wu, JHP AF Li, Chao-Te Kubo, Derek Y. Wilson, Warwick Lin, Kai-Yang Chen, Ming-Tang Ho, P. T. P. Chen, Chung-Cheng Han, Chih-Chiang Oshiro, Peter Martin-Cocher, Pierre Chang, Chia-Hao Chang, Shu-Hao Altamirano, Pablo Jiang, Homin Chiueh, Tzi-Dar Lien, Chun-Hsien Wang, Huei Wei, Ray-Ming Yang, Chia-Hsiang Peterson, Jeffrey B. Chang, Su-Wei Huang, Yau-De Hwang, Yuh-Jing Kesteven, Michael Koch, Patrick Liu, Guo-Chin Nishioka, Hiroaki Umetsu, Keiichi Wei, Tashun Wu, Jiun-Huei Proty TI AMiBA WIDEBAND ANALOG CORRELATOR SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; instrumentation: interferometers; telescopes ID MICROWAVE BACKGROUND ANISOTROPY; LAG-CORRELATOR; ARRAY; INTERFEROMETRY; COSMOLOGY; IMAGER; SYSTEM AB A wideband analog correlator has been constructed for the Yuan-Tseh Lee Array for Microwave Background Anisotropy. Lag correlators using analog multipliers provide large bandwidth and moderate frequency resolution. Broadband intermediate frequency distribution, back-end signal processing, and control are described. Operating conditions for optimum sensitivity and linearity are discussed. From observations, a large effective bandwidth of around 10 GHz has been shown to provide sufficient sensitivity for detecting cosmic microwave background variations. C1 [Li, Chao-Te; Kubo, Derek Y.; Lin, Kai-Yang; Chen, Ming-Tang; Ho, P. T. P.; Chen, Chung-Cheng; Han, Chih-Chiang; Oshiro, Peter; Martin-Cocher, Pierre; Chang, Chia-Hao; Chang, Shu-Hao; Altamirano, Pablo; Jiang, Homin; Chang, Su-Wei; Huang, Yau-De; Hwang, Yuh-Jing; Koch, Patrick; Liu, Guo-Chin; Nishioka, Hiroaki; Umetsu, Keiichi; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wilson, Warwick; Kesteven, Michael] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Lin, Kai-Yang; Chiueh, Tzi-Dar; Lien, Chun-Hsien; Wang, Huei; Wei, Ray-Ming; Yang, Chia-Hsiang; Wu, Jiun-Huei Proty] Natl Taiwan Univ, Taipei 106, Taiwan. [Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peterson, Jeffrey B.] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. [Liu, Guo-Chin] Tamkang Univ, Tamsui 25137, Taipei County, Taiwan. RP Li, CT (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM ctli@asiaa.sinica.edu.tw RI Peterson, Jeffrey/O-4794-2014; OI Peterson, Jeffrey/0000-0003-1340-818X; WU, JIUN-HUEI/0000-0001-9608-7662; Umetsu, Keiichi/0000-0002-7196-4822; YANG, CHIA-HSIANG/0000-0003-1163-321X; CHIUEH, TZI-DAR/0000-0003-0851-6629 FU Ministry of Education; National Science Council; Academia Sinica; National Science Council of Taiwan [NSC98-2119-M-001-024-MY4] FX We thank the administrative staff for their support over the years. We thank A. Harris for useful discussions and notes. We thank the Ministry of Education, the National Science Council, and the Academia Sinica for their support of this project. We thank the NOAA for accommodating the AMiBA project on their site on Mauna Loa. We thank the Hawaiian people for allowing astronomers to work on their mountains in order to study the universe. This work is partially supported by the National Science Council of Taiwan under the grant NSC98-2119-M-001-024-MY4. NR 27 TC 6 Z9 6 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 746 EP 757 DI 10.1088/0004-637X/716/1/746 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000055 ER PT J AU Huang, CWL Wu, JHP Ho, PTP Koch, PM Liao, YW Lin, KY Liu, GC Molnar, SM Nishioka, H Umetsu, K Wang, FC Altamirano, P Birkinshaw, M Chang, CH Chang, SH Chang, SW Chen, MT Chiueh, T Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, D Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, TS Wilson, W AF Huang, Chih-Wei Locutus Wu, Jiun-Huei Proty Ho, Paul T. P. Koch, Patrick M. Liao, Yu-Wei Lin, Kai-Yang Liu, Guo-Chin Molnar, Sandor M. Nishioka, Hiroaki Umetsu, Keiichi Wang, Fu-Cheng Altamirano, Pablo Birkinshaw, Mark Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Chiueh, Tzihong Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI AMiBA: SCALING RELATIONS BETWEEN THE INTEGRATED COMPTON-y AND X-RAY-DERIVED TEMPERATURE, MASS, AND LUMINOSITY SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general; X-rays: galaxies: clusters ID MICROWAVE BACKGROUND ANISOTROPY; ZELDOVICH EFFECT MEASUREMENTS; REDSHIFT GALAXY CLUSTERS; COSMIC DISTANCE SCALE; LENSING CLUSTER; COOLING FLOWS; ARRAY; FRACTIONS; DENSITY; PROFILE AB We investigate the scaling relations between the X-ray and the thermal Sunyaev-Zel'dovich effect properties of clusters of galaxies, using data taken during 2007 by the Y. T. Lee Array for Microwave Background Anisotropy (AMiBA) at 94 GHz for the six clusters A1689, A1995, A2142, A2163, A2261, and A2390. The scaling relations relate the integrated Compton-y parameter Y(2500) to the X-ray-derived gas temperature T(e), total mass M(2500), and bolometric luminosity L(X) within r(2500). Our results for the power-law index and normalization are both consistent with the self-similar model and other studies in the literature except for the Y(2500)-L(X) relation, for which a physical explanation is given though further investigation may be still needed. Our results not only provide confidence for the AMiBA project but also support our understanding of galaxy clusters. C1 [Huang, Chih-Wei Locutus; Wu, Jiun-Huei Proty; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, Inst Astrophys, Dept Phys, Taipei 10617, Taiwan. [Huang, Chih-Wei Locutus; Wu, Jiun-Huei Proty; Liao, Yu-Wei; Lin, Kai-Yang; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Huang, Chih-Wei Locutus; Wu, Jiun-Huei Proty; Liao, Yu-Wei; Umetsu, Keiichi; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, LeCosPA Ctr, Taipei 10617, Taiwan. [Ho, Paul T. P.; Koch, Patrick M.; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M.; Nishioka, Hiroaki; Umetsu, Keiichi; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Birkinshaw, Mark] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Huang, CWL (reprint author), Natl Taiwan Univ, Inst Astrophys, Dept Phys, Taipei 10617, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; CHIUEH, TZI-HONG/0000-0003-2654-8763; Umetsu, Keiichi/0000-0002-7196-4822 FU Ministry of Education; National Science Council; Academia Sinica; National Taiwan University; National Center for Theoretical Science; Center for Theoretical Sciences, National Taiwan University; STFC FX We thank the Ministry of Education, the National Science Council, the Academia Sinica, and the National Taiwan University for their support of this project. We thank the Smithsonian Astrophysical Observatory for hosting the AMiBA project staff at the SMA Hilo Base Facility. We thank the NOAA for locating the AMiBA project on their site on Mauna Loa. We thank the Hawaiian people for allowing astronomers to work on their mountains in order to study the universe. We are grateful for computing support from the National Center for High-Performance Computing, Taiwan. This work is also supported by the National Center for Theoretical Science, and the Center for Theoretical Sciences, National Taiwan University, for J.-H.P. Wu. We appreciate the extensive comments on this paper from Katy Lancaster. Support from the STFC for M. B. is also acknowledged. NR 47 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 758 EP 765 DI 10.1088/0004-637X/716/1/758 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000056 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Dickherber, R Duke, C Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Millis, J Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Rovero, AC Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Theiling, M Thibadeau, S Varlotta, A Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Zitzer, B Harris, DE Massaro, F AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Dickherber, R. Duke, C. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Rovero, A. C. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Thibadeau, S. Varlotta, A. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. Harris, D. E. Massaro, F. TI VERITAS 2008-2009 MONITORING OF THE VARIABLE GAMMA-RAY SOURCE M 87 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M87, VER J1230+123); gamma rays: galaxies ID RADIO GALAXY M87; TEV EMISSION; BLACK-HOLE; JET; TELESCOPE; HST-1; M-87; VARIABILITY; ASTRONOMY; SITE AB M 87 is a nearby radio galaxy that is detected at energies ranging from radio to very high energy (VHE) gamma rays. Its proximity and its jet, misaligned from our line of sight, enable detailed morphological studies and extensive modeling at radio, optical, and X-ray energies. Flaring activity was observed at all energies, and multi-wavelength correlations would help clarify the origin of the VHE emission. In this paper, we describe a detailed temporal and spectral analysis of the VERITAS VHE gamma-ray observations of M 87 in 2008 and 2009. In the 2008 observing season, VERITAS detected an excess with a statistical significance of 7.2 standard deviations (sigma) from M 87 during a joint multi-wavelength monitoring campaign conducted by three major VHE experiments along with the Chandra X-ray Observatory. In 2008 February, VERITAS observed a VHE flare from M 87 occurring over a 4 day timespan. The peak nightly flux above 250 GeV was (1.14 +/- 0.26) x 10(-11) cm(-2) s(-1), which corresponded to 7.7% of the Crab Nebula flux. M 87 was marginally detected before this 4 day flare period, and was not detected afterward. Spectral analysis of the VERITAS observations showed no significant change in the photon index between the flare and pre-flare states. Shortly after the VHE flare seen by VERITAS, the Chandra X-ray Observatory detected the flux from the core of M 87 at a historical maximum, while the flux from the nearby knot HST-1 remained quiescent. Acciari et al. presented the 2008 contemporaneous VHE gamma-ray, Chandra X-ray, and Very Long Baseline Array radio observations which suggest the core as the most likely source of VHE emission, in contrast to the 2005 VHE flare that was simultaneous with an X-ray flare in the HST-1 knot. In 2009, VERITAS continued its monitoring of M 87 and marginally detected a 4.2 sigma excess corresponding to a flux of similar to 1% of the Crab Nebula. No VHE flaring activity was observed in 2009. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Fortin, P.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Arlen, T.; Chow, Y. C.; Ong, R. A.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.; Otte, A. N.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Cui, W.; Finley, J. P.; Gall, D.; Sembroski, G. H.; Varlotta, A.; Zitzer, B.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finnegan, G.; Godambe, S.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Imran, A.; Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Konopelko, A.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Pichel, A.; Rovero, A. C.] Inst Astron & Fis Espacio, RA-1428 Buenos Aires, DF, Argentina. [Reyes, L. C.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. [Senturk, G. Demet] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Harris, D. E.; Massaro, F.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM cmhui@physics.utah.edu RI Massaro, Francesco/L-9102-2016; OI Massaro, Francesco/0000-0002-1704-9850; 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 US Department of Energy; US National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK; NASA [GO8-9116X, GO90108X]; Foundation BLANCEFLOR Boncompagni-Ludovisi, nee Bildt FX VERITAS is supported by grants from the US Department of Energy, the US National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK.; The Chandra M 87 monitoring work at SAO was supported by NASA grants GO8-9116X and GO90108X.; F. Massaro acknowledges the Foundation BLANCEFLOR Boncompagni-Ludovisi, nee Bildt for the grant awarded him in 2009 to support his research. NR 37 TC 20 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 819 EP 824 DI 10.1088/0004-637X/716/1/819 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000062 ER PT J AU Oberg, KIR Bottinelli, S Jorgensen, JK van Dishoeck, EF AF Oberg, Karin I. R. Bottinelli, Sandrine Jorgensen, Jes K. van Dishoeck, Ewine F. TI A COLD COMPLEX CHEMISTRY TOWARD THE LOW-MASS PROTOSTAR B1-b: EVIDENCE FOR COMPLEX MOLECULE PRODUCTION IN ICES SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; astrobiology; ISM: abundances; ISM: molecules ID YOUNG STELLAR OBJECTS; ORGANIC-MOLECULES; METHYL FORMATE; HOT CORINOS; OUTFLOW; CORES; IRAS-16293-2422; DESORPTION; CLOUDS; EMISSION AB Gas-phase complex organic molecules have been detected toward a range of high-and low-mass star-forming regions at abundances which cannot be explained by any known gas-phase chemistry. Recent laboratory experiments show that UV irradiation of CH(3)OH-rich ices may be an important mechanism for producing complex molecules and releasing them into the gas phase. To test this ice formation scenario, we mapped the B1-b dust core and nearby protostar in CH(3)OH gas using the IRAM 30 m telescope to identify locations of efficient non-thermal ice desorption. We find three CH(3)OH abundance peaks tracing two outflows and a quiescent region on the side of the core facing the protostar. The CH(3)OH gas has a rotational temperature of similar to 10 K at all locations. The quiescent CH(3)OH abundance peak and one outflow position were searched for complex molecules. Narrow, 0.6-0.8 km s-1 wide, HCOOCH(3) and CH(3)CHO lines originating in cold gas are clearly detected, CH(3)OCH(3) is tentatively detected, and C(2)H(5)OH and HOCH(2)CHO are undetected toward the quiescent core, while no complex molecular lines were found toward the outflow. The core abundances with respect to CH(3)OH are similar to 2.3% and 1.1% for HCOOCH(3) and CH(3)CHO, respectively, and the upper limits are 0.7%-1.1%, which is similar to most other low-mass sources. The observed complex molecule characteristics toward B1-b and the pre-dominance of HCO-bearing species suggests a cold ice (below 25 K, the sublimation temperature of CO) formation pathway followed by non-thermal desorption through, e. g., UV photons traveling through outflow cavities. The observed complex gas composition together with the lack of any evidence of warm gas-phase chemistry provides clear evidence of efficient complex molecule formation in cold interstellar ices. C1 [Oberg, Karin I. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oberg, Karin I. R.; van Dishoeck, Ewine F.] Sterrewacht Leiden, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Bottinelli, Sandrine] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Jorgensen, Jes K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Oberg, KIR (reprint author), Harvard Smithsonian Ctr Astrophys, MS 42,60 Garden St, Cambridge, MA 02138 USA. RI Jorgensen, Jes Kristian/L-7936-2014 OI Jorgensen, Jes Kristian/0000-0001-9133-8047 FU RadioNet; Space Telescope Science Institute; NASA [NAS 5-26555]; Netherlands Organization for Scientific Research (NWO); Danish National Research Foundation; University of Copenhagen FX We are grateful to the IRAM staff for help with the observations and reduction of the resulting data. This work has benefitted from discussions with Herma Cuppen, Robin Garrod, and Lars Kristensen, and from comments by an anonymous referee. Umut Yildiz carried out the second round of observations at the IRAM 30 m with the financial support of RadioNet. Support for K.I.O is provided by NASA through Hubble Fellowship grant awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. Astrochemistry in Leiden is supported by an SPINOZA grant of the Netherlands Organization for Scientific Research (NWO). The Centre for Star and Planet Formation is funded by the Danish National Research Foundation and the University of Copenhagen's programme of excellence. NR 40 TC 61 Z9 61 U1 1 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 JUN 10 PY 2010 VL 716 IS 1 BP 825 EP 834 DI 10.1088/0004-637X/716/1/825 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000063 ER PT J AU Hatsukade, B Iono, D Yoshikawa, T Akiyama, M Dunlop, JS Ivison, RJ Peck, AB Ikarashi, S Biggs, A Ezawa, H Hanami, H Ho, P Hughes, DH Kawabe, R Kohno, K Matsushita, S Nakanishi, K Padilla, N Petitpas, G Tamura, Y Wagg, J Wilner, DJ Wilson, GW Yamada, T Yun, MS AF Hatsukade, B. Iono, D. Yoshikawa, T. Akiyama, M. Dunlop, J. S. Ivison, R. J. Peck, A. B. Ikarashi, S. Biggs, A. Ezawa, H. Hanami, H. Ho, P. Hughes, D. H. Kawabe, R. Kohno, K. Matsushita, S. Nakanishi, K. Padilla, N. Petitpas, G. Tamura, Y. Wagg, J. Wilner, D. J. Wilson, G. W. Yamada, T. Yun, M. S. TI UNVEILING THE NATURE OF SUBMILLIMETER GALAXY SXDF 850.6 (vol 711, pg 974, 2010) SO ASTROPHYSICAL JOURNAL LA English DT Correction C1 [Hatsukade, B.; Ikarashi, S.; Kohno, K.] Univ Tokyo, Inst Astron, Tokyo 1810015, Japan. [Iono, D.; Kawabe, R.; Nakanishi, K.; Tamura, Y.] Nobeyama Radio Observ, Minamisa Ku, Nagano 3841805, Japan. [Yoshikawa, T.; Akiyama, M.; Yamada, T.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Dunlop, J. S.; Ivison, R. J.] Univ Edinburgh, Sch Phys & Astron, Inst Astron, Scottish Univ Phys Alliance,Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.] Royal Observ, Sci & Technol Res Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Peck, A. B.] Joint ALMA Observ, Santiago 7550108, Chile. [Biggs, A.] European So Observ, D-85748 Garching, Germany. [Ezawa, H.] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Hanami, H.] Iwate Univ, Fac Humanities & Social Sci, Phys Sect, Morioka, Iwate 0208550, Japan. [Ho, P.; Matsushita, S.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Hughes, D. H.; Wagg, J.] INAOE, Puebla 72000, Pue, Mexico. [Kohno, K.] Univ Tokyo, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan. [Padilla, N.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago, Chile. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Wagg, J.] European So Observ, Santiago 19, Chile. [Wagg, J.; Wilner, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wilson, G. W.; Yun, M. S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. RP Hatsukade, B (reprint author), Univ Tokyo, Inst Astron, 2-21-1 Osawa, Tokyo 1810015, Japan. EM hatsukade@ioa.s.u-tokyo.ac.jp RI Ivison, R./G-4450-2011 OI Ivison, R./0000-0001-5118-1313 NR 1 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2010 VL 716 IS 1 BP 891 EP 891 DI 10.1088/0004-637X/716/1/891 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600CD UT WOS:000277960000069 ER PT J AU Pogue, MG AF Pogue, Michael G. TI The Acontiinae and Eustrotiinae (Lepidoptera: Noctuidae) of Great Smoky Mountains National Park SO ZOOTAXA LA English DT Article DE systematics; all taxa biodiversity inventory; North Carolina; Tennessee; species richness estimators AB Five species of Acontiinae and nine species of Eustrotiinae are known to occur in Great Smoky Mountains National Park. Each species is documented with an adult image, description/diagnosis, flight period, park distribution, abundance, elevational range, general distribution, and larval hosts. Species accumulation curves using the abundance-based estimators Chao 1 and ACE, and the incidence-based estimators Chao 2 and ICE are presented for each subfamily. The results from these estimators indicate that the number of species observed is equal to or very close to the number of estimated species and, therefore, it is unlikely that additional species will be added to the fauna of GSMNP in these subfamilies. C1 ARS, Systemat Entomol Lab, PSI, US Dept Agr,Smithsonian Inst,NMNH, Washington, DC 20013 USA. RP Pogue, MG (reprint author), ARS, Systemat Entomol Lab, PSI, US Dept Agr,Smithsonian Inst,NMNH, POB 37012,MRC-168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov FU Discover Life in America (DLIA) FX Discover Life in America (DLIA) provided partial funding for this project in 2003, 2004, and 2007. Jeanie Hilten of DLIA was helpful in providing logistic support during my stays in GSNMP and Keith Langdon of the National Park Service was instrumental in providing collecting permits. David L. Wagner (University of Connecticut, Storrs, CT) and Brian Scholtens (College of Charleston, Charleston, SC) helped organize and invited me to participate in the Lepidoptera BioBlitzes held during 2000, 2002, and 2004. Brian Scholtens provided his main database of the Noctuidae, which was helpful in obtaining records that were new to me. David Wagner provided specimens included in this study. David Adamski (Systematic Entomology Laboratory, U. S. D. A., Washington, DC) prepared the maps and figures. Eric H. Metzler (Alamogordo, New Mexico) and Thomas J. Henry and David A. Nickle (Systematic Entomology Laboratory, U.S.D.A., Washington, DC) critically reviewed a draft of this paper. NR 25 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 JUN 9 PY 2010 IS 2499 BP 1 EP 20 PG 20 WC Zoology SC Zoology GA 607XF UT WOS:000278539900001 ER PT J AU Caldwell, MS Johnston, GR McDaniel, JG Warkentin, KM AF Caldwell, Michael S. Johnston, Gregory R. McDaniel, J. Gregory Warkentin, Karen M. TI Vibrational Signaling in the Agonistic Interactions of Red-Eyed Treefrogs SO CURRENT BIOLOGY LA English DT Article ID BREEDING-BEHAVIOR; SEISMIC COMMUNICATION; LEAF-FROG; ANURA; HYLIDAE; CALLIDRYAS; EVOLUTION; ECOLOGY; MAMMALS; TOADS AB Sensitivity to substrate-borne vibrations is widespread in animals and evolutionarily precedes hearing but, compared with other sensory modalities, we know little about vibrational communication, particularly in vertebrates [1]. For plant-dwelling arthropods, vibrations are likely as important as sound [1-3]. Arboreal vertebrates excite plant vibrations with most movements [4], but the behavioral relevance of these vibrations has not been tested experimentally [5, 6]. In playback experiments using a robotic model frog and an electrodynamic shaker, we demonstrate that plant-borne vibrations generated by the shaking (tremulation) display of male red-eyed treefrogs (Agalychnis callidryas) are a vibrational signal, necessary and sufficient to elicit tremulations in response. A trend toward increased aggression during visual playbacks suggests that the visual component of tremulations may also convey information. In male-male contests, tremulations were the most frequent aggressive display, and their use and vibrational characteristics varied with male size and conflict context. Nearly all of A. callidryas' signaling behaviors, including tremulations and acoustic calls, excite strong, stereotyped vibrations that travel through plants and could be informative to receivers. Our results demonstrate that vibrational signals serve a key role in the biology of one well-known arboreal frog and suggest that consideration of the vibrational modality may significantly broaden our appreciation of the behavior and evolution of arboreal vertebrates. C1 [Caldwell, Michael S.; Warkentin, Karen M.] Boston Univ, Dept Biol, Boston, MA 02215 USA. [Johnston, Gregory R.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. [Johnston, Gregory R.] Adelaide Zoo, Royal Zool Soc S Australia, Adelaide, SA 5000, Australia. [Johnston, Gregory R.; Warkentin, Karen M.] Smithsonian Trop Res Inst, Panama City, Panama. [McDaniel, J. Gregory] Boston Univ, Dept Mech Engn, Boston, MA 02215 USA. RP Caldwell, MS (reprint author), Boston Univ, Dept Biol, 5 Cummington St, Boston, MA 02215 USA. EM mpod3@alum.bu.edu RI Johnston, Greg/F-9917-2010 FU Smithsonian Tropical Research Institute; National Science Foundation [IOS-0710247, IBN-0234439]; Boston University FX We thank S. Poo, S. Galeano, V. Briggs, and A. Trillo for field assistance; D. McCornack for building the models; J. Robertson for information on A. callidryas' vision; J. Christy, AS. Rand, and the Gamboa Frog Seminar group for advice; and the Autoridad Nacional del Ambiente (Panama) for research permits. This work was supported by the Smithsonian Tropical Research Institute, Boston University, and the National Science Foundation (IOS-0710247 and IBN-0234439). NR 31 TC 31 Z9 31 U1 3 U2 31 PU CELL PRESS PI CAMBRIDGE PA 600 TECHNOLOGY SQUARE, 5TH FLOOR, CAMBRIDGE, MA 02139 USA SN 0960-9822 J9 CURR BIOL JI Curr. Biol. PD JUN 8 PY 2010 VL 20 IS 11 BP 1012 EP 1017 DI 10.1016/j.cub.2010.03.069 PG 6 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 609NC UT WOS:000278662500026 PM 20493702 ER PT J AU Yoo, J Zaldarriaga, M Hernquist, L AF Yoo, Jaiyul Zaldarriaga, Matias Hernquist, Lars TI Lensing reconstruction of cluster-mass cross correlation with cosmic microwave background polarization SO PHYSICAL REVIEW D LA English DT Article ID PARTICLE HYDRODYNAMICS SIMULATIONS; GALAXY CLUSTERS; DARK-MATTER; CMB; TEMPERATURE; FRACTION; CHANDRA AB We extend our maximum likelihood method for reconstructing the cluster-mass cross correlation from cosmic microwave background (CMB) temperature anisotropies and develop new estimators that utilize six different quadratic combinations of CMB temperature and polarization fields. Our maximum likelihood estimators are constructed with delensed CMB temperature and polarization fields by using an assumed model of the convergence field, and they can be iteratively applied to a set of clusters, approaching the optimal condition for the lensing reconstruction as the assumed initial model is refined. Using smoothed particle hydrodynamics simulations, we create a catalog of realistic clusters obtainable from the current Sunyaev-Zel'dovich surveys, and we demonstrate the ability of the maximum likelihood estimators to reconstruct the cluster-mass cross correlation from the massive clusters. The iTT temperature estimator provides a signal-to-noise ratio of a factor of 3 larger than the iEB polarization estimator, unless the detector noise for measuring polarization anisotropies is controlled under 3 mu K. C1 [Yoo, Jaiyul; Zaldarriaga, Matias; Hernquist, Lars] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zaldarriaga, Matias] Inst Adv Study, Sch Nat Sci, Princeton, NJ 08540 USA. [Zaldarriaga, Matias] Harvard Univ, Jefferson Phys Lab, Cambridge, MA 02138 USA. RP Yoo, J (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jyoo@cfa.harvard.edu FU Harvard College Observatory; David and Lucile Packard; Alfred P. Sloan; John D. and Catherine T. MacArthur Foundations; NSF [AST 05-06556]; NASA ATP [NNG 05GJ40G] FX J.Y. acknowledges useful discussions with Adam Lidz, Jonathan Pritchard, and Amit Yadav. J.Y. is supported by the Harvard College Observatory under the Donald H. Menzel fund. M.Z. is supported by the David and Lucile Packard, the Alfred P. Sloan, and the John D. and Catherine T. MacArthur Foundations. This work was further supported by NSF Grant No. AST 05-06556 and NASA ATP Grant No. NNG 05GJ40G. NR 31 TC 7 Z9 7 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 EI 1550-2368 J9 PHYS REV D JI Phys. Rev. D PD JUN 8 PY 2010 VL 81 IS 12 AR 123006 DI 10.1103/PhysRevD.81.123006 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 607IG UT WOS:000278493100001 ER PT J AU Chang, GQ Li, CH Phillips, DF Walsworth, RL Kartner, FX AF Chang, Guoqing Li, Chih-Hao Phillips, David F. Walsworth, Ronald L. Kaertner, Franz X. TI Toward a broadband astro-comb: effects of nonlinear spectral broadening in optical fibers SO OPTICS EXPRESS LA English DT Article ID LASER FREQUENCY COMBS; GENERATION; PULSE; COMPRESSION; CALIBRATION; PRECISION; NM AB We propose and analyze a new approach to generate a broadband astro-comb by spectral broadening of a narrowband astro-comb inside a highly nonlinear optical fiber. Numerical modeling shows that cascaded four-wave-mixing dramatically degrades the input comb's side-mode suppression and causes side-mode amplitude asymmetry. These two detrimental effects can systematically shift the center-of-gravity of astro-comb spectral lines as measured by an astrophysical spectrograph with resolution approximate to 100,000; and thus lead to wavelength calibration inaccuracy and instability. Our simulations indicate that this performance penalty, as a result of nonlinear spectral broadening, can be compensated by using a filtering cavity configured for double-pass. As an explicit example, we present a design based on an Yb-fiber source comb (with 1 GHz repetition rate) that is filtered by double-passing through a low finesse cavity (finesse = 208), and subsequent spectrally broadened in a 2-cm, SF6-glass photonic crystal fiber. Spanning more than 300 nm with 16 GHz line spacing, the resulting astro-comb is predicted to provide 1 cm/s (similar to 10 kHz) radial velocity calibration accuracy for an astrophysical spectrograph. Such extreme performance will be necessary for the search for and characterization of Earth-like extra-solar planets, and in direct measurements of the change of the rate of cosmological expansion. (C) 2010 Optical Society of America C1 [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. [Li, Chih-Hao; Phillips, David F.; Walsworth, Ronald L.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Chang, GQ (reprint author), MIT, Dept Elect Engn & Comp Sci, 77 Mass Ave, Cambridge, MA 02139 USA. EM guoqing@mit.edu FU NASA [NNX09AC92G]; NSF [AST-0905214, 0905592] FX This work was funded under NASA award number NNX09AC92G and NSF grants AST-0905214 and 0905592. NR 13 TC 30 Z9 32 U1 0 U2 11 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 7 PY 2010 VL 18 IS 12 BP 12736 EP 12747 DI 10.1364/OE.18.012736 PG 12 WC Optics SC Optics GA 607SU UT WOS:000278527700077 PM 20588402 ER PT J AU Li, CH Glenday, AG Benedick, AJ Chang, GQ Chen, LJ Cramer, C Fendel, P Furesz, G Kartner, FX Korzennik, S Phillips, DF Sasselov, D Szentgyorgyi, A Walsworth, RL AF Li, Chih-Hao Glenday, Alexander G. Benedick, Andrew J. Chang, Guoqing Chen, Li-Jin Cramer, Claire Fendel, Peter Furesz, Gabor Kaertner, Franz X. Korzennik, Sylvain Phillips, David F. Sasselov, Dimitar Szentgyorgyi, Andrew Walsworth, Ronald L. TI In-situ determination of astro-comb calibrator lines to better than 10 cm s(-1) SO OPTICS EXPRESS LA English DT Article ID LASER FREQUENCY COMBS; DECELERATION; PRECISION AB Improved wavelength calibrators for high-resolution astrophysical spectrographs will be essential for precision radial velocity (RV) detection of Earth-like exoplanets and direct observation of cosmological deceleration. The astro-comb is a combination of an octave-spanning femtosecond laser frequency comb and a Fabry-Perot cavity used to achieve calibrator line spacings that can be resolved by an astrophysical spectrograph. Systematic spectral shifts associated with the cavity can be 0.1-1 MHz, corresponding to RV errors of 10-100 cm/s, due to the dispersive properties of the cavity mirrors over broad spectral widths. Although these systematic shifts are very stable, their correction is crucial to high accuracy astrophysical spectroscopy. Here, we demonstrate an in-situ technique to determine the systematic shifts of astro-comb lines due to finite Fabry-Perot cavity dispersion. The technique is practical for implementation at a telescope-based spectrograph to enable wavelength calibration accuracy better than 10 cm/s. (C) 2010 Optical Society of America C1 [Li, Chih-Hao; Glenday, Alexander G.; Cramer, Claire; Sasselov, Dimitar; Walsworth, Ronald L.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Li, Chih-Hao; Glenday, Alexander G.; Furesz, Gabor; Korzennik, Sylvain; Phillips, David F.; Sasselov, Dimitar; Szentgyorgyi, Andrew; Walsworth, Ronald L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Benedick, Andrew J.; Chang, Guoqing; Chen, Li-Jin; Fendel, Peter; Kaertner, Franz X.] MIT, Cambridge, MA 02139 USA. RP Li, CH (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM chli@cfa.harvard.edu NR 20 TC 20 Z9 21 U1 0 U2 2 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD JUN 7 PY 2010 VL 18 IS 12 BP 13239 EP 13249 DI 10.1364/OE.18.013239 PG 11 WC Optics SC Optics GA 607SU UT WOS:000278527700128 PM 20588453 ER PT J AU Catlos, EJ Baker, C Sorensen, SS Cemen, I Hancer, M AF Catlos, Elizabeth J. Baker, Courteney Sorensen, Sorena S. Cemen, Ibrahim Hancer, Mete TI Geochemistry, geochronology, and cathodoluminescence imagery of the Salihli and Turgutlu granites (central Menderes Massif, western Turkey): Implications for Aegean tectonics SO TECTONOPHYSICS LA English DT Article DE Monazite; Extension tectonics; Turkish Aegean region; Geochronology; Menderes Massif ID METAMORPHIC CORE COMPLEX; HIGH-PRESSURE METAMORPHISM; U-PB GEOCHRONOLOGY; ANATOLIDE BELT; GEDIZ GRABEN; SW TURKEY; DISCRIMINATION DIAGRAMS; GEODYNAMIC IMPLICATIONS; EXTENSIONAL TECTONICS; NORTHWESTERN ANATOLIA AB The Menderes Massif (western Turkey) is an important metamorphic core complex located in the Aegean region; geochemical and geochronological data from this extensional domain facilitates our understanding of large-scale extension of the Earth's lithosphere. S-type, peraluminous granites (Salihli and Turgutlu) that intrude the Alasehir detachment which bounds the northern edge of the central Menderes Massif may have been generated due to subduction of the Eastern Mediterranean floor along the Hellenic trench. In situ Th-Pb ion microprobe monazite ages from the granites range from 21.7 +/- 4.5 Ma to 9.6 +/- 1.6 Ma (+/- 1 sigma). Higher uncertainty in the ages is attributed to monazite common Pb, but the range is consistent with cathodoluminescence (CL) imagery that document complex textures within the samples. Salihli and Turgutlu granites share many similar characteristics, including multiple generations of plagioclase (some with shocked cores), plagioclase replacing K-feldspar and the development of myrmekite, evidence for fluid interaction, and multiple generations of microcracks and microfaults. The granites may have evolved from compositionally distinct magma sources, as Salihli samples in general contain allanite as the major accessory mineral, whereas Turgutlu granites contain monazite. However, the CL imagery document similar alteration textures. The youngest Turgutlu monazite grain (11.5 +/- 0.8 Ma) is located in the rim of a K-feldspar grain close to myrmekite, and the youngest Salihli monazite grain (9.6 +/- 1.6 Ma) is located in the outer edge of an altered plagioclase crystal. These ages likely time episodes of deformation as the granites were subjected to exhumation along the Alasehir detachment. Ages reported here are similar to dates constraining extension reported elsewhere in the Aegean, but indicate a level of complexity when linking movement within the Menderes Massif to the large-scale geodynamic processes that created other metamorphic core complexes in the region. Difficulties exist in linking the ages obtained from the granites to specific tectonic events due to the presence of secondary alteration textures, generations of mineral growth, and multiple episodes of deformation. (C) 2009 Elsevier B.V. All rights reserved. C1 [Catlos, Elizabeth J.] Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, Austin, TX 78712 USA. [Baker, Courteney; Cemen, Ibrahim] Oklahoma State Univ, Sch Geol, Stillwater, OK 74078 USA. [Sorensen, Sorena S.] Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Hancer, Mete] Pamukkale Univ, Muhendislik Fak Jeoloji Muh, TR-20070 Denizli, Turkey. RP Catlos, EJ (reprint author), Univ Texas Austin, Jackson Sch Geosci, Dept Geol Sci, 1 Univ Stn C1100, Austin, TX 78712 USA. EM ejcatlos@gmail.com RI Catlos, Elizabeth/B-7943-2011; UCLA, SIMS/A-1459-2011 FU National Science Foundation [NSF-0440169]; Division of Earth Sciences, National Science Foundation; Smithsonian Institution's National Museum of Natural History FX This work was supported by an award to E.J Catlos, I. Cemen, and M.J. Kohn from the National Science Foundation (NSF-0440169). We thank the UCLA Ion Microprobe Facility, which is partly supported by a grant from the Instrumentation and Facilities Program, Division of Earth Sciences, National Science Foundation. CL images were generated with the support of the Smithsonian Institution's National Museum of Natural History Fellowship Program. CC and EB samples were collected with assistance from Matthew J. Kohn, M. Cemal Goncuoglu, and Emre Diniz. Rock samples were analyzed for their bulk and trace element chemistry by Activation Laboratories in Ontario, Canada. We acknowledge and thank Dr. Nesat Konak for providing detailed geologic maps of the granites, which aided us in locating them in the field. We are grateful to Andres Villavicencio for the editorial handling, and thank Michael Jercinovic and an anonymous reviewer for their constructive comments that improved the original manuscript. NR 116 TC 20 Z9 20 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0040-1951 J9 TECTONOPHYSICS JI Tectonophysics PD JUN 5 PY 2010 VL 488 IS 1-4 SI SI BP 110 EP 130 DI 10.1016/j.tecto.2009.06.001 PG 21 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 621YY UT WOS:000279624200008 ER PT J AU Cardoso, P Morano, E AF Cardoso, Pedro Morano, Eduardo TI The Iberian spider checklist (Araneae) SO ZOOTAXA LA English DT Article DE Arthropoda; Balearic Islands; catalogue; distribution; endemic species; Portugal; Spain; species list ID TAXONOMY AB We compiled all the available information regarding spider species distribution in the Iberian Peninsula (including the Balearic Islands). At present, 1335 species are known from the region, of which 236 are Iberian endemics, in 373 genera and 55 families. Portugal presents 768 species and Spain (including Andorra and Gibraltar), 1213 species. Although the work developed during recent decades has allowed a major increase in our knowledge of this group, there are certainly many species yet to be found and, for those already listed, the distribution is largely unknown. Although linyphiids present the highest number of known species (267), dysderids present the highest endemic richness (46 species). Information regarding the provinces from where each species was referenced is also presented and reveals large differences in the knowledge about each province, with most presenting very few known records and species. This checklist is accompanied by an online catalogue where all the information here presented is exhaustively listed and regularly updated. C1 [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Cardoso, Pedro] Univ Acores, Dept Ciencias Agr, Azorean Biodivers Grp CITA A, P-9701851 Terra Cha, Angra Heroismo, Portugal. [Morano, Eduardo] Santo Tomas Vilanueva, Ciudad Real 13170, Spain. RP Cardoso, P (reprint author), Natl Museum Nat Hist, Smithsonian Inst, 10th & Constitut NW,MRC 105,Room E-509, Washington, DC 20560 USA. EM pcardoso@ennor.org RI Cardoso, Pedro/A-8820-2008 OI Cardoso, Pedro/0000-0001-8119-9960 FU Fundacao para a Ciencia e Tecnologia [SFRH/BPD/40688/2007] FX We thank Gustavo Hormiga, Miguel Ferrandez and two anonymous referee for suggestions that improved the manuscript. Pedro Cardoso was supported by Fundacao para a Ciencia e Tecnologia (SFRH/BPD/40688/2007). NR 50 TC 13 Z9 30 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUN 4 PY 2010 IS 2495 BP 1 EP 52 PG 52 WC Zoology SC Zoology GA 607GZ UT WOS:000278488400001 ER PT J AU Robinson, H Skvarla, JJ AF Robinson, Harold Skvarla, John J. TI A new genus, Okia, from northern Myanmar (Vernonieae, Asteraceae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article AB We establish here a new Asian genus of Vernonieae, Okia, for Cacalla birmanica O. Kuntze. It is most closely related to the similarly calcicolous Koyamasia of Thailand, and more distantly to the widespread tropical Asian Adkins. C1 [Robinson, Harold] Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, Washington, DC 20013 USA. [Skvarla, John J.] Univ Oklahoma, Dept Bot & Microbiol, Norman, OK 73019 USA. [Skvarla, John J.] Univ Oklahoma, Oklahoma Biol Survey, Norman, OK 73019 USA. RP Robinson, H (reprint author), Smithsonian Inst, Dept Bot, MRC 166, Natl Museum Nat Hist, POB 37012, Washington, DC 20013 USA. EM robinsoh@si.edu; jskvarla@ou.edu FU New York Botanical Garden FX We thank the New York Botanical Garden for the loan of the type specimen of Cacalia birmanica. The contributions of Marjorie Knowles, former technician in the Department Botany, National Museum of Natural History, are fully appreciated. We gratefully acknowledge Alice Tangerini for her artwork. We thank Bill Chissoe, University of Oklahoma, for help with scanning electron microscopy. NR 13 TC 3 Z9 3 U1 0 U2 1 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUN 3 PY 2010 VL 123 IS 1 BP 87 EP 91 DI 10.2988/09-26.1 PG 5 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 609QH UT WOS:000278671700009 ER PT J AU Stokes, D AF Stokes, Deborah TI Fish/Fetish(!?): A Note on "Mami Wata: Arts for Water Spirits in Africa and Its Diasporas" SO AFRICAN ARTS LA English DT Editorial Material C1 [Stokes, Deborah] Smithsonian Inst, Natl Museum African Art, Leading Youth Program, Washington, DC 20560 USA. [Stokes, Deborah] Smithsonian Inst, Natl Museum African Art, Publ Sch Program, Washington, DC 20560 USA. RP Stokes, D (reprint author), Smithsonian Inst, Natl Museum African Art, Leading Youth Program, Washington, DC 20560 USA. EM DStokes@si.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU MIT PRESS PI CAMBRIDGE PA 55 HAYWARD STREET, CAMBRIDGE, MA 02142 USA SN 0001-9933 J9 AFR ARTS JI Afr. Arts PD SUM PY 2010 VL 43 IS 2 BP 8 EP 9 DI 10.1162/afar.2010.43.2.8 PG 2 WC Art SC Art GA 608DM UT WOS:000278562700002 ER PT J AU Jones, LA Petty, A Shultz, M Sharpless, R Walker, M AF Jones, Lu Ann Petty, Adrienne Shultz, Mark Sharpless, Rebecca Walker, Melissa TI AGRICULTURAL HISTORY ROUNDTABLE COMPLICATING THE STORY: ORAL HISTORY AND THE STUDY OF THE RURAL SOUTH: LU ANN JONES, ADRIENNE PETTY, MARK SCHULTZ, REBECCA SHARPLESS, AND MELISSA WALKER SO AGRICULTURAL HISTORY LA English DT Editorial Material ID AMERICAN SOUTH AB Five historians who have used oral history to study the rural South assess the ways that oral history methodology and content have complicated our understanding of the region's agricultural past. They explore two major themes: first, the ways that the information gathered in oral history interviews revealed the diversity and complexity of the rural South and second, how the dialectical process of the interview the give and take between interviewer and informant shaped their interpretation of that rural past. Sharpless and Jones examine new content gained through interviews with German Americans and plantation managers, who have been excluded from most studies. Through their personal experiences, Petty and Schultz consider the ways in which relationships between interviewer and interviewee shape the narrative, often obviating differences of class and particularly race. Walker frames the discussion from her experiences in interviewing a variety of rural Southerners. C1 [Jones, Lu Ann] Natl Pk Serv, Washington, DC 20240 USA. [Jones, Lu Ann] Univ S Florida, Tampa, FL 33620 USA. [Jones, Lu Ann] E Carolina Univ, Greenville, NC 27858 USA. [Jones, Lu Ann] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. [Petty, Adrienne] CUNY City Coll, New York, NY USA. [Shultz, Mark] Lewis Univ, Romeoville, IL USA. [Sharpless, Rebecca] Texas Christian Univ, Ft Worth, TX 76129 USA. [Sharpless, Rebecca] Baylor Univ, Inst Oral Hist, Waco, TX 76798 USA. [Walker, Melissa] Converse Coll, Spartanburg, SC USA. RP Jones, LA (reprint author), Natl Pk Serv, Washington, DC 20240 USA. NR 66 TC 1 Z9 1 U1 0 U2 0 PU AGRICULTURAL HISTORY SOCIETY PI LITTLE ROCK PA UALR, DEPT HISTORY, 2801 S UNIVERSITY AVE, LITTLE ROCK, AR 72324-1099 USA SN 0002-1482 J9 AGR HIST JI Agric. Hist. PD SUM PY 2010 VL 84 IS 3 BP 281 EP 326 DI 10.3098/ah.2010.84.3.281 PG 46 WC Agriculture, Multidisciplinary; History; History & Philosophy Of Science SC Agriculture; History; History & Philosophy of Science GA 611BP UT WOS:000278785800001 ER PT J AU Ceron-Souza, I Rivera-Ocasio, E Medina, E Jimenez, JA McMillan, WO Bermingham, E AF Ceron-Souza, Ivania Rivera-Ocasio, Elsie Medina, Ernesto Jimenez, Jorge A. McMillan, W. Owen Bermingham, Eldredge TI HYBRIDIZATION AND INTROGRESSION IN NEW WORLD RED MANGROVES, RHIZOPHORA (RHIZOPHORACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Central American Isthmus; evolutionary history; hybridiation; introgression; Rhizophora harrisonii; Rhizophora mangle; Rhizophora racemosa; Rhizophoraceae ID MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; NATURAL HYBRIDIZATION; HYBRID SPECIATION; MULTIPLE ALLELES; CHLOROPLAST DNA; HARDY-WEINBERG; GENE FLOW; EVOLUTION; INFERENCE AB Premise of the study: Hybridization is common in both animals and plants and can lead to a diverse array of outcomes ranging from the generation of new ecotypes or species to the breakdown of morphological differences. Here, we explore the extent of hybridization in the three currently recognized New World Rhizophora species-R. mangle, R. racemosa, and the putative hybrid species R. harrisonii. Methods: We assayed variation across the three recognized Rhizophora species using two noncoding chloroplast (cpDNA), two flanking microsatellite regions (FMRs), and six microsatellite loci. Key results: Gene genealogies of cpDNA and FMRs showed a strong phylogeographic break across the Central American Isthmus, but little relationship to recognized species boundaries. Instead, individuals collected in the same ocean basin and classified as R. mangle and R. racemosa by morphological characteristics were more closely related to each other than with similar looking individuals collected in the other ocean basin. Nonetheless, there were low, yet significant differences at microsatellite loci among co-occurring populations of R. mangle and R. racemosa in both ocean basins, suggesting that two taxonomic groups coexist. However, we found no genetic evidence that R. harrisonii was a hybrid species. Rather, R. harrisonii appears to represent a morphotype produced by ongoing hybridization and backcrossing between R. mangle and R. racemosa. Conclusions: Our data support ancient and persistent introgressive hybridization among new world Rhizophora and argue for a full revision of the systematic relationships of the group based on much finer morphological, ecological, and genetic analyses. C1 [Ceron-Souza, Ivania; McMillan, W. Owen; Bermingham, Eldredge] Smithsonian Trop Res Inst, Panama City, Panama. [Ceron-Souza, Ivania; Rivera-Ocasio, Elsie] Univ Puerto Rico, Dept Biol, San Juan, PR 00931 USA. [Medina, Ernesto] IVIC, Ctr Ecol, Caracas 1020A, Venezuela. [Jimenez, Jorge A.] Fdn MarViva, San Jose, Costa Rica. [McMillan, W. Owen] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA. RP Ceron-Souza, I (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Panama City, Panama. EM iviceron@gmail.com FU STRI; University of Puerto Rico; NSF [HRD 0206200, IBN-0344705]; Microsoft Corporation FX The authors thank STRI and the University of Puerto Rico for financial support (DEGI and NSF-EPSCor fellowships) to ICS and NSF grants (HRD 0206200 and IBN-0344705) to WOM. Thanks to ANAM (Panama), MINAE and OTS (Costa Rica) for collection permits and logistical support and E. Diaz, L. M. Garcia, N. Giraldo, G. Thomas, and D. Portuguez for field support. The authors especially thank C. Dick and A. Schwarzbach for their generous donation of samples. Finally, the authors thank F. Alda, C. Arias, A. Crawford, L. Geyer, C. Salazar, K. Saltonstall, O. Sanjur, and the anonymous reviewers for invaluable suggestions to previous versions of this manuscript. Part of this work was carried out using the resources of the Computational Biology Service Unit of Cornell University, which is partially funded by Microsoft Corporation. NR 99 TC 25 Z9 26 U1 0 U2 16 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 EI 1537-2197 J9 AM J BOT JI Am. J. Bot. PD JUN PY 2010 VL 97 IS 6 BP 945 EP 957 DI 10.3732/ajb.0900172 PG 13 WC Plant Sciences SC Plant Sciences GA 603MJ UT WOS:000278212400005 PM 21622465 ER PT J AU Hinde, K Captanio, JP AF Hinde, Katie Captanio, John P. TI Lactational Programming? Mother's Milk Energy Predicts Infant Behavior and Temperament in Rhesus Macaques (Macaca mulatta) SO AMERICAN JOURNAL OF PRIMATOLOGY LA English DT Article DE behavioral syndromes; infant development; nutritional programming; personality; lactation ID CERVUS-ELAPHUS-HISPANICUS; MATERNAL-CARE; LIFE-HISTORY; INDIVIDUAL-DIFFERENCES; REPRODUCTIVE SUCCESS; NUTRIENT DEPOSITION; CALF GROWTH; MONKEYS; YOUNG; FETAL AB There are many aspects of "mothering" that may provide information to the mammalian infant about environmental conditions during critical periods of development. One essential element of mothering involves the quantity and quality of milk that mothers provide for their infants, but little is known about the consequences of variation in milk production. Mother's milk may affect infant behavior by contributing to brain development and to the development of behavioral dispositions. Here we present the first evidence for any mammal that natural variation in available milk energy (AME) from the mother is associated with later variation in infant behavior and temperament in rhesus macaques (Macaca mulatta, N = 59). In the early postnatal period, heavier mothers with more reproductive experience produced greater AME, which is the product of milk energy density (kcal/g) and milk yield (g). Moreover, infants whose mothers produced greater AME in the early postnatal period showed higher activity levels and greater confidence in a stressful setting later in infancy. Our results suggest that the milk energy available soon after birth may be a nutritional cue that calibrates the infant's behavior to environmental or maternal conditions. These data provide new insight into potential mechanisms for the development of behavior and temperament and illuminate new directions for investigating maternal effects, nutritional programming, and developmental plasticity. Am. J. Primatol. 72:522-529, 2010. (C) 2010 Wiley-Liss, Inc. C1 [Hinde, Katie] Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA 95616 USA. [Hinde, Katie] Smithsonian Natl Zool Pk, Nutr Lab, Washington, DC USA. [Captanio, John P.] Univ Calif Davis, Dept Psychol, Davis, CA 95616 USA. RP Hinde, K (reprint author), Univ Calif Davis, Calif Natl Primate Res Ctr, Brain Mind & Behav Unit, Davis, CA 95616 USA. EM kjhinde@ucdavis.edu OI Hinde, Katie/0000-0002-0528-866X FU National Science Foundation [DDIG 0525025]; American Society of Primatologists Small Research; National Institute of Health [RR019970, RR000169] FX Contract grant sponsor: National Science Foundation; Contract grant number: DDIG 0525025; Contract grant sponsors: American Society of Primatologists Small Research; National Institute of Health; Contract grant numbers: RR019970; RR000169. NR 64 TC 34 Z9 34 U1 2 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0275-2565 EI 1098-2345 J9 AM J PRIMATOL JI Am. J. Primatol. PD JUN PY 2010 VL 72 IS 6 BP 522 EP 529 DI 10.1002/ajp.20806 PG 8 WC Zoology SC Zoology GA 599YI UT WOS:000277949800008 PM 20162547 ER PT J AU Baldwin, BG Wagner, WL AF Baldwin, Bruce G. Wagner, Warren L. TI Hawaiian angiosperm radiations of North American origin SO ANNALS OF BOTANY LA English DT Review DE Angiosperms; adaptive radiation; disjunctions; flora; island biogeography; long-distance dispersal; ecological opportunity; Hawaiian Islands; North America; Pacific; phytogeography; sky islands ID NUCLEAR RIBOSOMAL DNA; SILVERSWORD ALLIANCE COMPOSITAE; LONG-DISTANCE DISPERSAL; MOLECULAR PHYLOGENY; ADAPTIVE RADIATION; SEQUENCE DATA; HISTORICAL BIOGEOGRAPHY; METROSIDEROS MYRTACEAE; SELF-INCOMPATIBILITY; LYCIUM SOLANACEAE AB Putative phytogeographical links between America (especially North America) and the Hawaiian Islands have figured prominently in disagreement and debate about the origin of Pacific floras and the efficacy of long-distance (oversea) plant dispersal, given the obstacles to explaining such major disjunctions by vicariance. Review of past efforts, and of progress over the last 20 years, toward understanding relationships of Hawaiian angiosperms allows for a historically informed re-evaluation of the American (New World) contribution to Hawaiian diversity and evolutionary activity of American lineages in an insular setting. Temperate and boreal North America is a much more important source of Hawaiian flora than suggested by most 20th century authorities on Pacific plant life, such as Fosberg and Skottsberg. Early views of evolution as too slow to account for divergence of highly distinctive endemics within the Hawaiian geological time frame evidently impeded biogeographical understanding, as did lack of appreciation for the importance of rare, often biotically mediated dispersal events and ecological opportunity in island ecosystems. Molecular phylogenetic evidence for North American ancestry of Hawaiian plant radiations, such as the silversword alliance, mints, sanicles, violets, schiedeas and spurges, underlines the potential of long-distance dispersal to shape floras, in accordance with hypotheses championed by Carlquist. Characteristics important to colonization of the islands, such as dispersibility by birds and ancestral hybridization or polyploidy, and ecological opportunities associated with 'sky islands' of temperate or boreal climate in the tropical Hawaiian archipelago may have been key to extensive diversification of endemic lineages of North American origin that are among the most species-rich clades of Hawaiian plants. Evident youth of flowering-plant lineages from North America is highly consistent with recent geological evidence for lack of high-elevation settings in the Hawaiian chain immediately prior to formation of the oldest, modern high-elevation island, Kaua'i. C1 [Baldwin, Bruce G.] Univ Calif Berkeley, Jepson Herbarium, Berkeley, CA 94720 USA. [Baldwin, Bruce G.] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Wagner, Warren L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Baldwin, BG (reprint author), Univ Calif Berkeley, Jepson Herbarium, Berkeley, CA 94720 USA. EM bbaldwin@berkeley.edu FU National Tropical Botanical Garden, Kaleheo, Hawaii; Walcott Botanical Publication Fund, Department of Botany, Smithsonian Institution FX We thank Sue Bainbridge and Rick Hanna for technical assistance; Gerry Carr, G. Diada, Joe DiTomaso, Dianne Fristrom, Matt Goff, John Obata, Ya Yang, George Yatskievych and Saint Mary's College for providing plant images, and Gerry Carr for providing the image files by Obata and Diada; Danica Harbaugh for providing the map in Fig. 1; Joachim Kadereit and Gudren Kadereit for German-to-English translations of Engler (1879-1882) and Hillebrand (1888b); John L. Strother and two anonymous reviewers for helpful comments on the manuscript; Alice Tangerini for preparing the plates; and the Hunt Institute for Botanical Documentation and the Smithsonian Institution Libraries for permission to reproduce images of people in Fig. 2. Special thanks to the many researchers who generously allowed us to cite and summarize their unpublished results on relationships of Hawaiian plants. This work was supported by the National Tropical Botanical Garden, Kaleheo, Hawaii (Senior McBryde Research Fellowship to B.G.B. and McBryde Chair to W.L.W.). Funding for images was obtained from the Walcott Botanical Publication Fund, Department of Botany, Smithsonian Institution. NR 200 TC 51 Z9 52 U1 2 U2 50 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 JUN PY 2010 VL 105 IS 6 BP 849 EP 879 DI 10.1093/aob/mcq052 PG 31 WC Plant Sciences SC Plant Sciences GA 603RJ UT WOS:000278225400002 PM 20382966 ER PT J AU Sammarco, PW Porter, SA Cairns, SD AF Sammarco, Paul W. Porter, Scott A. Cairns, Stephen D. TI A new coral species introduced into the Atlantic Ocean - Tubastraea micranthus (Ehrenberg 1834) (Cnidaria, Anthozoa, Scleractinia): An invasive threat? SO AQUATIC INVASIONS LA English DT Article DE coral; Tubastraea coccinea; Tubastraea micranthus; introduction; invasive species; Atlantic Ocean; Indo-Pacific AB Over the past 60-70 years, the invasive Indo-Pacific coral Tubastraea coccinea (Lesson 1830; Cnidaria, Scleractinia) has colonized the western tropical Atlantic Ocean - the Americas, the Antilles, northern Gulf of Mexico (GOM), and many of its 3,600 oil/gas platforms. It is now the single, most abundant coral on artificial substrata in the GOM, with hundreds of thousands of colonies on a single platform. Here, we report for the first time the observation of a closely related congener in the western Atlantic - the Indo-Pacific azooxanthellate Tubastraea micranthus (Ehrenberg 1834) - and suggest that it may pose a threat similar to T. coccinea. A total of 83 platforms, including deep-water, toppled, Rigs-to-Reefs structures, were surveyed in the northern Gulf of Mexico between 2000 and 2009, from Matagorda Island, Texas to Mobile, Alabama, USA, between the depths of 7 and 37 m, by SCUBA divers. Five platforms were surveyed by Remotely Operated Vehicle (ROV) to depths of up to 117 m. T. micranthus was found on only one platform - Grand Isle 93 (GI-93), off Port Fourchon, Louisiana, near the Mississippi River mouth, at the cross-roads of two major safety fairways/shipping lanes transited by large international commercial ships. The introduction appears to be recent, probably derived from the ballast water or hull of a vessel from the Indo-Pacific. If the growth and reproductive rates of T. micranthus, both sexual and asexual, are similar to those of T. coccinea, this species could dominate this region like its congener. It is not known whether this species is an opportunist/pioneer species, like T. coccinea, a trait protecting benthic communities from its dominance. The question of rapid-response eradication is raised. C1 [Sammarco, Paul W.] Louisiana Univ Marine Consortium LUMCON, Chauvin, LA 70344 USA. [Porter, Scott A.] EcoLog Environm Consulting, Houma, LA 70361 USA. [Cairns, Stephen D.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Sammarco, PW (reprint author), Louisiana Univ Marine Consortium LUMCON, 8124 Hwy 56, Chauvin, LA 70344 USA. EM psammarco@lumcon.edu; Ecologic2020@aol.com; cairnss@si.edu FU Louisiana State University Coastal Marine Institute; US Dept. Interior Minerals Management Service; U.S. Department of the Interior - Minerals Management Service [32806/TO, 36188]; Louisiana State University MMS-Coastal Marine Institute; Louisiana Universities Marine Consortium (LUMCON) FX Many thanks to all of the divers who assisted in visual surveys: A. D. Atchison, D. Ball, A. Barker, M. Boatwright, G. Boland, G. Bunch, H. Butler, C. Chauffe, S. Childs, J. Collins, K. Collins, J. Conklin, J. Culbertson, L. Dauterive, R. DeFelice, D. Delger, T. Dempre, D. Dowdy, T. Empey, C. Gentry, R. Harris, C. Horrell, S. Kolian, H. Leedy, A. Lirette, L. Logan, D. Marcel, A. Miller, K. de Mutsert, D. Perrenod, G. Rainey, A. Schultze, A. Sebastian, J. Sinclair, P. Sjordal, G. Speyrer, J. Van der Ham, K. Wheelock, and D. Woodall. Special thanks to my son J.I. Sammarco for topside assistance. J. Blitch, A. Campbell, and J. Vice of ARACAR provided ROV operations and services using the SeaBotix LBV-300, with assistance from C. Chauvin, J. Dunn, K. Fiand, and M. Wike. M. Wike of LUMCON provided ROV ops assistance using the Phantom-2. H. Boudreaux, W. Hebert, C. Luke, and S. Parrott assisted with accounting; and C. Salmonsen with on-site assistance. We thank the crew of the M/V Fling (Gulf Diving, Inc; *captains) - R. Adkins, R. Bailey, N. Baltz, K. Beardon, K. Bush*, J. Byron, P. Combs*, J. Denton, L. DeWeese, P. Dagenais*, J. Dibble, B. Ellen*, D. Fanning, A. Felth, K. Foster, C. Gentry, G. Harding*, J. Heiser, S. Heuer, S. Hodges, Jason, B. Joy*, S. Kerr, T. Kilpatrick, K. Kimmey*, J. Koobles-Matel, C. Kozio, M. McReynolds, G. Phillips, J. Prentice, S. Richman, B. Shurtleff*, J. Smale, K. B. Strychar, A. Thronson, R. Travis*, R. Widaman*; and all of the oil and gas companies and their staff who provided us access to their offshore platforms: Anadarko Petroleum - J. Davidson, S. Hathcock, S. Jensen; Apache Oil - J. Bordelon, G. Thibodaux; Chevron-Texaco Exploration and Production - D. Lucas, K. Mire, S. Ulm; Coastal Oil and Gas, Devon Oil - B. Gary, R. Hebert, V. Mile, B. Moody; Dominion Exploration and Production - B. Ventura, K. Schlogel, M. Sledge; El Paso Energy - C. Thornton, S. Lesiker; Forcenergy/Forest Oil - W. Fontenot, W. Myers, G. Ruiz; Kerr-McGee Oil and Gas - C. Bradford; Merit Energy - T. Lambert, P. Maiberger; Newfield Exploration - A. Comeaux, E. Haas, M. Prosper, J. Zernell; Noble Energy S. Shuman; Offshore Energy; UNOCAL - D. Crusan, M. Hebert; Samedan Oil - R. Bemis, S. Berryhill, S. Mulbert, T. Spintzenberger, P. Tullos; and W&T Offshore - S. Schroeder. We also thank L. Rouse of the Louisiana State University Coastal Marine Institute and the US Dept. Interior Minerals Management Service for their support and for funding this study. This project was funded by the U.S. Department of the Interior - Minerals Management Service (Cooperative Agreement #32806/TO#36188 to Sammarco), the Louisiana State University MMS-Coastal Marine Institute, and the Louisiana Universities Marine Consortium (LUMCON). NR 67 TC 20 Z9 23 U1 2 U2 27 PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC PI HELSINKI PA PL 3, HELSINKI, 00981, FINLAND SN 1798-6540 J9 AQUAT INVASIONS JI Aquat. Invasions PD JUN PY 2010 VL 5 IS 2 BP 131 EP 140 DI 10.3391/ai.2010.5.2.02 PG 10 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA V24CZ UT WOS:000208389800002 ER PT J AU Torchin, ME AF Torchin, Mark E. TI Native fish grows faster in the presence of a potential introduced competitor SO AQUATIC INVASIONS LA English DT Article DE biotic resistance; competition; predation; Poecilia latipinna; Fundulus parvipinnis AB Biotic resistance, through competition from native species, can limit the success of invasive species. Similarly, invasive species can impact natives when they reduce shared resources. Alternatively, some invaders may benefit natives if they either directly or indirectly increase resource acquisition by natives. I predicted that the native California killifish, Fundulus parvipinnis would reduce the fitness of the morphologically similar introduced sailfin molly, Poecilia latipinna in a California estuary. A field experiment found no effect of competition; increasing the density of the native killifish did not affect sailfin molly growth. However, there was an unanticipated positive association of female sailfin molly density on growth of native killifish. Unlike any other native fish in the estuary, the introduced molly is a live bearer and I hypothesize that the presence of female mollies may have generated a novel food source (newborn fish) for the native competitor. This potential food source could have overcompensated for any potential competition for other resources. The positive effect was not mutual, i.e., the presence of killifish did not increase the growth of adult mollies (killifish are oviparous and lay eggs on the substrate). While killifish may not limit mollies through competitive effects, they could provide partial resistance to invasion by preying on juvenile mollies. Additional experiments designed specifically to test whether juvenile mollies increase killifish growth would confirm the mechanism and potentially reveal the importance of this in nature. Considering the role of all life stages of an invader is a key step when evaluating interactions with natives and determining the success and impacts of introduced species. C1 Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Torchin, ME (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM torchinm@si.edu FU UC-Mexus; STRI FX I thank K. Lafferty for advice and discussion in designing the study as well as comments on the manuscript. A. Kuris and A. Brooks provided useful advice. P. A. Amundsen, J. Bills, R. Hechinger, N. Kalodimos, R. King, V. McKenzie, V. Minnich and R. Torchin graciously provided assistance in the field and laboratory. I thank three anonymous reviewers for improving the manuscript. I acknowledge UC-Mexus and STRI for financial support. NR 20 TC 0 Z9 0 U1 1 U2 14 PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC PI HELSINKI PA PL 3, HELSINKI, 00981, FINLAND SN 1798-6540 J9 AQUAT INVASIONS JI Aquat. Invasions PD JUN PY 2010 VL 5 IS 2 BP 163 EP 167 DI 10.3391/ai.2010.5.2.05 PG 5 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA V24CZ UT WOS:000208389800005 ER PT J AU Collin, R Ramos-Espla, AA Izquierdo, A AF Collin, Rachel Ramos-Espla, Alfonso A. Izquierdo, Andres TI Identification of the South Atlantic spiny slipper limpet Bostrycapulus odites Collin, 2005 (Caenogastropoda: Calyptraeidae) on the Spanish Mediterranean coast SO AQUATIC INVASIONS LA English DT Article DE Western Mediterranean; Crepidula; barcode; COI; Bostrycapulus aculeatus; exotic species AB Calyptraeid gastropods are common fouling organisms in some areas, and have been introduced frequently into bays and ports in the northern hemisphere. In some cases, introduced calyptraeids have spread extensively, while several other calyptraeid introductions have persisted but failed to expand geographically. Calyptraeid species are often difficult to identify to species making it difficult to identify the origin of many introductions. Here we use DNA sequence data to confirm that a Mediterranean population of the spiny slipper snail Bostrycapulus, previously referred to as B. aculeatus and B. calyptraeformis, is in fact B. odites from the South Atlantic, and that this population probably originated in South America. C1 [Collin, Rachel] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Ramos-Espla, Alfonso A.; Izquierdo, Andres] Univ Alicante Ayuntamiento Santa Pola, Ctr Invest Marina CIMAR, Alicante, Spain. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@si.edu; alfonso.ramos@ua.es; andres.izquierdo@ua.es OI Collin, Rachel/0000-0001-5103-4460 NR 19 TC 5 Z9 5 U1 0 U2 1 PU REGIONAL EURO-ASIAN BIOLOGICAL INVASIONS CENTRE-REABIC PI HELSINKI PA PL 3, HELSINKI, 00981, FINLAND SN 1798-6540 J9 AQUAT INVASIONS JI Aquat. Invasions PD JUN PY 2010 VL 5 IS 2 BP 197 EP 200 DI 10.3391/ai.2010.5.2.11 PG 4 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA V24CZ UT WOS:000208389800011 ER PT J AU Fitzhugh, WW AF Fitzhugh, William W. TI ELMER HARP JR. (1913-2009) Obituary SO ARCTIC LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Arctic Studies Ctr, Washington, DC 20013 USA. RP Fitzhugh, WW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Arctic Studies Ctr, POB 37012, Washington, DC 20013 USA. EM Fitzhugh@si.edu NR 1 TC 1 Z9 1 U1 0 U2 1 PU ARCTIC INST N AMER PI CALGARY PA UNIV OF CALGARY 2500 UNIVERSITY DRIVE NW 11TH FLOOR LIBRARY TOWER, CALGARY, ALBERTA T2N 1N4, CANADA SN 0004-0843 J9 ARCTIC JI Arctic PD JUN PY 2010 VL 63 IS 2 BP 252 EP 254 PG 3 WC Environmental Sciences; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 618TY UT WOS:000279379800012 ER PT J AU Martin, S George, MR Wilner, DJ Espada, D AF Martin, Sergio George, Matthew R. Wilner, David J. Espada, Daniel TI IMAGING CARBON MONOXIDE EMISSION IN THE STARBURST GALAXY NGC 6000 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: fundamental parameters; galaxies: ISM; galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: starburst; radio lines: galaxies ID (CO)-C-13 J=1-0 DEPRESSION; BARRED SPIRAL GALAXIES; CIRCUMNUCLEAR REGIONS; INFRARED GALAXIES; SECULAR EVOLUTION; NEARBY GALAXIES; GALACTIC NUCLEI; MOLECULAR GAS; CO EMISSION; KINEMATICS AB We present measurements of carbon monoxide emission in the central region of the nearby starburst NGC 6000 taken with the Submillimeter Array. The J = 2-1 transition of (12)CO, (13)CO, and C(18)O were imaged at a resolution of similar to 3 '' x 2 '' (450 x 300 pc). We accurately determine the dynamical center of NGC 6000 at alpha(J2000.0) = 15(h)49(m)49(8).5 and delta(J2000.0) = -29 degrees 23'13 '' which agrees with the peak of molecular emission position. The observed CO dynamics could be explained in the context of the presence of a bar potential affecting the molecular material, likely responsible for the strong nuclear concentration where more than 85% of the gas is located. We detect a kinematically detached component of dense molecular gas at relatively high velocity which might be fueling the star formation. A total nuclear dynamical mass of 7 x 10(9) M(circle dot) is derived and a total mass of gas of 4.6 x 10(8) M(circle dot), yielding a M(gas)/M(dyn) similar to 6%, similar to other previously studied barred galaxies with central starbursts. We determined the mass of molecular gas with the optically thin isotopologue C(18)O and we estimate a CO-to-H(2) conversion factor X(CO) = 0.4 x 10(20) cm(-2)(K km s(-1))(-1) in agreement with that determined in other starburst galaxies. C1 [Martin, Sergio] European So Observ, Santiago 19, Chile. [Martin, Sergio; George, Matthew R.; Wilner, David J.; Espada, Daniel] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [George, Matthew R.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Espada, Daniel] CSIC, Inst Astrofis Andalucia, Granada, Spain. RP Martin, S (reprint author), European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile. EM smartin@eso.org FU Smithsonian Astrophysical Observatory; Academia Sinica Institute of Astronomy and Astrophysics; Smithsonian Institution; Academia Sinica FX This paper uses data taken with the SMA on Director's discretionary time as part of the Astronomy 191 course for Harvard University undergraduates. We want to thank Prof. Carl Heiles for his valuable comments on the manuscript. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. NR 49 TC 6 Z9 6 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 JUN PY 2010 VL 139 IS 6 BP 2241 EP 2248 DI 10.1088/0004-6256/139/6/2241 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595WG UT WOS:000277643700011 ER PT J AU Kraemer, KE Hora, JL Egan, MP Adams, J Allen, LE Bontemps, S Carey, SJ Fazio, GG Gutermuth, R Keto, E Koenig, XP Megeath, ST Mizuno, DR Motte, F Price, SD Schneider, N Simon, R Smith, HA AF Kraemer, Kathleen E. Hora, Joseph L. Egan, Michael P. Adams, Joseph Allen, Lori E. Bontemps, Sylvain Carey, Sean J. Fazio, Giovanni G. Gutermuth, Robert Keto, Eric Koenig, Xavier P. Megeath, S. Thomas Mizuno, Donald R. Motte, Frederique Price, Stephan D. Schneider, Nicola Simon, Robert Smith, Howard A. TI CIRCUMSTELLAR STRUCTURE AROUND EVOLVED STARS IN THE CYGNUS-X STAR FORMATION REGION SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: AGB and post-AGB; stars: individual (BD+43 3710, HBHA 4202-22, G79.29-0.46) ID SPITZER-SPACE-TELESCOPE; SHORT-WAVELENGTH SPECTROMETER; MULTIBAND IMAGING PHOTOMETER; INFRARED SPECTROGRAPH IRS; RING NEBULA G79.29+0.46; INNER GALACTIC PLANE; WOLF-RAYET STAR; MU-M; EMISSION FEATURE; MICRON SPECTRA AB We present observations of newly discovered 24 mu m circumstellar structures detected with MIPS around three evolved stars in the Cygnus-X star-forming region. One of the objects, BD+43 3710, has a bipolar nebula, possibly due to an outflow or a torus of material. A second, HBHA 4202-22, a Wolf-Rayet candidate, shows a circular shell of 24 mu m emission suggestive of either a limb-brightened shell or disk seen face-on. No diffuse emission was detected around either of these two objects in the Spitzer 3.6-8 mu m IRAC bands. The third object is the luminous blue variable candidate G79.29+0.46. We resolved the previously known inner ring in all four IRAC bands. The 24 mu m emission from the inner ring extends similar to 1.'2 beyond the shorter wavelength emission, well beyond what can be attributed to the difference in resolutions between MIPS and IRAC. Additionally, we have discovered an outer ring of 24 mu m emission, possibly due to an earlier episode of mass loss. For the two shell stars, we present the results of radiative transfer models, constraining the stellar and dust shell parameters. The shells are composed of amorphous carbon grains, plus polycyclic aromatic hydrocarbons in the case of G79.29+0.46. Both G79.29+0.46 and HBHA 4202-22 lie behind the main Cygnus-X cloud. Although G79.29+0.46 simply may be on the far side of the cloud, HBHA 4202-22 is unrelated to the Cygnus-X star formation region. C1 [Kraemer, Kathleen E.; Price, Stephan D.] USAF, Res Lab, Space Vehicles Directorate, Hanscom AFB, MA 01731 USA. [Hora, Joseph L.; Fazio, Giovanni G.; Keto, Eric; Koenig, Xavier P.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Egan, Michael P.] Natl Geo Spatial Intelligence Agcy, Reston, VA 20191 USA. [Adams, Joseph] Cornell Univ, Ithaca, NY 14853 USA. [Allen, Lori E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Bontemps, Sylvain] Observ Bordeaux, Floirac, France. [Carey, Sean J.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Gutermuth, Robert] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA. [Gutermuth, Robert] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Mizuno, Donald R.] Boston Coll, Inst Sci Res, Chestnut Hill, MA 02467 USA. [Motte, Frederique; Schneider, Nicola] Commissariat Energie Atom, Paris, France. [Simon, Robert] Univ Cologne, Cologne, Germany. RP Kraemer, KE (reprint author), USAF, Res Lab, Space Vehicles Directorate, 29 Randolph Rd, Hanscom AFB, MA 01731 USA. EM afrl.rvb.pa@hanscom.af.mil; jhora@cfa.harvard.edu; michael.p.egan@nga.mil; jdadams@astro.cornell.edu; lallen@noao.edu; Sylvain.Bontemps@obs.u-bordeaux1.fr; carey@ipac.caltech.edu; gfazio@cfa.harvard.edu; rgutermu@smith.edu; eketo@cfa.harvard.edu; xkoenig@cfa.harvard.edu; meageath@astro1.panet.utoledo.edu; afrl.rvb.pa@hanscom.af.mil; motte@discovery.saclay.cea.fr; nschneid@cea.fr; simonr@ph1.uni-koeln.de; hsmith@cfa.harvard.edu OI Koenig, Xavier/0000-0002-9478-4170; Hora, Joseph/0000-0002-5599-4650; Kraemer, Kathleen/0000-0002-2626-7155 NR 52 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUN PY 2010 VL 139 IS 6 BP 2319 EP 2329 DI 10.1088/0004-6256/139/6/2319 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595WG UT WOS:000277643700019 ER PT J AU Lacy, CHS Torres, G Claret, A Charbonneau, D O'Donovan, FT Mandushev, G AF Lacy, Claud H. Sandberg Torres, Guillermo Claret, Antonio Charbonneau, David O'Donovan, Francis T. Mandushev, Georgi TI ABSOLUTE PROPERTIES OF THE ECLIPSING TRIPLE STAR CO ANDROMEDAE: CONSTRAINTS ON CONVECTIVE CORE OVERSHOOTING SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; stars: fundamental parameters; stars: individual (CO And); stars: rotation; stars: solar-type ID LIMB-DARKENING COEFFICIENTS; SPECTROSCOPIC BINARIES; LIGHT CURVES; MODEL ATMOSPHERES; TIDAL-EVOLUTION; Y-2 ISOCHRONES; STELLAR MODELS; MAIN-SEQUENCE; TRANSFORMATIONS; TEMPERATURES AB Accurate absolute properties have been determined for the eclipsing triple star CO And (F8+F8) based on extensive differential photometry obtained by three robotic observatories and CfA spectroscopy. The eclipsing binary star orbit is circular with a period of 3.655 days. The triple nature of this system is revealed by more than a century of timings of minimum light, and by the presence of third light in the photometric orbits. The masses of the eclipsing pair are 1.289 +/- 0.007 and 1.264 +/- 0.007 solar masses, and the corresponding radii are 1.727 +/- 0.021 and 1.694 +/- 0.017 solar radii. These stars are synchronously rotating and are near the end of their main-sequence phase, at an age of about 3.6 Gyr. The much fainter widely separated third body appears to have a mass of about 0.8 solar masses. The distance to the system is 377 +/- 25 pc. C1 [Lacy, Claud H. Sandberg] Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. [Torres, Guillermo; Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Claret, Antonio] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [O'Donovan, Francis T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mandushev, Georgi] Lowell Observ, Flagstaff, AZ 86001 USA. RP Lacy, CHS (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. EM clacy@uark.edu; gtorres@cfa.harvard.edu; claret@iaa.es; dcharbonneau@cfa.harvard.edu; ftod@caltech.edu; gmand@lowell.edu RI O'Donovan, Francis/I-2423-2014; OI O'Donovan, Francis/0000-0002-4858-6106; Charbonneau, David/0000-0002-9003-484X NR 79 TC 11 Z9 11 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 JUN PY 2010 VL 139 IS 6 BP 2347 EP 2359 DI 10.1088/0004-6256/139/6/2347 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595WG UT WOS:000277643700021 ER PT J AU Eisenhardt, PRM Griffith, RL Stern, D Wright, EL Ashby, MLN Brodwin, M Brown, MJI Bussmann, RS Dey, A Ghez, AM Glikman, E Gonzalez, AH Kirkpatrick, JD Konopacky, Q Mainzer, A Vollbach, D Wright, SA AF Eisenhardt, Peter R. M. Griffith, Roger L. Stern, Daniel Wright, Edward L. Ashby, Matthew L. N. Brodwin, Mark Brown, Michael J. I. Bussmann, R. S. Dey, Arjun Ghez, A. M. Glikman, Eilat Gonzalez, Anthony H. Kirkpatrick, J. Davy Konopacky, Quinn Mainzer, Amy Vollbach, David Wright, Shelley A. TI ULTRACOOL FIELD BROWN DWARF CANDIDATES SELECTED AT 4.5 mu m SO ASTRONOMICAL JOURNAL LA English DT Article DE brown dwarfs; infrared: galaxies; infrared: stars; stars: individual (SDWFS J142831.46+354923.1; SDWFS J143524.44+335334.6; SDWFS J143356.62+351849.2); stars: low-mass ID ARRAY CAMERA IRAC; ADAPTIVE OPTICS SYSTEM; DUST-OBSCURED GALAXIES; LONG-PERIOD VARIABLES; DIGITAL SKY SURVEY; T-DWARFS; MIDINFRARED SELECTION; LOW-MASS; SPITZER; STARS AB We have identified a sample of cool field brown dwarf candidates using IRAC data from the Spitzer Deep, Wide-Field Survey (SDWFS). The candidates were selected from 400,000 SDWFS sources with [4.5] <= 18.5 mag and were required to have [3.6] - [4.5] >= 1.5 and [4.5] - [8.0] <= 2.0 on the Vega system. The first color requirement selects objects redder than all but a handful of presently known brown dwarfs with spectral classes later than T7, while the second eliminates 14 probable reddened active galactic nuclei (AGNs). Optical detection of four of the remaining 18 sources implies they are likely also AGNs, leaving 14 brown dwarf candidates. For two of the brightest candidates (SDWFS J143524.44+335334.6 and SDWFS J143222.82+323746.5), the spectral energy distributions including near-infrared detections suggest a spectral class of similar to T8. The proper motion is <0 ''.25 yr(-1), consistent with expectations for a luminosity-inferred distance of >70 pc. The reddest brown dwarf candidate (SDWFS J143356.62+351849.2) has [3.6] - [4.5] = 2.24 and H - [4.5] > 5.7, redder than any published brown dwarf in these colors, and may be the first example of the elusive Y-dwarf spectral class. Models from Burrows et al. predict that larger numbers of cool brown dwarfs should be found for a Chabrier mass function. Suppressing the model [4.5] flux by a factor of 2, as indicated by previous work, brings the Burrows models and observations into reasonable agreement. The recently launched Wide-field Infrared Survey Explorer will probe a volume similar to 40x larger and should find hundreds of brown dwarfs cooler than T7. C1 [Eisenhardt, Peter R. M.; Griffith, Roger L.; Stern, Daniel; Mainzer, Amy] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Wright, Edward L.; Ghez, A. M.; Konopacky, Quinn] Univ Calif Los Angeles, Los Angeles, CA 90095 USA. [Ashby, Matthew L. N.; Brodwin, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Bussmann, R. S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Dey, Arjun] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Glikman, Eilat] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Gonzalez, Anthony H.; Vollbach, David] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Kirkpatrick, J. Davy] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Wright, Shelley A.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94709 USA. RP Eisenhardt, PRM (reprint author), CALTECH, Jet Prop Lab, MS 169-327,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Peter.Eisenhardt@jpl.nasa.gov RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Wright, Shelley/0000-0003-1034-8054 FU National Optical Astronomy Observatory (NOAO); W. M. Keck Foundation; NASA; National Science Foundation (NSF) [0708490]; NSF Science & Technology Center; UCSC [AST-9876783]; Levine-Leichtman Family Foundation FX The authors thank Emanuele Daddi, Mark Dickinson, Jason Melbourne, and Tom Soifer for assistance obtaining observations; Nick Seymour for assistance with SDWFS and WIRC reductions; and Vandana Desai for the Mrk 231 spectrum and information about DOG SED's. Tom Soifer, Marcia Rieke, Dan Weedman, and Jim Houck are thanked for allowing access to the GTO MIPS survey of the NDWFS, and we acknowledge Buell Jannuzi's central role in the NDWFS and related surveys of the field. Discussions with Roc Cutri helped us understand the mid-IR characteristics of AGB stars, and Szymon Kozlowski clarified questions about SDWFS variability measurements. We thank the anonymous referee for a detailed and careful review which improved the accuracy of the presentation. 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 contract with NASA. This work made use of images and data products provided by the NOAO Deep Wide-Field Survey (NDWFS), which is supported by the National Optical Astronomy Observatory (NOAO), and follow-up NOAO surveys. NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. 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, which also provided support for M.B. Some data were obtained at the Hale Telescope, Palomar Observatory as part of a continuing collaboration between Caltech, NASA/JPL, and Cornell University. Support for this work was provided by NASA through an award issued by JPL/Caltech. A.H.G. acknowledges support for this work by the National Science Foundation (NSF) under grant 0708490. Support for A.M.G. and Q.K.'s contribution to this work was provided by the NSF Science & Technology Center for AO, managed by UCSC (AST-9876783), and the Levine-Leichtman Family Foundation. NR 58 TC 19 Z9 19 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 JUN PY 2010 VL 139 IS 6 BP 2455 EP 2464 DI 10.1088/0004-6256/139/6/2455 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595WG UT WOS:000277643700029 ER PT J AU Gramajo, LV Whitney, BA Gomez, M Robitaille, TP AF Gramajo, Luciana V. Whitney, Barbara A. Gomez, Mercedes Robitaille, Thomas P. TI COMBINED ANALYSIS OF IMAGES AND SPECTRAL ENERGY DISTRIBUTIONS OF TAURUS PROTOSTARS SO ASTRONOMICAL JOURNAL LA English DT Article DE circumstellar matter; infrared: stars; stars: formation; stars: imaging ID YOUNG STELLAR OBJECTS; AURIGA MOLECULAR CLOUD; CLASS-I PROTOSTARS; LOW-MASS STAR; SUBMILLIMETER CONTINUUM OBSERVATIONS; MAIN-SEQUENCE; CIRCUMPROTOSTELLAR ENVIRONMENTS; MULTIWAVELENGTH OBSERVATIONS; CIRCUMSTELLAR ENVIRONMENT; PROTOSTELLAR ENVELOPES AB We present an analysis of spectral energy distributions (SEDs), near- and mid-infrared images, and Spitzer spectra of eight embedded Class I/II objects in the Taurus-Auriga molecular cloud. The initial model for each source was chosen using the grid of young stellar objects (YSOs) and SED fitting tool of Robitaille et al. Then the models were refined using the radiative transfer code of Whitney et al. to fit both the spectra and the infrared images of these objects. In general, our models agree with previous published analyses. However, our combined models should provide more reliable determinations of the physical and geometrical parameters since they are derived from SEDs, including the Spitzer spectra, covering the complete spectral range; and high-resolution near-infrared and Spitzer IRAC images. The combination of SED and image modeling better constrains the different components (central source, disk, envelope) of the YSOs. Our derived luminosities are higher, on average, than previous estimates because we account for the viewing angles (usually nearly edge-on) of most of the sources. Our analysis suggests that the standard rotating collapsing protostar model with disks and bipolar cavities works well for the analyzed sample of objects in the Taurus molecular cloud. C1 [Gramajo, Luciana V.; Gomez, Mercedes] Univ Nacl Cordoba, Astron Observ, RA-5000 Cordoba, Argentina. [Whitney, Barbara A.] Space Sci Inst, Boulder, CO 80301 USA. [Robitaille, Thomas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gramajo, LV (reprint author), Univ Nacl Cordoba, Astron Observ, Laprida 854, RA-5000 Cordoba, Argentina. EM luciana@oac.uncor.edu; bwhitney@spacescience.org; mercedes@oac.uncor.edu; trobitaille@cfa.harvard.edu OI Robitaille, Thomas/0000-0002-8642-1329 NR 78 TC 12 Z9 12 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 JUN PY 2010 VL 139 IS 6 BP 2504 EP 2524 DI 10.1088/0004-6256/139/6/2504 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595WG UT WOS:000277643700032 ER PT J AU Nantais, JB Huchra, JP AF Nantais, Julie B. Huchra, John P. TI SPECTROSCOPY OF M81 GLOBULAR CLUSTERS SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (M81); galaxies: spiral; galaxies: star clusters: general ID WIDE-FIELD; WASHINGTON PHOTOMETRY; NGC 4472; SYSTEM; GALAXY; KINEMATICS; METALLICITY; M31; DYNAMICS AB We obtained spectra of 74 globular clusters (GCs) in M81. These GCs had been identified as candidates in a Hubble Space Telescope (HST) Advanced Camera for Surveys I-band survey. Sixty-eight of these 74 clusters lie within 7 ' of the M81 nucleus. Sixty-two of these clusters are newly spectroscopically confirmed, more than doubling the number of confirmed M81 GCs from 46 to 108. We determined metallicities for our 74 observed clusters using an empirical calibration based on Milky Way GCs. We combined our results with 34 M81 GC velocities and 33 metallicities from the literature and analyzed the kinematics and metallicity of the M81 GC system. The mean of the total sample of 107 metallicities is -1.06 +/- 0.07, higher than either M31 or the Milky Way. We suspect that this high mean metallicity is due to an overrepresentation of metal-rich (MR) clusters in our sample created by the spatial limits of the HST I-band survey. The metallicity distribution shows marginal evidence for bimodality, with the mean metallicities of MR and metal-poor (MP) GCs similar to those of M31 and the Milky Way. The GC system as a whole, and the MP GCs alone, show evidence of a radial metallicity gradient. The M81 GC system as a whole shows strong evidence of rotation, with V(r) (deprojected) = 108 +/- 22 km s(-1) overall. This result is likely biased toward high rotational velocity due to overrepresentation of MR inner clusters. The rotation patterns among GC subpopulations are roughly similar to those of the Milky Way: clusters at small projected radii and MR clusters rotate strongly, while clusters at large projected radii and MP clusters show weaker evidence of rotation. C1 [Nantais, Julie B.; Huchra, John P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Nantais, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [GO-10250, NNG06GD33G]; Space Telescope Science Institute; National Science Foundation [AST 05077229]; Harvard College Observatory FX This research was supported by the NASA grant GO-10250 from the Space Telescope Science Institute, the National Science Foundation grant AST 05077229, and the NASA grant NNG06GD33G from the GALEX Guest Observers Program. We would also like to thank the staff of the Harvard College Observatory for their support, and Dr. Jay Strader for helpful feedback. NR 42 TC 12 Z9 12 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 JUN PY 2010 VL 139 IS 6 BP 2620 EP 2638 DI 10.1088/0004-6256/139/6/2620 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595WG UT WOS:000277643700041 ER PT J AU Frebel, A AF Frebel, A. TI Stellar archaeology: Exploring the Universe with metal-poor stars Ludwig Biermann Award Lecture 2009 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE early Universe; Galaxy: halo; Galaxy: stellar content; stars: abundances; stars: Population II ID NEUTRON-CAPTURE ELEMENTS; DWARF SPHEROIDAL GALAXY; HIGH-DISPERSION-SPECTROGRAPH; COMPREHENSIVE ABUNDANCE ANALYSIS; NEAR-ULTRAVIOLET OBSERVATIONS; CARBON-RICH OBJECTS; GIANT BRANCH STARS; LESS-THAN -5.0; R-PROCESS; 1ST STARS AB The abundance patterns of the most metal-poor stars in the Galactic halo and small dwarf galaxies provide us with a wealth of information about the early Universe. In particular, these old survivors allow us to study the nature of the first stars and supernovae, the relevant nucleosynthesis processes responsible for the formation and evolution of the elements, early star- and galaxy formation processes, as well as the assembly process of the stellar halo from dwarf galaxies a long time ago. This review presents the current state of the field of "stellar archaeology" - the diverse use of metal-poor stars to explore the high-redshift Universe and its constituents. In particular, the conditions for early star formation are discussed, how these ultimately led to a chemical evolution, and what the role of the most iron-poor stars is for learning about Population III supernovae yields. Rapid neutron-capture signatures found in metal-poor stars can be used to obtain stellar ages, but also to constrain this complex nucleosynthesis process with observational measurements. Moreover, chemical abundances of extremely metal-poor stars in different types of dwarf galaxies can be used to infer details on the formation scenario of the halo and the role of dwarf galaxies as Galactic building blocks. I conclude with an outlook as to where this field may be heading within the next decade. A table of similar to 1000 metal-poor stars and their abundances as collected from the literature is provided in electronic format. (C) 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Frebel, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 20, Cambridge, MA 02138 USA. EM afrebel@cfa.harvard.edu FU Astronomische Gesellschaft; Clay Postdoctoral Fellowship FX I am very grateful to the Astronomische Gesellschaft and its selection committee for awarding me the 2009 Ludwig-Biermann Award. Lars Hernquist and Ian Roederer have given useful comments to the manuscript, and John Norris provided the spectrum of G66-30 shown in Fig. 1. I warmly thank my many wonderful collaborators who have always inspired me, and make working in this field a great pleasure: Wako Aoki, Martin Asplund, Tim Beers, Volker Bromm, Norbert Christlieb, Karl-Ludwig Kratz, Evan Kirby, John Norris, Ian Roederer, Josh Simon, Chris Sneden and many others. This work has been supported by a Clay Postdoctoral Fellowship administered by the Smithsonian Astrophysical Observatory. This research has made use of NASA's Astrophysics Data System. This research has made use of the SIM-BAD database, operated at CDS, Strasbourg, France. NR 151 TC 68 Z9 68 U1 2 U2 7 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD JUN PY 2010 VL 331 IS 5 BP 474 EP 488 DI 10.1002/asna.201011362 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 607ZD UT WOS:000278544900002 ER PT J AU Brunken, S Belloche, A Martin, S Verheyen, L Menten, KM AF Bruenken, S. Belloche, A. Martin, S. Verheyen, L. Menten, K. M. TI Interstellar HOCN in the Galactic center region SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; stars: formation; ISM: individual objects: Sagittarius B2; ISM: abundances; radio lines: ISM ID MILLIMETER-WAVE SPECTRUM; MOLECULAR LINE SURVEY; SAGITTARIUS B2; ISOCYANIC ACID; ORION-KL; CHEMISTRY; HNCO; CLOUDS; GAS; CORE AB Aims. Our aim is to confirm the interstellar detection of cyanic acid, HOCN, in the Galactic center clouds. It has previously been tentatively detected only in Sgr B2(OH). Methods. We used a complete line survey of the hot cores Sgr B2(N) and (M) in the 3 mm range, complemented by additional observations carried out with the IRAM 30 m telescope at selected frequencies in the 2 mm band and towards four additional positions in the Sgr B2 cloud complex in the 2 and 3 mm bands. The spectral survey was analysed in the local thermodynamical equilibrium approximation (LTE) by modeling the emission of all identified molecules simultaneously. This allowed us to distinguish weak features of HOCN from the rich line spectrum observed in Sgr B2(N) and (M). Lines of the more stable (by 1.1 eV) isomer isocyanic acid, HNCO, in these sources, as well as those of HOCN and HNCO towards the other positions, were analysed in the LTE approximation as well. Results. Four transitions of HOCN were detected in a quiescent molecular cloud in the Galactic center at a position offset in (RA, Dec) by (20 '', 100 '') from the hot core source Sgr B2(M), confirming its previous tentative interstellar detection. Up to four transitions were detected toward five other positions in the Sgr B2 complex, including the hot cores Sgr B2(M), (S), and (N). A fairly constant abundance ratio of similar to 0.3-0.8% for HOCN relative to HNCO was derived for the extended gas components, suggesting a common formation process of these isomers. C1 [Bruenken, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Belloche, A.; Verheyen, L.; Menten, K. M.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Martin, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martin, S.] European So Observ, Santiago 19, Chile. RP Brunken, S (reprint author), Univ Cologne, Inst Phys 1, Zulpicher Str 77, D-50937 Cologne, Germany. EM bruenken@ph1.uni-koeln.de RI Brunken, Sandra/B-1880-2010 OI Brunken, Sandra/0000-0001-7175-4828 FU CNRS/INSU (France); MPG (Germany); IGN (Spain) FX Based on observations with the IRAM 30-m telescope. IRAM is supported by CNRS/INSU (France), the MPG (Germany) and the IGN (Spain). NR 38 TC 20 Z9 20 U1 0 U2 7 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN-JUL PY 2010 VL 516 AR A109 DI 10.1051/0004-6361/200912456 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400124 ER PT J AU Brunthaler, A Marti-Vidal, I Menten, KM Reid, MJ Henkel, C Bower, GC Falcke, H Feng, H Kaaret, P Butler, NR Morgan, AN Weiss, A AF Brunthaler, A. Marti-Vidal, I. Menten, K. M. Reid, M. J. Henkel, C. Bower, G. C. Falcke, H. Feng, H. Kaaret, P. Butler, N. R. Morgan, A. N. Weiss, A. TI VLBI observations of SN2008iz I. Expansion velocity and limits on anisotropic expansion SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: supernovae: general; stars: supernovae: individual: SN2008iz; radio continuum: general; galaxies: individual: M 82 ID SYNCHROTRON SELF-ABSORPTION; SN 1993J VLBI; RADIO-EMISSION; STARBURST GALAXIES; SN-1993J VLBI; SUPERNOVA; M81; DECELERATION; DISCOVERY; SPECTRUM AB We present observations of the recently discovered supernova 2008iz in M 82 with the VLBI High Sensitivity Array at 22 GHz, the Very Large Array at frequencies of 1.4, 4.8, 8.4, 22 and 43 GHz, and the Chandra X-ray observatory. The supernova was clearly detected in two VLBI images separated by 11 months. The source shows a ring-like morphology and expands with a velocity of similar to 23 000 km s(-1). The most likely explosion date is in mid-February 2008. The measured expansion speed is a factor of similar to 2 higher than expected under the assumption that synchrotron self-absorption dominates the light curve at the peak, indicating that this absorption mechanism may not be important for the radio emission. We find no evidence for an asymmetric explosion. The VLA spectrum shows a broken power law, indicating that the source was still optically thick at 1.4 GHz in April 2009. Finally, we report upper limits on the X-ray emission from SN2008iz and a second radio transient recently discovered by MERLIN observations. C1 [Brunthaler, A.; Marti-Vidal, I.; Menten, K. M.; Henkel, C.; Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Reid, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bower, G. C.; Butler, N. R.; Morgan, A. N.] UC Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Bower, G. C.; Butler, N. R.; Morgan, A. N.] UC Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Falcke, H.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Falcke, H.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Feng, H.] Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China. [Feng, H.] Tsinghua Univ, Ctr Astrophys, Beijing 100084, Peoples R China. [Kaaret, P.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. RP Brunthaler, A (reprint author), Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn, Germany. EM brunthal@mpifr-bonn.mpg.de RI Falcke, Heino/H-5262-2012; Marti-Vidal, Ivan/A-8799-2017 OI Falcke, Heino/0000-0002-2526-6724; Marti-Vidal, Ivan/0000-0003-3708-9611 NR 46 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 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN-JUL PY 2010 VL 516 AR A27 DI 10.1051/0004-6361/201014133 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400042 ER PT J AU Decin, L De Beck, E Brunken, S Muller, HSP Menten, KM Kim, H Willacy, K de Koter, A Wyrowski, F AF Decin, L. De Beck, E. Bruenken, S. Mueller, H. S. P. Menten, K. M. Kim, H. Willacy, K. de Koter, A. Wyrowski, F. TI Circumstellar molecular composition of the oxygen-rich AGB star IK Tauri II. In-depth non-LTE chemical abundance analysis SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; molecular processes; radiative transfer; submillimeter: stars; stars: AGB and post-AGB; stars: mass-loss ID MASS-LOSS RATES; SILICON ISOTOPIC ABUNDANCES; ROTATIONAL LINE-PROFILES; GIANT BRANCH STARS; VY-CANIS MAJORIS; EVOLVED STARS; WATER-VAPOR; EXPLOSIVE NUCLEOSYNTHESIS; COLLISIONAL EXCITATION; RADIATIVE-TRANSFER AB Context. The interstellar medium is enriched primarily by matter ejected from evolved low and intermediate mass stars. The outflow from these stars creates a circumstellar envelope in which a rich gas-phase chemistry takes place. Complex shock-induced non-equilibrium chemistry takes place in the inner wind envelope, dust-gas reactions and ion-molecule reactions alter the abundances in the intermediate wind zone, and the penetration of cosmic rays and ultraviolet photons dissociates the molecules in the outer wind region. Aims. Little observational information exists on the circumstellar molecular abundance stratifications of many molecules. Furthermore, our knowledge of oxygen-rich envelopes is not as profound as for the carbon-rich counterparts. The aim of this paper is therefore to study the circumstellar chemical abundance pattern of 11 molecules and isotopologs ((12)CO, (13)CO, SiS, (28)SiO, (29)SiO, (30)SiO, HCN, CN, CS, SO, SO(2)) in the oxygen-rich evolved star IK Tau. Methods. We have performed an in-depth analysis of a large number of molecular emission lines excited in the circumstellar envelope around IK Tau. The analysis is done based on a non-local thermodynamic equilibrium (non-LTE) radiative transfer analysis, which calculates the temperature and velocity structure in a self-consistent way. The chemical abundance pattern is coupled to theoretical outer wind model predictions including photodestruction and cosmic ray ionization. Not only the integrated line intensities, but also the line shapes are used as diagnostic tool to study the envelope structure. Results. The deduced wind acceleration is much slower than predicted from classical theories. SiO and SiS are depleted in the envelope, possibly due to the adsorption onto dust grains. For HCN and CS a clear difference with respect to inner wind non-equilibrium predictions is found, either indicating uncertainties in the inner wind theoretical modeling or the possibility that HCN and CS (or the radical CN) participate in the dust formation. The low signal-to-noise profiles of SO and CN prohibit an accurate abundance determination; the modeling of high-excitation SO2 lines is cumbersome, possibly related to line misidentifications or problems with the collisional rates. The SiO isotopic ratios ((29)SiO/(28)SiO and (30)SiO/ (28)SiO) point toward an enhancement in (28)SiO compared to results of classical stellar evolution codes. Predictions for H(2)O emission lines in the spectral range of the Herschel/HIFI mission are performed. C1 [Decin, L.; De Beck, E.] Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, B-3001 Heverlee, Belgium. [Decin, L.; de Koter, A.] Univ Amsterdam, Sterrenkundig Inst Anton Pannekock, NL-1090 CE Amsterdam, Netherlands. [Bruenken, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bruenken, S.; Mueller, H. S. P.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Mueller, H. S. P.; Menten, K. M.; Kim, H.; Wyrowski, F.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Kim, H.] MPI Gravitat Phy, D-30167 Hannover, Germany. [Willacy, K.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [de Koter, A.] Univ Utrecht, Astron Inst, NL-3584 CC Utrecht, Netherlands. RP Decin, L (reprint author), Katholieke Univ Leuven, Inst Astron, Dept Phys & Astron, Celestijnenlaan 200D, B-3001 Heverlee, Belgium. EM Leen.Decin@ster.kuleuven.ac.be RI Brunken, Sandra/B-1880-2010; OI Brunken, Sandra/0000-0001-7175-4828; Mueller, Holger/0000-0002-0183-8927 FU Fund for Scientific Research - Flanders (FWO) [G.0470.07]; Bundesministerium for Bildung und Forschung (BMBF) FX We thank I. Cherchneff for useful discussion on the circumstellar non-TE chemistry, and F. Schoier for providing us with an updated HCN linelist in the LAMDA database. L.D. acknowledges financial support from the Fund for Scientific Research - Flanders (FWO). E.D.B. acknowledges support from the FWO under grant number G.0470.07. H.S.P.M. is very grateful to the Bundesministerium for Bildung und Forschung (BMBF) for financial support aimed at maintaining the Cologne Database for Molecular Spectroscopy, CDMS. This support has been administered by the Deutsches Zentrum fur Luft-und Raumfahrt (DLR). The computations for this research have been done on the VIC HPC Cluster of the KULeuven. We are grateful to the LUDIT HPC team for their support. NR 92 TC 44 Z9 44 U1 1 U2 3 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN-JUL PY 2010 VL 516 AR A69 DI 10.1051/0004-6361/201014136 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400084 ER PT J AU Hebrard, G Desert, JM Diaz, RF Boisse, I Bouchy, F des Etangs, AL Moutou, C Ehrenreich, D Arnold, L Bonfils, X Delfosse, X Desort, M Eggenberger, A Forveille, T Gregorio, J Lagrange, AM Lovis, C Pepe, F Perrier, C Pont, F Queloz, D Santerne, A Santos, NC Segransan, D Sing, DK Udry, S Vidal-Madjar, A AF Hebrard, G. Desert, J. -M. Diaz, R. F. Boisse, I. Bouchy, F. des Etangs, A. Lecavelier Moutou, C. Ehrenreich, D. Arnold, L. Bonfils, X. Delfosse, X. Desort, M. Eggenberger, A. Forveille, T. Gregorio, J. Lagrange, A. -M. Lovis, C. Pepe, F. Perrier, C. Pont, F. Queloz, D. Santerne, A. Santos, N. C. Segransan, D. Sing, D. K. Udry, S. Vidal-Madjar, A. TI Observation of the full 12-hour-long transit of the exoplanet HD 80606b Warm-Spitzer photometry and SOPHIE spectroscopy SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE techniques: radial velocities; techniques: photometric; stars: individual: HD 80606 ID SPIN-ORBIT ALIGNMENT; EXTRA-SOLAR PLANETS; ROSSITER-MCLAUGHLIN OBSERVATIONS; HUBBLE-SPACE-TELESCOPE; RETROGRADE ORBIT; GIANT PLANET; SYSTEM; SEARCH; STAR; 189733B AB We present new observations of a transit of the 111.4-day-period exoplanet HD 80606b. Due to this long orbital period and to the orientation of the eccentric orbit (e = 0.9), HD 80606b's transits last for about 12 hours. This makes the observation of a full transit practically impossible from a given ground-based observatory. With the Spitzer Space Telescope and its IRAC camera on the post-cryogenic mission, we performed a 19-h photometric observation of HD 80606 that covers the full 2010 January 13-14 transit as well as off-transit references immediately before and after the event. We complement these photometric data by new spectroscopic observations that we simultaneously performed with SOPHIE at the Haute-Provence Observatory. This provides radial velocity measurements of the first half of the transit that was previously uncovered with spectroscopy. This new dataset allows the parameters of this singular planetary system to be significantly refined. We obtained a planet-to-star radius ratio R-p/R-* = 0.1001 +/- 0.0006 that is more accurate but slightly lower than the one measured from previous ground observations in the optical. We found no astrophysical interpretations able to explain this difference between optical and infrared radii; we rather favor underestimated systematic uncertainties, maybe in the ground-based composite light curve. We detected a feature in the Spitzer light curve that could be due to a stellar spot. We also found a transit timing about 20 minutes earlier than the ephemeris prediction; this could be caused by actual transit-timing variations due to an additional body in the system, or again by underestimated systematic uncertainties. The actual angle between the spin-axis of HD 80606 and the normal to the planetary orbital plane is found to be near 40 degrees thanks to the fit of the Rossiter-McLaughlin anomaly, with a sky-projected value lambda = 42 degrees +/- 8 degrees. This allows scenarios with aligned spin-orbit to be definitively rejected. Over the twenty planetary systems with measured spin-orbit angles, a few are misaligned; this is probably the signature of two different evolution scenarios for misaligned and aligned systems, depending whether or not they experienced gravitational interaction with a third body. As in the case of HD 80606, most of the planetary systems including a massive planet are tilted; this could be the signature of a separate evolution scenario for massive planets compared with Jupiter-mass planets. C1 [Hebrard, G.; Desert, J. -M.; Diaz, R. F.; Boisse, I.; Bouchy, F.; des Etangs, A. Lecavelier; Vidal-Madjar, A.] Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, F-75014 Paris, France. [Desert, J. -M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bouchy, F.; Arnold, L.] Observ Haute Provence, CNRS, OAMP, F-04870 St Michel, France. [Moutou, C.; Santerne, A.] Univ Aix Marseille 1, CNRS, UMR6110, Lab Astrophys Marseille, F-13388 Marseille, France. [Ehrenreich, D.; Bonfils, X.; Delfosse, X.; Desort, M.; Eggenberger, A.; Forveille, T.; Lagrange, A. -M.; Perrier, C.] Univ Grenoble 1, CNRS, UMR5571, Lab Astrophys Grenoble, F-38041 Grenoble 9, France. [Gregorio, J.] CROW Observ Portalegre, Portalegre, Portugal. [Bonfils, X.; Lovis, C.; Pepe, F.; Queloz, D.; Segransan, D.; Udry, S.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Pont, F.; Sing, D. K.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. RP Hebrard, G (reprint author), Univ Paris 06, CNRS, UMR7095, Inst Astrophys Paris, 98bis Blvd Arago, F-75014 Paris, France. EM hebrard@iap.fr RI Santos, Nuno/E-9957-2011; Diaz, Rodrigo/H-1487-2011; Santerne, Alexandre/M-9265-2013; OI Santos, Nuno/0000-0003-4422-2919; Santerne, Alexandre/0000-0002-3586-1316; Boisse, Isabelle/0000-0001-8388-8399; Bonfils, Xavier/0000-0001-9003-8894; Diaz, Rodrigo/0000-0001-9289-5160; Sing, David /0000-0001-6050-7645; Ehrenreich, David/0000-0001-9704-5405 FU NASA; Spitzer; CNRS/INSU; Swiss National Science Foundation; French National Research Agency [ANR-08-JCJC-0102-01, ANR-NT05-4-44463]; CNES; European Research Council/European Community; FCT/MCTES (Portugal); POPH/FSE (EC); [PTDC/CTE-AST/66643/2006]; [PTDC/CTE-AST/098528/2008] FX Based on observations collected with the SOPHIE spectrograph on the 1.93-m telescope at the Observatoire de Haute-Provence (CNRS), France, and with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Radial velocity and photometry tables are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr ( 130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A95; We thank the Haute-Provence Observatory staff that allowed SOPHIE observations despite the ongoing break of the 193-cm telescope, and in particular Fabien Fillion, Francois Moreau, Jacky Taupenas, Jean-Pierre Troncin and Stephane Favard. We are grateful to C. Adami, D. Russeil and M. Dennefeld for their flexibility in the OHP 120-cm photometry observations, M. Gillon and J. N. Winn for useful discussions, and the referee G. Laughlin. We thank the Spitzer director for having awarded us discretionary time, and the Spitzer staff and in particular Nancy Silbermann for their assistance in the preparation of the observation. We acknowledge support of the "Programme National de Planetologie" (PNP) of CNRS/INSU, the Swiss National Science Foundation, and the French National Research Agency (ANR-08-JCJC-0102-01 and ANR-NT05-4-44463). D. E. is supported by CNES. A. E. is supported by a fellowship for advanced researchers from the Swiss National Science Foundation. N. C. S. acknowledges the support of the European Research Council/European Community under the FP7 through a Starting Grant, and the Fundacao para a Ciencia e a Tecnologia (FCT), Portugal, for a Ciencia 2007 contract funded by FCT/MCTES (Portugal) and POPH/FSE (EC), and in the form of grants reference PTDC/CTE-AST/66643/2006 and PTDC/CTE-AST/098528/2008. NR 89 TC 48 Z9 48 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN-JUL PY 2010 VL 516 AR A95 DI 10.1051/0004-6361/201014327 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400110 ER PT J AU Kristensen, LE van Dishoeck, EF van Kempen, TA Cuppen, HM Brinch, C Jorgensen, JK Hogerheijde, MR AF Kristensen, L. E. van Dishoeck, E. F. van Kempen, T. A. Cuppen, H. M. Brinch, C. Jorgensen, J. K. Hogerheijde, M. R. TI Methanol maps of low-mass protostellar systems I. The Serpens molecular core SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: abundances; ISM: molecules; stars: formation; ISM: individual objects: Serpens ID YOUNG STELLAR OBJECTS; GRAIN CHEMICAL-MODELS; STAR-FORMATION; INTERSTELLAR CLOUDS; HOT CORE; SUBMILLIMETER-CONTINUUM; NONTHERMAL DESORPTION; ENVELOPE STRUCTURE; LINE OBSERVATIONS; SILICON MONOXIDE AB Context. Methanol has a rich rotational spectrum providing a large number of transitions at sub-millimetre wavelengths from a range of energy levels in one single telescope setting, thus making it a good tracer of physical conditions in star-forming regions. Furthermore, it is formed exclusively on grain surfaces and is therefore a clean tracer of surface chemistry. Aims. Determining the physical and chemical structure of low-mass, young stellar objects, in particular the abundance structure of CH(3)OH, to investigate where and how CH(3)OH forms and how it is eventually released back to the gas phase. Methods. Observations of the Serpens molecular core have been performed at the James Clerk Maxwell Telescope using the array receiver, Harp-B. Maps over a 4'.5 x 5'.4 region were made in a frequency window around 338 GHz, covering the 7(K)-6(K) transitions of methanol. Data are compared with physical models of each source based on existing sub-millimetre continuum data. Results. Methanol emission is extended over each source, following the column density of H(2) but showing up also particularly strongly around outflows. The rotational temperature is low, 15-20 K, and does not vary with position within each source. None of the Serpens Class 0 sources show the high-K lines seen in several other Class 0 sources. The abundance is typically 10(-9)-10(-8) with respect to H(2) in the outer envelope, whereas "jumps" by factors of up to 10(2)-10(3) inside the region where the dust temperature exceeds 100 K are not excluded. A factor of up to similar to 10(3) enhancement is seen in outflow gas, consistent with previous studies. In one object, SMM4, the ice abundance has been measured to be similar to 3 x 10(-5) with respect to H(2) in the outer envelope, i.e., a factor of 10(3) larger than the gas-phase abundance. Comparison with C(18)O J = 3-2 emission shows that strong CO depletion leads to a high gas-phase abundance of CH(3)OH not just for the Serpens sources, but also for a larger sample of deeply embedded protostars. Conclusions. The observations illustrate the large-scale, low-level desorption of CH(3)OH from dust grains, extending out to and beyond 7500 AU from each source, a scenario which is consistent with non-thermal (photo-) desorption from the ice. The observations also illustrate the usefulness of CH(3)OH as a tracer of energetic input in the form of outflows, where methanol is sputtered from the grain surfaces. Finally, the observations provide further evidence of CH(3)OH formation through CO hydrogenation proceeding on grain surfaces in low-mass envelopes. C1 [Kristensen, L. E.; van Dishoeck, E. F.; Cuppen, H. M.; Brinch, C.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [van Kempen, T. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jorgensen, J. K.] Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. RP Kristensen, LE (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM kristensen@strw.leidenuniv.nl RI Kristensen, Lars/F-4774-2011; Brinch, Christian/G-5157-2015; Cuppen, Herma/F-9729-2015 OI Kristensen, Lars/0000-0003-1159-3721; Brinch, Christian/0000-0002-5074-7183; Cuppen, Herma/0000-0003-4397-0739 FU Spinoza; NWO [614.041.004] FX Astrochemistry at Leiden Observatory is supported by a Spinoza prize and by NWO grant 614.041.004. The authors would like to thank the staff at the JCMT for technical help. Floris van der Tak is thanked for help with updating the LAMDA database and Karin Oberg for very stimulating disucssions. T.v.K. is grateful to the SMA for supporting his research at the CfA. NR 82 TC 18 Z9 18 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 JUN-JUL PY 2010 VL 516 AR A57 DI 10.1051/0004-6361/201014182 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400072 ER PT J AU Marcelino, N Brunken, S Cernicharo, J Quan, D Roueff, E Herbst, E Thaddeus, P AF Marcelino, N. Bruenken, S. Cernicharo, J. Quan, D. Roueff, E. Herbst, E. Thaddeus, P. TI The puzzling behavior of HNCO isomers in molecular clouds SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; line: identification; ISM: abundances; ISM: clouds; ISM: molecules ID MASS STAR-FORMATION; CHEMISTRY; ABUNDANCES; IRAS-16293-2422; PHASE; CORES; CH2; THERMOCHEMISTRY; CONTINUUM; HCN AB Context. Isocyanic acid (HNCO) has been observed in different physical environments in the interstellar medium (ISM) and in external galaxies. HNCO has several metastable isomers with a ground electronic singlet state: HOCN, HCNO, and HONC. The recent detection of fulminic acid (HCNO) in prestellar and protostellar cores and cyanic acid (HOCN) in warm molecular sources (e. g. hot cores) in the Galactic center proves that these species could also be common constituents of the ISM. Aims. To shed some light on the possible formation pathways of these species, we searched for HCNO in the sources where HOCN has been previously detected and vice versa. We have also included the low-mass protostar IRAS 16293-2422, where HNCO is found to be prominent. Methods. Using the new EMIR receivers at the IRAM 30-m telescope, we performed deep searches for three rotational transitions of HOCN and four of HCNO. Results. We report the detection of HOCN in four sources - three dense cores and the lukewarm corino L1527 - where HCNO has been previously observed. HOCN is tentatively detected toward the protostellar binary IRAS 16293-2422. However, HCNO has been detected neither in this source nor in the sources of the Galactic center where HOCN has been previously reported. The derived abundance ratios HCNO/HOCN are close to unity in quiescent clouds, while they are less than 0.01-0.1 in warm clouds. We attempt to explain these results by using both gas-phase and gas-grain chemical models. C1 [Marcelino, N.; Cernicharo, J.] Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain. [Bruenken, S.] Univ Cologne, Inst Phys 1, D-50937 Cologne, Germany. [Quan, D.] Ohio State Univ, Chem Phys Program, Columbus, OH 43210 USA. [Roueff, E.] Observ Paris, LUTH UMR 8102, F-92195 Meudon, France. [Herbst, E.] Ohio State Univ, Dept Phys, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Herbst, E.] Ohio State Univ, Dept Chem, Columbus, OH 43210 USA. [Thaddeus, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Marcelino, N (reprint author), Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Ctra Ajalvir Km 4, Madrid 28850, Spain. EM nmarcelino@cab.inta-csic.es; bruenken@ph1.uni-koeln.de; jcernicharo@cab.inta-csic.es; dquan@chemistry.ohio-state.edu; evelyne.roueff@obspm.fr; herbst@mps.ohio-state.edu; pthaddeus@cfa.harvard.edu RI Brunken, Sandra/B-1880-2010 OI Brunken, Sandra/0000-0001-7175-4828 FU INSU/CNRS (France); MPG (Germany); IGN (Spain); Spanish Ministerio de Ciencia e Innovacion [AYA2006-14876, ESP2007-65812-CO2-01]; DGU of the Madrid community government [S-0505/ESP-0237 (ASTROCAM)]; National Science Foundation [AST-0702876]; NASA FX This work was based on observations carried out with the IRAM 30-m telescope. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).; We thank the referee for pointing out additional information on the reaction between CH2 and NO and for other useful comments. We thank M. Gerin for useful discussions concerning the chemistry. This work has been supported by Spanish Ministerio de Ciencia e Innovacion through grants AYA2006-14876 and ESP2007-65812-CO2-01, and by DGU of the Madrid community government under IV-PRICIT project S-0505/ESP-0237 (ASTROCAM). E. H. acknowledges the support of the National Science Foundation for his astrochemistry program through grant AST-0702876 and for his program on chemical kinetics through the Center for the Chemistry of the Universe. E. H. also acknowledges the support of NASA for studies in the evolution of pre-planetary matter. NR 44 TC 23 Z9 23 U1 1 U2 13 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN-JUL PY 2010 VL 516 AR A105 DI 10.1051/0004-6361/200913806 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400120 ER PT J AU Moullet, A Gurwell, M Carry, B AF Moullet, A. Gurwell, M. Carry, B. TI Thermal rotational lightcurve of dwarf-planet (1) Ceres at 235 GHz with the Submillimeter Array SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE minor planets, asteroids: individual: Ceres ID MIXED VERTICAL PROFILE; ASTEROIDS; TITAN; CO; PHOTOMETRY AB Context. Previously published measurements of the millimeter-wave thermal rotational lightcurve of dwarf-planet (1) Ceres show incompatible results, proposing peak-to-peak lightcurve amplitudes during the similar to 9 h rotation period of either 4% or 50%, the latter being difficult to explain physically. Aims. Better calibrated measurements are necessary to firmly assess the behavior of Ceres' thermal lightcurve, and to relate possible brightness temperature variations to the distribution of local surface properties such as bolometric albedo and emissivity. Methods. One partial lightcurve of 6.5 h was obtained with the Submillimeter Array (Hawaii) in subcompact configuration at 235 GHz in January 2009, providing better absolute and relative calibration than the previously used single-dish facilities. Results. The observed disk-averaged lightcurve is compatible with no variation over the measurement window, and has an upper limit of 3% on its amplitude. Conclusions. The results obtained rule out the possibility of extreme brightness temperature variations, and the upper limit on the lightcurve amplitude could be physically realized by a combination of albedo distribution and realistic ground emissivity variations. C1 [Moullet, A.; Gurwell, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Carry, B.] Observ Paris, LESIA, F-92195 Meudon, France. [Carry, B.] Univ Paris 07, F-75205 Paris, France. RP Moullet, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amoullet@cfa.harvard.edu FU Smithsonian Institution; Academia Sinica FX We thank Mark Sykes for his helpful review of this letter, and SMA operators and staff for carrying out the observations. 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 18 TC 2 Z9 2 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 JUN-JUL PY 2010 VL 516 AR L10 DI 10.1051/0004-6361/201014792 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400010 ER PT J AU Risaliti, G Elvis, M AF Risaliti, G. Elvis, M. TI A non-hydrodynamical model for acceleration of line-driven winds in active galactic nuclei SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: active; quasars: general; acceleration of particules ID QUASI-STELLAR OBJECTS; SEYFERT 1 GALAXIES; X-RAY; DISK WINDS; ACCRETION DISKS; EMISSION-LINES; BLACK-HOLES; ABSORPTION-LINES; RADIATIVE DISK; RADIO-QUIET AB Context. Radiation driven winds are the likely origin of AGN outflows, and are believed to be a fundamental component of the inner structure of AGNs. Several hydrodynamical models have been developed, showing that these winds can be effectively launched from AGN accretion disks. Aims. Here we want to study the acceleration phase of line-driven winds in AGNs, in order to examine the physical conditions required for the existence of such winds for a wide variety of initial conditions. Methods. We built a simple and fast non-hydrodynamic model QWIND, where we assume that a wind is launched from the accretion disk at supersonic velocities of a few 100 km s(-1), and we concentrated on the subsequent supersonic phase, when the wind is accelerated to final velocities up to 10(4) km s(-1). Results. We show that, with a set of initial parameters in agreement with observations in AGNs, this model can produce a wind with terminal velocities on the order of 10(4) km s(-1). There are three zones in the wind, only the middle one of which can launch a wind: in the inner zone the wind is too ionized and so experiences only the Compton radiation force, which is not effective in accelerating gas. This inner "failed wind" is important for shielding the next zone by lowering the ionization parameter there. In the middle zone the lower ionization of the gas leads to a much larger radiation force and the gas achieves escape velocity This middle zone is quite thin (about 100 gravitational radii). The outer, third zone is shielded from the UV radiation by the central wind zone, so does not achieve a high enough acceleration to reach escape velocity. We also describe a simple analytic approximation of our model, in which we neglect the effects of gravity during the acceleration phase. This analytic approach agrees with the results of the numerical code, and is a powerful way to check whether a radiation driven wind can be accelerated with a given set of initial parameters. Conclusions. Our analytical analysis and the fast QWIND model agree with more complex hydrodynamical models, and allow exploration of the dependence of the wind properties for a wide set of initial parameters: black hole mass, Eddington ratio, initial density profile, X-ray to UV ratio. C1 [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, G.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Risaliti, G (reprint author), Osserv Astrofis Arcetri, INAF, Largo E Fermi 5, I-50125 Florence, Italy. EM risaliti@arcetri.astro.it OI Risaliti, Guido/0000-0002-3556-977X FU NASA [NNX08AX78G, NNX07AI22G, GO7-8136A]; ASI-INAF [I/088/06/0] FX We are grateful to Jonathan Mc Dowell for his help with the numerical code, and to the anonymous referee for his/her comments and a close reading of the text, which greatly improved the clarity of the work. This work has been partially supported by NASA grants NNX08AX78G, NNX07AI22G and GO7-8136A, and by grant ASI-INAF I/088/06/0. NR 62 TC 20 Z9 20 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 JUN-JUL PY 2010 VL 516 AR A89 DI 10.1051/0004-6361/200912579 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 630LT UT WOS:000280275400104 ER PT J AU Claret, A Torres, G Wolf, M AF Claret, A. Torres, G. Wolf, M. TI DI Herculis as a test of internal stellar structure and general relativity New apsidal motion rate and evolutionary models SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: eclipsing; stars: interiors; stars: rotation ID CLOSE BINARY STARS; ECLIPSING BINARIES; TIDAL-EVOLUTION; Y-2 ISOCHRONES; SYSTEM; OPACITIES AB Context. For the past three decades there has been a serious discrepancy between the observed and theoretical values of the apsidal motion rate. omega of the eccentric eclipsing binary DI Her, which has even been interpreted occasionally as a possible failure of general relativity (GR). A number of plausible explanations have been put forward. Recent observations of the Rossiter-McLaughlin effect have shown convincingly that the reason for the anomaly is that the rotational axes of the stars and the orbital axis are misaligned, which changes the predicted rate of precession significantly. Aims. Although the disagreement is now drastically smaller as a result of those measurements, it formally remains at the level of 50%, owing possibly to errors in the measured apsidal motion rate, outdated stellar models, or inaccuracies in the stellar parameters. The aim of this paper is to address each of these issues to improve the agreement even more. Methods. New times of minimum have been collected and used for redetermining of the apsidal motion rate. Based on the latest determinations of the absolute dimensions of the binary, we computed new stellar evolution models with updated physical inputs, and derived improved apsidal motion constants for the components. We performed Monte Carlo simulations to infer the theoretical distribution of. omega, including the contributions from GR, as well as tidal and rotational distortions. All observational errors have been accounted for. Results. Our simulations yield a retrograde apsidal motion rate due to the rotationally-induced oblateness of -0.00056 deg cycle(-1) (mode of the distribution), a GR contribution of +0.00068 deg cycle(-1), and a tidal contribution of +0.00034 deg cycle(-1), leading to a total predicted rate of +0.00046 deg cycle(-1). This is in excellent agreement with the newly measured value of +0.00042 deg cycle(-1). The formal difference is now reduced to 10%, a small fraction of the observational uncertainties. C1 [Claret, A.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wolf, M.] Charles Univ Prague, Fac Math & Phys, Astron Inst, CR-18000 Prague 8, Czech Republic. RP Claret, A (reprint author), CSIC, Inst Astrofis Andalucia, Apartado 3004, E-18080 Granada, Spain. EM claret@iaa.es FU Spanish MEC [AYA2006-06375]; US National Science Foundation [AST-0708229]; Ministry of Education of the Czech Republic [MSM0021620860] FX The Spanish MEC (AYA2006-06375) is gratefully acknowledged for its support during the development of this work. G. T. acknowledges partial support through grant AST-0708229 from the US National Science Foundation. The research of M.W. was supported by the Research Program MSM0021620860 of the Ministry of Education of the Czech Republic. We would like to thank Ms. Hana Kucakova, Ostrava Observatory, and Mr. Ladislav Smelcer, Valasske Mezirici Observatory, for their valuable assistance with the photometric observations, and the anonymous referee for helpful suggestions. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Abstract Service. NR 32 TC 6 Z9 6 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 JUN PY 2010 VL 515 AR A4 DI 10.1051/0004-6361/200913942 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 606CN UT WOS:000278399000004 ER PT J AU Gielen, C Van Wincke, H Min, M Waters, LBFM Evans, TL Matsuura, M Deroo, P Dominik, C Reyniers, M Zijlstra, A Gordon, KD Kemper, F Indebetouw, R Marengo, M Meixner, M Sloan, GC Tielens, AGGM Woods, PM AF Gielen, C. Van Wincke, H. Min, M. Waters, L. B. F. M. Evans, T. Lloyd Matsuura, M. Deroo, P. Dominik, C. Reyniers, M. Zijlstra, A. Gordon, K. D. Kemper, F. Indebetouw, R. Marengo, M. Meixner, M. Sloan, G. C. Tielens, A. G. G. M. Woods, P. M. TI SPITZER-IRS spectral fitting of discs around binary post-AGB stars Corrigendum SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: abundances; stars: AGB and post-AGB; circumstellar matter; binaries: general; Magellanic Clouds; errata, addenda C1 [Gielen, C.; Van Wincke, H.; Waters, L. B. F. M.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Louvain, Belgium. [Waters, L. B. F. M.; Dominik, C.] Univ Amsterdam, Sterrenkundig Inst Anton Pannckock, NL-1098 Amsterdam, Netherlands. [Evans, T. Lloyd] Univ St Andrews, Sch Phys & Astron, SUPA, St Andrews KY16 9SS, Fife, Scotland. [Matsuura, M.] UCL, Dept Phys & Astron, UCL Inst Origins, London WC1E 6BT, England. [Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, UCL Inst Origins, Dorking RH5 6NT, Surrey, England. [Deroo, P.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Dominik, C.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Reyniers, M.] Royal Meteorol Inst Belgium, Dept Observat, B-1180 Brussels, Belgium. [Zijlstra, A.; Kemper, F.; Woods, P. M.] Univ Manchester, Jodrell Bank, Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Gordon, K. D.; Meixner, M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sloan, G. C.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Tielens, A. G. G. M.] Leiden Observ, NL-2333 CA Leiden, Netherlands. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA 22906 USA. [Min, M.] Univ Utrecht, Astron Inst Utrecht, NL-3584 CC Utrecht, Netherlands. RP Gielen, C (reprint author), Katholieke Univ Leuven, Inst Sterrenkunde, Celestijnenlaan 200D, B-3001 Louvain, Belgium. EM clio.gielen@ster.kuleuven.be FU Fund for Scientific Research of Flanders (FWO) [G.0178.02, G.0470.07]; NASA FX C.G. and H.V.W. acknowledge support of the Fund for Scientific Research of Flanders (FWO) under the grant G.0178.02. and G.0470.07. 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. NR 3 TC 1 Z9 1 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 JUN PY 2010 VL 515 AR C2 DI 10.1051/0004-6361/200912982e PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633LS UT WOS:000280505000002 ER PT J AU James, DJ Barnes, SA Meibom, S Lockwood, GW Levine, SE Deliyannis, C Platais, I Steinhauer, A Hurley, BK AF James, D. J. Barnes, S. A. Meibom, S. Lockwood, G. W. Levine, S. E. Deliyannis, C. Platais, I. Steinhauer, A. Hurley, B. K. TI New rotation periods in the open cluster NGC 1039 (M 34), and a derivation of its gyrochronology age SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE methods: data analysis; starspots; stars: fundamental parameters; globular clusters: individual: NGC 1039 (M34) ID SOLAR-TYPE STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; SUPERCOSMOS SKY SURVEY; DWARF LUMINOSITY FUNCTION; LITHIUM-DEPLETION; CHROMOSPHERIC EMISSION; ANGULAR-MOMENTUM; STELLAR EVOLUTION; BINARY STARS AB Aims. Employing photometric rotation periods for solar-type stars in NGC 1039 [M34], a young, nearby open cluster, we use its mass-dependent rotation period distribution to derive the cluster's age in a distance independent way, i.e., the so-called gyrochronology method. Methods. We present an analysis of 55 new rotation periods, using light curves derived from differential photometry, for solar type stars in the open cluster NGC 1039 [M34]. We also exploit the results of a recently-completed, standardized, homogeneous BVIc CCD survey of the cluster, performed by the Indiana Group of the WIYN open cluster survey, in order to establish photometric cluster membership and assign B-V colours to each photometric variable. We describe a methodology for establishing the gyrochronology age for an ensemble of solar-type stars. Empirical relations between rotation period, photometric colour and stellar age (gyrochronology) are used to determine the age of M34. Based on its position in a colour-period diagram, each M34 member is designated as being either a solid-body rotator (interface or I-star), a differentially rotating star (convective or C-star) or an object which is in some transitory state in between the two (gap or g-star). Fitting the period and photometric colour of each I-sequence star in the cluster, we derive the cluster's mean gyrochronology age. Results. Of the photometric variable stars in the cluster field, for which we derive a period, 47 out of 55 of them lie along the loci of the cluster main sequence in V/B - V and V/V - I space. We are further able to confirm kinematic membership of the cluster for half of the periodic variables [21/55], employing results from an on-going radial velocity survey of the cluster. For each cluster member identified as an I-sequence object in the colour-period diagram, we derive its individual gyrochronology age, where the mean gyro age of M34 is found to be 193 +/- 9 Myr. Conclusions. Using differential photometry, members of a young open cluster can be easily identified in a colour-magnitude diagram from their periodic photometric variability alone. Such periodicity can be used to establish a period-colour distribution for the cluster, which for M34, we have used to derive its gyrochronology age of 193 +/- 9 Myr. Formally, our gyro age of M34 is consistent (within the errors) with that derived using several distance-dependent, photometric isochrone methods (250 +/- 67 Myr). C1 [James, D. J.; Hurley, B. K.] Univ Hawaii, Hoko Kea Observ, Dept Phys & Astron, Hilo, HI 96720 USA. [James, D. J.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Barnes, S. A.; Lockwood, G. W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Meibom, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Levine, S. E.] USN Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Deliyannis, C.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. [Platais, I.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Steinhauer, A.] SUNY Coll Geneseo, Dept Phys & Astron, Geneseo, NY 14454 USA. RP James, DJ (reprint author), Univ Hawaii, Hoko Kea Observ, Dept Phys & Astron, 200 W Kawili St, Hilo, HI 96720 USA. EM david.james@hawaii.edu FU Vanderbilt University [AST-0349075] FX This research has been supported by NSF grant AST-0349075 (Vanderbilt University), which is gratefully acknowledged. This research has made extensive use of the WEBDA database, operated by the Institute for Astronomy at the University of Vienna, as well as the SIMBAD database, operated at CDS, Strasbourg, France. Insightful discussions with Jonathon Irwin concerning his original M 34 rotation period dataset are appreciated. NR 94 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUN PY 2010 VL 515 AR A100 DI 10.1051/0004-6361/200913138 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633LS UT WOS:000280505000069 ER PT J AU Lommen, DJP van Dishoeck, EF Wright, CM Maddison, ST Min, M Wilner, DJ Salter, DM van Langevelde, HJ Bourke, TL van der Burg, RFJ Blake, GA AF Lommen, D. J. P. van Dishoeck, E. F. Wright, C. M. Maddison, S. T. Min, M. Wilner, D. J. Salter, D. M. van Langevelde, H. J. Bourke, T. L. van der Burg, R. F. J. Blake, G. A. TI Grain growth across protoplanetary discs: 10 mu m silicate feature versus millimetre slope' SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE accretion, accretion disks; circumstellar matter; stars: pre-main sequence; stars: formation ID T-TAURI STARS; HERBIG AE/BE STARS; MAIN-SEQUENCE STARS; SPECTRAL ENERGY-DISTRIBUTIONS; CIRCUMSTELLAR DISKS; MOLECULAR CLOUD; STELLAR POPULATION; RADIATIVE-TRANSFER; ISO SPECTROSCOPY; FORMING REGION AB Context. Young stars are formed with dusty discs around them. The dust grains in the disc are originally of the same size as interstellar dust, i.e., of the order of 0.1 mu m. Models predict that these grains will grow in size through coagulation. Observations of the silicate features around 10 and 20 mu m are consistent with growth from submicron to micron sizes in selected sources whereas the slope of the spectral energy distribution (SED) at mm and cm wavelengths traces growth up to mm sizes and larger. Aims. We here look for a correlation between these two grain growth indicators. Methods. A large sample of T-Tauri and Herbig-Ae/Be stars, spread over the star-forming regions in Chamaeleon, Lupus, Serpens, Corona Australis, and the Gum nebula in Vela, was observed with the Spitzer Space Telescope at 5-13 mu m, and a subsample was observed with the SMA, ATCA, CARMA, and VLA at mm wavelengths. We complement this subsample with data from the literature to maximise the overlap between mu m and mm observations and search for correlations in the grain-growth signatures. Synthetic spectra are produced to determine which processes may produce the dust evolution observed in protoplanetary discs. Results. Dust disc masses in the range <1 to 7 x 10(-4) M-circle dot are obtained. The majority of the sources have a mm spectral slope consistent with grain growth. There is a tentative correlation between the strength and the shape of the 10-mu m silicate feature and the slope of the SED between 1 and 3 mm. The observed sources seem to be grouped per star-forming region in the 10-mu m-feature vs. mm-slope diagram. The modelling results show that, if only the maximum grain size is increased, first the 10-mu m feature becomes flatter and subsequently the mm slope becomes shallower. To explain the sources with the shallowest mm slopes, a grain size distribution shallower than that of the interstellar medium is required. Furthermore, the strongest 10-mu m features can only be explained with bright (L similar to 6 L-circle dot), hot (T-eff = 4000 K) central stars. Settling of larger grains towards the disc midplane results in a stronger 10-mu m feature, but has a very limited effect on the mm slope. Conclusions. A tentative correlation between the strength of the 10-mu m feature and the mm slope is found, which would imply that the inner and outer disc evolve simultaneously. Dust with a mass dominated by large, similar to mm-sized, grains is required to explain the shallowest mm slopes. Other processes besides grain growth, such as the clearing of an inner disc by binary interaction, may also be responsible for the removal of small grains. Observations with future telescopes with larger bandwidths or collecting areas are required to provide the necessary statistics to study these processes of disc and dust evolution. C1 [Lommen, D. J. P.; van Dishoeck, E. F.; Salter, D. M.; van Langevelde, H. J.; van der Burg, R. F. J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-37075 Garching, Germany. [Wright, C. M.] UNSW ADFA, Sch Phys Environm & Math Sci, Canberra, ACT 2600, Australia. [Maddison, S. T.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Min, M.] Astron Inst, NL-3584 CC Utrecht, Netherlands. [Min, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Wilner, D. J.; Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Langevelde, H. J.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Blake, G. A.] CALTECH, Pasadena, CA 91125 USA. RP Lommen, DJP (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM dave@strw.leidenuniv.nl FU Netherlands Research School For Astronomy; Netherlands Organisation for Scientific Research; ARC [DP0345227] FX We are indebted to Kees Dullemond for the use of his RADMC and RAYTRACE codes and to Stephen Bourke for help with AIPS. A special thanks to the ATNF and SMA staff for assistance with the observations. Ruud Visser's help on all things computer is greatly appreciated and Carsten Dominik is thanked for his useful comments. Partial support for this work was provided by a Netherlands Research School For Astronomy network 2 grant, and by a Netherlands Organisation for Scientific Research Spinoza grant. C.M.W. acknowledges financial support from an ARC Australian Research Fellowship, Discovery Project DP0345227. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. NR 79 TC 29 Z9 29 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 JUN PY 2010 VL 515 AR A77 DI 10.1051/0004-6361/200913150 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633LS UT WOS:000280505000046 ER PT J AU Revnivtsev, M van den Berg, M Burenin, R Grindlay, JE Karasev, D Forman, W AF Revnivtsev, M. van den Berg, M. Burenin, R. Grindlay, J. E. Karasev, D. Forman, W. TI Interstellar extinction and the distribution of stellar populations in the direction of the ultra-deep Chandra Galactic field SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: general; Hertzsrung-Russell (HR) and C-M diagrams; stars: luminosity fonction, mass function; Galaxy: bulge; galaxies: stellar content; X-rays: galaxies ID X-RAY-EMISSION; MILKY-WAY; LUMINOSITY FUNCTION; POINT SOURCES; BULGE; RIDGE; 2MASS; CALIBRATION; BINARIES; DISTANCE AB We studied the stellar population in the central 6.6' x 6.6' region of the ultra-deep (1Msec) Chandra Galactic field - the "Chandra bulge field" (CBF) approximately 1.5 degrees away from the Galactic Center - using the Hubble Space Telescope ACS/WFC blue (F435W) and red (F625W) images. We mainly focus on the behavior of red clump giants - a distinct stellar population, which is known to have an essentially constant intrinsic luminosity and color. By studying the variation in the position of the red clump giants on a spatially resolved color-magnitude diagram, we confirm the anomalous total-to-selective extinction ratio, as reported in previous work for other Galactic bulge fields. We show that the interstellar extinction in this area is < A(F625W)> = 4 on average, but varies significantly between similar to 3-5 on angular scales as small as 1 arcminute. Using the distribution of red clump giants in an extinction-corrected color-magnitude diagram, we constrain the shape of a stellar-mass distribution model in the direction of this ultra-deep Chandra field, which will be used in a future analysis of the population of X-ray sources. We also show that the adopted model for the stellar density distribution predicts an infrared surface brightness in the direction of the "Chandra bulge field" in good agreement (i.e. within similar to 15%) with the actual measurements derived from the Spitzer/IRAC observations. C1 [Revnivtsev, M.] Tech Univ Munich, Excellence Cluster Univ, D-85748 Garching, Germany. [Revnivtsev, M.; Burenin, R.; Karasev, D.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Revnivtsev, M.; van den Berg, M.; Grindlay, J. E.; Forman, W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Revnivtsev, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mikej@mpa-garching.mpg.de OI Forman, William/0000-0002-9478-1682 FU Russian Foundation of Basic Research [07-02-01051, 07-02-00961-a, 08-08-13734, 07-02-01004, 08-02-00974, NSh-5579.2008.2]; STScI/HST [HST-GO-10353.01] FX The authors thank Annamaria Donnarumma and Maxim Markevitch for their help in obtaining Magellan observations of the field. This research made use of data obtained from the High Energy Astrophysics Science Archive Research Center Online Service, provided by the NASA/Goddard Space Flight Center. This work was supported by grants of the Russian Foundation of Basic Research (07-02-01051, 07-02-00961-a, 08-08-13734, 07-02-01004, 08-02-00974, NSh-5579.2008.2) and programs of Presidium of RAS P04 and OFN-17. MvdB was supported in part by STScI/HST grant HST-GO-10353.01. Results in this paper are based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Institute which is operated by the Association of Universities for Research in Astronomy, Inc. under the NASA contract NAS 5-26555. NR 33 TC 10 Z9 10 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 JUN PY 2010 VL 515 AR A49 DI 10.1051/0004-6361/200913527 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633LS UT WOS:000280505000018 ER PT J AU Kelly, PL Hicken, M Burke, DL Mandel, KS Kirshner, RP AF Kelly, Patrick L. Hicken, Malcolm Burke, David L. Mandel, Kaisey S. Kirshner, Robert P. TI HUBBLE RESIDUALS OF NEARBY TYPE Ia SUPERNOVAE ARE CORRELATED WITH HOST GALAXY MASSES SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general ID DIGITAL SKY SURVEY; LIGHT-CURVE SHAPES; GAMMA-RAY BURSTS; STAR-FORMATION; DARK ENERGY; METALLICITY RELATION; SPACE-TELESCOPE; LEGACY SURVEY; SN-IA; LUMINOSITY AB From Sloan Digital Sky Survey u'g'r'i'z' imaging, we estimate the stellar masses of the host galaxies of 70 low-redshift Type Ia supernovae (SNe Ia, 0.015 < z < 0.08) from the hosts' absolute luminosities and mass-to-light ratios. These nearby SNe were discovered largely by searches targeting luminous galaxies, and we find that their host galaxies are substantially more massive than the hosts of SNe discovered by the flux-limited Supernova Legacy Survey (SNLS). Testing four separate light curve fitters, we detect similar to 2.5 sigma correlations of Hubble residuals with both host galaxy size and stellar mass, such that SNe Ia occurring in physically larger, more massive hosts are similar to 10% brighter after light curve correction. The Hubble residual is the deviation of the inferred distance modulus to the SN, calculated from its apparent luminosity and light curve properties, away from the expected value at the SN redshift. Marginalizing over linear trends in Hubble residuals with light curve parameters shows that the correlations cannot be attributed to a light-curve-dependent calibration error. Combining 180 higher-redshift ESSENCE, SNLS, and HigherZ SNe with 30 nearby SNe whose host masses are less than 10(10.8) M-circle dot in a cosmology fit yields 1 + w = 0.22(-0.108)(+0.152), while a combination where the 30 nearby SNe instead have host masses greater than 10(10.8) M-circle dot yields 1 + w = -0.03(-0.143)(+0.217). Progenitor metallicity, stellar population age, and dust extinction correlate with galaxy mass and may be responsible for these systematic effects. Host galaxy measurements will yield improved distances to SNe Ia. C1 [Kelly, Patrick L.; Burke, David L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. [Kelly, Patrick L.; Burke, David L.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Hicken, Malcolm; Mandel, Kaisey S.; Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kelly, PL (reprint author), Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, 382 Via Pueblo Mall, Stanford, CA 94305 USA. EM pkelly3@stanford.edu FU NSF [AST0907903, AST0606772]; U.S. Department of Energy [DE-AC02-70SF00515]; Alfred P. Sloan Foundation; Participating Institutions; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank especially R. Romani, M. Blanton, A. von der Linden, S. Allen, A. Mantz, C. Zhang, M. Sako, B. Haussler, and C. Peng as well as D. Rapetti, B. Holden, D. Applegate, M. Allen, P. Behroozi, O. Ilbert, S. Arnouts, and J. Gallagher. NSF grants AST0907903 and AST0606772 as well as the U.S. Department of Energy contract DE-AC02-70SF00515 support research on SN at Harvard University.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.; The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, Cambridge University, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. NR 82 TC 119 Z9 120 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 743 EP 756 DI 10.1088/0004-637X/715/2/743 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100003 ER PT J AU Olivares, F Hamuy, M Pignata, G Maza, J Bersten, M Phillips, MM Suntzeff, NB Filippenko, AV Morrel, NI Kirshner, RP Matheson, T AF Olivares E, Felipe Hamuy, Mario Pignata, Giuliano Maza, Jose Bersten, Melina Phillips, Mark M. Suntzeff, Nicholas B. Filippenko, Alexei V. Morrel, Nidia I. Kirshner, Robert P. Matheson, Thomas TI THE STANDARDIZED CANDLE METHOD FOR TYPE II PLATEAU SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE distance scale; galaxies: distances and redshifts; supernovae: general ID EXPANDING PHOTOSPHERE METHOD; SOUTHERN SPECTROPHOTOMETRIC STANDARDS; QUANTITATIVE SPECTROSCOPIC ANALYSIS; PROBE WMAP OBSERVATIONS; IA SUPERNOVAE; DARK ENERGY; P SUPERNOVAE; LIGHT CURVES; HUBBLE DIAGRAM; SN 2005CS AB In this paper, we study the "standardized candle method" using a sample of 37 nearby (redshift z < 0.06) Type II plateau supernovae having BVRI photometry and optical spectroscopy. An analytic procedure is implemented to fit light curves, color curves, and velocity curves. We find that the V-I color toward the end of the plateau can be used to estimate the host-galaxy reddening with a precision of sigma(A(V)) = 0.2 mag. The correlation between plateau luminosity and expansion velocity previously reported in the literature is recovered. Using this relation and assuming a standard reddening law (R(V) = 3.1), we obtain Hubble diagrams (HDs) in the BVI bands with dispersions of similar to 0.4 mag. Allowing R(V) to vary and minimizing the spread in the HDs, we obtain a dispersion range of 0.25-0.30 mag, which implies that these objects can deliver relative distances with precisions of 12%-14%. The resulting best-fit value of R(V) is 1.4 +/- 0.1. C1 [Olivares E, Felipe; Hamuy, Mario; Pignata, Giuliano; Maza, Jose; Bersten, Melina] Univ Chile, Dept Astron, Santiago, Chile. [Olivares E, Felipe] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Pignata, Giuliano] Univ Andres Bello, Dept Ciencias Fis, Santiago, Chile. [Phillips, Mark M.; Morrel, Nidia I.] Carnegie Observ, Las Campanas Observ, La Serena, Chile. [Suntzeff, Nicholas B.] Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. [Filippenko, Alexei V.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kirshner, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matheson, Thomas] Natl Opt Astron Observ, Tucson, AZ 85719 USA. RP Olivares, F (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM felipe@mpe.mpg.de RI Hamuy, Mario/G-7541-2016; Maza, Jose/I-5722-2016; OI Maza, Jose/0000-0003-2068-1328; Olivares E., Felipe/0000-0002-5115-6377 FU Programa Bicentenario de Ciencia y Tecnologia de CONICYT [Pas06-045-F]; Programa Iniciativa Cientifica Milenio de MIDEPLAN; Centro de Astrofisica FONDAP [15010003]; Fondecyt [1060808]; NSF [AST-0607485, AST-0908886, AST-0606772]; TABASGO Foundation; Comite Mixto ESO-GOBIERNO DE CHILE FX We thank Luc Dessart, who generously provided the reddening estimates calculated by means of spectral fitting and the models plotted in Figure 4. F.O.E. also thanks him for stimulating discussions, as well as for accurate comments and suggestions. We are grateful to D. Leonard, J. Vinko, D. Sahu, and A. Pastorello for providing digital spectra of SN 1999gi, SN 2004dj, SN 2004et, and SN 2005cs, respectively. F.O.E., M.H., G.P., and J.M. acknowledge support from the Millennium Center for Supernova Science through grant Pas06-045-F funded by "Programa Bicentenario de Ciencia y Tecnologia de CONICYT" and "Programa Iniciativa Cientifica Milenio de MIDEPLAN," as well as support provided by Centro de Astrofisica FONDAP 15010003 and by Fondecyt through grant 1060808 from the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). The supernova research of A.V.F.'s group at U.C. Berkeley has been financed by NSF grants AST-0607485 and AST-0908886, as well as by the TABASGO Foundation. Supernova research at the Harvard College Observatory has been supported by NSF grant AST-0606772. G.P. acknowledges partial support from Comite Mixto ESO-GOBIERNO DE CHILE. This paper is based in part on observations taken at the Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the NSF. Partly based on observations collected at the European Southern Observatory, Chile, in the course of program 163.H-0285. NR 105 TC 52 Z9 52 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 833 EP 853 DI 10.1088/0004-637X/715/2/833 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100010 ER PT J AU Nicastro, F Krongold, Y Fields, D Conciatore, ML Zappacosta, L Elvis, M Mathur, S Papadakis, I AF Nicastro, F. Krongold, Y. Fields, D. Conciatore, M. L. Zappacosta, L. Elvis, M. Mathur, S. Papadakis, I. TI XMM-NEWTON AND FUSE TENTATIVE EVIDENCE FOR A WHIM FILAMENT ALONG THE LINE OF SIGHT TO PKS 0558-504 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: Seyfert; intergalactic medium; line: identification; methods: data analysis ID HOT INTERGALACTIC MEDIUM; ULTRAVIOLET-SPECTROSCOPIC-EXPLORER; PROBE WMAP OBSERVATIONS; X-RAY-ABSORPTION; IONIZED ABSORBER; MISSING BARYONS; WARM ABSORBERS; LOCAL GROUP; LY-ALPHA; GALAXY AB We present a possible OVIII X-ray absorption line at z = 0.117 +/- 0.001 which, if confirmed, will be the first one associated with a broad Hi Ly beta (BLB: FWHM = 160(-30)(+50) km s(-1)) absorber. The absorber lies along the line of sight to the nearby (z = 0.1372) Seyfert 1 galaxy PKS 0558-504, consistent with being a WHIM filament. The X-ray absorber is marginally detected in two independent XMM-Newton spectra of PKS 0558-504, a long similar to 600 ks guest-observer observation and a shorter, similar to 300 ks total, calibration observation, with a combined single line statistical significance of 2.8 sigma (2.7 sigma and 1.2 sigma in the two spectra, respectively). When fitted with our self-consistent hybrid-photoionization WHIM models, the combined XMM-Newton spectrum is consistent with the presence of OVIII K alpha at z = (0.117 +/- 0.001). This model gives best-fitting temperature and equivalent H column density of the absorber of log T = 6.56(-0.17)(+0.19) K, and log N(H) = (21.5 +/- 0.3)(Z/Z0.01(circle dot))(-1) cm(-2), and predicts the marginal contribution of only two more lines within the XMM-Newton Reflection Grating Spectrometer band pass, Ne IX K alpha (lambda = 13.45 angstrom) and Fe XVII L (lambda = 15.02 angstrom), both with equivalent widths well within the 1 sigma sensitivity of the combined XMM-Newton spectrum of PKS 0558-504 (EW(1 sigma) < 3 m angstrom). The lack of detection of associated OVI in the archival FUSE spectrum of PKS 0558-504 allows us to infer a tighter lower limit on the temperature, of log T > 6.52 K (at 1 sigma ). The statistical significance of this single X-ray detection is increased by the detection of BLB and complex HI Ly beta absorption in archival FUSE spectra of PKS 0558-504, at redshifts z = 0.1183 +/- 0.0001 consistent with the best-fitting redshift of the X-ray absorber. The FUSE spectrum shows a broad (FWHM = 160(-30)(+ 50) km s(-1)) absorption complex, which we identify as HI Ly beta z(BLB) = (0.1183 +/- 0.0001). The single line statistical significance of this line is 4.1 sigma (3.7 sigma if systematics are considered). A possible HI Ly alpha is marginally hinted in an archival low-resolution (Delta lambda similar to 6 angstrom) International Ultraviolet Explorer (IUE) spectrum of PKS 0558-504, at a redshift of z = (0.119 +/- 0.001) and with single line significance of 1.7 sigma. Thus, the combined significance of the three (XMM-Newton, FUSE, and IUE) independent tentative detections, is 5.2 sigma (5.0 sigma if the HI Ly alpha is not considered, and 4.6 sigma if the systematics in FUSE are considered). The detection of both metal and H lines at a consistent redshift, in this hot absorbing system, allows us to speculate on its metallicity. By associating the bulk of the X-ray absorber with the BLB line detected in the FUSE spectrum at z(BLB) = 0.1183 +/- 0.0001, we obtain a metallicity of 1%-4% Solar. Although the absorber is only blueshifted by similar to-6000 km s(-1) from the systemic redshift of PKS 0558-504, the identification of the absorbing gas with a high velocity nuclear ionized outflow, is unlikely. The physical, chemical, and dynamical properties of the detected absorber are all quite different from those typically found in the warm absorber (WA) outflows, commonly detected in Seyferts and higher luminosity quasars. WA outflow velocities typically span a range of few hundreds to similar to 1-2 thousands km s(-1) WA metallicities, when measured, are typically found to be at least Solar; high-ionization WAs are virtually always found to coexist with lower-ionization X-ray and UV phases. All this strongly suggests that the absorber, if confirmed, is an intervening WHIM system. C1 [Nicastro, F.] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, RM, Italy. [Nicastro, F.] Fdn Res & Technol, IESL, Iraklion 71110, Crete, Greece. [Nicastro, F.; Conciatore, M. L.; Zappacosta, L.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Fields, D.] LA Pierce Coll, Woodland Hills, CA USA. [Mathur, S.] Ohio State Univ, Columbus, OH 43210 USA. [Papadakis, I.] Univ Crete, Dept Phys, GR-71003 Iraklion, Crete, Greece. RP Nicastro, F (reprint author), Osservatorio Astron Roma INAF, Via Frascati 33, I-00040 Monte Porzio Catone, RM, Italy. RI Papadakis, Iossif/C-3235-2011; OI Nicastro, Fabrizio/0000-0002-6896-1364 FU LTSA [NNG04GD49G]; EU [206469] FX F.N., L.Z., and M.L.C. acknowledge support from the LTSA grant NNG04GD49G. F.N. acknowledges support from the FP7-REGPOT-2007-1 EU grant no. 206469. 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 51 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 854 EP 865 DI 10.1088/0004-637X/715/2/854 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100011 ER PT J AU Arce, HG Borkin, MA Goodman, AA Pineda, JE Halle, MW AF Arce, Hector G. Borkin, Michelle A. Goodman, Alyssa A. Pineda, Jaime E. Halle, Michael W. TI THE COMPLETE SURVEY OF OUTFLOWS IN PERSEUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (Perseus); ISM: jets and outflows; ISM: kinematics and dynamics; stars: formation; turbulence ID STAR-FORMING REGIONS; HERBIG-HARO OBJECTS; VELOCITY MOLECULAR OUTFLOWS; SMALL-SCALE STRUCTURE; DARK CLOUD BARNARD-5; EMBEDDED YOUNG STARS; DEEP IMAGING SURVEYS; SPITZER C2D SURVEY; NGC 1333; MULTIPLE OUTFLOWS AB We present a study on the impact of molecular outflows in the Perseus molecular cloud complex using the COMPLETE Survey large-scale (12)CO(1-0) and (13)CO(1-0) maps. We used three-dimensional isosurface models generated in right ascension-declination-velocity space to visualize the maps. This rendering of the molecular line data allowed for a rapid and efficient way to search for molecular outflows over a large (similar to 16 deg(2)) area. Our outflow-searching technique detected previously known molecular outflows as well as new candidate outflows. Most of these new outflow-related high-velocity features lie in regions that have been poorly studied before. These new outflow candidates more than double the amount of outflow mass, momentum, and kinetic energy in the Perseus cloud complex. Our results indicate that outflows have significant impact on the environment immediately surrounding localized regions of active star formation, but lack the energy needed to feed the observed turbulence in the entire Perseus complex. This implies that other energy sources, in addition to protostellar outflows, are responsible for turbulence on a global cloud scale in Perseus. We studied the impact of outflows in six regions with active star formation within Perseus of sizes in the range of 1-4pc. We find that outflows have enough power to maintain the turbulence in these regions and enough momentum to disperse and unbind some mass from them. We found no correlation between outflow strength and star formation efficiency (SFE) for the six different regions we studied, contrary to results of recent numerical simulations. The low fraction of gas that potentially could be ejected due to outflows suggests that additional mechanisms other than cloud dispersal by outflows are needed to explain low SFEs in clusters. C1 [Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Borkin, Michelle A.] Harvard Univ, Sch Engn & Appl Sci, Cambridge, MA 02138 USA. [Goodman, Alyssa A.; Pineda, Jaime E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Halle, Michael W.] Brigham & Womens Hosp, Dept Radiol, Surg Planning Lab, Boston, MA 02115 USA. [Halle, Michael W.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. RP Arce, HG (reprint author), Yale Univ, Dept Astron, POB 208101, New Haven, CT 06520 USA. EM hector.arce@yale.edu RI Pineda, Jaime/J-7405-2013; Goodman, Alyssa/A-6007-2010 OI Pineda, Jaime/0000-0002-3972-1978; Goodman, Alyssa/0000-0003-1312-0477 NR 120 TC 71 Z9 71 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 1170 EP 1190 DI 10.1088/0004-637X/715/2/1170 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100036 ER PT J AU Rahoui, F Chaty, S Rodriguez, J Fuchs, Y Mirabel, IF Pooley, GG AF Rahoui, F. Chaty, S. Rodriguez, J. Fuchs, Y. Mirabel, I. F. Pooley, G. G. TI LONG-TERM MULTI-WAVELENGTH STUDIES OF GRS 1915+105. I. A HIGH-ENERGY AND MID-INFRARED FOCUS WITH RXTE/INTEGRAL AND SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; binaries: close; dust, extinction; infrared: stars; stars: individual (GRS 1915+105); X-rays: binaries ID HERBIG AE/BE STARS; X-RAY BINARIES; POLYCYCLIC AROMATIC-HYDROCARBONS; MAGNETIC CATACLYSMIC VARIABLES; SPACE-TELESCOPE OBSERVATIONS; IRRADIATED ACCRETION DISKS; IR EMISSION FEATURES; BLACK-HOLE BINARIES; MU-M; SUPERLUMINAL SOURCE AB To date, mid-infrared properties of Galactic black hole binaries have barely been investigated in the framework of multi-wavelength campaigns. Yet, studies in this spectral domain are crucial to get complementary information on the presence of dust and/or on the physical processes such as dust heating and thermal bremsstrahlung. Here, we report a long-term multi-wavelength study of the microquasar GRS 1915+105. On the one hand, we aimed at understanding the origins of the mid-infrared emission, and on the other hand, at searching for correlation with the high-energy and/or radio activities. We observed the source at several epochs between 2004 and 2006 with the photometer IRAC and spectrometer IRS, both mounted on the Spitzer Space Telescope. When available, we completed our set of data with quasi-simultaneous RXTE/INTEGRAL high-energy and/or Ryle radio observations from public archives. We then studied themid-infrared environment and activities of GRS 1915+105 through spectral analysis and broadband fitting of its radio to X-ray spectral energy distributions. We detected polycyclic aromatic hydrocarbon molecules in all but one IRS spectra of GRS 1915+105 which unambiguously proves the presence of a dust component, likely photoionized by the high-energy emission. We also argue that this dust is distributed in a disk-like structure heated by the companion star, as observed in some Herbig Ae/Be and isolated cool giant stars. Moreover, we show that some of the soft X-ray emission emanating from the inner regions of the accretion disk is reprocessed and thermalized in the outer part. This leads to a mid-infrared excess that is very likely correlated to the soft X-ray emission. We exclude thermal bremsstrahlung as contributing significantly in this spectral domain. C1 [Rahoui, F.] Univ Paris 07, CNRS, CEA, Observ Paris, F-75205 Paris 13, France. [Mirabel, I. F.] Consejo Nacl Invest Cient & Tecn, Inst Astron & Fis Espacio, RA-1033 Buenos Aires, DF, Argentina. [Rahoui, F.; Chaty, S.; Rodriguez, J.; Fuchs, Y.; Mirabel, I. F.] Univ Paris Diderot, CNRS, CEA, Lab AIM,DSM,Irfu Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Pooley, G. G.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. RP Rahoui, F (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM frahoui@cfa.harvard.edu OI Rodriguez, Jerome/0000-0002-4151-4468; Chaty, Sylvain/0000-0002-5769-8601 FU European Commission [ITN 215212]; Centre National d'Etudes Spatiales (CNES) FX J.R. acknowledges partial funding by the European Commission under contract ITN 215212/Black Hole Universe. This work was supported by the Centre National d'Etudes Spatiales (CNES), based on observations obtained through MINE-the Multi-wavelength INTEGRAL NEtwork. This research has made use of NASA's Astrophysics Data System, of the SIMBAD and VizieR databases operated at CDS, Strasbourg, France, of products from the US Naval Observatory catalogues, of products from the Two Micron All Sky Survey as well as products from the Galactic Legacy Infrared MidPlane Survey Extraordinaire, which is a Spitzer Space Telescope Legacy Science Program. NR 99 TC 16 Z9 16 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 1191 EP 1202 DI 10.1088/0004-637X/715/2/1191 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100037 ER PT J AU McArthur, BE Benedict, GF Barnes, R Martioli, E Korzennik, S Nelan, E Butler, RP AF McArthur, Barbara E. Benedict, G. Fritz. Barnes, Rory Martioli, Eder Korzennik, Sylvain Nelan, Ed Butler, R. Paul TI NEW OBSERVATIONAL CONSTRAINTS ON THE nu ANDROMEDAE SYSTEM WITH DATA FROM THE HUBBLE SPACE TELESCOPE AND HOBBY-EBERLY TELESCOPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; planetary systems; planets and satellites: dynamical evolution and stability; planets and satellites: fundamental parameters ID PLANET-PLANET SCATTERING; EXOPLANET HOST STARS; ECCENTRIC EXTRASOLAR PLANETS; PRECISION RADIAL-VELOCITIES; UPSILON-ANDROMEDAE; V-ANDROMEDAE; COOL STARS; SPECTROSCOPIC BINARIES; FUNDAMENTAL PARAMETERS; EFFECTIVE TEMPERATURES AB We have used high-cadence radial velocity (RV) measurements from the Hobby-Eberly Telescope with existing velocities from the Lick, Elodie, Harlan J. Smith, and Whipple 60 '' telescopes combined with astrometric data from the Hubble Space Telescope Fine Guidance Sensors to refine the orbital parameters and determine the orbital inclinations and position angles of the ascending node of components v And A c and d. With these inclinations and using M(*) = 1.31M(circle dot) as a primary mass, we determine the actual masses of two of the companions: And A c is 13.98+ 2.3 -5.3 MJUP, and. And A d is 10.25(-3.3)(+0.7) M(JUP). These measurements represent the first astrometric determination of mutual inclination between objects in an extrasolar planetary system, which we find to be 29 degrees.9 +/- 1 degrees. The combined RV measurements also reveal a long-period trend indicating a fourth planet in the system. We investigate the dynamic stability of this system and analyze regions of stability, which suggest a probable mass of v And A b. Finally, our parallaxes confirm that v And B is a stellar companion of v And A. C1 [McArthur, Barbara E.; Benedict, G. Fritz.; Martioli, Eder] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Barnes, Rory] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Martioli, Eder] Inst Nacl Pesquisas Espaciais, Div Astrofis, Sao Jose Dos Campos, SP, Brazil. [Korzennik, Sylvain] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nelan, Ed] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Butler, R. Paul] Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP McArthur, BE (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM mca@astro.as.utexas.edu RI Butler, Robert/B-1125-2009 NR 98 TC 53 Z9 53 U1 1 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 1203 EP 1220 DI 10.1088/0004-637X/715/2/1203 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100038 ER PT J AU Chen, XP Arce, HG Zhang, QZ Bourke, TL Launhardt, R Schmalzl, M Henning, T AF Chen, Xuepeng Arce, Hector G. Zhang, Qizhou Bourke, Tyler L. Launhardt, Ralf Schmalzl, Markus Henning, Thomas TI L1448 IRS2E: A CANDIDATE FIRST HYDROSTATIC CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (L1448, L1448IRS2, L1448IRS2E); ISM: jets and outflows; stars: formation ID SPITZER C2D SURVEY; RADIATION HYDRODYNAMIC MODEL; NEARBY DENSE CORES; STAR-FORMATION; PROTOSTELLAR COLLAPSE; YOUNGEST PROTOSTARS; INTERSTELLAR CLOUDS; MOLECULAR CLOUD; EMBEDDED SOURCE; PERSEUS AB Intermediate between the prestellar and Class 0 protostellar phases, the first core is a quasi-equilibrium hydrostatic object with a short lifetime and an extremely low luminosity. Recent magnetohydrodynamic (MHD) simulations suggest that the first core can even drive a molecular outflow before the formation of the second core (i.e., protostar). Using the Submillimeter Array and the Spitzer Space Telescope, we present high angular resolution observations toward the embedded dense core IRS2E in L1448. We find that source L1448 IRS2E is not visible in the sensitive Spitzer infrared images (at wavelengths from 3.6 to 70 mu m) and has weak (sub-) millimeter dust continuum emission. Consequently, this source has an extremely low bolometric luminosity (<0.1 L(circle dot)). Infrared and (sub-) millimeter observations clearly show an outflow emanating from this source; L1448 IRS2E represents thus far the lowest luminosity source known to be driving a molecular outflow. Comparisons with prestellar cores and Class 0 protostars suggest that L1448 IRS2E is more evolved than prestellar cores but less evolved than Class 0 protostars, i.e., at a stage intermediate between prestellar cores and Class 0 protostars. All these results are consistent with the theoretical predictions of the radiative/MHD simulations, making L1448 IRS2E the most promising candidate of the first hydrostatic core revealed so far. C1 [Chen, Xuepeng; Arce, Hector G.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Zhang, Qizhou; Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Launhardt, Ralf; Schmalzl, Markus; Henning, Thomas] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Chen, XP (reprint author), Yale Univ, Dept Astron, Box 208101, New Haven, CT 06520 USA. OI Zhang, Qizhou/0000-0003-2384-6589 NR 53 TC 60 Z9 60 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 1344 EP 1351 DI 10.1088/0004-637X/715/2/1344 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100049 ER PT J AU Masters, KL Jordan, A Cote, P Ferrarese, L Blakeslee, JP Infante, L Peng, EW Mei, S West, MJ AF Masters, Karen L. Jordan, Andres Cote, Patrick Ferrarese, Laura Blakeslee, John P. Infante, Leopoldo Peng, Eric W. Mei, Simona West, Michael J. TI THE ADVANCED CAMERA FOR SURVEYS FORNAX CLUSTER SURVEY. VII. HALF-LIGHT RADII OF GLOBULAR CLUSTERS IN EARLY-TYPE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: star clusters: general; globular clusters: general ID ACS-VIRGO-CLUSTER; STRUCTURAL PARAMETERS; FUNDAMENTAL PLANE; ELLIPTIC GALAXY; SIZE DIFFERENCE; DWARF GALAXIES; LOCAL GROUP; SYSTEMS; DISTANCE; EVOLUTION AB We measure the half-light radii of globular clusters (GCs) in 43 galaxies from the Advanced Camera for Surveys (ACS) Fornax Cluster Survey. We use these data to extend previous work in which the environmental dependencies of the half-light radii of GCs in early-type galaxies in the ACS Virgo Cluster Survey were studied, and a corrected mean half-light radius (corrected for the observed environmental trends) was suggested as a reliable distance indicator. This work both increases the sample size for the study of the environmental dependencies, and adds leverage to the study of the corrected half-light radius as a possible distance indicator (since Fornax lies at a larger distance than the Virgo cluster). We study the environmental dependencies of the size of GCs using both a Principal Component Analysis as well as two-dimensional scaling relations. We largely confirm the environmental dependencies shown in Jordan et al., but find evidence that there is a residual correlation in the mean half-light radius of GC systems with galaxy magnitude, and subtle differences in the other correlations-so there may not be a universal correction for the half-light radii of lower luminosity galaxy GC systems. The main factor determining the size of a GC in an early-type galaxy is the GC color. Red GCs have < r(h)> = 2.8 +/- 0.3 pc, while blue GCs have < r(h)> = 3.4 +/- 0.3 pc. We show that for bright early-type galaxies (M(B) < -19 mag), the uncorrected mean half-light radius of the GC system is by itself an excellent distance indicator (with error similar to 11%), having the potential to reach cosmologically interesting distances in the era of high angular resolution adaptive optics on large optical telescopes. C1 [Masters, Karen L.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Masters, Karen L.; Jordan, Andres] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jordan, Andres; Infante, Leopoldo] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 7820436, Chile. [Cote, Patrick; Ferrarese, Laura; Blakeslee, John P.] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. [Peng, Eric W.] Peking Univ, Dept Astron, Beijing 100871, Peoples R China. [Peng, Eric W.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Mei, Simona] Observ Paris, Sect Meudon, GEPI, F-92195 Meudon, France. [West, Michael J.] ESO, Santiago, Chile. RP Masters, KL (reprint author), Univ Portsmouth, Inst Cosmol & Gravitat, Dennis Sciama Bldg,Burnaby Rd, Portsmouth PO1 3FX, Hants, England. EM karen.masters@port.ac.uk OI Jordan, Andres/0000-0002-5389-3944; Masters, Karen/0000-0003-0846-9578; Blakeslee, John/0000-0002-5213-3548 FU Space Telescope Science Institute [GO-10217, GO-9401]; Peter and Patricia Gruber Foundation [2008]; University of Portsmouth; Chilean Center of Excellence in Astrophysics and Associated Technologies [PFB-06]; Chilean Center for Astrophysics [FONDAP 15010003]; MIDEPLAN ICM Nucleus [P07-021F] FX Support for programs GO-10217 and GO-9401 was provided through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. K. L. M. acknowledges funding from the Peter and Patricia Gruber Foundation as the 2008 Peter and Patricia Gruber Foundation International Astronomical Union Fellow, and from the University of Portsmouth. A.J. and L. I. acknowledge support from the Chilean Center of Excellence in Astrophysics and Associated Technologies PFB-06, and from the Chilean Center for Astrophysics FONDAP 15010003. A.J. acknowledges additional support from MIDEPLAN ICM Nucleus P07-021F. NR 45 TC 36 Z9 36 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 1 PY 2010 VL 715 IS 2 BP 1419 EP 1437 DI 10.1088/0004-637X/715/2/1419 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 595VR UT WOS:000277642100056 ER PT J AU Lee, JJ Raymond, JC Park, S Blair, WP Ghavamian, P Winkler, PF Korreck, K AF Lee, Jae-Joon Raymond, John C. Park, Sangwook Blair, William P. Ghavamian, Parviz Winkler, P. F. Korreck, Kelly TI RESOLVED SHOCK STRUCTURE OF THE BALMER-DOMINATED FILAMENTS IN TYCHO'S SUPERNOVA REMNANT: COSMIC-RAY PRECURSOR? SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (G120.1+1.4); ISM: supernova remnants- shock waves ID HIGH-RESOLUTION SPECTROSCOPY; LARGE-MAGELLANIC-CLOUD; CYGNUS LOOP; OPTICAL-EMISSION; DEM L71; ACCELERATION; NOVA; EXPANSION; ORIGIN; RCW-86 AB We report on the results from H alpha imaging observations of the eastern limb of Tycho's supernova remnant (SN1572) using the Wide Field Planetary Camera 2 on the Hubble Space Telescope. We resolve the detailed structure of the fast, collisionless shock wave into a delicate structure of nearly edge-on filaments. We find a gradual increase of H alpha intensity just ahead of the shock front, which we interpret as emission from the thin (similar to 1 '') shock precursor. We find that a significant amount of the H alpha emission comes from the precursor and that this could affect the amount of temperature equilibration derived from the observed flux ratio of the broad and narrow H alpha components. The observed H alpha emission profiles are fit using simple precursor models, and we discuss the relevant parameters. We suggest that the precursor is likely due to cosmic rays and discuss the efficiency of cosmic-ray acceleration at this position. C1 [Lee, Jae-Joon; Park, Sangwook] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Raymond, John C.; Korreck, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Ghavamian, Parviz] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Winkler, P. F.] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. RP Lee, JJ (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. EM lee@astro.psu.edu FU STScI [GO-11184.01-A-R] FX We thank the anonymous referee for valuable comments. This research was supported by STScI grant GO-11184.01-A-R to the Smithsonian Astrophysical Observatory. NR 21 TC 20 Z9 20 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2010 VL 715 IS 2 BP L146 EP L149 DI 10.1088/2041-8205/715/2/L146 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608NU UT WOS:000278591800018 ER PT J AU Rines, K Geller, MJ Diaferio, A AF Rines, Kenneth Geller, Margaret J. Diaferio, Antonaldo TI COMPARISON OF HECTOSPEC VIRIAL MASSES WITH SUNYAEV-ZEL'DOVICH EFFECT MEASUREMENTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmology: observations; galaxies: clusters: individual; galaxies: kinematics and dynamics ID X-RAY MEASUREMENTS; DIGITAL SKY SURVEY; LUMINOUS GALAXY CLUSTERS; POWER SPECTRUM; DARK ENERGY; CONSTRAINTS; NORMALIZATION; COSMOLOGY; PROFILES; CATALOG AB We present the first comparison of virial masses of galaxy clusters with their Sunyaev-Zel'dovich Effect (SZE) signals. We study 15 clusters from the Hectospec Cluster Survey (HeCS) with MMT/Hectospec spectroscopy and published SZE signals. We measure virial masses of these clusters from an average of 90 member redshifts inside the radius r(100). The virial masses of the clusters are strongly correlated with their SZE signals (at the 99% confidence level using a Spearman rank-sum test). This correlation suggests that Y(SZ) can be used as a measure of virial mass. Simulations predict a power-law scaling of Y(SZ) proportional to M(200)(alpha) with alpha approximate to 1.6. Observationally, we find alpha = 1.11 +/- 0.16, significantly shallower (given the formal uncertainty) than the theoretical prediction. However, the selection function of our sample is unknown and a bias against less massive clusters cannot be excluded (such a selection bias could artificially flatten the slope). Moreover, our sample indicates that the relation between velocity dispersion (or virial mass estimate) and SZE signal has significant intrinsic scatter, comparable to the range of our current sample. More detailed studies of scaling relations are therefore needed to derive a robust determination of the relation between cluster mass and SZE. C1 [Rines, Kenneth] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. [Rines, Kenneth; Geller, Margaret J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Diaferio, Antonaldo] Univ Turin, Dipartimento Fis Gen Amedeo Avogadro, Turin, Italy. [Diaferio, Antonaldo] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. RP Rines, K (reprint author), Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. EM kenneth.rines@wwu.edu FU INFN [PD51] FX We thank Stefano Andreon for fruitful discussions about fitting scaling relations with measurement errors and intrinsic scatter in both quantities. A. D. gratefully acknowledges partial support from INFN grant PD51. We thank Susan Tokarz for reducing the spectroscopic data and Perry Berlind and Mike Calkins for assisting with the observations. NR 40 TC 14 Z9 14 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2010 VL 715 IS 2 BP L180 EP L184 DI 10.1088/2041-8205/715/2/L180 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608NU UT WOS:000278591800025 ER PT J AU van Spaandonk, L Steeghs, D Marsh, TR Parsons, SG AF van Spaandonk, L. Steeghs, D. Marsh, T. R. Parsons, S. G. TI THE MASS OF THE WHITE DWARF IN GW LIBRA SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: spectroscopic; novae, cataclysmic variables; stars: individual (GW Lib) ID VARIABLE WZ-SAGITTAE; CATACLYSMIC VARIABLES; U-GEMINORUM; SPECTROSCOPY; SPECTROGRAPH; SUPERHUMPS; TELESCOPE; BINARIES; PERIOD; NOVAE AB We report a mass and rotational broadening (v sin i) for the pulsating white dwarf (WD) component of the WZ Sge type Dwarf Nova GW Lib based on high-resolution Very Large Telescope spectroscopy that resolves the Mg II 4481 angstrom absorption feature. Its gravitational redshift combined with WD mass-radius models provides us with a direct measurement of the WD mass of M-1 = 0.84 +/- 0.02 M-circle dot. The line is clearly resolved and if associated with rotational broadening gives v sin i = 87.0 +/- 3.4 km s(-1), equivalent to a spin period of 97 +/- 12 s. C1 [van Spaandonk, L.; Steeghs, D.; Marsh, T. R.; Parsons, S. G.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Steeghs, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP van Spaandonk, L (reprint author), Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. EM van-spaandonk@warwick.ac.uk RI Steeghs, Danny/C-5468-2009 OI Steeghs, Danny/0000-0003-0771-4746 FU STFC FX D. S. acknowledges an STFC Advanced Fellowship. T. R. M. was supported by an STFC Rolling Grant. Based on observations made with ESO Telescopes at the Paranal Observatory under program ID 69.D-0591. NR 24 TC 9 Z9 9 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 1 PY 2010 VL 715 IS 2 BP L109 EP L112 DI 10.1088/2041-8205/715/2/L109 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 608NU UT WOS:000278591800010 ER PT J AU Wu, JW Evans, NJ Shirley, YL Knez, C AF Wu, Jingwen Evans, Neal J., II Shirley, Yancy L. Knez, Claudia TI THE PROPERTIES OF MASSIVE, DENSE CLUMPS: MAPPING SURVEYS OF HCN AND CS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: formation; ISM: clouds; ISM: molecules; stars: formation; submillimeter: ISM ID STAR-FORMATION RATE; LUMINOUS INFRARED GALAXIES; MOLECULAR CLOUD CORES; COMPACT HII-REGIONS; H-II REGIONS; PROTOSTELLAR CANDIDATES; PHYSICAL CONDITIONS; CONTINUUM OBSERVATIONS; DUST CONTINUUM; OUTER GALAXY AB We have mapped over 50 massive, dense clumps with four dense gas tracers: HCN J = 1-0 and 3-2; and CS J = 2-1 and 7-6 transitions. Spectral lines of optically thin H(13)CN 3-2 and C(34)S 5-4 were also obtained toward the map centers. These maps usually demonstrate single well-peaked distributions at our resolution, even with higher J transitions. The size, virial mass, surface density, and mean volume density within a well-defined angular size ( FWHM) were calculated from the contour maps for each transition. We found that transitions with higher effective density usually trace the more compact, inner part of the clumps but have larger linewidths, leading to an inverse linewidth-size relation using different tracers. The mean surface densities are 0.29, 0.33, 0.78, 1.09 g cm(-2) within FWHM contours of CS 2-1, HCN 1-0, HCN 3-2, and CS 7-6, respectively. We find no correlation of L(IR) with surface density and a possible inverse correlation with mean volume density, contrary to some theoretical expectations. Molecular line luminosities L'(mol) were derived for each transition. We see no evidence in the data for the relation between L'(mol) and mean density posited by modelers. The correlation between L'(mol) and the virial mass is roughly linear for each dense gas tracer. No obvious correlation was found between the line luminosity ratio and infrared luminosity, bolometric temperature, or the L(IR)/M(Vir) ratio. A nearly linear correlation was found between the infrared luminosity and the line luminosity of all dense gas tracers for these massive, dense clumps, with a lower cutoff in luminosity at L(IR) = 10(4.5) L(circle dot). The L(IR)-L'(HCN1-0) correlation agrees well with the one found in galaxies. These correlations indicate a constant star formation rate per unit mass from the scale of dense clumps to that of distant galaxies when the mass is measured for dense gas. These results support the suggestion that starburst galaxies may be understood as having a large fraction of gas in dense clumps. C1 [Wu, Jingwen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wu, Jingwen] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Evans, Neal J., II] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Shirley, Yancy L.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Knez, Claudia] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Wu, JW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS78, Cambridge, MA 02138 USA. EM jwu@cfa.harvard.edu; nje@astro.as.utexas.edu; yshirley@as.arizona.edu FU Submillimeter Array of the Smithsonian Observatory; NSF [AST-0607793]; McDonald Observatory FX We thank D. Narayanan and M. Krumholz for lively discussions that illuminated their models. J.W. thanks the postdoctoral fellowship support from the Submillimeter Array of the Smithsonian Observatory while completing this work. This work was supported in part by NSF Grant AST-0607793 and by McDonald Observatory. NR 99 TC 91 Z9 91 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2010 VL 188 IS 2 BP 313 EP 357 DI 10.1088/0067-0049/188/2/313 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613HG UT WOS:000278969400001 ER PT J AU Nichols, JS Henden, AA Huenemoerder, DP Lauer, JL Martin, E Morgan, DL Sundheim, BA AF Nichols, Joy S. Henden, Arne A. Huenemoerder, David P. Lauer, Jennifer L. Martin, Eric Morgan, Douglas L. Sundheim, Beth A. TI THE CHANDRA VARIABLE GUIDE STAR CATALOG SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; methods: observational; space vehicles: instruments; stars: statistics; stars: variables: general ID INITIAL PERFORMANCE; PHOTOMETRY; MISSION AB Variable stars have been identified among the optical-wavelength light curves of guide stars used for pointing control of the Chandra X-ray Observatory. We present a catalog of these variable stars along with their light curves and ancillary data. Variability was detected to a lower limit of 0.02 mag amplitude in the 4000-10000 angstrom range using the photometrically stable Aspect Camera on board the Chandra spacecraft. The Chandra Variable Guide Star Catalog (VGUIDE) contains 827 stars, of which 586 are classified as definitely variable and 241 are identified as possibly variable. Of the 586 definite variable stars, we believe 319 are new variable star identifications. Types of variables in the catalog include eclipsing binaries, pulsating stars, and rotating stars. The variability was detected during the course of normal verification of each Chandra pointing and results from analysis of over 75,000 guide star light curves from the Chandra mission. The VGUIDE catalog represents data from only about 9 years of the Chandra mission. Future releases of VGUIDE will include newly identified variable guide stars as the mission proceeds. An important advantage of the use of space data to identify and analyze variable stars is the relatively long observations that are available. The Chandra orbit allows for observations up to 2 days in length. Also, guide stars were often used multiple times for Chandra observations, so many of the stars in the VGUIDE catalog have multiple light curves available from various times in the mission. The catalog is presented as both online data associated with this paper and as a public Web interface. Light curves with data at the instrumental time resolution of about 2 s, overplotted with the data binned at 1 ks, can be viewed on the public Web interface and downloaded for further analysis. VGUIDE is a unique project using data collected during the mission that would otherwise be ignored. The stars available for use as Chandra guide stars are generally 6-11 mag and are commonly spectral types A and later. Due to the selection of guide stars entirely for positional convenience, this catalog avoids the possible bias of searching for variability in objects where it is to be expected. Statistics of variability compared to spectral type indicate the expected dominance of A-F stars as pulsators. Eclipsing binaries are consistently 20%-30% of the detected variables across all spectral types. C1 [Nichols, Joy S.; Lauer, Jennifer L.; Morgan, Douglas L.; Sundheim, Beth A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Henden, Arne A.] Amer Assoc Variable Star Observers, Cambridge, MA 02138 USA. [Huenemoerder, David P.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Martin, Eric] Northrop Grumman Aerosp Syst, Redondo Beach, CA 90278 USA. RP Nichols, JS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jnichols@cfa.harvard.edu FU NASA through the Smithsonian Astrophysical Observatory (SAO) [NAS 8-03060, SV3-73016] FX Chandra is operated by the Smithsonian Astrophysical Observatory under NASA contract NAS 8-03060. This work was supported by NASA through the Smithsonian Astrophysical Observatory (SAO) contracts NAS 8-03060 and SV3-73016 for the Chandra X-Ray Center and Science Instruments. NR 19 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2010 VL 188 IS 2 BP 473 EP 487 DI 10.1088/0067-0049/188/2/473 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613HG UT WOS:000278969400007 ER PT J AU Cotton, WD Ragland, S Pluzhnik, EA Danchi, WC Traub, WA Willson, LA Lacasse, MG AF Cotton, W. D. Ragland, S. Pluzhnik, E. A. Danchi, W. C. Traub, W. A. Willson, L. A. Lacasse, M. G. TI SiO MASERS IN ASYMMETRIC MIRAS. IV. chi CYGNI, R AQUILAE, R LEO MINORIS, RU HERCULIS, U HERCULIS, AND U ORIONIS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE radio lines: stars; stars: AGB and post-AGB; stars: atmospheres ID LATE-TYPE STARS; GIANT BRANCH STARS; VARIABLE-STARS; WATER MASERS; RADIO PHOTOSPHERES; ANGULAR DIAMETERS; VLBA OBSERVATIONS; EVOLVED STARS; STELLAR IMAGE; IK TAURI AB This is the fourth paper in a series of multi-epoch observations at 7 mm wavelength of the SiO masers in several asymptotic giant branch stars from a sample of Mira variable stars showing evidence of asymmetric structure in the infrared. These stars have been observed interferometrically in the infrared by IOTA and with VLBA measurements of the SiO masers. In this paper, we present the observations of chi Cygni (chi Cyg), R Aquilae (R Aql), R Leo Minoris (R LMi), RU Herculis (RU Her), U Herculis (U Her), and U Orionis (U Ori). Several radial features with velocity gradients were observed, all with velocities close to systemic furthest from the star and redshifted closer to the stellar surface. Systemic velocities are estimated for several of the stars. No compelling evidence of asymmetry is seen in the maser distributions. All maser rings are approximately twice the near-IR uniform disk diameter and are comparable in size to the extended molecular envelope when such measurements are available. C1 [Cotton, W. D.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Ragland, S.] WM Keck Observ, Kamuela, HI 96743 USA. [Pluzhnik, E. A.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Danchi, W. C.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Traub, W. A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Willson, L. A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50014 USA. [Lacasse, M. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cotton, WD (reprint author), Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA. EM bcotton@nrao.edu FU NSF [AST-0456047] FX We acknowledge support from NSF of the IOTA observations through grant AST-0456047. The authors thank the anonymous referee for comments leading to an improved paper. NR 50 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUN PY 2010 VL 188 IS 2 BP 506 EP 525 DI 10.1088/0067-0049/188/2/506 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 613HG UT WOS:000278969400010 ER PT J AU Duncan, BN Yoshida, Y Olson, JR Sillman, S Martin, RV Lamsal, L Hu, YT Pickering, KE Retscher, C Allen, DJ Crawford, JH AF Duncan, Bryan N. Yoshida, Yasuko Olson, Jennifer R. Sillman, Sanford Martin, Randall V. Lamsal, Lok Hu, Yongtao Pickering, Kenneth E. Retscher, Christian Allen, Dale J. Crawford, James H. TI Application of OMI observations to a space-based indicator of NOx and VOC controls on surface ozone formation SO ATMOSPHERIC ENVIRONMENT LA English DT Article DE Surface ozone; Air quality indicator; OMI; HCHO; NO2 ID EASTERN UNITED-STATES; ISOPRENE EMISSIONS; NITROGEN-OXIDES; AIR-QUALITY; PRECURSOR RELATIONSHIPS; NEW-YORK; URBAN; PHOTOCHEMISTRY; SENSITIVITY; REDUCTIONS AB We investigated variations in the relative sensitivity of surface ozone formation in summer to precursor species concentrations of volatile organic compounds (VOCs) and nitrogen oxides (NOx) as inferred from the ratio of the tropospheric columns of formaldehyde to nitrogen dioxide (the "Ratio") from the Aura Ozone Monitoring Instrument (OMI). Our modeling study suggests that ozone formation decreases with reductions in VOCs at Ratios <1 and NOx at Ratios >2; both NOx and VOC reductions may decrease ozone formation for Ratios between 1 and 2. Using this criteria, the OMI data indicate that ozone formation became: 1. more sensitive to NOx over most of the United States from 2005 to 2007 because of the substantial decrease in NOx emissions, primarily from stationary sources, and the concomitant decrease in the tropospheric column of NO2, and 2. more sensitive to NOx with increasing temperature, in part because emissions of highly reactive, biogenic isoprene increase with temperature, thus increasing the total VOC reactivity. In cities with relatively low isoprene emissions (e.g., Chicago), the data clearly indicate that ozone formation became more sensitive to NOx from 2005 to 2007. In cities with relatively high isoprene emissions (e.g., Atlanta), we found that the increase in the Ratio due to decreasing NOx emissions was not obvious as this signal was convolved with variations in the Ratio associated with the temperature dependence of isoprene emissions and, consequently, the formaldehyde concentration. Published by Elsevier Ltd. C1 [Duncan, Bryan N.; Yoshida, Yasuko; Pickering, Kenneth E.; Retscher, Christian] NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. [Yoshida, Yasuko; Retscher, Christian] Univ Maryland, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21201 USA. [Olson, Jennifer R.; Crawford, James H.] NASA, Langley Res Ctr, Chem & Dynam Branch, Hampton, VA 23665 USA. [Sillman, Sanford] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Martin, Randall V.; Lamsal, Lok] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hu, Yongtao] Georgia Inst Technol, Sch Civil & Environm Engn, Atlanta, GA 30332 USA. [Allen, Dale J.] Univ Maryland, Dept Atmospher & Ocean Sci, College Pk, MD 20742 USA. RP Duncan, BN (reprint author), NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. EM Bryan.N.Duncan@nasa.gov RI Duncan, Bryan/A-5962-2011; Pickering, Kenneth/E-6274-2012; Lamsal, Lok/G-4781-2012; Pfister, Gabriele/A-9349-2008; Crawford, James/L-6632-2013; Martin, Randall/C-1205-2014; Hu, Yongtao/H-7543-2016; Allen, Dale/F-7168-2010; OI Crawford, James/0000-0002-6982-0934; Martin, Randall/0000-0003-2632-8402; Hu, Yongtao/0000-0002-5161-0592; Allen, Dale/0000-0003-3305-9669; Sillman, Sanford/0000-0001-6250-1191 FU NASA FX This work was supported by the NASA's Earth Science Research Program. NR 55 TC 47 Z9 51 U1 10 U2 88 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1352-2310 EI 1873-2844 J9 ATMOS ENVIRON JI Atmos. Environ. PD JUN PY 2010 VL 44 IS 18 BP 2213 EP 2223 DI 10.1016/j.atmosenv.2010.03.010 PG 11 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 613ON UT WOS:000278988700006 ER PT J AU Forman, P AF Forman, Paul TI (Re)cognizing Postmodernity: Helps for Historians - of Science Especially SO BERICHTE ZUR WISSENSCHAFTSGESCHICHTE LA English DT Article DE Barry Barnes; entrepreneur; method; modernity; neoliberal; personhood; resource; technoscience; transgression; voluntarism AB (Re)cognizing Postmodernity: Helps for Historians - of Science Especially. Postmodernity, a historical era demarcated from modernity by a broad reversal in cultural presuppositions, is distinguished from postmodernism, an intellectual posture adopted by self-identified postmodernists early in postmodernity. Two principal features of postmodernity are addressed: first, the downgrading of science and the upgrading of technology in cultural rank - on which postmodernity and postmodernism are in accord; second, the displacement of the methodical, disinterested scientist, modernity's beau ideal, not by a fragmented subject as postmodernism claims, but by the single-minded entrepreneur, resourcefully pursuing his self-interest in disregard of all rules. The reversal in rank and role as between science and technology, setting in circa 1980, is a marker of the transition from modernity to postmodernity. That reversal is to be cognized primarily as rejection of rule-following, of proceeding methodically - 'methodism' being the cultural perspective that uniquely distinguished modernity - but also as rejection of disinterestedness, the quality of mind especially highly esteemed in modernity. Postmodernity is constituted by this transvaluation of values, whose well-spring is the egocentric, transgressive (hence 'risk taking'), postmodern personality and its anti-social presumptions regarding personhood. Within the history of science itself there has been since circa 1980 a corresponding turn of scholarly attention away from science to technology, and a growing distaste for social perspectives, reflected, i.a., in the rejection of causalist 'influence' explanations in favor of voluntarist 'resource' explanations. C1 Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA. RP Forman, P (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20013 USA. EM formanp@si.edu NR 72 TC 18 Z9 19 U1 0 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0170-6233 J9 BER WISSGESCH JI Ber. Wissgesch. PD JUN PY 2010 VL 33 IS 2 BP 157 EP 175 DI 10.1002/bewi.201001464 PG 19 WC History & Philosophy Of Science SC History & Philosophy of Science GA 623CJ UT WOS:000279714900003 PM 20695412 ER PT J AU Adams, RMM Jones, TH Jeter, AW AF Adams, Rachelle M. M. Jones, Tappey H. Jeter, Andrew W. TI Male specific tyramides from three additional myrmicine genera SO BIOCHEMICAL SYSTEMATICS AND ECOLOGY LA English DT Article DE Tyramide; Megalomyrmex; Trachymyrmex; Cyphomyrmex; Male ants; Semiochemical ID ANTS C1 [Adams, Rachelle M. M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Adams, Rachelle M. M.] Smithsonian Inst, Natl Museum Nat Hist, Labs Analyt Biol, Washington, DC 20560 USA. [Jones, Tappey H.; Jeter, Andrew W.] Virginia Mil Inst, Dept Chem, Lexington, VA 24450 USA. RP Adams, RMM (reprint author), Univ Copenhagen, Dept Biol, Ctr Social Evolut, Univ Pk 15, DK-2100 Copenhagen O, Denmark. EM rmmadams@gmail.com; JonesTH@vmi.edu RI Adams, Rachelle/J-8846-2013 OI Adams, Rachelle/0000-0002-0918-9861 FU Organization of Tropical Biology/Smithsonian Mellon Foundation; Amazon Conservation Association; Society of Systematic Biologists; P.E.O. Scholar Award; National Science Foundation [DEB-0508698]; University of Texas; Smithsonian Tropical Research Institute, Panama; Amazon Explorama Lodge, Peru; La Selva Biological Station; El Ceibo Ranger Station, Costa Rica FX This work was supported by the Organization of Tropical Biology/Smithsonian Mellon Foundation, the Amazon Conservation Association, the Society of Systematic Biologists, a P.E.O. Scholar Award, the National Science Foundation DDIG program (DEB-0508698) and the University of Texas (Hartman Summer Merit Stipend) awarded to RMMA. For field research support, we are grateful to the Smithsonian Tropical Research Institute, Panama; Amazon Explorama Lodge, Peru; and La Selva Biological Station and El Ceibo Ranger Station, Costa Rica and the respective permitting agencies. We would also like to thank Steve A. Rehner, Ted R. Schultz, Jeffery Sossa-Calvo for ant specimens and Dr. H. M. Garraffo and Dr. T.F. Spande from the Laboratory of Bioorganic Chemistry NIDDK/NIH, Bethesda, MD for obtaining the high-resolution mass spectrum. NR 20 TC 1 Z9 1 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0305-1978 EI 1873-2925 J9 BIOCHEM SYST ECOL JI Biochem. Syst. Ecol. PD JUN PY 2010 VL 38 IS 3 BP 454 EP 456 DI 10.1016/j.bse.2010.03.008 PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 610DD UT WOS:000278709900029 ER PT J AU Martin, JL Cardoso, P Arechavaleta, M Borges, PAV Faria, BF Abreu, C Aguiar, AF Carvalho, JA Costa, AC Cunha, RT Fernandes, FM Gabriel, R Jardim, R Lobo, C Martins, AMF Oliveira, P Rodrigues, P Silva, L Teixeira, D Amorim, IR Homem, N Martins, B Martins, M Mendonca, E AF Martin, Jose L. Cardoso, Pedro Arechavaleta, Manuel Borges, Paulo A. V. Faria, Bernardo F. Abreu, Cristina Aguiar, Antonio F. Carvalho, Jose A. Costa, Ana C. Cunha, Regina T. Fernandes, Francisco M. Gabriel, Rosalina Jardim, Roberto Lobo, Carlos Martins, Antonio M. F. Oliveira, Paulo Rodrigues, Pedro Silva, Luis Teixeira, Dinarte Amorim, Isabel R. Homem, Nidia Martins, Berta Martins, Monica Mendonca, Enesima TI Using taxonomically unbiased criteria to prioritize resource allocation for oceanic island species conservation SO BIODIVERSITY AND CONSERVATION LA English DT Article DE Azores; Biodiversity management; Canary Islands; Conservation priority; Macaronesia; Madeira; Ranking criteria; Risk assessment; Threatened species ID TOP PREDATORS; PROTECTED AREAS; BIODIVERSITY; EXTINCTION; BIRDS; IRREPLACEABILITY; PATTERNS; AZORES; GOAL AB Oceanic islands have been the grand stage of documented extinctions. In view of limited resources, efficient prioritization is crucial to avoid the extinction of taxa. This work lists the top 100 management priority species for the European archipelagos of the Macaronesian region (Azores, Madeira and the Canary Islands), taking into account both their protection priority and their management feasibility. Bryophytes, vascular plants, molluscs, arthropods and vertebrates were scored by species experts following two sets of criteria: (i) protection priority, including ecological value, singularity, public institutions' management responsibilities and social value; (ii) management feasibility, including threats knowledge and control feasibility, external socio-economical support for management and biological recovery potential. Environmental managers weighted the same criteria according to their management importance. Final species scores were determined by the combination of both species valuation and criteria weighting. Vascular plants dominate the Top 100 list, followed by arthropods and vertebrates. The majority of listed taxa are endemic to one archipelago or even to a single island. The management feasibility criteria did not dictate that all taxa must be eminently endangered, as for most of the species it should be relatively easy to control threats. The main advantages of this process are the independent participation of scientists and conservation managers, the inclusion of criteria on both protection priority and management feasibility and the taxonomically unbiased nature of the process. This study provides a potentially useful biodiversity conservation tool for the Macaronesian archipelagos that could be readily implemented by the respective regional governments in future legislation. C1 [Cardoso, Pedro] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Oliveira, Paulo] Parque Nat Madeira CEM, P-9050251 Caminho Do Meio, Funchal, Portugal. [Costa, Ana C.; Cunha, Regina T.; Martins, Antonio M. F.; Rodrigues, Pedro; Silva, Luis; Martins, Monica] Univ Acores, Dept Biol, CIBIO Res Ctr Biodivers & Genet Resources, P-9501801 Ponta Delgada, Portugal. [Martin, Jose L.; Arechavaleta, Manuel] Ctr Planificac Ambiental, Serv Biodiversidad, Consejeria Medio Ambiente & Ordenac Terr, San Cristobal la Laguna, Santa Cruz De T, Spain. [Cardoso, Pedro; Borges, Paulo A. V.; Gabriel, Rosalina; Amorim, Isabel R.; Homem, Nidia; Martins, Berta; Mendonca, Enesima] Univ Acores, Dept Ciencias Agr, Azorean Biodivers Grp, CITAA, P-9701851 Terra Cha, Angra Do Herois, Portugal. [Faria, Bernardo F.; Teixeira, Dinarte] Secretaria Reg Ambiente & Recursos Nat, Direccao Reg Ambiente, P-9064506 Funchal, Portugal. [Abreu, Cristina] Univ Madeira, Dept Biol, CEM, P-9000390 Funchal, Portugal. [Aguiar, Antonio F.] Nucleo Entomol, Lab Agr Madeira, P-9135372 Camacha, Portugal. [Carvalho, Jose A.; Fernandes, Francisco M.; Jardim, Roberto; Lobo, Carlos] Jardim Bot Madeira, P-9064512 Caminho Do Meio, Funchal, Portugal. RP Cardoso, P (reprint author), Natl Museum Nat Hist, Smithsonian Inst, POB 37012,MRC 105,Room E-509, Washington, DC 20013 USA. EM pcardoso@ennor.org RI Amorim do Rosario, Isabel/P-5140-2015; Martins, Antonio/L-7932-2013; Borges, Paulo/B-2780-2008; Gabriel, Rosalina/F-1598-2013; Costa, Ana Cristina/L-8023-2013; Tristao da Cunha, Regina/M-3489-2013; Rodrigues, Pedro/L-6682-2014; Cardoso, Pedro/A-8820-2008 OI Silva, Luis/0000-0002-3434-6056; Amorim do Rosario, Isabel/0000-0001-6847-3320; Martins, Antonio/0000-0001-5358-8424; Borges, Paulo/0000-0002-8448-7623; Gabriel, Rosalina/0000-0002-3550-8010; Costa, Ana Cristina/0000-0002-0258-3460; Tristao da Cunha, Regina/0000-0003-4234-3223; Rodrigues, Pedro/0000-0002-2974-5909; Cardoso, Pedro/0000-0001-8119-9960 NR 55 TC 23 Z9 24 U1 2 U2 21 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0960-3115 J9 BIODIVERS CONSERV JI Biodivers. Conserv. PD JUN PY 2010 VL 19 IS 6 BP 1659 EP 1682 DI 10.1007/s10531-010-9795-z PG 24 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 592HH UT WOS:000277368600010 ER PT J AU Henry, JJ Collin, R Perry, KJ AF Henry, Jonathan J. Collin, Rachel Perry, Kimberly J. TI The Slipper Snail, Crepidula: An Emerging Lophotrochozoan Model System SO BIOLOGICAL BULLETIN LA English DT Article ID BITHYNIA-TENTACULATA PROSOBRANCHIA; GASTROPOD CREPIPATELLA-DILATATA; MOLLUSK PATELLA-VULGATA; POLAR LOBE; MARINE GASTROPOD; D-QUADRANT; SEX-CHANGE; CALYPTRAEID GASTROPODS; CILIARY BANDS; CHAETOPTERUS-VARIOPEDATUS AB Recent developmental and genomic research focused on "slipper snails" in the genus Crepidula has positioned Crepidula fornicata as a de facto model system for lophotrochozoan development. Here we review recent developments, as well as earlier reports demonstrating the widespread use of this system in studies of development and life history. Recent studies have resulted in a well-resolved fate map of embryonic cell lineage, documented mechanisms for axis determination and D quadrant specification, preliminary gene expression patterns, and the successful application of loss- and gain-of-function assays. The recent development of expressed sequence tags and preliminary genomics work will promote the use of this system, particularly in the area of developmental biology. A wealth of comparative information on phylogenetic relationships, variation in mode of development within the family, and numerous studies on larval biology and metamorphosis, primarily in Crepidula fornicata, make these snails a powerful tool for studies of the evolution of the mechanisms of development in the Mollusca and Lophotrochozoa. By bringing a review of the current state of knowledge of Crepidula life histories and development together with some detailed experimental methods, we hope to encourage further use of this system in various fields of investigation. C1 [Henry, Jonathan J.; Perry, Kimberly J.] Univ Illinois, Dept Cell & Dev Biol, Urbana, IL 61801 USA. [Collin, Rachel] Smithsonian Trop Res Inst, Balboa, Panama. RP Henry, JJ (reprint author), Univ Illinois, Dept Cell & Dev Biol, 601 S Goodwin Ave, Urbana, IL 61801 USA. EM j-henry4@illinois.edu RI Collin, Rachel/G-2001-2010 FU National Science Foundation [IOB 05-16799]; Smithsonian Tropical Research Institute FX The authors' research described in this paper was supported by National Science Foundation research grant IOB 05-16799 (to JJH) and the Smithsonian Tropical Research Institute (to RC). We thank K. MacDonald, M. Lesoway, F. Viard, and three anonymous reviewers for comments on the manuscript, and F. Viard for permission to cite personal communications. NR 154 TC 45 Z9 45 U1 2 U2 12 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 EI 1939-8697 J9 BIOL BULL-US JI Biol. Bull. PD JUN PY 2010 VL 218 IS 3 BP 211 EP 229 PG 19 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 618PE UT WOS:000279367300001 PM 20570845 ER PT J AU Hershler, R Liu, HP Clark, WH AF Hershler, Robert Liu, Hsiu-Ping Clark, William H. TI Microsatellite evidence of invasion and rapid spread of divergent New Zealand mudsnail (Potamopyrgus antipodarum) clones in the Snake River basin, Idaho, USA SO BIOLOGICAL INVASIONS LA English DT Article DE Invasive species; New Zealand mudsnail; Potamopyrgus; Microsatellites; Genetic diversity; Population structuring ID POPULATION-STRUCTURE; LIFE-HISTORY; SNAIL; HYDROBIIDAE; DIVERSITY; RECONSTRUCTION; PROSOBRANCHIA; DINUCLEOTIDE; AUSTRALIA; GRAY AB We used microsatellites to assess genetic diversity and spatial structuring of the invasive apomictic New Zealand mudsnail (Potamopyrgus antipodarum) in the initial focal area of its recent North American invasion, a portion of the upper Snake River basin (Idaho) that is segmented by a series of hydropower dams. Thirty-four samples (812 total snails) from a 368 km reach of this drainage were genotyped for six loci. Sixty-five distinct clones were detected and grouped into four divergent clusters based on chord distances. Genetic structuring of populations was generally low. Our results indicate that the founding population(s) of this invasion was composed of a small number of putative clonal lineages which spread rapidly within this fragmented watershed owing to the enhanced dispersal ability of these parthenogens. The substantial genetic variation documented in this study suggests that caution should be used in the application of biological control measures for this pest species. 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.] Albertson 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 FU Idaho Power Company [1600] FX Barry Bean and Mike Stephenson (IPC) provided a large amount of field assistance. Mike Radko (IPC) calculated the stream distances between sampling sites and Molly Ryan (Smithsonian Institution) assisted with preparation of the figures. Tom Quinn (University of Denver) and Sara Oyler-McCance (United States Geological Survey) generously shared bench space and equipment in the Rocky Mountain Center for Conservation Genetics and Systematics. This project was supported (in part) by a contract (to RH) from the Idaho Power Company (Award #1600). NR 48 TC 8 Z9 8 U1 2 U2 12 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD JUN PY 2010 VL 12 IS 6 BP 1521 EP 1532 DI 10.1007/s10530-009-9564-7 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 592VX UT WOS:000277410800011 ER PT J AU Parker, JD Richie, LJ Lind, EM Maloney, KO AF Parker, John D. Richie, Lauren J. Lind, Eric M. Maloney, Kelly O. TI Land use history alters the relationship between native and exotic plants: the rich don't always get richer SO BIOLOGICAL INVASIONS LA English DT Article DE Soil compaction; Land use history ID SOIL COMPACTION; SPECIES COMPOSITION; EARTHWORM INVASION; FOREST SUCCESSION; NEW-ENGLAND; DIVERSITY; VEGETATION; PATTERNS; CARBON; CONSERVATION AB Observational studies of diversity have consistently found positive correlations between native and exotic species, suggesting that the same environmental factors that drive native species richness also drive exotic species richness, i.e., "the rich get richer". We examined patterns of native and exotic plant species richness in temperate forests that have been undergoing reforestation since the turn of the twentieth century to test the influence of disturbance arising from land-use history on this relationship. Overall, we found no relationship between native and exotic plant species richness. Instead, we found a positive relationship between native and exotic richness in older but not younger-growth forests, suggesting that the same processes that drove exotic plant richness in older forests also facilitated native plants. In contrast, younger forests had similar numbers of native species relative to older forests, but 41% more exotic species and 24% more compacted soils. Moreover, exotic but not native species richness was positively correlated with increasing soil compaction across all sites. Overall, our results suggest that elevated exotic plant invasions in younger forests are a legacy of soil disturbance arising from agricultural practices at the turn of the century, and that native and exotic plants may respond differentially to disparate environmental drivers. C1 [Parker, John D.; Richie, Lauren J.; Lind, Eric M.; Maloney, Kelly O.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Richie, Lauren J.] Swarthmore Coll, Swarthmore, PA 19081 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; Lind, Eric/0000-0003-3051-7724 FU NSF [DBI 0353759] FX We thank E. Myron and C. Latimer for field assistance and two anonymous reviewers for constructive comments on the manuscript. This research was supported by NSF (DBI 0353759). NR 55 TC 24 Z9 24 U1 7 U2 48 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1387-3547 J9 BIOL INVASIONS JI Biol. Invasions PD JUN PY 2010 VL 12 IS 6 BP 1557 EP 1571 DI 10.1007/s10530-009-9568-3 PG 15 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 592VX UT WOS:000277410800014 ER PT J AU Hamilton, AM Zug, GR Austin, CC AF Hamilton, Alison M. Zug, George R. Austin, Christopher C. TI Biogeographic anomaly or human introduction: a cryptogenic population of tree skink (Reptilia: Squamata) from the Cook Islands, Oceania SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE colonization; Emoia samoensis species group; Fiji; human-mediated introduction; phylogeography; Samoa; Scincidae; Solomon Islands; Tonga; Vanuatu Archipelago; waif dispersal ID MITOCHONDRIAL-DNA SEQUENCES; HOUSE GECKOS HEMIDACTYLUS; SOUTH-PACIFIC; PHYLOGENETIC-RELATIONSHIPS; PREHISTORIC EXTINCTION; GENETIC-VARIATION; MORPHOLOGICAL EVOLUTION; MULTIPLE INTRODUCTIONS; NATURAL COLONIZATION; GEKKONID-LIZARDS AB Archaeological and molecular data have revealed that the present day faunas of many island groups in Melanesia, Polynesia, and Micronesia are not representative of the biodiversity generated within this region on an evolutionary timescale. Erroneous inferences regarding the mechanisms of speciation and the significance of long distance dispersal in shaping the present diversity of these island systems have resulted from this incomplete diversity and distributional data. The lizard fauna east of Samoa has been suggested to derive entirely from human-mediated introductions, a distribution congruent with biogeographic patterns for other Pacific species. Distinguishing between introduced populations and those that result from natural colonization events is difficult, although molecular data provide a useful means for elucidating population history and identifying the likely sources of introductions. We use molecular data (1726 bp of mitochondrial DNA and 286 bp of nuclear DNA) to evaluate a population of arboreal lizards from the Cook Islands and to determine whether this arboreal skink population is the sole endemic component of the lizard fauna east of Samoa or the result of human-mediated introduction. (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 100, 318-328. C1 [Hamilton, Alison M.; Austin, Christopher C.] Louisiana State Univ, Museum Nat Sci, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Zug, George R.] Natl Museum Nat Hist, Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Hamilton, AM (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM ahamilton@ucla.edu FU National Science Foundation [DEB 0408010, DEB 0445213, DBI 0400797]; EPSCoR Fellowship; Graduate Women in Science; American Society of Ichthyologists Herpetologists; Society for the Study of Amphibians Reptiles; Sigma Xi (LSU chapter); University of North Dakota; LSU Museum of Natural Science BioGrads; National Museum of Natural History programs FX A.M.H. thanks Ernest Bani and Donna Kalfatak of the Republic of Vanuatu Environment Unit for research, collecting and export permits (2000-2005); numerous ni-Vanuatu chiefs and villagers for access to land and assistance; and E. Klein, E. Hartfield, M. Eckstut, K. Blaha, and K. Grazyck for field assistance. G.R.Z. was generously granted permission to conduct biodiversity surveys and obtain voucher specimens by governmental representatives of the Cook Islands (National Research Committee: T. Okotai; Cook Islands Natural Heritage Project: G. McGormack), Fiji (Ministry of Agriculture, Fisheries & Forests: N. Tabunakawai), Samoa (Department of Agriculture, Forests & Fisheries: T. E. J. Thomsen), Tonga (Prime Minister's Office: 'A. L. Tangi & T. 'O. Folaumoetu'i; Ministry of Lands, Survey & Natural Resources: S. L. Tongilava), Vanuatu (Ministry of Natural Resources: E. Bani). Funding was provided to A.M.H. and C.C.A. by the National Science Foundation (DEB 0408010, DEB 0445213, DBI 0400797 and an EPSCoR Fellowship) and grant support to A.M.H. from Graduate Women in Science, American Society of Ichthyologists & Herpetologists, Society for the Study of Amphibians & Reptiles, Sigma Xi (LSU chapter), University of North Dakota (Graduate School, Office of Research & Program Development, Department of Biology), LSU Museum of Natural Science & BioGrads, and to G.R.Z. by various Smithsonian and National Museum of Natural History programs (Department of Vertebrate Zoology, Fluid Research Fund, Research Opportunities Awards, Scholarly Studies Program, 402-Discretionary Fund) that provided resources encouraging and supporting his research and travel to study the biology and evolution of Pacific lizards. We thank J. Allen, A. Freedman, Z. Cheviron, and an anonymous reviewer for discussions and suggestions crucial to the development of this manuscript. NR 91 TC 9 Z9 9 U1 0 U2 6 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD JUN PY 2010 VL 100 IS 2 BP 318 EP 328 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 599LP UT WOS:000277914500005 ER PT J AU Silvera, K Santiago, LS Cushman, JC Winter, K AF Silvera, Katia Santiago, Louis S. Cushman, John C. Winter, Klaus TI The incidence of crassulacean acid metabolism in Orchidaceae derived from carbon isotope ratios: a checklist of the flora of Panama and Costa Rica SO BOTANICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE carbon isotopes; Central America; epiphytes; herbarium; orchids; photosynthetic pathway ID VASCULAR EPIPHYTES; DELTA-C-13 VALUES; LIFE-FORMS; BROMELIACEAE; PLANTS; CAM; EXPRESSION; CLUSIA; LEAVES AB Leaf carbon stable isotopic composition data for 1002 orchid species representing 61% of the total number of orchid species described for Panama and Costa Rica were obtained from herbarium specimens to survey the occurrence of crassulacean acid metabolism (CAM). Carbon isotopic composition of leaf material showed a bimodal distribution with modes at -28 parts per thousand, indicating C(3) photosynthesis, and at -15 parts per thousand, indicating pronounced CAM photosynthesis. Strong CAM was present in 9.5% of species and in 31 of 162 genera studied. Twelve of these genera were not previously known to contain species exhibiting CAM. A checklist of orchids of Panama and Costa Rica with their delta 13C values and an updated list of all known orchid genera that possess species with the ability to perform CAM are presented. (C) 2010 The Linnean Society of London, Botanical Journal of the Linnean Society, 2010, 163, 194-222. C1 [Silvera, Katia; Cushman, John C.] Univ Nevada, Reno, NV 89557 USA. [Silvera, Katia; Winter, Klaus] Smithsonian Trop Res Inst, Ancon, Panama. [Santiago, Louis S.] Univ Calif Riverside, Riverside, CA 92521 USA. RP Silvera, K (reprint author), Univ Nevada, Biochem & Mol Biol MS 200, Reno, NV 89557 USA. EM katias@ucr.edu RI Santiago, Louis/E-3185-2016 OI Santiago, Louis/0000-0001-5994-6122 FU US Environmental Protection Agency [91685201]; National Science Foundation [NSF IOB-0543659, NSF DEB-0706813]; Andrew W. Mellon Foundation through the Smithsonian Tropical Research Institute FX We are extremely grateful to Dr Bruce Holst from the Marie Selby Botanical Gardens, Kent Perkins, Dr Mark Whitten and Dr Norris Williams from the University of Florida Herbarium, Dr Jim Solomon from the Missouri Botanical Gardens Herbarium, Mireya Correa from the University of Panama Herbarium and Carmen Galdames from the Smithsonian Tropical Research Institute Herbarium for access to herbarium collections. We are indebted to Dr Todd Dawson and Dr Stefania Mambelli (UC Berkeley) for assistance with isotopic analysis. This work was supported by funding from the US Environmental Protection Agency under the Greater Research Opportunities Graduate Program (agreement no. MA 91685201 to K.S.); National Science Foundation NSF IOB-0543659 (to J.C.C.); NSF DEB-0706813 (to L.S.S.); and the Andrew W. Mellon Foundation through the Smithsonian Tropical Research Institute (to K.W.). EPA has not formally reviewed this publication. The views expressed in this publication are solely those of the authors and the EPA does not endorse any products or commercial services mentioned in this publication. NR 30 TC 18 Z9 19 U1 3 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4074 J9 BOT J LINN SOC JI Bot. J. Linnean Soc. PD JUN PY 2010 VL 163 IS 2 BP 194 EP 222 DI 10.1111/j.1095-8339.2010.01058.x PG 29 WC Plant Sciences SC Plant Sciences GA 615SU UT WOS:000279158000006 ER PT J AU Lorence, DH Wagner, WL Laidlaw, WG AF Lorence, David H. Wagner, Warren L. Laidlaw, William G. TI Kadua haupuensis (Rubiaceae: Spermacoceae), a new endemic species from Kaua'i, Hawaiian Islands SO BRITTONIA LA English DT Article DE Endemic; Kadua; Kaua'i; Hawaiian Islands; Rubiaceae; subdioecious ID TRIBE SPERMACOCEAE; DIOECY; PHYLOGENY; FLORA AB The new species Kadua haupuensis is described and illustrated from the isolated Mt. Ha'upu region of Kaua'i, Hawaiian Islands. This new species belongs to Kadua subg. Kadua sect. Wiegmannia. It is characterized by a subdioecious (leaky dioecious) breeding system and appears most closely related to another apparently dioecious species endemic to Kaua'i, Kadua flynnii, with which it is compared. Although the only original wild population is critically endangered and may possibly be extinct, this new species has been successfully propagated and is currently secure in cultivation. C1 [Lorence, David H.; Laidlaw, William G.] Natl Trop Bot Garden, Kalaheo, HI 96741 USA. [Wagner, Warren L.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP Lorence, DH (reprint author), Natl Trop Bot Garden, 3530 Papalina Rd, Kalaheo, HI 96741 USA. EM lorence@ntbg.org; wagnerw@si.edu; laidlaw@ucalgary.ca FU Smithsonian Research Opportunities Fund FX Our sincere thanks go to Kenneth R. Wood who made the original field collections and pointed out the distinctiveness of this species as well as providing the map, and Robert Nishek who carefully grew and tended the plants in the NTBG nursery. The assistance of the NTBG "Na Lima Kokua" volunteers in the experimental work of WGL, alluded to in this paper, is gratefully acknowledged. Stephen G. Weller provided insightful discussions of breeding systems. The illustration was skillfully drawn by Alice Tangerini of the Smithsonian Institution. We thank Rae Matthews and Mel Gabel for formatting the figures and Marjorie Knowles and Harold Robinson of the Smithsonian Institution for preparing the SEM seed images. Our reviewers Harold Robinson and Edward Terrell provided most helpful suggestions for improving the manuscript. The contribution by WLW to this study was partially supported by the Smithsonian Research Opportunities Fund and while appointed as McBryde Chair at the National Tropical Botanical Garden. NR 12 TC 0 Z9 3 U1 0 U2 2 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0007-196X J9 BRITTONIA JI Brittonia PD JUN PY 2010 VL 62 IS 2 BP 137 EP 144 DI 10.1007/s12228-009-9103-y PG 8 WC Plant Sciences SC Plant Sciences GA 606CZ UT WOS:000278400400007 ER PT J AU Stellaccio, AE AF Stellaccio, Anthony E. TI Translation SO CERAMICS-ART AND PERCEPTION LA English DT Article RP Stellaccio, AE (reprint author), Smithsonian Inst, Natl Museum African Art, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU CERAMICS-ART & PERCEPTION PTY LTD PI SHERIDAN PA 23 N SCOTT ST, STE 16, SHERIDAN, WYOMING 82801 USA SN 1035-1841 J9 CERAMICS-ART PERCEPT JI Ceramics-Art Percept. PD JUN-AUG PY 2010 IS 80 BP 107 EP 109 PG 3 WC Art SC Art GA 602QA UT WOS:000278152700031 ER PT J AU Deocampo, DM Behrensmeyer, AK Potts, R AF Deocampo, Daniel M. Behrensmeyer, Anna K. Potts, Richard TI ULTRAFINE CLAY MINERALS OF THE PLEISTOCENE OLORGESAILIE FORMATION, SOUTHERN KENYA RIFT: DIAGENESIS AND PALEOENVIRONMENTS OF EARLY HOMININS SO CLAYS AND CLAY MINERALS LA English DT Article DE Authigenic Clay; East Africa; Hominin; Olorgesailie; Rift Basin; Smectite ID OLDUVAI-GORGE; EAST-AFRICA; PLIOCENE-PLEISTOCENE; NGORONGORO CRATER; NORTHERN TANZANIA; LAKE; SEDIMENTS; SMECTITE; CARBONATE; EVOLUTION AB The Pleistocene Olorgesailie Formation in the southern Kenya Rift has yielded a remarkable assemblage of Acheulean artifacts and vertebrate fossils, including hominin specimen KNM-OG 45500. Members 1 and 7 both contain clay-rich deposits that have been pedogenically modified into paleosols (UM1p and UM7p, respectively). This study provides the first detailed mineralogical and geochemical analyses of the clays of this important Pleistocene basin. The smectitic clays, which show abundant evidence for pedogenesis, were apparently originally deposited under lacustrinc conditions. They have an average structural formula of (Ca0.01Na0.32K0.26)(Si3.76Al0.24)(Al0.86Ti0.04Fe0.68Mg0.42)O-10(OH)(2). The high layer charge clays indicate diagenetic alteration of detrital clay derived from the volcanic drainage basin, probably involving alkaline waters of variable salinity. Despite overall lower salinity compared to other Plio-Pleistocene basins of the region (e.g. Olduvai Gorge), the basin still shows evidence for authigenic clay mineral precipitation. Clay chemistry and bulk geochemical indicators of pedogenesis imply that UM1p clays more closely reflect depositional paleo-waters, whereas UM7p clays have been more pedogenically altered due to subaerial exposure. UM1p smectites show some Mg enrichment near the western Lava Hump locality, consistent with discharge of Mg-bearing paleo-waters from a volcanic aquifer into a siliceous and alkaline (though not highly saline) paleo-lake. UM7p smectites were deposited in a more saline paleo-lake, but have lost substantial amounts of Mg due to post-depositional weathering. Locally abundant artifacts and vertebrate fossils found in these deposits accumulated at times following deposition of the lacustrine clay, probably concurrent with pedogenesis. The limnological conditions associated with initial clay deposition, therefore, preceded hominin occupation of the exposed surfaces. C1 [Deocampo, Daniel M.] Georgia State Univ, Dept Geosci, Atlanta, GA 30302 USA. [Behrensmeyer, Anna K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Potts, Richard] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. [Potts, Richard] Natl Museums Kenya, Dept Earth Sci, Paleontol Sect, Nairobi, Kenya. RP Deocampo, DM (reprint author), Georgia State Univ, Dept Geosci, Atlanta, GA 30302 USA. EM deocampo@gsu.edu FU Smithsonian Institution Office of Fellowships; National Science Foundation [0202612]; Natural History Museum, UK; Wenner Gren Foundation [6764] FX Olorgesailie fieldwork is a long-term collaborative project of the National Museums of Kenya and the Human Origins Program of the Smithsonian Institution. The research reported here was supported by the Smithsonian Institution Office of Fellowships, the National Science Foundation (#0202612), the Natural History Museum, UK, and the Wenner Gren Foundation (#6764). NR 58 TC 6 Z9 6 U1 1 U2 9 PU CLAY MINERALS SOC PI CHANTILLY PA 3635 CONCORDE PKWY, STE 500, CHANTILLY, VA 20151-1125 USA SN 0009-8604 EI 1552-8367 J9 CLAY CLAY MINER JI Clay Clay Min. PD JUN PY 2010 VL 58 IS 3 BP 294 EP 310 DI 10.1346/CCMN.2010.0580301 PG 17 WC Chemistry, Physical; Geosciences, Multidisciplinary; Mineralogy; Soil Science SC Chemistry; Geology; Mineralogy; Agriculture GA 749EL UT WOS:000289446300002 ER PT J AU Ritson-Williams, R AF Ritson-Williams, R. TI Surface brooding in the Caribbean gorgonian Pterogorgia anceps SO CORAL REEFS LA English DT Editorial Material ID FERTILIZATION C1 Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. RP Ritson-Williams, R (reprint author), Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. EM williams@si.edu RI Johnson, Selena/K-3541-2013 NR 6 TC 3 Z9 3 U1 0 U2 4 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD JUN PY 2010 VL 29 IS 2 BP 437 EP 437 DI 10.1007/s00338-010-0585-6 PG 1 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 592WJ UT WOS:000277412000019 ER PT J AU Ryan, MJ Bernal, XE Rand, AS AF Ryan, Michael J. Bernal, Ximena E. Rand, A. Stanley TI Female mate choice and the potential for ornament evolution in tungara frogs Physalaemus pustulosus SO CURRENT ZOOLOGY LA English DT Article DE Mate choice; Ornament evolution; Tungara frogs; Physalaemus pustulosus ID SEXUAL SELECTION; ADVERTISEMENT CALLS; COMPLEX CALLS; SPECIES GROUP; MALE TRAITS; ANIMAL COMMUNICATION; SENSORY EXPLOITATION; POPULATION VARIATION; MATING PREFERENCES; SIGNAL EVOLUTION AB The potential for ornament evolution in response to sexual selection rests on the interaction between the permissiveness or selectivity of female preferences and the constraints on male development of signaling related traits. We investigate the former by determining how latent female preferences either exaggerate the magnitude of current traits (i.e. elaborations) or favor novel traits (i.e. innovations). In tungara frogs, females prefer complex mating calls (whine-chucks) to simple calls (whine only). The whine is critical for mate recognition while the chuck further enhances the attractiveness of the call. Here we use a combination of synthetic and natural stimuli to examine latent female preferences. Our results show that a diversity of stimuli, including conspecific and heterospecific calls as well as predator-produced and human-made sounds, increase the attractiveness of a call when added to a whine. These stimuli do not make simple calls more attractive than a whine-chuck, however. In rare cases we found stimuli that added to the whine decrease the attractiveness of the call. Overall, females show strong preferences for both elaborations and innovations of the chuck. We argue that the emancipation of these acoustic adornments from mate recognition allows such female permissiveness, and that male constraints on signal evolution are probably more important in explaining why males evolved their specific adornment. Experimentally probing latent female preferences for stimuli out of the species' range is a useful means to gain insights about the potential of female choice to influence signal evolution and thus the astounding diversity in male sexually-selected traits [Current Zoology 56 (3): 343-357, 2010]. C1 [Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol C0930, Austin, TX 78712 USA. [Ryan, Michael J.; Rand, A. Stanley] Smithsonian Trop Res Inst, Balboa, Panama. [Bernal, Ximena E.] Texas Tech Univ, Dept Biol Sci, Lubbock, TX 79409 USA. RP Ryan, MJ (reprint author), Univ Texas Austin, Sect Integrat Biol C0930, Austin, TX 78712 USA. EM mryan@mail.utexas.edu FU National Science Foundation; Smithsonian Scholarly Studies Program FX We are especially grateful to the assistants who aided in the phonotaxis experiments that contributed to this study. The suggestions of M. Stevens, R. Marquez and an anonymous reviewer greatly improved the quality of the manuscript. We also wish to thank Autoridad Nacional del Ambiente of the Republic of Panama for research permits. The Smithsonian Tropical Research Institute provided invaluable logistic support. The frogs were marked following the Guidelines for the Use of Live Amphibians and Reptiles in Field Research compiled by the American Society of Ichthyologists and Herpetologists (ASIH), the Herpetologists' League (HL), and the Society for the Study of Amphibians and Reptiles (SSAR) and all procedures were approved by animal care committees at the University of Texas and STRI. This work was funded by several grants from both the National Science Foundation and the Smithsonian Scholarly Studies Program for which we are most grateful. NR 78 TC 13 Z9 14 U1 2 U2 18 PU CURRENT ZOOLOGY PI BEIJING PA CHINESE ACAD SCIENCES, INST ZOOLOGY, BEICHEN XILU, CHAOYANG DISTRICT, BEIJING, 100101, PEOPLES R CHINA SN 1674-5507 J9 CURR ZOOL JI Curr. Zool. PD JUN PY 2010 VL 56 IS 3 SI SI BP 343 EP 357 PG 15 WC Zoology SC Zoology GA 610FB UT WOS:000278715600009 ER PT J AU Fulford, RS Breitburg, DL Luckenbach, M Newell, RIE AF Fulford, Richard S. Breitburg, Denise L. Luckenbach, Mark Newell, Roger I. E. TI Evaluating ecosystem response to oyster restoration and nutrient load reduction with a multispecies bioenergetics model SO ECOLOGICAL APPLICATIONS LA English DT Article DE ecosystem; eutrophication; food web; modeling; oyster; restoration ID ANCHOVY ANCHOA-MITCHILLI; SUBMERGED AQUATIC VEGETATION; CHESAPEAKE BAY ECOSYSTEM; TOP-DOWN CONTROL; WATER-QUALITY; GELATINOUS ZOOPLANKTON; PHYTOPLANKTON BIOMASS; FEEDING BIVALVES; ECOLOGICAL RISKS; TROPHIC CASCADES AB Many of the world's coastal ecosystems are impacted by multiple stressors each of which may be subject to different management strategies that may have overlapping or even conflicting objectives. Consequently, management results may be indirect and difficult to predict or observe. We developed a network simulation model intended specifically to examine ecosystem-level responses to management and applied this model to a comparison of nutrient load reduction and restoration of highly reduced stocks of bivalve suspension feeders (eastern oyster, Crassostrea virginica) in an estuarine ecosystem (Chesapeake Bay, USA). Model results suggest that a 50% reduction in nutrient inputs from the watershed will result in lower phytoplankton production in the spring and reduced delivery of organic material to the benthos that will limit spring and summer pelagic secondary production. The model predicts that low levels of oyster restoration will have no effect in the spring but does result in a reduction in phytoplankton standing stocks in the summer. Both actions have a negative effect on pelagic secondary production, but the predicted effect of oyster restoration is larger. The lower effect of oysters on phytoplankton is due to size-based differences infiltration efficiency and seasonality that result in maximum top-down grazer control of oysters at a time when the phytoplankton is already subject to heavy grazing. These results suggest that oyster restoration must be achieved at levels as much as 25-fold present biomass to have a meaningful effect on phytoplankton biomass and as much as 50-fold to achieve effects similar to a 50% nutrient load reduction. The unintended effect of oyster restoration at these levels on other consumers represents a trade-off to the desired effect of reversing eutrophication. C1 [Fulford, Richard S.] Univ So Mississippi, Dept Coastal Sci, Gulf Coast Res Lab, Ocean Springs, MS 39564 USA. [Breitburg, Denise L.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Luckenbach, Mark] Virginia Inst Marine Sci, Eastern Shore Lab, Wachapreague, VA 23480 USA. [Newell, Roger I. E.] Univ Maryland, Horn Point Lab, Ctr Environm Sci, Cambridge, MD 21613 USA. RP Fulford, RS (reprint author), Univ So Mississippi, Dept Coastal Sci, Gulf Coast Res Lab, 703 E Beach Dr, Ocean Springs, MS 39564 USA. EM richard.fulford@usm.edu FU EPA Chesapeake Bay Program; NOAA Coastal Ocean Program FX This work would not have been possible without the assistance of many people with data compilation, model development, and model interpretation, including Steve Bartell, Michael Kemp, Carl Cerco, Charles Gallegos, Michael Roman, David Kimmel, Cindy Gilmour, Raleigh Hood, Kevin Sellner, Wayne Coats, and Claire Buchanan. This project was also highly dependent on data collected and analyzed as a part of the Chesapeake Bay Program (CBP), and we thank David Jasinski (CBP), Jeni Keisman (UMCES/CBP), and all those involved in making these data available. This project was funded by grants from the EPA Chesapeake Bay Program and the NOAA Coastal Ocean Program. NR 87 TC 15 Z9 15 U1 0 U2 33 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 1051-0761 J9 ECOL APPL JI Ecol. Appl. PD JUN PY 2010 VL 20 IS 4 BP 915 EP 934 DI 10.1890/08-1796.1 PG 20 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 611ZV UT WOS:000278865200003 PM 20597280 ER PT J AU Corre, MD Veldkamp, E Arnold, J Wright, SJ AF Corre, Marife D. Veldkamp, Edzo Arnold, Julia Wright, S. Joseph TI Impact of elevated N input on soil N cycling and losses in old-growth lowland and montane forests in Panama SO ECOLOGY LA English DT Article DE abiotic N immobilization; gross nitrification; gross N mineralization; litterfall (15)N signature; long-term nutrient manipulation experiment; montane forest organic horizon; nitrogen deposition; N leaching; NH(4)(+) immobilization; NO(3)(-) immobilization; N-oxide emissions; tropical lowland forest ID NITROGEN-OXIDE EMISSIONS; TROPICAL FOREST; ORGANIC-MATTER; RAIN-FOREST; ABIOTIC IMMOBILIZATION; COMMUNITY COMPOSITION; ISOTOPIC COMPOSITION; MICROBIAL COMMUNITY; RETENTION PROCESSES; NITRATE REDUCTION AB Nitrogen deposition is projected to increase rapidly in tropical ecosystems, but changes in soil-N-cycling processes in tropical ecosystems under elevated N input are less well understood. We used N-addition experiments to achieve N-enriched conditions in mixed-species, lowland and montane forests in Panama. Our objectives were to (1) assess changes in soil mineral N production (gross rates of N mineralization and nitrification) and retention (microbial immobilization and rapid reactions to organic N) during 1- and 9-yr N additions in the lowland forest and during 1-yr N addition in the montane forest and (2) relate these changes to N leaching and N-oxide emissions. In the old-growth lowland forest located on an Inceptisol, with high base saturation and net primary production not limited by N, there was no immediate effect of first-year N addition on gross rates of mineral-N production and N-oxide emissions. Changes in soil-N processes were only apparent in chronic (9 yr) N-addition plots: gross N mineralization and nitrification rates, NO(3)(-) leaching, and N-oxide emissions increased, while microbial biomass and NH(4)(+) immobilization rates decreased compared to the control. Increased mineral-N production under chronic N addition was paralleled by increased substrate quality (e.g., reduced C: N ratios of litterfall), while the decrease in microbial biomass was possibly due to an increase in soil acidity. An increase in N losses was reflected in the increase in (15)N signatures of litterfall under chronic N addition. In contrast, the old-growth montane forest located on an Andisol, with low base saturation and aboveground net primary production limited by N, reacted to first-year N addition with increases in gross rates of mineral-N production, microbial biomass, NO(3)(-) leaching, and Noxide emissions compared to the control. The increased N-oxide emissions were attributed to increased nitrification activity in the organic layer, and the high NO(3)(-) availability combined with the high rainfall on this sandy loam soil facilitated the instantaneous increase in NO(3)(-) leaching. These results suggest that soil type, presence of an organic layer, changes in soil-N cycling, and hydrological properties are more important indicators than vegetation as an N sink on how tropical forests respond to elevated N input. C1 [Corre, Marife D.; Veldkamp, Edzo; Arnold, Julia] Univ Gottingen, Buesgen Inst, D-37077 Gottingen, Germany. [Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Panama. RP Corre, MD (reprint author), Univ Gottingen, Buesgen Inst, Busgenweg 2, D-37077 Gottingen, Germany. EM mcorre@gwdg.de RI Veldkamp, Edzo/A-6660-2008; Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU Robert Bosch Foundation (Germany); Deutsche Forschungsgemeinschaft [Ve 219/7-1,2] FX The Robert Bosch Foundation (Germany) funded the NITROF research project of M. D. Corre, under which this study was conducted. The dry-season sampling was supported by the Deutsche Forschungsgemeinschaft (Ve 219/7-1,2). The Smithsonian Tropical Research Institute provided invaluable administrative and technical support. The help of the research assistants of the long-term nutrient manipulation experiment in the lowland forest, the NITROF assistants (Erick Diaz, Rodolfo Rojas, and Carlos Sanchez), and the SSTSE laboratory technicians (especially Kerstin Langs) are highly appreciated. James Dalling provided background information and assisted in the site selection of the montane forest. We thank also the three anonymous reviewers for their very helpful reviews. NR 65 TC 57 Z9 59 U1 8 U2 87 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 JUN PY 2010 VL 91 IS 6 BP 1715 EP 1729 DI 10.1890/09-0274.1 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 611YB UT WOS:000278859700017 PM 20583713 ER PT J AU Parker, IM Lopez, I Petersen, JJ Anaya, N Cubilla-Rios, L Potter, D AF Parker, Ingrid M. Lopez, Isis Petersen, Jennifer J. Anaya, Natalia Cubilla-Rios, Luis Potter, Daniel TI Domestication Syndrome in Caimito (Chrysophyllum cainito L.): Fruit and Seed Characteristics SO ECONOMIC BOTANY LA English DT Article DE Domestication; Caimito; Star apple; Fruit size; Chemistry; Phenolics; Trait correlations; Discriminant analysis ID TRADITIONAL MANAGEMENT; PHENOTYPIC VARIATION; CROP DOMESTICATION; MOLECULAR-GENETICS; WILD RELATIVES; SOUTH-AFRICA; OLD-WORLD; SELECTION; DIVERSITY; EVOLUTION AB Domestication Syndrome in Caimito ( Chrysophyllum cainito L.): Fruit and Seed Characteristics: The process of domestication is understudied and poorly known for many tropical fruit tree crops. The star apple or caimito tree (Chrysophyllum cainito L., Sapotaceae) is cultivated throughout the New World tropics for its edible fruits. We studied this species in central Panama, where it grows wild in tropical moist forests and is also commonly cultivated in backyard gardens. Using fruits collected over two harvest seasons, we tested the hypothesis that cultivated individuals of C. cainito show distinctive fruit and seed characteristics associated with domestication relative to wild types. We found that cultivated fruits were significantly and substantially larger and allocated more to pulp and less to exocarp than wild fruits. The pulp of cultivated fruits was less acidic; also, the pulp had lower concentrations of phenolics and higher concentrations of sugar. The seeds were larger and more numerous and were less defended with phenolics in cultivated than in wild fruits. Discriminant Analysis showed that, among the many significant differences, fruit size and sugar concentration drove the great majority of the variance distinguishing wild from cultivated classes. Variance of pulp phenolics among individuals was significantly higher among wild trees than among cultivated trees, while variance of fruit mass and seed number was significantly higher among cultivated trees. Most traits showed strong correlations between years. Overall, we found a clear signature of a domestication syndrome in the fruits of cultivated caimito in Panama. C1 [Parker, Ingrid M.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Lopez, Isis] Smithsonian Trop Res Inst, Panama City, Panama. [Petersen, Jennifer J.; Potter, Daniel] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. [Anaya, Natalia; Cubilla-Rios, Luis] Univ Panama, Lab Bioorgan Trop, Panama City, Panama. RP Parker, IM (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. EM parker@biology.ucsc.edu FU UCSC Committee on Research; Jane Carver Foundation; Jean H. Langenheim Endowed Chair in Plant Ecology and Evolution; Fulbright Fellowship FX We thank Humberto Membache, Amaranto Membache, and Harold Henry for field assistance, and Carl Jones for help in adapting the fruit chemistry protocols. Barry Nickel designed and created the map. Sara Grove, Sarah Swope, John Banks, Justin Cummings, Krikor Andonian, and Carla Fresquez provided comments on the manuscript, and Jorge Zegbe helped edit the Spanish abstract. Financial support for this project was provided by the UCSC Committee on Research, the Jane Carver Foundation, the Jean H. Langenheim Endowed Chair in Plant Ecology and Evolution, and a Fulbright Fellowship to IMP. NR 55 TC 23 Z9 23 U1 2 U2 13 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0013-0001 J9 ECON BOT JI Econ. Bot. PD JUN PY 2010 VL 64 IS 2 BP 161 EP 175 DI 10.1007/s12231-010-9121-4 PG 15 WC Plant Sciences SC Plant Sciences GA 607QU UT WOS:000278522200006 ER PT J AU van Donkelaar, A Martin, RV Brauer, M Kahn, R Levy, R Verduzco, C Villeneuve, PJ AF van Donkelaar, Aaron Martin, Randall V. Brauer, Michael Kahn, Ralph Levy, Robert Verduzco, Carolyn Villeneuve, Paul J. TI Global Estimates of Ambient Fine Particulate Matter Concentrations from Satellite-Based Aerosol Optical Depth: Development and Application SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article DE aerosol; aerosol optical depth; AOD; particulate matter; PM2.5 ID GROUND-LEVEL PM2.5; AIR-POLLUTION; UNITED-STATES; QUALITY; MORTALITY; THICKNESS; MODIS; CITIES; COHORT AB BACKGROUND: Epidemiologic and health impact studies of fine particulate matter with diameter < 2.5 mu m (PM2.5) are limited by the lack of monitoring data, especially in developing countries. Satellite observations offer valuable global information about PM2.5 concentrations. OBJECTIVE: In this study, we developed a technique for estimating surface PM2.5 concentrations from satellite observations. METHODS: We mapped global ground-level PM2.5 concentrations using total column aerosol optical depth (AOD) from the MODIS (Moderate Resolution Imaging Spectroradiometer) and MISR (Multiangle Imaging Spectroradiometer) satellite instruments and coincident aerosol vertical profiles from the GEOS-Chem global chemical transport model. RESULTS: We determined that global estimates of long-term average (1 January 2001 to 31 December 2006) PM2.5 concentrations at approximately 10 km x 10 km resolution indicate a global population-weighted geometric mean PM2.5 concentration of 20 mu g/m(3). The World Health Organization Air Quality PM2.5 Interim Target-1 (35 mu g/m(3) annual average) is exceeded over central and eastern Asia for 38% and for 50% of the population, respectively. Annual mean PM2.5 concentrations exceed 80 mu g/m(3) over eastern China. Our evaluation of the satellite-derived estimate with ground-based in situ measurements indicates significant spatial agreement with North American measurements (r = 0.77; slope = 1.07; n = 1057) and with noncoincident measurements elsewhere (r = 0133; slope = 0.86; n = 244). The 1 SD of uncertainty in the satellite-derived PM2.5 is 25%, which is inferred from the AOD retrieval and from aerosol vertical profile errors and sampling. The global population-weighted mean uncertainty is 6.7 mu g/m(3). CONCLUSIONS: Satellite-derived total-column AOD, when combined with a chemical transport model, provides estimates of global long-term average PM2.5 concentrations. C1 [van Donkelaar, Aaron; Martin, Randall V.; Verduzco, Carolyn] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brauer, Michael] Univ British Columbia, Sch Environm Hlth, Vancouver, BC V5Z 1M9, Canada. [Kahn, Ralph; Levy, Robert] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Villeneuve, Paul J.] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada. [Villeneuve, Paul J.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0L2, Canada. RP van Donkelaar, A (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, 6300 Coburg Rd, Halifax, NS B3H 3J5, Canada. EM Aaron.van.Donkelaar@dal.ca RI Levy, Robert/M-7764-2013; Martin, Randall/C-1205-2014; Kahn, Ralph/D-5371-2012; Chem, GEOS/C-5595-2014; OI Levy, Robert/0000-0002-8933-5303; Martin, Randall/0000-0003-2632-8402; Kahn, Ralph/0000-0002-5234-6359; Brauer, Michael/0000-0002-9103-9343 FU Health Canada [4500171909, 4500220294]; Natural Sciences and Engineering Research of Canada; Killam Trust FX This study was funded by contracts from Health Canada (4500171909 and 4500220294). A.v.D. was supported by graduate fellowships from the Natural Sciences and Engineering Research of Canada and the Killam Trust. NR 45 TC 398 Z9 402 U1 43 U2 301 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 EI 1552-9924 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD JUN PY 2010 VL 118 IS 6 BP 847 EP 855 DI 10.1289/ehp.0901623 PG 9 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 608NP UT WOS:000278591300031 PM 20519161 ER PT J AU Hesselberg, T AF Hesselberg, Thomas TI Ontogenetic Changes in Web Design in Two Orb-Web Spiders SO ETHOLOGY LA English DT Article ID BUILDING BEHAVIOR; WEAVING SPIDER; BIOGENETIC LAW; JUMPING SPIDER; SP ARANEAE; EXPERIENCE; ARANEIDAE; BRAINS; SIZE; CONSTRUCTION AB The first orb web built by newly hatched spiders resembles the adult web in its overall form and structure. However, many details show ontogenetic changes. One possible explanation for these changes is that the tiny early-instar spiders with their minute brains will make more mistakes and build less 'perfect' orb webs than older and larger juveniles and adults. To test this hypothesis, known as the size limitation hypothesis, I analysed orb webs from three developmental stages, spiderlings, juveniles and adult females, in two neotropical orb-web spiders, the araneid Eustala illicita and the nephilid Nephila clavipes. Neither species showed clear signs of being behaviourally limited or more prone to committing errors as spiderlings than were older juveniles or adults. These findings therefore do not support the size limitation hypothesis in either species. Finally, I looked for evidence of the 'biogenetic law', which predicts that juveniles should build less derived orb webs than the adults. Evidence for this was found in E. illicita, but not in N. clavipes. C1 [Hesselberg, Thomas] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Hesselberg, T (reprint author), Univ Oxford, Dept Zool, S Parks Rd, Oxford OX1 3PS, England. EM thomas.hesselberg@zoo.ox.ac.uk RI Hesselberg, Thomas/A-1711-2008 FU Smithsonian Postdoctoral Fellowship FX The author thanks William Eberhard and two anonymous referees for very helpful suggestions to an earlier version of this manuscript. The author gratefully acknowledges the permission granted by the Parque Natural Metropolitano and the Autoridad Nacional del Ambiente (ANAM permit nos. SE/A-81-08 and SE/A-104-08) to carry out this study. The study was funded by a Smithsonian Postdoctoral Fellowship. NR 47 TC 22 Z9 24 U1 1 U2 14 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0179-1613 J9 ETHOLOGY JI Ethology PD JUN PY 2010 VL 116 IS 6 BP 535 EP 545 DI 10.1111/j.1439-0310.2010.01760.x PG 11 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 592UJ UT WOS:000277405700007 ER PT J AU Gaillou, E Wang, WY Post, JE King, JM Butler, JE Collins, AT Moses, TM AF Gaillou, Eloise Wang, Wuyi Post, Jeffrey E. King, John M. Butler, James E. Collins, Alan T. Moses, Thomas M. TI THE WITTELSBACH-GRAFF AND HOPE DIAMONDS: NOT CUT FROM THE SAME ROUGH SO GEMS & GEMOLOGY LA English DT Article ID TEMPERATURE TREATMENT; HIGH-PRESSURE; BLUE AB Two historic blue diamonds, the Hope and the Wittelsbach-Graff, appeared together for the first time at the Smithsonian Institution in 2010 Both diamonds were apparently purchased in India in the 17th century and later belonged to European royalty. In addition to the parallels in their histories, their comparable color and bright, long-lasting orange-red phosphorescence have led to speculation that these two diamonds might have come from the same piece of rough. Although the diamonds are similar spectroscopically, their dislocation patterns observed with the Diamond View differ in scale and texture, and they do not show the same internal strain features The results indicate that the two diamonds did not originate from the same crystal, though they likely experienced similar geologic histories. C1 [Gaillou, Eloise; Post, Jeffrey E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Wang, Wuyi; King, John M.; Moses, Thomas M.] GIA Lab, New York, NY USA. [Butler, James E.] USN, Res Lab, Washington, DC 20375 USA. [Collins, Alan T.] Kings Coll London, London, England. RP Gaillou, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RI Gaillou, Eloise/D-1753-2009; Butler, James/B-7965-2008 OI Gaillou, Eloise/0000-0002-7949-268X; Butler, James/0000-0002-4794-7176 NR 19 TC 6 Z9 7 U1 0 U2 5 PU GEMOLOGICAL INST AMER PI CARLSBAD PA 5345 ARMADA DR, CARLSBAD, CA 92008 USA SN 0016-626X J9 GEMS GEMOL JI Gems Gemol. PD SUM PY 2010 VL 46 IS 2 BP 80 EP 88 PG 9 WC Mineralogy SC Mineralogy GA 639XS UT WOS:000281011000001 ER PT J AU Rondeau, B Fritsch, E Mazzero, F Gauthier, JP Cenki-Tok, B Bekele, E Gaillou, E AF Rondeau, Benjamin Fritsch, Emmanuel Mazzero, Francesco Gauthier, Jean-Pierre Cenki-Tok, Benedicte Bekele, Eyassu Gaillou, Eloise TI PLAY-OF-COLOR OPAL FROM WEGEL TENA, WOLLO PROVINCE, ETHIOPIA SO GEMS & GEMOLOGY LA English DT Article ID SPECTRA AB A new opal deposit was discovered in 2008 near the village of Wegel Tena, in volcanic rocks of Ethiopia's Wollo Province. Unlike previous Ethiopian opals, the new material is mostly white, with some brown opal, fire opal, and colorless "crystal" opal. Some of it resembles Australian and Brazilian sedimentary opals, with play-of-color that is often very vivid. However, its properties are consistent with those of opal-CT and most volcanic opals. Inclusions consist of pyrite, barium-manganese oxides, and native carbon Some samples show "digit patterns", interpenetrating play-of-color and common opal, resembling fingers. The opaque-to-translucent Wegel Tena opals become transparent when soaked in water, showing a remarkable hydrophane character. White opals from this deposit contain an elevated Ba content, which has not been reported so far in opal-CT. The fire and crystal opals are prone to breakage, while the white, opaque-to-translucent opals are remarkably durable. The proportion of gem-quality material in the Wegel Tena deposit seems unusually high, and 1,500 kg have already been extracted using rudimentary mining techniques. The deposit may extend over several kilometers and could become a major source of gem-quality opal C1 [Rondeau, Benjamin] Univ Nantes, Lab Planetol & Geodynam, F-44035 Nantes, France. [Rondeau, Benjamin] CNRS, Team 6112, F-75700 Paris, France. [Fritsch, Emmanuel] Univ Nantes, Inst Mat Jean Rouxel IMN CNRS, Team 6205, F-44035 Nantes, France. [Mazzero, Francesco; Bekele, Eyassu] Opalinda, Paris, France. [Mazzero, Francesco; Bekele, Eyassu] Eyaopal, Addis Ababa, Ethiopia. [Gauthier, Jean-Pierre] Univ Lyon, Lyon, France. [Cenki-Tok, Benedicte] Univ Bern, Inst Geol Sci, CH-3012 Bern, Switzerland. [Gaillou, Eloise] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Rondeau, B (reprint author), Univ Nantes, Lab Planetol & Geodynam, F-44035 Nantes, France. RI Gaillou, Eloise/D-1753-2009 OI Gaillou, Eloise/0000-0002-7949-268X NR 25 TC 8 Z9 8 U1 2 U2 5 PU GEMOLOGICAL INST AMER PI CARLSBAD PA 5345 ARMADA DR, CARLSBAD, CA 92008 USA SN 0016-626X J9 GEMS GEMOL JI Gems Gemol. PD SUM PY 2010 VL 46 IS 2 BP 90 EP 105 PG 16 WC Mineralogy SC Mineralogy GA 639XS UT WOS:000281011000002 ER PT J AU Cottrell, E Kelley, KA AF Cottrell, E. Kelley, K. A. TI Basaltic glasses as records of mantle oxygen fugacity SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Cottrell, E.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kelley, K. A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. EM cottrellE@si.edu NR 5 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A192 EP A192 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941400634 ER PT J AU Fischer, TB Heaney, PJ Brantley, SL Post, JE Tien, M AF Fischer, T. B. Heaney, P. J. Brantley, S. L. Post, J. E. Tien, M. TI Time-resolved XRD of the siderophore-promoted dissolution of birnessite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Fischer, T. B.; Heaney, P. J.; Brantley, S. L.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, J. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. [Tien, M.] Penn State Univ, Dept Biochem & Mol Biol, University Pk, PA 16802 USA. EM tfischer@psu.edu NR 2 TC 0 Z9 0 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A295 EP A295 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941400840 ER PT J AU Fleeger, CR Heaney, PJ Post, JE AF Fleeger, Claire R. Heaney, Peter J. Post, Jeffrey E. TI Sequestration of Cs by Na- and H-birnessite from pH 3 to 11 as measured with time-resolved synchrotron X-ray diffraction SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Fleeger, Claire R.; 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 crf163@psu.edu; pjheaney@psu.edu; postj@si.edu NR 1 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A297 EP A297 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941400843 ER PT J AU Fritsch, E Gaillou, E Massuyeau, F Rondeau, B AF Fritsch, E. Gaillou, E. Massuyeau, F. Rondeau, B. TI Luminescence of opals: A witness to their geochemistry SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Fritsch, E.; Gaillou, E.; Massuyeau, F.] Univ Nantes, CNRS, Inst Materiaux Jean Rouxel IMN, UMR 6205, F-44322 Nantes 3, France. [Gaillou, E.] NMNH, Smithsonian Inst, Washington, DC 20560 USA. [Rondeau, B.] Univ Nantes, CNRS, LPGN, UMR 6112, F-44035 Nantes, France. EM emmanuel.fritsch@cnrs-imn.fr RI Gaillou, Eloise/D-1753-2009 OI Gaillou, Eloise/0000-0002-7949-268X NR 1 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A307 EP A307 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941400863 ER PT J AU Gaillou, E Rost, D Post, JE Butler, JE AF Gaillou, E. Rost, D. Post, J. E. Butler, J. E. TI Quantifying boron in natural type IIb blue diamonds SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Gaillou, E.; Post, J. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. [Rost, D.] Univ Manchester, SEAES, Manchester M13 9PL, Lancs, England. [Butler, J. E.] USN, Res Lab, Washington, DC 20375 USA. EM gailloue@si.edu; detlef.rost@manchester.ac.uk; postj@si.edu; james.butler@nrl.navy.mil RI Gaillou, Eloise/D-1753-2009 OI Gaillou, Eloise/0000-0002-7949-268X NR 4 TC 1 Z9 1 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A313 EP A313 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941401002 ER PT J AU Gilmour, CC Elias, DA Kucken, A Brown, SD Palumbo, AV Wall, JD AF Gilmour, C. C. Elias, D. A. Kucken, A. Brown, S. D. Palumbo, A. V. Wall, J. D. TI The sulfate-reducing bacterium Desulfovibrio desulfuricans ND132 as a model for understanding bacterial mercury methylation SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Gilmour, C. C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Elias, D. A.; Brown, S. D.; Palumbo, A. V.] Oak Ridge Natl Lab, Oak Ridge, TN 37831 USA. [Kucken, A.; Wall, J. D.] Univ Missouri, Dept Biochem, Columbia, MO 65211 USA. EM gilmourc@si.edu RI Palumbo, Anthony/A-4764-2011; Elias, Dwayne/B-5190-2011; Brown, Steven/A-6792-2011 OI Palumbo, Anthony/0000-0002-1102-3975; Elias, Dwayne/0000-0002-4469-6391; Brown, Steven/0000-0002-9281-3898 NR 0 TC 0 Z9 0 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A333 EP A333 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941401042 ER PT J AU Hummer, DR Heaney, PJ Post, JE AF Hummer, D. R. Heaney, P. J. Post, J. E. TI Probing the aqueous nucleation and growth of TiO2 with high time-resolution small-angle and wide-angle X-ray scattering SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Hummer, D. R.; Heaney, P. J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, J. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. EM drh232@psu.edu NR 3 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A438 EP A438 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941401251 ER PT J AU Kelley, KA Cottrell, E Brounce, M Parks, B AF Kelley, K. A. Cottrell, E. Brounce, M. Parks, B. TI The influence of magmatic differentiation on the oxidation state of Fe in arc magmas SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Kelley, K. A.; Brounce, M.] Univ Rhode Isl, GSO, Narragansett, RI 02882 USA. [Cottrell, E.] Smithsonian Inst, NMNH, Washington, DC 20560 USA. [Parks, B.] Carleton Coll, Northfield, MN 55057 USA. EM kelley@gso.uri.edu NR 2 TC 0 Z9 0 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A505 EP A505 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941401579 ER PT J AU Logan, MAV AF Logan, M. Amelia V. TI Evaluation of some feldspar specimens as candidates to be characterized as Reference Materials for their minor and trace element contents SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Logan, M. Amelia V.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. EM logana@si.edu NR 1 TC 0 Z9 0 U1 1 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A628 EP A628 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941401824 ER PT J AU Ostrom, PH Wiley, A James, H Welch, A Fleischer, R AF Ostrom, P. H. Wiley, A. James, H. Welch, A. Fleischer, R. TI Temporal and spatial isotopic and genetic variation reveal the ecological history of an endangered seabird SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. Smithsonian Inst, Div Birds, Washington, DC 20013 USA. Univ Maryland, College Pk, MD 20742 USA. Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. EM ostrom@msu.edu; jamesh@si.edu; welcha@si.edu; fleischerr@si.edu NR 0 TC 0 Z9 0 U1 0 U2 3 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A781 EP A781 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941402265 ER PT J AU Peltzer, DA Wardle, DA Allison, VJ Baisden, TW Bardgett, RD Chadwick, OA Condron, LM Parfitt, RL Porder, S Richardson, SJ Turner, BL Vitousek, PM Walker, J Walker, LR AF Peltzer, D. A. Wardle, D. A. Allison, V. J. Baisden, T. W. Bardgett, R. D. Chadwick, O. A. Condron, L. M. Parfitt, R. L. Porder, S. Richardson, S. J. Turner, B. L. Vitousek, P. M. Walker, J. Walker, L. R. TI Causes and consequences of ecosystem retrogression SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Peltzer, D. A.; Wardle, D. A.; Richardson, S. J.; Walker, J.] Landcare Res, Lincoln, New Zealand. [Wardle, D. A.; Walker, J.] Swedish Univ Agr Sci, S-90183 Umea, Sweden. [Allison, V. J.] Minist Agr & Forestry, Auckland, New Zealand. [Baisden, T. W.] Geol & Nucl Sci, Wellington, New Zealand. [Bardgett, R. D.] Univ Lancaster, Lancaster LA1 4YQ, England. [Chadwick, O. A.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Condron, L. M.] Lincoln Univ, Lincoln, New Zealand. [Parfitt, R. L.] Landcare Res, Palmerston North, New Zealand. [Porder, S.] Brown Univ, Providence, RI 02912 USA. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Vitousek, P. M.] Stanford Univ, Stanford, CA 94305 USA. CSIRO Land & Water, Canberra, ACT 2601, Australia. [Walker, L. R.] Univ Nevada, Las Vegas, NV 89154 USA. EM peltzerd@landcareresearch.co.nz RI Peltzer, Duane/A-9463-2009; Turner, Benjamin/E-5940-2011; Wardle, David/F-6031-2011; Condron, Leo/E-9458-2013; Baisden, Troy/B-9831-2008 OI Peltzer, Duane/0000-0001-7724-3738; Turner, Benjamin/0000-0002-6585-0722; Wardle, David/0000-0002-0476-7335; Baisden, Troy/0000-0003-1814-1306 NR 0 TC 0 Z9 0 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A802 EP A802 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941402308 ER PT J AU Penniston-Dorland, SC Walker, RJ Pitcher, L Sorensen, SS AF Penniston-Dorland, S. C. Walker, R. J. Pitcher, L. Sorensen, S. S. TI Highly siderophile elements as tracers of mantle-crust interactions in subduction zone metamorphic rocks: Evidence from the Franciscan Complex, CA SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Penniston-Dorland, S. C.; Walker, R. J.; Pitcher, L.] Univ Maryland, Dept Geol, College Pk, MD 20742 USA. [Sorensen, S. S.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. EM sarahpd@umd.edu NR 0 TC 0 Z9 0 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A804 EP A804 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941402312 ER PT J AU Peterson, KM Heaney, PJ Post, JE AF Peterson, K. M. Heaney, P. J. Post, J. E. TI Time-resolved X-ray diffraction study of the in situ hydrothermal phase transformation from akaganeite to hematite SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Peterson, K. M.; Heaney, P. J.] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Post, J. E.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. EM kmp286@psu.edu; postj@si.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A810 EP A810 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941402324 ER PT J AU Plank, T Zimmer, M Cottrell, E Kelley, K AF Plank, T. Zimmer, M. Cottrell, E. Kelley, K. TI The oxidation state of magmas from melt inclusions and olivine hosts SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Meeting Abstract CT Conference on Goldschmidt 2010 - Earth, Energy, and the Environment CY JUN 13-18, 2010 CL Knoxville, TN C1 [Plank, T.] Lamont Doherty Earth Observ, Palisades, NY 10964 USA. [Zimmer, M.] Boston Univ, Boston, MA 02215 USA. [Cottrell, E.] Smithsonian Inst, NMNH, Washington, DC 20560 USA. [Kelley, K.] URI, Grad Sch Oceanog, Narragansett, RI 02882 USA. EM tplank@ldeo.columbia.edu NR 5 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 0016-7037 J9 GEOCHIM COSMOCHIM AC JI Geochim. Cosmochim. Acta PD JUN PY 2010 VL 74 IS 12 SU 1 BP A819 EP A819 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 676TL UT WOS:000283941402342 ER PT J AU Crawford, AJ Ryan, MJ Jaramillo, CA AF Crawford, Andrew J. Ryan, Mason J. Jaramillo, Cesar A. TI A NEW SPECIES OF PRISTIMANTIS (ANURA: STRABOMANTIDAE) FROM THE PACIFIC COAST OF THE DARIEN PROVINCE, PANAMA, WITH A MOLECULAR ANALYSIS OF ITS PHYLOGENETIC POSITION SO HERPETOLOGICA LA English DT Article DE Gonads; Histology; Molecular phylogenetics; Pristimantis; Species description; Sperm development; tRNA secondary structure ID DNA-SEQUENCES; MITOCHONDRIAL GENOME; EVOLUTIONARY TREES; CENTRAL-AMERICA; SOUTH-AMERICA; FROGS; ELEUTHERODACTYLUS; LEPTODACTYLIDAE; BIOGEOGRAPHY; INFERENCE AB We describe a new species of Pristimantis (Anura: Strabomantidae) from the Pacific coast of the Darien Province, Panama. The type locality is on Cerro Pina, in the Serrania de Sapo, at 700-800 in elevation. This new species is readily distinguished from all other known congeners from the region based on external morphology. Despite the small size of the two type specimens, histological analysis of the gonads shows these individuals were potentially reproductive males. Molecular phylogenetic analyses based on the ND2-WANCY mitochondrial gene region reveal that this new species is genetically distinct. Molecular and morphological data place the new species in the Pristimantis (Hypodictyon) ridens species series, and suggest that P. cerasinus be moved to this group as well. Molecular analyses also reveal a potential synapomophy of the genus Pristimantis relative to the other five genera sampled here: the loss of the D-stem of the tRNA(CYS) gene. Our finding of another endemic frog from eastern Panama lends further support to the concept of the Darien as a center of endemism and not just a conduit between continents. C1 [Crawford, Andrew J.; Jaramillo, Cesar A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Crawford, Andrew J.; Jaramillo, Cesar A.] Circulo Herpetol Panama, Panama City, Panama. [Crawford, Andrew J.] Univ Los Andes, Dept Ciencias Biol, Bogota 4976, Colombia. [Ryan, Mason J.] Univ New Mexico, Albuquerque, NM 87131 USA. [Jaramillo, Cesar A.] Univ Panama, Fac Med, Dept Histol & Neuroanat Humana, Panama City, Panama. RP Crawford, AJ (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM andrew@dna.ac OI Crawford, Andrew J./0000-0003-3153-6898 FU National Science Foundation (NSF) [DEB-0844624] FX We thank the owners and managers of Tropic Star Lodge (http://www.tropicstar.com/) for inviting us to survey their property, and B. and A. Coates for organizing the expedition. We thank R. Ibanez for help in identifying the gonads in these very small frogs, I. Wang for sequencing the Louisiana State University (LSU) samples, and D. Medina for help reviewing specimens. We thank D. Dittmann and R. Brumfield of LSU and J. P. Caldwell of Oklahoma University for loaning tissue samples. Many thanks go to the Autoridad Nacional del Ambiente of Panama for their gracious and continued approval of our research activities, and to O. Arosemena for administrative help in acquiring permits. B. Moon, C. J. Raxworthy, J. Padial, one anonymous reviewer, and El Brujo S. Poe provided much appreciated comments on an earlier draft of this manuscript. Research on live animals conformed to the Smithsonian Tropical Research Institute's Animal Care and Use Protocol. AJC was supported by an National Science Foundation (NSF) International Programs postdoctoral fellowship during fieldwork, and a Smithsonian Molecular Evolution postdoctoral fellowship during laboratory work. MJR was supported by NSF DEB-0844624 to S. Poe and by the Panama Frog Rescue Project 2004. NR 60 TC 8 Z9 8 U1 0 U2 6 PU HERPETOLOGISTS LEAGUE PI EMPORIA PA EMPORIA STATE UNIV, DIVISION BIOLOGICAL SCIENCES, 1200 COMMERCIAL ST, EMPORIA, KS 66801-5087 USA SN 0018-0831 EI 1938-5099 J9 HERPETOLOGICA JI Herpetologica PD JUN PY 2010 VL 66 IS 2 BP 192 EP 206 PG 15 WC Zoology SC Zoology GA 599WR UT WOS:000277945200009 ER PT J AU Bouley, S Craddock, RA Mangold, N Ansan, V AF Bouley, S. Craddock, R. A. Mangold, N. Ansan, V. TI Characterization of fluvial activity in Parana Valles using different age-dating techniques SO ICARUS LA English DT Article DE Mars ID DIGITAL ELEVATION MODELS; MARS; NETWORKS; CHANNELS; SURFACE; AREAS; PRECIPITATION; CHRONOLOGY; LANDSCAPE; EVOLUTION AB Martian valley networks provide the best evidence that the climate on Mars was different in the past. Although these features are located primarily in heavily cratered terrain of Noachian age (>3.7 Ga), the ages of the features and the time when they were active is not well understood. From superposed craters several recent global studies determined that most valley networks formed during the Late Noachian to Early Hesperian; however, there were some disparities between the techniques. In this study, our principal objective was to test the reliability of the different age-dating techniques to better understand their accuracy and limitations. We applied these techniques to Parana Valles using a variety of high-resolution images taken from different instruments that allow us to identify smaller craters (D > 125 m) while providing sufficient coverage to support a statistically reliable sampling of crater populations, which is necessary to reduce the uncertainties in age determination. Our results indicate that Parana Valles formed during the Early Hesperian Period but that the crater density (D > 353 m) is heterogeneous inside the Parana Valles basin. The crater population decreases from the headwaters downstream recording a resurfacing event that is most likely related to the erosion of downstream sub-basins. The terrain near the source area is Late Noachian to Early Hesperian in age while terrains closer to the outlet are Early to Late Hesperian in age. Crater densities (D > 125 m) inside the valley are also heterogeneous and record several resurfacing events on the valley floor. Where the width of the valley network narrows to <2 km we found evidence of an Amazonian age eolian deposit that is a relatively thin layer of only few meters that was probably deposited as a result of topographic influences. Our results validate the reliability of several proposed age-dating techniques, but we also determined the accuracy and applicability of these techniques. Our results also demonstrate that crater populations can be used to not only determine the relative ages of valley networks, but also to map the distribution of sedimentary materials and the extent of resurfacing events that occurred after valley network formation. (C) 2010 Elsevier Inc. All rights reserved. C1 [Bouley, S.] Univ Paris 11, IDES, UMR8148, F-91405 Orsay, France. [Bouley, S.; Craddock, R. A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. [Bouley, S.; Mangold, N.; Ansan, V.] Univ Nantes, LPG Nantes, UMR6112, CNRS, F-44322 Nantes, France. RP Bouley, S (reprint author), Univ Paris 11, IDES, UMR8148, Bat 509, F-91405 Orsay, France. EM sylvain.bouley@u-psud.fr; craddockb@si.edu RI Craddock, Robert/B-3884-2013 FU NASA [NNX09AI40G]; INSU (Institut des Sciences de l'Univers) France; CNES (Centre National d'Etudes Spatiales) FX We gratefully acknowledge valuable discussions with Caleb Fassett, Monica Hoke, and Brian Hynek at the Second Workshop on Mars Valley Networks. Ana Baptista and Cathy Quantin provided useful comments throughout the preparation of this manuscript. This research was supported by NASA Grant NNX09AI40G (Mars Data Analysis Program) and the French Projet National de Planetologie (PNP) of the INSU (Institut des Sciences de l'Univers) France and CNES (Centre National d'Etudes Spatiales). NR 50 TC 17 Z9 17 U1 0 U2 5 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2010 VL 207 IS 2 BP 686 EP 698 DI 10.1016/j.icarus.2009.12.030 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 597VS UT WOS:000277790900020 ER PT J AU Vernazza, P Carry, B Emery, J Hora, JL Cruikshank, D Binzel, RP Jackson, J Helbert, J Maturilli, A AF Vernazza, P. Carry, B. Emery, J. Hora, J. L. Cruikshank, D. Binzel, R. P. Jackson, J. Helbert, J. Maturilli, A. TI Mid-infrared spectral variability for compositionally similar asteroids: Implications for asteroid particle size distributions SO ICARUS LA English DT Article DE Asteroids, Surfaces; Spectroscopy; Mineralogy; Meteorites ID THERMAL EMISSION-SPECTROSCOPY; SPITZER-SPACE-TELESCOPE; MAIN BELT ASTEROIDS; IRRADIANCE CALIBRATION; PARTICULATE SURFACES; MU-M; INFRARED OBSERVATIONS; REFLECTANCE SPECTRA; ANALOG MATERIALS; 13-MU-M SPECTRA AB We report an unexpected variability among mid-infrared spectra (IRTF and Spitzer data) of eight S-type asteroids for which all other remote sensing interpretations (e.g. VNIR spectroscopy, albedo) yield similar compositions. Compositional fitting making use of their mid-IR spectra only yields surprising alternative conclusions: (1) these objects are not "compositionally similar" as the inferred abundances of their main surface minerals (olivine and pyroxene) differ from one another by 35% and (2) carbonaceous chondrite and ordinary chondrite meteorites provide an equally good match to each asteroid spectrum. Following the laboratory work of Ramsey and Christensen (Ramsey, M.S., Christensen, P.R. [1998]. J. Geophys. Res, 103, 577-596), we interpret this variability to be physically caused by differences in surface particle size and/or the effect of space weathering processes. Our results suggest that the observed asteroids must be covered with very fine (<5 mu m) dust that masks some major and most minor spectral features. We speculate that the compositional analysis may be improved with a spectral library containing a wide variety of well characterized spectra (e.g., olivine, orthopyroxene, feldspar, iron, etc.) obtained from very fine powders. In addition to the grain size effect, space weathering processes may contribute as well to the reduction of the spectral contrast. This can be directly tested via new laboratory irradiation experiments. (C) 2010 Elsevier Inc. All rights reserved. C1 [Vernazza, P.] European Space Agcy, Res & Sci Support Dept, NL-2201 AZ Noordwijk, Netherlands. [Carry, B.] Observ Paris, Lab Etud Spatiales & Instrumentat Astrophys, F-92195 Meudon, France. [Carry, B.] European So Observ, Santiago 19, Chile. [Emery, J.] Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. [Hora, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cruikshank, D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Binzel, R. P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Jackson, J.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Helbert, J.; Maturilli, A.] DLR, Inst Planetary Res, D-12489 Berlin, Germany. RP Vernazza, P (reprint author), ESA ESTEC RSSD SCI, Keplerlaan 1, NL-2201 AZ Noordwijk, Netherlands. EM pierre.vernazza@esa.int OI Helbert, Jorn/0000-0001-5346-9505; Hora, Joseph/0000-0002-5599-4650 NR 84 TC 22 Z9 22 U1 0 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD JUN PY 2010 VL 207 IS 2 BP 800 EP 809 DI 10.1016/j.icarus.2010.01.011 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 597VS UT WOS:000277790900028 ER PT J AU Schwartz, DA Massaro, F Siemiginowska, A Worrall, DM Birkinshaw, M Marshall, H Evans, D Perlman, E Gelbord, JM Lovell, JEJ Godfrey, L Bicknell, G Ojha, R Hardcastle, M Jester, S Jorstad, S Stawarz, L AF Schwartz, D. A. Massaro, F. Siemiginowska, A. Worrall, D. M. Birkinshaw, M. Marshall, H. Evans, D. Perlman, E. Gelbord, J. M. Lovell, J. E. J. Godfrey, L. Bicknell, G. Ojha, R. Hardcastle, M. Jester, S. Jorstad, S. Stawarz, L. TI MODELING X-RAY EMISSION OF A STRAIGHT JET: PKS 0920-397 SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article; Proceedings Paper CT International Meeting on High-Energy Phenomena in Relativistic Outflows II CY OCT 26-30, 2009 CL Burnod Aires, ARGENTINA DE Quasar jets; X-ray jets; jet emission mechanisms ID INVERSE COMPTON; QUASAR JETS; RADIATION AB We summarize a study of PKS 0920-397 using our 42 ks Chandra observation in conjunction with our ATCA 20GHz image, and HST/ACS F814W and F475W images. We investigate the hypothesis that the jet X-ray emission is due to inverse-Compton ( IC) scattering on the cosmic microwave background (CMB) from the same population of relativistic electrons that give rise to the radio emission. To calculate parameters intrinsic to the source, one must finesse the fact that we do not know the true angle of the jet to our line of sight. Typical assumptions are that the Doppler factor equals the bulk Lorentz factor, or that the Lorentz factor takes some fixed numerical value. While giving useful estimates, neither assumption can be exact in general. We try different constraints to determine the jet quantities. It is plausible that the kinetic flux is constant along the jet, prior to a terminal hotspot or lobe, and with minimal bending of the jet. Alternatively, because PKS 0920-397 appears straight in projection on the sky, we might assume the jet maintains a constant angle to our line of sight. Either approach gives bulk Lorentz factors of 6 to 8, with kinetic energy flux of order 1046 erg s(-1), and with the jet at an angle 2 degrees to 4 degrees from our line of sight. C1 [Schwartz, D. A.; Massaro, F.; Siemiginowska, A.] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA 02138 USA. [Worrall, D. M.; Birkinshaw, M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Marshall, H.; Evans, D.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Perlman, E.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Gelbord, J. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Lovell, J. E. J.] Univ Tasmania, Sch Math & Phys, Hobart, Tas 7001, Australia. [Godfrey, L.; Bicknell, G.] Mt Stromlo & Siding Spring Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Ojha, R.] USN Observ, Washington, DC 20392 USA. [Hardcastle, M.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Jester, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Jorstad, S.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Stawarz, L.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, Stanford, CA 94305 USA. RP Schwartz, DA (reprint author), Smithsonian Astrophys Observ, Div High Energy Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM das@head.cfa.harvard.edu; fmassaro@head.cfa.harvard.edu; asiemiginowska@head.cfa.harvard.edu; d.worrall@bristol.ac.uk; Mark.Birkinshaw@bristol.ac.uk; hermanm@space.mit.edu; devans@space.mit.edu; eperlman@fit.edu; j.m.gelbord@durham.ac.uk; jim.lovell@utas.edu.au; lgodfrey@mso.anu.edu.au; geoff@mso.anu.edu.au; rojha@usno.navy.mil; m.j.hardcastle@herts.ac.uk; jester@mpia-hd.mpg.de; jorstad@bu.edu; stawarz@slac.stanford.edu RI Hardcastle, Martin/E-2264-2012; Godfrey, Leith/B-5283-2013; Massaro, Francesco/L-9102-2016; OI Hardcastle, Martin/0000-0003-4223-1117; Massaro, Francesco/0000-0002-1704-9850; Jorstad, Svetlana/0000-0001-9522-5453 NR 14 TC 1 Z9 1 U1 0 U2 3 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD JUN PY 2010 VL 19 IS 6 BP 879 EP 885 DI 10.1142/S0218271810017147 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 615MU UT WOS:000279140200033 ER PT J AU Weekes, TC Acciari, VA Arlen, T Aune, T Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Chow, YC Cogan, P Cui, W Duke, C Fegan, SJ Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Horan, D Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ Maier, G Mcarthur, S Mccann, A Mccutcheon, M Millis, J Moriarty, P Ong, RA Otte, AN Pandel, D Perkins, JS Pichel, A Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Rovero, A Schroedter, M Sembroski, GH Smith, AW Steele, D Swordy, SP Theiling, M Thibadeau, S Toner, JA Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weinstein, A Williams, DA Wissel, S Wood, M Zitzer, B AF Weekes, T. C. Acciari, V. A. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Chow, Y. C. Cogan, P. Cui, W. Duke, C. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Horan, D. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. Maier, G. Mcarthur, S. Mccann, A. Mccutcheon, M. Millis, J. Moriarty, P. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Rovero, A. Schroedter, M. Sembroski, G. H. Smith, A. W. Steele, D. Swordy, S. P. Theiling, M. Thibadeau, S. Toner, J. A. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weinstein, A. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. CA VERITAS Collaboration TI VERITAS: STATUS SUMMARY 2009 SO INTERNATIONAL JOURNAL OF MODERN PHYSICS D LA English DT Article; Proceedings Paper CT International Meeting on High-Energy Phenomena in Relativistic Outflows II CY OCT 26-30, 2009 CL Burnod Aires, ARGENTINA DE Gamma-ray; atmospheric Cherenkov telescopes; active galactic nuclei ID ENERGY GAMMA-RAYS; COSMIC-RAYS; IC 443; DISCOVERY; TELESCOPE; BINARY; RADIATION; EMISSION AB VERITAS is a ground-based gamma-ray observatory that uses the imaging atmospheric Cherenkov technique and operates in the very-high energy (VHE) region of the gamma-ray spectrum from 100 GeV to 50 TeV. The observatory consists of an array of four 12m-diameter imaging atmospheric Cherenkov telescopes located in southern Arizona, USA. The four-telescope array has been fully operational since September 2007, and over the last two years, VERITAS has been operating with high reliability and sensitivity. It is currently one of the most sensitive VHE observatories. This paper summarizes the status of VERITAS as of October 2009, and describes the detection of several new VHE gamma-ray sources. C1 [Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85629 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, POB 6369, Amado, AZ 85629 USA. EM tweekes@cfa.harvard.edu OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 NR 24 TC 3 Z9 3 U1 0 U2 1 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0218-2718 J9 INT J MOD PHYS D JI Int. J. Mod. Phys. D PD JUN PY 2010 VL 19 IS 6 BP 1003 EP 1012 DI 10.1142/S0218271810016932 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 615MU UT WOS:000279140200051 ER PT J AU Neufeld, MJ AF Neufeld, Michael J. TI Truth, Lies, and O-Rings: Inside the Space Shuttle Challenger Disaster SO ISIS LA English DT Book Review C1 [Neufeld, Michael J.] Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. RP Neufeld, MJ (reprint author), Smithsonian Inst, Natl Air & Space Museum, Space Hist Div, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 3 U2 12 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0021-1753 J9 ISIS JI Isis PD JUN PY 2010 VL 101 IS 2 BP 452 EP 453 PG 3 WC History & Philosophy Of Science SC History & Philosophy of Science GA 611IE UT WOS:000278807900047 ER PT J AU Cardoso, P Arnedo, MA Triantis, KA Borges, PAV AF Cardoso, Pedro Arnedo, Miquel A. Triantis, Kostas A. Borges, Paulo A. V. TI Drivers of diversity in Macaronesian spiders and the role of species extinctions SO JOURNAL OF BIOGEOGRAPHY LA English DT Article DE Araneae; Azores; Canary Islands; deforestation; habitat loss; indicator taxa; island age; Madeira; Selvagens; species-area relationship ID GENUS DYSDERA ARANEAE; OCEANIC ISLAND BIOGEOGRAPHY; EASTERN CANARY-ISLANDS; SEQUENTIAL COLONIZATION; BEETLES COLEOPTERA; AREA RELATIONSHIP; HAWAIIAN-ISLANDS; FOREST FRAGMENTS; PHOLCUS ARANEAE; ENERGY THEORY AB Aim To identify the biogeographical factors underlying spider species richness in the Macaronesian region and assess the importance of species extinctions in shaping the current diversity. Location The European archipelagos of Macaronesia with an emphasis on the Azores and Canary Islands. Methods Seven variables were tested as predictors of single-island endemics (SIE), archipelago endemics and indigenous spider species richness in the Azores, Canary Islands and Macaronesia as a whole: island area; geological age; maximum elevation; distance from mainland; distance from the closest island; distance from an older island; and natural forest area remaining per island - a measure of deforestation (the latter only in the Azores). Different mathematical formulations of the general dynamic model of oceanic island biogeography (GDM) were also tested. Results Island area and the proportion of remaining natural forest were the best predictors of species richness in the Azores. In the Canary Islands, area alone did not explain the richness of spiders. However, a hump-shaped relationship between richness and time was apparent in these islands. The island richness in Macaronesia was correlated with island area, geological age, maximum elevation and distance to mainland. Main conclusions In Macaronesia as a whole, area, island age, the large distance that separates the Azores from the mainland, and the recent disappearance of native habitats with subsequent unrecorded extinctions seem to be the most probable explanations for the current observed richness. In the Canary Islands, the GDM model is strongly supported by many genera that radiated early, reached a peak at intermediate island ages, and have gone extinct on older, eroded islands. In the Azores, the unrecorded extinctions of many species in the oldest, most disturbed islands seem to be one of the main drivers of the current richness patterns. Spiders, the most important terrestrial predators on these islands, may be acting as early indicators for the future disappearance of other insular taxa. C1 [Cardoso, Pedro; Triantis, Kostas A.; Borges, Paulo A. V.] Univ Acores, Azorean Biodivers Grp CITA A, Dept Ciencias Agr, P-9701851 Terra Cha, Angra Heroismo, Portugal. [Cardoso, Pedro] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Arnedo, Miquel A.] Univ Barcelona, Biodivers Res Inst, E-08028 Barcelona, Spain. [Arnedo, Miquel A.] Univ Barcelona, Dept Anim Biol, E-08028 Barcelona, Spain. [Triantis, Kostas A.] Univ Oxford, Ctr Environm, Biodivers Res Grp, Oxford OX1 3QY, England. RP Cardoso, P (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,MRC 105,Room E-509, Washington, DC 20013 USA. EM pcardoso@ennor.org RI Triantis, Kostas/A-1018-2009; Borges, Paulo/B-2780-2008; Cardoso, Pedro/A-8820-2008 OI Borges, Paulo/0000-0002-8448-7623; Cardoso, Pedro/0000-0001-8119-9960 FU Fundacao para a Ciencia e Tecnologia [SFRH/BPD/40688/2007, SFRH/BPD/44306/2008]; ICREA Academia; Generalitat de Catalunya; CITA-A; DRCT [M2.1.2/I/017/2007, M.2.1.2/I/003/2008]; EU FX We thank Lawrence Heaney, Robert Whittaker and Gustavo Hormiga for useful suggestions concerning previous versions of the manuscript. Antonio de Frias Martins disclosed a great deal of interesting data regarding a number of new species of snails in Sao Miguel. P.C. and K.A.T. were supported by Fundacao para a Ciencia e Tecnologia (SFRH/BPD/40688/2007 and SFRH/BPD/44306/2008, respectively). Further funding support was provided by an ICREA Academia award for excellence in research from the Generalitat de Catalunya to M.A. P.B. has been funded for several years by a science management grant from CITA-A, and recently under the DRCT projects M2.1.2/I/017/2007 and M.2.1.2/I/003/2008, and the EU projects INTERREGIII B 'ATLNTICO' (2004-2006) and BIONATURA (2006-2008). NR 71 TC 63 Z9 65 U1 2 U2 24 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0305-0270 J9 J BIOGEOGR JI J. Biogeogr. PD JUN PY 2010 VL 37 IS 6 BP 1034 EP 1046 DI 10.1111/j.1365-2699.2009.02264.x PG 13 WC Ecology; Geography, Physical SC Environmental Sciences & Ecology; Physical Geography GA 596OL UT WOS:000277694500006 ER PT J AU Munoz, AG Salazar, C Castano, J Jiggins, CD Linares, M AF Munoz, A. G. Salazar, C. Castano, J. Jiggins, C. D. Linares, M. TI Multiple sources of reproductive isolation in a bimodal butterfly hybrid zone SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE Haldane's rule; Heliconius; parapatric; post-mating isolation; pre-mating isolation; speciation ID ECOLOGICAL SPECIATION; HELICONIUS-CYDNO; SEXUAL SELECTION; POSTZYGOTIC ISOLATION; MATING FREQUENCIES; HALDANES RULE; EVOLUTION; LEPIDOPTERA; MELPOMENE; INTROGRESSION AB An important evolutionary question concerns whether one or many barriers are involved in the early stages of speciation. We examine pre- and post-zygotic reproductive barriers between two species of butterflies (Heliconius erato chestertonii and H. e. venus) separated by a bimodal hybrid zone in the Cauca Valley, Colombia. We show that there is both strong pre- and post-mating reproductive isolation, together leading to a 98% reduction in gene flow between the species. Pre-mating isolation plays a primary role, contributing strongly to this isolation (87%), similar to previous examples in Heliconius. Post-mating isolation was also strong, with absence of Haldane's rule, but an asymmetric reduction in fertility (< 11%) in inter-specific crosses depending on maternal genotype. In summary, this is one of the first examples of post-zygotic reproductive isolation playing a significant role in early stages of parapatric speciation in Heliconius and demonstrates the importance of multiple barriers to gene flow in the speciation process. C1 [Munoz, A. G.; Salazar, C.; Castano, J.; Linares, M.] Univ Los Andes, Inst Genet, Bogota, Colombia. [Salazar, C.; Jiggins, C. D.] Univ Cambridge, Dept Zool, Cambridge, England. [Salazar, C.] Smithsonian Trop Res Inst, Balboa, Panama. RP Munoz, AG (reprint author), Univ Los Andes, Inst Genet, Carrera 1 18A-70,POB 4976, Bogota, Colombia. EM as-munoz@uniandes.edu.co RI Jiggins, Chris/B-9960-2008; Salazar, camilo/A-1647-2010; Linares, Mauricio/I-3509-2016 OI Jiggins, Chris/0000-0002-7809-062X; Salazar, camilo/0000-0001-9217-6588; Linares, Mauricio/0000-0002-1021-0226 FU Facultad de Ciencias, Universidad de los Andes; Banco de la Republica; COLCIENCIAS [120 440 520 138]; Royal Society University; Leverhulme Trust FX We thank members of Instituto de Genetica at Bogota for their help in maintaining the butterflies stocks at La Vega. AM was partially supported by Facultad de Ciencias, Universidad de los Andes. ML was funded by Banco de la Republica, and private donations (Continautos S.A., Proficol El Carmen S.A. and Didacol S.A). Both ML and CS received funds from COLCIENCIAS grant number 120 440 520 138. CJ was fund by a Royal Society University Research Fellowship and a Leverhulme Trust grant. NR 42 TC 19 Z9 19 U1 1 U2 25 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD JUN PY 2010 VL 23 IS 6 BP 1312 EP 1320 DI 10.1111/j.1420-9101.2010.02001.x PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 596UD UT WOS:000277710100019 PM 20456567 ER PT J AU Wolfe, JD Ryder, TB Pyle, P AF Wolfe, Jared D. Ryder, Thomas B. Pyle, Peter TI Using molt cycles to categorize the age of tropical birds: an integrative new system SO JOURNAL OF FIELD ORNITHOLOGY LA English DT Article DE age classification; molt; molt cycle; plumage; tropical birds ID LANDBIRDS; CRITERIA; PATTERNS AB Accurately differentiating age classes is essential for the long-term monitoring of resident New World tropical bird species. Molt and plumage criteria have long been used to accurately age temperate birds, but application of temperate age-classification models to the Neotropics has been hindered because annual life-cycle events of tropical birds do not always correspond with temperate age-classification nomenclature. However, recent studies have shown that similar molt and plumage criteria can be used to categorize tropical birds into age classes. We propose a categorical age-classification system for tropical birds based on identification of molt cycles and their inserted plumages. This approach allows determination of the age ranges (in months) of birds throughout plumage succession. Although our proposed cycle-based system is an improvement over temperate calendar-based models, we believe that combining both systems provides the most accurate means of categorizing age and preserving age-related data. Our proposed cycle-based age-classification system can be used for all birds, including temperate species, and provides a framework for investigating molt and population dynamics that could ultimately influence management decisions. C1 [Wolfe, Jared D.] US Forest Serv, USDA, Pacific SW Res Stn, Redwood Sci Lab, Arcata, CA 95521 USA. [Wolfe, Jared D.] Louisiana State Univ, Sch Renewable Nat Resources, Baton Rouge, LA 70803 USA. [Wolfe, Jared D.] Louisiana State Univ, AgCtr, Baton Rouge, LA 70803 USA. [Ryder, Thomas B.] Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20013 USA. [Pyle, Peter] Inst Bird Populat, Point Reyes Stn, CA 94956 USA. RP Wolfe, JD (reprint author), US Forest Serv, USDA, Pacific SW Res Stn, Redwood Sci Lab, 1700 Bayview Dr, Arcata, CA 95521 USA. EM jwolfe5@lsu.edu FU International Center for Tropical Ecology; AFO's Alexander Bergstrom Award; National Geographic Society [7113-01]; National Science Foundation [IBN 0235141, IOB 0508189, OISE 0513341] FX Special thanks to L. Wolfe and D. Wilde for their help with figure formatting. Thanks also to personnel at the Klamath Bird Observatory, Institute for Bird Populations, Point Reyes Bird Observatory, and Redwood Sciences Laboratory. Special thanks to C. J. Ralph, D. and C. Romo, K. Swing, J. Guerra, E. Johnson and all the staff at the Tiputini Biodiversity Station and Caribbean Conservation Corporation for their tireless logistical and field support. IACUC protocol number 5-12-20. This research was conducted in accordance with permit number 13-IC-FAUDFN, Ministerio de Ambiente, Distrito Forestal Napo, Tena, Ecuador. We thank them for allowing us to conduct our research at the Tiputini Biodiversity Station. Funding was provided by the International Center for Tropical Ecology, AFO's Alexander Bergstrom Award, National Geographic Society (7113-01), and National Science Foundation (IBN 0235141, IOB 0508189, OISE 0513341). This is contribution #386 of the Institute for Bird Populations. This is also a contribution of Land Bird Monitoring of the Americas (LaMNA) and the Tortuguero Integrated Bird Monitoring Project (TIBMP). NR 23 TC 17 Z9 18 U1 3 U2 15 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0273-8570 J9 J FIELD ORNITHOL JI J. Field Ornithol. PD JUN PY 2010 VL 81 IS 2 BP 186 EP 194 DI 10.1111/j.1557-9263.2010.00276.x PG 9 WC Ornithology SC Zoology GA 600HB UT WOS:000277975000008 ER PT J AU Gordon, IE Chance, K Flaud, JM AF Gordon, Iouli E. Chance, Kelly Flaud, Jean-Marie TI Special issue dedicated to Laurence S. Rothman on the occasion of his 70(th) birthday SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Editorial Material C1 [Gordon, Iouli E.; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Flaud, Jean-Marie] Univ Paris Est, F-94010 Creteil, France. [Flaud, Jean-Marie] CNRS, F-94010 Creteil, France. [Flaud, Jean-Marie] Univ Paris 07, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM igordon@cfa.harvard.edu OI Chance, Kelly/0000-0002-7339-7577; Gordon, Iouli/0000-0003-4763-2841 NR 0 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 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUN PY 2010 VL 111 IS 9 SI SI BP 1041 EP 1042 DI 10.1016/j.jqsrt.2010.02.008 PG 2 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 593OY UT WOS:000277469800001 ER PT J AU Gordon, IE Kassi, S Campargue, A Toon, GC AF Gordon, Iouli E. Kassi, Samir Campargue, Alain Toon, Geoffrey C. TI First identification of the a(1) Delta(g)-X-3 Sigma(-)(g) electric quadrupole transitions of oxygen in solar and laboratory spectra SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Electric quadrupole; Singlet delta; Oxygen; Solar spectrum; Cavity ring down spectroscopy ID CAVITY RINGDOWN SPECTROSCOPY; LINE PARAMETERS COMPILATION; 1.5 MU-M; ATMOSPHERIC OXYGEN; MOLECULAR-OXYGEN; BAND; INTENSITIES; EINSTEIN; COEFFICIENTS; ISOTOPOMERS AB Electric quadrupole transitions in the a(1)Delta(g)-X-3 Sigma(-)(g) band of O-16(2) near 1.27 mu m are reported for the first time. They were first detected in atmospheric solar spectra acquired with a ground-based Fourier transform spectrometer (FTS) in Park Falls, WI. Subsequently high-sensitivity ON cavity ring down spectroscopy (CW-CRDS) experiments were carried out at Grenoble University in the 7717-7917 cm(-1) region in order to provide quantitative intensity information for the electric quadrupole transitions. Measured intensities were used as input data for the calculation of the complete list of electric quadrupole transitions with Delta J= +/- 2, +/- 1 and 0. The calculation was carried out for the intermediate coupling case and assuming that these transitions are possible only through mixing of the Omega=0 component of the ground electronic state and b(1)Sigma(+)(g) state induced by spin-orbit coupling. The calculated line list agrees well with experimental measurements and was used to improve the residuals of the fitted solar atmospheric spectrum. Emission probability for the electric quadrupole band was determined to be (1.02 +/- 0.10) x 10(-6)s(-1). (C) 2010 Elsevier Ltd. All rights reserved. C1 [Gordon, Iouli E.] Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. [Kassi, Samir; Campargue, Alain] Univ Grenoble 1, CNRS, Spectrometrie Phys Lab, F-38402 St Martin Dheres, France. [Toon, Geoffrey C.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Gordon, IE (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. EM igordon@cfa.harvard.edu OI Gordon, Iouli/0000-0003-4763-2841 FU NASA; ANR; NASA EOS HITRAN FX The authors are grateful to Rebecca Washenfelder and Jean-Francois Blavier who set up the TCCON FTS at Park Falls, WI, and recorded the atmospheric solar absorption spectra used here. We acknowledge Paul Wennberg for the use of these data and the NASA Carbon Cycle program which funds TCCON. We also thank Andrew Orr-Ewing for providing such a good O2 magnetic dipole line list, that the missing quadrupole lines became so prominent. We also thank Robert Field and Charles Miller for fruitful discussions and Laurence Rothman and Robert Gamache for providing input parameters and the program for calculation of HITRAN line positions calculation. The HITRAN database managed for over 35 years by Dr. Rothman is an essential tool in many fields. The authors have all benefited from using it many times and are honored to contribute to it or validate its data. Part of this work was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA and at Grenoble University under the ANR project "IDEO". IEG is supported through NASA EOS HITRAN Grant. NR 35 TC 22 Z9 22 U1 0 U2 11 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUN PY 2010 VL 111 IS 9 SI SI BP 1174 EP 1183 DI 10.1016/j.jqsrt.2010.01.008 PG 10 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 593OY UT WOS:000277469800012 ER PT J AU Chance, K Kurucz, RL AF Chance, K. Kurucz, R. L. TI An improved high-resolution solar reference spectrum for earth's atmosphere measurements in the ultraviolet, visible, and near infrared SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article DE Solar spectrum; Remote sensing; Atmospheric spectroscopy ID OZONE MONITORING INSTRUMENT; RAYLEIGH-SCATTERING; NM AB We have developed an improved solar reference spectrum for use in the analysis of atmospheric spectra from vacuum wavelengths of 200.07 through 1000.99 nm. The spectrum is developed by combining high spectral resolution ground-based and balloon-based solar measurements with lower spectral resolution but higher accuracy irradiance information. The new reference spectrum replaces our previous reference spectrum, and its derivatives, for use in a number of physical applications for analysis of atmospheric spectra, including: wavelength calibration; determination of instrument transfer (slit) functions; Ring effect (Raman scattering) correction; and correction for spectral undersampling of atmospheric spectra, particularly those that are dilute in absorbers. The applicability includes measurements from the COME. SCIAMACHY, OMI, and OMPS satellite instruments as well as aircraft-, balloon-, and ground-based measurements. Published by Elsevier Ltd. C1 [Chance, K.; Kurucz, R. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chance, K (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM Kchance@CfA.Harvard.edu OI Chance, Kelly/0000-0002-7339-7577 FU NASA; Smithsonian Institution FX We congratulate Dr. Laurence Rothman on the occasion of his 70th birthday. We gratefully acknowledge substantial contributions to this work by G.P. Anderson and the late L.A. Hall and also note with sadness the recent passing of J. Brault, whose genius in Fourier transform spectroscopy will be sorely missed. Input from the anonymous reviewers made this paper stronger and more useful. This research has been supported by NASA and the Smithsonian Institution. NR 30 TC 90 Z9 94 U1 2 U2 16 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD JUN PY 2010 VL 111 IS 9 SI SI BP 1289 EP 1295 DI 10.1016/j.jqsrt.2010.01.036 PG 7 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 593OY UT WOS:000277469800022 ER PT J AU Schultz, RA Hauber, E Kattenhorn, SA Okubo, CH Watters, TR AF Schultz, Richard A. Hauber, Ernst Kattenhorn, Simon A. Okubo, Chris H. Watters, Thomas R. TI Interpretation and analysis of planetary structures SO JOURNAL OF STRUCTURAL GEOLOGY LA English DT Review DE Planetary structural geology; Faulting; Folding; Deformation bands; Joints; Fracture mechanics ID ORBITER LASER ALTIMETER; CANYONLANDS NATIONAL-PARK; LENGTH SCALING RELATIONS; NORMAL-FAULT SYSTEMS; BLIND THRUST FAULTS; ICE SHELL THICKNESS; EXPRESS HRSC DATA; VALLES-MARINERIS; NONSYNCHRONOUS ROTATION; DEFORMATION BANDS AB Structural geology is an integral part of planetary science. Planetary structures provide the framework for determining the character and sequence of crustal deformation while simultaneously establishing the observational basis required to test geodynamic hypotheses for the deformation of planetary and satellite lithospheres. The availability of datasets that record spatial and topographic information with a resolution that matches or, in many cases, exceeds, what is available for Earth-based studies permits the deformation of several planets and satellites to be investigated down to the local or outcrop scales. The geometry and kinematics of common planetary structures such as joints, igneous dikes, deformation bands, faults, and folds can be determined with confidence from their distinctive morphologic and topographic signatures, enabling the structural histories and deformation magnitudes to be determined. Segmentation, displacement profiles, relay ramps, footwall anticlines, displacement-controlled depocenters, and other well-known characteristics of terrestrial normal fault and graben systems reveal the sequence and processes of fault growth in numerous planetary examples. Systems of thrust faults having both blind and surface-breaking components are important elements on several bodies including Mercury, the Moon, and Mars. Strike-slip faults have been identified on bodies including Mars and Europa with oblique extension found on Ganymede. Using field-based studies of Earth-based structures as a guide, planetary structures provide a means to explore and evaluate the causative stresses. Despite the wide range in structural styles across the solar system, plate tectonics is recognized only on the Earth, with the other planets and satellites deforming in the absence of large-scale horizontal motions and attendant plate recycling. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Schultz, Richard A.] Univ Nevada, Dept Geol Sci & Engn 172, Geomech Rock Fracture Grp, Reno, NV 89557 USA. [Hauber, Ernst] DLR Inst Planetenforsch, D-12489 Berlin, Germany. [Kattenhorn, Simon A.] Univ Idaho, Dept Geol Sci, Moscow, ID 83844 USA. [Okubo, Chris H.] US Geol Survey, Flagstaff, AZ 86001 USA. [Watters, Thomas R.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Schultz, RA (reprint author), Univ Nevada, Dept Geol Sci & Engn 172, Geomech Rock Fracture Grp, Reno, NV 89557 USA. EM schultz@mines.unr.edu RI Schultz, Richard/J-4015-2015 OI Schultz, Richard/0000-0003-3198-5263 FU NASA's Planetary Geology and Geophysics [NNX06AC12G, NNX08AK71G, NNX08AQ94G, NNX08AM19G]; Mars Data Analysis Program [NNX06AE01G]; NASA [NNX07AR60G]; Helmoltz Association FX Thorough and helpful reviews by David Peacock and Robert Pappalardo helped streamline and sharpen the final paper. This work was supported by grants from NASA's Planetary Geology and Geophysics Program and the Mars Data Analysis Program to RAS. SAK acknowledges grants from NASA's Planetary Geology and Geophysics (NNX06AC12G and NNX08AK71G) and Outer Planets Research (NNX08AQ94G) Programs. CHO acknowledges support through Mars Data Analysis Program grant NNX06AE01G. TRW acknowledges support from NASA's Planetary Geology and Geophysics Program grant NNX08AM19G and from NASA grant NNX07AR60G. EH was partly supported by the Helmoltz Association through the research alliance "Planetary Evolution and Life". Thanks to Jason Barnes, Terry Hurford, Christina Coulter, Paul Schenk, and Christian Klimczak for providing their expertise on various facets of this work. We thank Marie Dowling of the National Space Science Data Center for providing the Apollo 10 image of Rima Ariadaeus. NR 209 TC 17 Z9 17 U1 1 U2 28 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0191-8141 J9 J STRUCT GEOL JI J. Struct. Geol. PD JUN PY 2010 VL 32 IS 6 BP 855 EP 875 DI 10.1016/j.jsg.2009.09.005 PG 21 WC Geosciences, Multidisciplinary SC Geology GA 663DG UT WOS:000282862600013 ER PT J AU Baeza, JA Bolanos, JA Fuentes, S Hernandez, JE Lira, C Lopez, R AF Antonio Baeza, J. Bolanos, Juan A. Fuentes, Soledad Hernandez, Jesus E. Lira, Carlos Lopez, Regulo TI Molecular phylogeny of enigmatic Caribbean spider crabs from the Mithrax-Mithraculus species complex (Brachyura: Majidae: Mithracinae): ecological diversity and a formal test of genera monophyly SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE Mithrax; Mithraculus; Mithracinae; emerald crab; spiny ciab; spider crab; Venezuela ID LARVAL STAGES; RIBOSOMAL-RNA; DECAPODA; EVOLUTION; CRUSTACEA; MAJOIDEA; REAPPRAISAL; CHARACTERS; MORPHOLOGY; MUTUALISM AB Crabs from the Mithrax - Mithraculus species complex are known for their diversity of lifestyles, habitats, and coloration Tins group Includes small, colourful, symbiotic species and much larger, reef-dwelling crabs targeted by fishermen The evolutionary relationships between the species within this complex are not well-defined Previous studies based upon morphological characters have proposed the separation of tins complex into two genera (Mithrax and Mithraculus), but cladistic analyses based upon larval characters do not support this division A molecular phylogeny of the group may help to resolve this long-standing taxonomic question and shed light on the ecological conditions driving the diversity of these crabs Using a 550-bp alignment of the 16S rRNA mitochondria! DNA segment we examined the phylogenetic relationships between 8 species within the Mithrax - Mithraculus complex native to the Caribbean The resulting phylogeny indicates that this complex is paraphykite, as it includes the genus Microphrys The analyses revealed a well-supported, monophyletic group containing four species of Mithraculus (M cinctimanus, M coryphe, M sculptus and M forceps) and supported one pair of sister species from the genus Mithrax (M caribbaeus and M spinosissimus) No complete segregation of species, according to genera, was evident, however, from tree topologies Bayesian-factor analyses revealed strong support for the unconstrained tree instead of alternative trees in winch monophyly of the two genera was forced Thus, the present molecular phylogeny does not support the separation of the species within tins complex Into the genera Mithrax and Mithraculus A review of the literature demonstrated considerable phenotypic variation within monophyletic clades in this group C1 [Antonio Baeza, J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Bolanos, Juan A.; Hernandez, Jesus E.; Lira, Carlos; Lopez, Regulo] Univ Oriente, Grp Invest Carcinol, Escuela Ciencias Aplicadas Mar, Isla Margarita, Venezuela. [Fuentes, Soledad] NOAA Fisheries, Milford Lab, Milford, CT 06460 USA. RP Baeza, JA (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. OI Baeza, Juan Antonio/0000-0002-2573-6773 NR 50 TC 5 Z9 5 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 EI 1469-7769 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD JUN PY 2010 VL 90 IS 4 BP 851 EP 858 DI 10.1017/S0025315409991044 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 620PE UT WOS:000279511000024 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Historical Dictionary of Film Noir SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2010 VL 135 IS 10 BP 102 EP + PG 2 WC Information Science & Library Science SC Information Science & Library Science GA 604TA UT WOS:000278300200122 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Historical Dictionary of Middle Eastern Cinema SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2010 VL 135 IS 10 BP 102 EP 102 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 604TA UT WOS:000278300200121 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Clothing Through American History: The Federal Era Through Antebellum, 1786-1860 SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD JUN 1 PY 2010 VL 135 IS 10 BP 108 EP 108 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 604TA UT WOS:000278300200131 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Baby Boom: People and Perspectives SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 1 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 JUN 1 PY 2010 VL 135 IS 10 BP 110 EP 110 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 604TA UT WOS:000278300200132 ER PT J AU Goodman, SM Helgen, KM AF Goodman, Steven M. Helgen, Kristofer M. TI Species limits and distribution of the Malagasy carnivoran genus Eupleres (Family Eupleridae) SO MAMMALIA LA English DT Article DE distribution; Eupleres; Madagascar; morphology; taxonomy ID IXODOIDEA IXODIDAE; MADAGASCAR; ORIGIN AB A review was conducted of members of the endemic Malagasy carnivoran genus Eupleres (family Eupleridae) based on published and unpublished records and museum specimens. Classically, one species has been recognized in this poorly known genus - E. goudotii, divided into two geographical forms with non-overlapping distributions: E. g. goudotii distributed in the mesic forests of the east and E. g. major found in the dry areas of the northwest. Drawing on external and craniodental comparisons, we demonstrate that these two forms are highly distinctive morphologically and can be readily distinguished from each another. Furthermore, there is some evidence that they both can occur on the slopes of Montagne d'Ambre in the far north of the island. On this basis, we recognize these taxa as distinct species, E. goudotii and E. major. C1 [Goodman, Steven M.] Field Museum Nat Hist, Chicago, IL 60605 USA. [Goodman, Steven M.] Vahatra, Antananarivo 101, Madagascar. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Goodman, SM (reprint author), Field Museum Nat Hist, 1400 S Lake Shore Dr, Chicago, IL 60605 USA. EM sgoodman@fieldmuseum.org NR 53 TC 5 Z9 11 U1 1 U2 11 PU WALTER DE GRUYTER & CO PI BERLIN PA GENTHINER STRASSE 13, D-10785 BERLIN, GERMANY SN 0025-1461 J9 MAMMALIA JI Mammalia PD JUN PY 2010 VL 74 IS 2 BP 177 EP 185 DI 10.1515/MAMM.2010.018 PG 9 WC Zoology SC Zoology GA 622CI UT WOS:000279636100008 ER PT J AU Matthew, S Ratnayake, R Becerro, MA Ritson-Williams, R Paul, VJ Luesch, H AF Matthew, Susan Ratnayake, Ranjala Becerro, Mikel A. Ritson-Williams, Raphael Paul, Valerie J. Luesch, Hendrik TI Intramolecular Modulation of Serine Protease Inhibitor Activity in a Marine Cyanobacterium with Antifeedant Properties SO MARINE DRUGS LA English DT Article DE cyanobacteria; Lyngbya; antifeedant activity; serine protease inhibitors; cyclodepsipeptides ID BLUE-GREEN-ALGA; SECONDARY METABOLITES; LYNGBYA-CONFERVOIDES; PLANKTOTHRIX-RUBESCENS; ELASTASE INHIBITORS; CHEMICAL DETERRENCE; CYCLIC-PEPTIDES; FLORIDA; BLOOM; WATERBLOOM AB Extracts of the Floridian marine cyanobacterium Lyngbya cf. confervoides were found to deter feeding by reef fish and sea urchins (Diadema antillarum). This antifeedant activity may be a reflection of the secondary metabolite content, known to be comprised of many serine protease inhibitors. Further chemical and NMR spectroscopic investigation led us to isolate and structurally characterize a new serine protease inhibitor 1 that is formally derived from an intramolecular condensation of largamide D (2). The cyclization resulted in diminished activity, but to different extents against two serine proteases tested. This finding suggests that cyanobacteria can endogenously modulate the activity of their protease inhibitors. C1 [Becerro, Mikel A.; Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Matthew, Susan; Ratnayake, Ranjala; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. RP Paul, VJ (reprint author), Smithsonian Marine Stn, 701 Seaway Dr, Ft Pierce, FL 34949 USA. EM susmatt@ufl.edu; rratnayake@ufl.edu; mikel@ceab.csic.es; williams@si.edu; paul@si.edu; luesch@cop.ufl.edu RI Becerro, Mikel/A-5325-2008; Matthew, Susan/E-3817-2012; OI Becerro, Mikel/0000-0002-6047-350X FU NIGMS [P41GM086210]; Smithsonian Marine Science Network FX This work was funded by NIGMS grant P41GM086210. Research conducted in Belize was supported by the Smithsonian Marine Science Network. We thank A. Erickson, G. Harrison, C. Ross, K. Arthur, S. Reed, and A. Capper for assistance with collections and extraction of the cyanobacterium over many years, which allowed us to thoroughly investigate its natural products chemistry. This is contribution #820 from the Smithsonian Marine Station at Fort Pierce and contribution #883 from the Caribbean Coral Reef Ecosystems Program. NR 33 TC 9 Z9 9 U1 1 U2 7 PU MDPI AG PI BASEL PA KANDERERSTRASSE 25, CH-4057 BASEL, SWITZERLAND SN 1660-3397 J9 MAR DRUGS JI Mar. Drugs PD JUN PY 2010 VL 8 IS 6 BP 1803 EP 1816 DI 10.3390/md8061803 PG 14 WC Chemistry, Medicinal SC Pharmacology & Pharmacy GA 631KZ UT WOS:000280347000007 PM 20631871 ER PT J AU Meyer, J AF Meyer, James TI Guests SO MASSACHUSETTS REVIEW LA English DT Fiction, Creative Prose C1 [Meyer, James] Emory Univ, Atlanta, GA 30322 USA. RP Meyer, J (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU UNIV MASSACHUSETTS MASSACHUSETTS REVIEW PI AMHERST PA MEMORIAL HALL, AMHERST, MA 01003 USA SN 0025-4878 J9 MASS REV JI Mass. Rev. PD SUM PY 2010 VL 51 IS 2 BP 362 EP 377 PG 16 WC Literary Reviews SC Literature GA 613NZ UT WOS:000278987300019 ER PT J AU Xu, XW Walters, C Antolin, MF Alexander, ML Lutz, S Ge, S Wen, J AF Xu, Xinwei Walters, Christina Antolin, Michael F. Alexander, Mara L. Lutz, Sue Ge, Song Wen, Jun TI Phylogeny and biogeography of the eastern Asian-North American disjunct wild-rice genus (Zizania L., Poaceae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Adh1a gene; Biogeography; Intercontinental disjunction; Wild-rice; Zizania ID FLORISTIC DISJUNCTION; NONCODING REGIONS; UNIVERSAL PRIMERS; GEOGRAPHIC RANGE; CHLOROPLAST DNA; EVOLUTION; SEQUENCES; AMPLIFICATION; MITOCHONDRIAL; INFERENCE AB The wild-rice genus Zizania includes four species disjunctly distributed in eastern Asia and North America, with three species (Z. aquatica, Z. palustris, and Z. texana) in North America and one (Z. latifolia) in eastern Asia. The phylogeny of Zizania was constructed using sequences of seven DNA fragments (atpB-rbcL, matK, rps16, trnL-F, trnH-psbA, nad1, and Adh1a) from chloroplast, mitochondrial, and nuclear genomes. Zizania is shown to be monophyletic with the North American species forming a clade and the eastern Asian Z. latifolia sister to the North American clade. The divergence between the eastern Asian Z. latifolia and the North American clade was dated to be 3.74(95% HPD: 1.04-7.23) million years ago (mya) using the Bayesian dating method with the combined atpB-rbcL, matK, rps16, trnL-F, and nad1 data. Biogeographic analyses using a likelihood method suggest the North American origin of Zizania and its migration into eastern Asia via the Bering land bridge. Among the three North American species, the organellar data and the haplotype network of the nuclear Adh1a gene show a close relationship between Z. palustris and the narrowly distributed endangered species Z. texana. Bayesian dating estimated the divergence of North American Zizania to be 0.71 (95% HPD: 0.12-1.54) mya in the Pleistocene. The non-monophyly of Z. palustris and Z. aquatica in the organellar and nuclear data is most likely caused by incomplete lineage sorting, yet low-frequency unidirectional introgression of Z palustris into Z. aquatica is present in the nuclear data as well. Published by Elsevier Inc. C1 [Lutz, Sue; Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. [Xu, Xinwei] Wuhan Univ, Freshwater Ecol Field Stn Liangzi Lake, Wuhan 430072, Peoples R China. [Walters, Christina] ARS, USDA, Natl Ctr Genet Resources Preservat, Ft Collins, CO 80521 USA. [Antolin, Michael F.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Alexander, Mara L.] San Marcos Natl Fish Hatchery & Technol Ctr, San Marcos, TX 78666 USA. [Ge, Song; Wen, Jun] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC 166, Washington, DC 20013 USA. EM wenj@si.edu FU John D. and Catherine T. MacArthur Foundation; Chinese Academy of Sciences; National Natural Science Foundation of China; Laboratory of Analytical Biology of the Smithsonian Institution FX This study was supported by grants from the John D. and Catherine T. MacArthur Foundation (to J. Wen), the Chinese Academy of Sciences (to J. Wen and S. Ge) and the National Natural Science Foundation of China (to J. Wen and T.-S. Yi), and by the Laboratory of Analytical Biology of the Smithsonian Institution. We thank Patrick Reeves, two anonymous reviewers, and Associate Editor Lena Hileman for constructive comments, and Guy Jolicoeur, Greg Kearns, Ken and Bess Weston, Dan Redondo, Dail Laughinghouse and Jinmei Lu for advice and field assistance. The views presented here do not necessarily reflect those of the U.S. Fish and Wildlife Service. NR 79 TC 18 Z9 20 U1 4 U2 24 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 JUN PY 2010 VL 55 IS 3 BP 1008 EP 1017 DI 10.1016/j.ympev.2009.11.018 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 596YM UT WOS:000277721800020 PM 19944174 ER PT J AU Hubert, N Delrieu-Trottin, E Irisson, JO Meyer, C Planes, S AF Hubert, Nicolas Delrieu-Trottin, Erwan Irisson, Jean-Olivier Meyer, Christopher Planes, Serge TI Identifying coral reef fish larvae through DNA barcoding: A test case with the families Acanthuridae and Holocentridae SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Coral reef; Barcoding; Larvae; Identification; Mitochondrial DNA ID ANIMAL MITOCHONDRIAL-DNA; COMMUNITY ECOLOGY; DIVERSITY; REPLENISHMENT; RECRUITMENT; POPULATIONS; EVOLUTION; TAXONOMY AB A reference collection of COI barcode (650 bp) for the Pacific Society Islands has been constituted for 22 species of Acanthuridae and 16 species of Holocentridae. Divergence between congeneric species was on average 20-fold to 87-fold higher than divergence between conspecific sequences and this set of DNA-identifiers was used to identify 40 larvae of both families. All larvae sequenced could be identified to species using DNA-barcodes. Pools of larvae constitute multi-specific assemblages and no additional species compared to adult reef communities were sampled in larval pools, suggesting that the larval assemblages originated from adult communities on neighboring reefs. (C) 2010 Elsevier Inc. All rights reserved. C1 [Hubert, Nicolas] Univ Reunion, Lab ECOMAR, St Denis 97715 9, Reunion. [Delrieu-Trottin, Erwan; Irisson, Jean-Olivier; Planes, Serge] Univ Perpignan, Ctr Biol & Ecol Trop & Mediteraneenne, CNRS, Equipe Recifs Coralliens,UPVD,EPHE,UMR 5244, F-66860 Perpignan, France. [Meyer, Christopher] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Planes, Serge] CNRS, EPHE, CRIOBE, UMS 2978, Moorea 98729, Fr Polynesia. RP Hubert, N (reprint author), Univ Reunion, Lab ECOMAR, 15 Ave Rene Cassin,BP 7151, St Denis 97715 9, Reunion. EM myloplus@excite.com FU ACI MOOREA; Agence Nationale de la Recherche (ANR); Delegation a la recherche du Haut Commissariat de la Republique en Polynesie; DIREN of French Polynesia; Agence Nationale de la Recherche (France: BIOTAS) [ANR-2006-BDIV002] FX This study was conducted during the Master 2 degree from PARIS VI of Erwan Delrieu-Trottin on the ecology of larval assemblages in the "Centre de Biologie et d'Ecologie Tropicale et Mediteraneenne" in Perpignan under the supervision of Serge Planes, Jean-Olivier Irisson and Nicolas Hubert. The authors wish to thank the crew of the N.O. Alis and the scientific team (R. Crechriou, C. Paris, C. Guigand, L. Carassou, D. Lecchini, P. Ung). Many thanks go to R.K. Cowen for providing facilities with the MOCNESS and J. Grondin for his help with the sorting of MOCNESS samples. The authors are also grateful to A. Fukui, D. Johnson, J.M. Leis, M.J. Miller, D. Richardson, and A. Suntsov for their advice on the identification of fish larvae, Elisabeth Rochel for genetic lab support, Emmanuel Paradis for his help with APE scripts, Benjamin Ciotti for his help in improving the manuscript and the staff of the CRIOBE, in Moorea, for pre and post-fieldwork support. Funding for this work came from the ACI MOOREA, the Agence Nationale de la Recherche (ANR, project Bioaqua), the "Delegation a la recherche du Haut Commissariat de la Republique en Polynesie", and the DIREN of French Polynesia. This work was supported by 'Agence Nationale de la Recherche' (France: BIOTAS, ANR-2006-BDIV002). NR 38 TC 43 Z9 44 U1 2 U2 26 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 JUN PY 2010 VL 55 IS 3 BP 1195 EP 1203 DI 10.1016/j.ympev.2010.02.023 PG 9 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 596YM UT WOS:000277721800037 PM 20188843 ER PT J AU Liu, JR Wang, QD Li, ZY Peterson, JR AF Liu, Jiren Wang, Q. Daniel Li, Zhiyuan Peterson, John R. TI X-ray spectroscopy of the hot gas in the M31 bulge SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE ISM: general; galaxies: bulges; galaxies: individual: M31; X-rays: galaxies ID EARLY-TYPE GALAXIES; XMM-NEWTON; PLANETARY-NEBULAE; ELLIPTIC GALAXIES; CHANDRA OBSERVATIONS; GALACTIC BULGE; CENTRAL REGION; EVOLUTION; EMISSION; ABUNDANCES AB We present an X-ray spectroscopic study of the nuclear region of the M31 bulge, based on observations of the XMM-Newton Reflection Grating Spectrometers. The obtained high-resolution grating spectra clearly show individual emission lines of highly ionized iron and oxygen, which unambiguously confirm the presence of diffuse hot gas in the bulge, as indicated from previous X-ray CCD imaging studies. We model the spectra with detailed Monte Carlo simulations, which provide a robust spectroscopic estimate of the hot gas temperature similar to 0.29 keV and the O/Fe ratio similar to 0.3 solar. The results indicate that iron ejecta of Type Ia supernovae are partly mixed with the hot gas. The observed spectra show an intensity excess at the O vii triplet, which most likely represents emission from charge exchanges at the interface between the hot gas and a known cool gas spiral in the same nuclear region. C1 [Liu, Jiren; Wang, Q. Daniel] Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. [Li, Zhiyuan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Peterson, John R.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Liu, JR (reprint author), Univ Massachusetts, Dept Astron, Amherst, MA 01002 USA. EM jiren@astro.umass.edu FU ESA; USA (NASA); NASA/SAO [GO8-9088B] FX We thank the referee for useful comments. This research has made use of XMM-Newton archival data. XMM-Newton is an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). This research is partially supported by NASA/SAO through the grant GO8-9088B. NR 32 TC 15 Z9 15 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2010 VL 404 IS 4 BP 1879 EP 1885 DI 10.1111/j.1365-2966.2010.16404.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600JG UT WOS:000277981400018 ER PT J AU de Oliveira-Costa, A Capodilupo, J AF de Oliveira-Costa, Angelica Capodilupo, John TI Clustering at 74 MHz SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; astronomical data bases: miscellaneous ID 21 CENTIMETER FLUCTUATIONS; SQUARE KILOMETER ARRAY; RADIO-SOURCES; REIONIZATION OBSERVATORIES; POWER SPECTRUM; CM TOMOGRAPHY; POINT SOURCES; SKY SURVEY; EPOCH; SENSITIVITY AB In order to construct accurate point sources simulations at the frequencies relevant to 21-cm experiments, the angular correlation of radio sources must be taken into account. Using the 74 MHz VLA Low-Frequency Sky Survey, we measured the angular two-point correlation function, w(theta). We obtain the first measurement of clustering at the low frequencies relevant to 21-cm tomography. We find that a single power law with shape w(theta) = A theta(-gamma) fits well the data. For a 10 degrees galactic cut, with all data at declinations delta < -10 degrees also discarded, and a flux limit of S = 770 mJy, we obtain a slope of gamma = (-1.21 +/- 0.35). This value of gamma is consistent with that measured from other radio catalogues at the metre wavelengths. The amplitude of clustering has a length of 0 degrees.2-0 degrees.6, and it is independent of the flux-density threshold. C1 [de Oliveira-Costa, Angelica] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [de Oliveira-Costa, Angelica; Capodilupo, John] MIT, MIT Kavli Inst, Cambridge, MA 02139 USA. [de Oliveira-Costa, Angelica; Capodilupo, John] MIT, Dept Phys, Cambridge, MA 02139 USA. RP de Oliveira-Costa, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM angelica@space.mit.edu FU NSF [AST-0607597, AST-0908950]; Center for Excellence in Education for holding the Research Science Institute (RSI) at MIT FX The authors wish to thank Joseph Lazio and Mike Matejek for helpful comments. Support for this work was provided by NSF through grants AST-0607597 and AST-0908950. JC acknowledges the Center for Excellence in Education for holding the Research Science Institute (RSI) at MIT to support this work. NR 44 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 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2010 VL 404 IS 4 BP 1962 EP 1965 DI 10.1111/j.1365-2966.2010.16412.x PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600JG UT WOS:000277981400026 ER PT J AU Hryniewicz, K Czerny, B Nikolajuk, M Kuraszkiewicz, J AF Hryniewicz, K. Czerny, B. Nikolajuk, M. Kuraszkiewicz, J. TI SDSS J094533.99+100950.1-the remarkable weak emission line quasar SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; quasars: absorption lines; quasars: emission lines; quasars: individual: SDSS J094533; 99+100950; 1 ID DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; BLACK-HOLE MASSES; SURVEY COMMISSIONING DATA; BROAD ABSORPTION-LINE; 5TH DATA RELEASE; ACCRETION DISK; HIGH-REDSHIFT; ENERGY-DISTRIBUTIONS; EDDINGTON RATIO AB Weak emission line quasars are a rare and puzzling group of objects. In this paper, we present one more object of this class found in the Sloan Digital Sky Survey (SDSS). The quasar SDSS J094533.99+100950.1, lying at z = 1.66, has practically no C iv emission line, a red continuum very similar to the second steepest of the quasar composite spectra of Richards et al., is not strongly affected by absorption and the Mg ii line, although relatively weak, is strong enough to measure the black hole mass. The Eddington ratio in this object is about 0.45, and the line properties are not consistent with the trends expected at high accretion rates. We propose that the most probable explanation of the line properties in this object, and perhaps in all weak emission line quasars, is that the quasar activity has just started. A disc wind is freshly launched so the low ionization lines which form close to the disc surface are already observed but the wind has not yet reached the regions where high ionization lines or narrow line components are formed. The relatively high occurrence of such a phenomenon may additionally indicate that the quasar active phase consists of several subphases, each starting with a fresh build-up of the broad-line region. C1 [Hryniewicz, K.; Czerny, B.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Hryniewicz, K.; Nikolajuk, M.] Univ Bialystok, Fac Phys, PL-15424 Bialystok, Poland. [Kuraszkiewicz, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hryniewicz, K (reprint author), Nicolaus Copernicus Astron Ctr, Bartycka 18, PL-00716 Warsaw, Poland. EM krhr@camk.edu.pl RI Czerny, Bozena/A-2363-2015 OI Czerny, Bozena/0000-0001-5848-4333 FU European Commission [RI031675, 011892, 212104]; Polish Astroparticle Network [62/-7/WSN-0068/2008]; [N N203 380136] FX We would like to thank an anonymous referee for useful comments that improved our paper. We are grateful to Marianne Vestergaard for providing us with the iron emission template. We would also like to thank Andrzej Soltan for data search in ROSAT catalogues, Alastair Edge for helpful remarks about GALEX and 2MASS missions and Belinda Wilkes for advices during improving this paper. This work makes use of EURO-VO software, tools or services. The EURO-VO has been funded by the European Commission through contract numbers RI031675 (DCA) and 011892 (VO-TECH) under the 6th Framework Programme and contract number 212104 (AIDA) under the 7th Framework Programme. This work was supported in part by N N203 380136 and by the Polish Astroparticle Network 62/-7/WSN-0068/2008. NR 61 TC 26 Z9 26 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2010 VL 404 IS 4 BP 2028 EP 2036 DI 10.1111/j.1365-2966.2010.16418.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600JG UT WOS:000277981400031 ER PT J AU Wijesinghe, DB Hopkins, AM Kelly, BC Welikala, N Connolly, AJ AF Wijesinghe, D. B. Hopkins, A. M. Kelly, B. C. Welikala, N. Connolly, A. J. TI Morphological classification of galaxies and its relation to physical properties SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: general ID DIGITAL SKY SURVEY; HUBBLE DEEP FIELD; STELLAR POPULATION; SHAPELET DECOMPOSITION; STAR-FORMATION; IMAGES; FORMS; PIPELINE; MONITOR; SYSTEM AB We extend a recently developed galaxy morphology classification method, Quantitative Multiwavelength Morphology (QMM), to connect galaxy morphologies to their underlying physical properties. The traditional classification of galaxies approaches the problem separately through either morphological classification or, in more recent times, analysis of physical properties. A combined approach has significant potential in producing a consistent and accurate classification scheme as well as shedding light on the origin and evolution of galaxy morphology. Here, we present an analysis of a volume-limited sample of 31 703 galaxies from the fourth data release of the Sloan Digital Sky Survey. We use an image analysis method called Pixel-z to extract the underlying physical properties of the galaxies, which is then quantified using the concentration, asymmetry and clumpiness parameters. The galaxies also have their multiwavelength morphologies quantified using QMM, and these results are then related to the distributed physical properties through a regression analysis. We show that this method can be used to relate the spatial distribution of physical properties with the morphological properties of galaxies. C1 [Wijesinghe, D. B.] Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. [Hopkins, A. M.] Anglo Australian Observ, Epping, NSW 1710, Australia. [Kelly, B. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Welikala, N.] Univ Aix Marseille, CNRS, Lab Astrophys Marseille, F-13388 Marseille 13, France. [Connolly, A. J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. RP Wijesinghe, DB (reprint author), Univ Sydney, Sch Phys, A28, Sydney, NSW 2006, Australia. EM D.Wijesinghe@physics.usyd.edu.au FU University of Sydney, School of Physics; Australian Research Council [DP0557850]; NASA [HF-01220.01]; CNRS; Agence Nationale de la Recherche (ANR); NSF [0851007, 0709394]; Space Telescope Science Institute [NAS 5-26555] FX We are grateful to the anonymous referee for positive and valuable comments. DBW acknowledges the support provided by the University of Sydney, School of Physics. AMH acknowledges support provided by the Australian Research Council through a QEII Fellowship (DP0557850). BCK acknowledges support from NASA through Hubble Fellowship grant #HF-01220.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NW acknowledges support from the CNRS and the Agence Nationale de la Recherche (ANR). AJC acknowledges partial support from NSF grants 0851007 and 0709394. NR 44 TC 10 Z9 10 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN 1 PY 2010 VL 404 IS 4 BP 2077 EP 2086 DI 10.1111/j.1365-2966.2010.16424.x PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600JG UT WOS:000277981400035 ER PT J AU Smith, FA Elliott, SM Lyons, SK AF Smith, Felisa A. Elliott, Scott M. Lyons, S. Kathleen TI Methane emissions from extinct megafauna SO NATURE GEOSCIENCE LA English DT Letter ID ATMOSPHERIC METHANE C1 [Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Elliott, Scott M.] Los Alamos Natl Lab, Climate Ocean Sea Ice Modelling Team, Los Alamos, NM 87545 USA. [Lyons, S. Kathleen] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Smith, FA (reprint author), Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. EM fasmith@unm.edu NR 14 TC 29 Z9 31 U1 3 U2 23 PU NATURE PUBLISHING GROUP PI NEW YORK PA 75 VARICK ST, 9TH FLR, NEW YORK, NY 10013-1917 USA SN 1752-0894 EI 1752-0908 J9 NAT GEOSCI JI Nat. Geosci. PD JUN PY 2010 VL 3 IS 6 BP 374 EP 375 PG 2 WC Geosciences, Multidisciplinary SC Geology GA 602IZ UT WOS:000278134100002 ER PT J AU de Stapf, MNS Ranga, NT Silva, TRD AF Sanchez de Stapf, Maria Natividad Ranga, Neusa Taroda dos Santos Silva, Tania Regina TI A New Species of Cordia (Cordiaceae, Boraginales) from Brazil SO NOVON LA English DT Article DE Bahia; Brazil; Cordia; Cordiaceae; IUCN Red List AB A new species from Brazil. Cordia pilosa M. Stapf & Taroda (Cordiaceae), is described from northeastern Brazil. Illustrations and data on habitat, distribution, and phenology are provided. The, new species belongs to Cordia sect. Superbiflorae Taroda, and it is distinguished from similar species in section Superbiflorae by its compact inflorescences and the pi lose indument on the twigs, leaves, and inflorescence axes. C1 [Sanchez de Stapf, Maria Natividad; dos Santos Silva, Tania Regina] Univ Estadual Feira de Santana, Dept Ciencias Biol, BR-44031460 Feira De Santana, Bahia, Brazil. [Sanchez de Stapf, Maria Natividad] Smithsonian Trop Res Inst, Balboa, Panama. [Ranga, Neusa Taroda] Univ Estadual Paulista, Dept Bot & Zool, Inst Biociencias Letras & Ciencias Exatas, BR-15054020 Sao Paulo, Brazil. RP de Stapf, MNS (reprint author), Univ Estadual Feira de Santana, Dept Ciencias Biol, Km 03,BR 116,Campus, BR-44031460 Feira De Santana, Bahia, Brazil. EM stapfm@si.edu FU Organization of American States (OAS); Secretaria Nacional de Ciencia y Tecnologia (SENACYT) of Panama; Kew Latin America Research Fellowship Programme (KLARF); Conselho Nacional Desenvolvimento Cientifico e Tecnologico (CNPq) FX We thank the Organization of American States (OAS) and the Secretaria Nacional de Ciencia y Tecnologia (SENACYT) of Panama for the Ph.D. fellowship for the first author and the Kew Latin America Research Fellowship Programme (KLARF) for providing support for visits to European herbaria. T. R. S. Silva was supported by the Conselho Nacional Desenvolvimento Cientifico e Tecnologico (CNPq). We are grateful to Victoria C. Hollowell, Javier Estrada, and Juan Caviria for their valuable suggestions to improve the manuscript. We thank the curators of the following herbaria for providing loans of specimens or access to collections: ALCB, G, HUEFS, MAC, MBM, P, and SJRP. We also thank Cassio van den Berg for helping with the Latin diagnosis and Carla de Lima for the illustration. NR 4 TC 1 Z9 2 U1 0 U2 0 PU MISSOURI BOTANICAL GARDEN PI ST LOUIS PA 2345 TOWER GROVE AVENUE, ST LOUIS, MO 63110 USA SN 1055-3177 J9 NOVON JI Novon PD JUN PY 2010 VL 20 IS 2 BP 212 EP 214 DI 10.3417/2007099 PG 3 WC Plant Sciences SC Plant Sciences GA 612IE UT WOS:000278889900022 ER PT J AU Heer, K Albrecht, L Kalko, EKV AF Heer, Katrin Albrecht, Larissa Kalko, Elisabeth K. V. TI Effects of ingestion by neotropical bats on germination parameters of native free-standing and strangler figs (Ficus sp., Moraceae) SO OECOLOGIA LA English DT Article DE Artibeus jamaicensis; Phyllostomidae; Gut passage; Seed dispersal; Frugivory ID TROPICAL RAIN-FOREST; SEED DISPERSAL; FRUIT BATS; ARTIBEUS-JAMAICENSIS; FRUGIVOROUS BATS; DIFFERENTIAL INGESTION; PHYLLOSTOMID BATS; DIVERSITY; COMMUNITY; BRAZIL AB Fruit-eating animals can influence the germination success of seeds through transportation and handling. We experimentally tested the contribution of ingestion by the common fruit-eating bat, Artibeus jamaicensis (Phyllostomidae, Chiroptera), to the percentage and rate of seed germination of figs (Ficus, Moraceae), which are considered keystone species for many frugivores. We collected fruits from three species of native free-standing figs (subgenus Pharmacosycea: F. insipida, F. maxima and F. yoponensis) and three species of native strangler figs (subgenus Urostigma: F. nymphiifolia, F. obtusifolia and F. popenoei) on Barro Colorado Island, Panama. The germination success of seeds removed from fruit pulp either manually or by ingestion was very high (> 92%), while seeds that were not removed from fruit pulp were destroyed by fast-growing fungi within a few days. The dynamics of seed germination were not influenced by ingestion, but differed between the two subgenera of figs. In free-standing figs, germination started significantly earlier (5.3 +/- A 0.7 days) than in strangler figs (8.6 +/- A 1.4 days). Furthermore, strangler seeds were covered with a sticky coating and their seedlings developed cotyledons faster than fine roots, in contrast to free-standing figs that showed the opposite pattern. Our results demonstrate that the germination of fig seeds is positively influenced by passage through the gut of A. jamaicensis. Furthermore, free-standing and strangler figs revealed differences in germination parameters that might be adaptive with respect to the suitability of microsites such as tree fall gaps or host trees for establishment. C1 [Heer, Katrin; Albrecht, Larissa; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Heer, K (reprint author), Univ Ulm, Inst Expt Ecol, Albert Einstein Allee 11, D-89069 Ulm, Germany. EM katrin.heer@uni-ulm.de FU DAAD (German Academic Exchange Service) FX This work was supported by a DAAD (German Academic Exchange Service) fellowship to K. Heer. We thank the Smithsonian Tropical Research Institute (STRI) in Panama for logistic support. We particularly thank Robert Hodgkison, Sonja Gassler and Kathrin Barboza-Marquez for help in the Weld. We also want to thank two anonymous reviewers for their helpful comments that considerably improved our manuscript. Animal capture and treatment comply with the current laws of Panama and have been approved by the Animal Care Committee of the Smithsonian Tropical Research Institute. NR 53 TC 23 Z9 23 U1 6 U2 42 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUN PY 2010 VL 163 IS 2 BP 425 EP 435 DI 10.1007/s00442-010-1600-x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 596WM UT WOS:000277716200016 PM 20354732 ER PT J AU Ando, A Huber, BT MacLeod, KG AF Ando, Atsushi Huber, Brian T. MacLeod, Kenneth G. TI Depth-habitat reorganization of planktonic foraminifera across the Albian/Cenomanian boundary SO PALEOBIOLOGY LA English DT Article ID SEA-SURFACE TEMPERATURES; STABLE ISOTOPIC EVIDENCE; OCEANIC ANOXIC EVENT; NORTH-ATLANTIC; GLOBOROTALIA FOHSELLA; CRETACEOUS GREENHOUSE; PELAGIC CARBONATES; FINE-FRACTION; PACIFIC-OCEAN; EVOLUTION AB New mid-Cretaceous stable isotope (delta(18)O and delta(13)C) records of multiple planktonic foraminiferal species and coexisting coccoliths from Blake Nose (western North Atlantic) document a major depth-ecology reorganization of planktonic foraminifera. Across the Albian/Cenomanian boundary, deep-dwelling Praeglobotruncana stephani and Rotalipora globotruncanoides adapted to living at a shallower depth, while, at the same time, the population of surface-dwelling Paracostellagerina libyca declined. Subsequently, the opportunistic species Hedbergella delrioensis shifted to a deep environment, and the deep-dwelling forms Rotalipora montsalveizsis and Rotalipora reicheli first appeared. The primary paleoenvironmental cause of the observed changes in planktonic adaptive strategies is uncertain, yet their coincidence with an earliest Cenomanian cooling trend reported elsewhere implicates the importance of reduced upper-ocean stratification. Although there has been an implicit assumption that the species-specific depth habitats of fossil planktonic foraminifera were invariant through time, planktonic paleoecology is a potential variable. Accordingly, the possibility of evolutionary changes in planktonic foraminiferal depth ecology should be a primary consideration (along with other environmental parameters) in paleoceanographic interpretations of foraminiferal stable isotope data. C1 [Ando, Atsushi; Huber, Brian T.] Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Ando, Atsushi] Chiba Univ, Fac Sci, Dept Earth Sci, Chiba 2638522, Japan. [Ando, Atsushi] Res Inst Humanity & Nat, Kyoto 6038047, Japan. [Ando, Atsushi] Pusan Natl Univ, Div Earth Environm Syst, Coastal Environm Syst Sch BK21, Pusan 609735, South Korea. [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Ando, A (reprint author), Smithsonian Natl Museum Nat Hist, Dept Paleobiol, MRC NHB 121, Washington, DC 20013 USA. EM ando@pusan.ac.kr RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 FU U.S. National Science Foundation; Japan Society for the Promotion of Science (JSPS); Smithsonian Charles Walcott Fund; Joint Oceanographic Institutions, Inc. FX This research used samples and data provided by the Ocean Drilling Program. The ODP is sponsored by the U.S. National Science Foundation and participating countries under management of the Joint Oceanographic Institutions, Inc. We thank Yukie Ando for generous help with sample processing, Boo-Keun Khim and Hee-Sun Yun for support of SEM study, and Helen Coxall and Wolfgang Kuhnt for helpful reviews. This work was financially supported by a grant-in-aid for the Japan Society for the Promotion of Science (JSPS) Research Fellow (to A.A.), the Smithsonian Charles Walcott Fund (to B.T.H.), and the U.S. National Science Foundation (to K.G.M.). NR 75 TC 22 Z9 23 U1 0 U2 8 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0094-8373 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 2010 VL 36 IS 3 BP 357 EP 373 PG 17 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 632TA UT WOS:000280450000001 ER PT J AU Pyenson, ND AF Pyenson, Nicholas D. TI Carcasses on the coastline: measuring the ecological fidelity of the cetacean stranding record in the eastern North Pacific Ocean SO PALEOBIOLOGY LA English DT Article ID CALIFORNIA CURRENT ECOSYSTEM; MOLLUSCAN DEATH ASSEMBLAGES; ASPARTIC-ACID RACEMIZATION; SPECIES RICHNESS; FOSSIL RECORD; RIGHT WHALES; GRAY WHALES; BERING-SEA; ABUNDANCE; POPULATION AB To understand how well fossil assemblages represent original communities, paleoecologists seek comparisons between death assemblages and their source communities. These comparisons have traditionally used nearshore, marine invertebrate assemblages for their logistical ease, high abundance, and comparable census data from living communities. For large marine vertebrates, like cetaceans, measuring their diversity in ocean ecosystems is difficult and expensive. Cetaceans, however, often beach or strand themselves along the coast, and archived data on stranded cetaceans have been recorded, in some areas, over several decades. If the stranding record is interpreted as a death assemblage, then the stranding record may represent a viable alternative for measuring diversity in living communities on directly adjacent coastlines. This study assessed the fidelity of the cetacean stranding record in the eastern North Pacific Ocean. The living community in this region has been studied for over 100 years and, recently, extensive and systematic live transect surveys using ship-based observing platforms have produced a valuable source of live diversity data. Over this same period, the U.S. Marine Mammal Stranding Program has collected and archived a record of cetacean strandings along the U.S. Pacific coastline, providing an ideal death assemblage for comparison. Using fidelity metrics commonly used in marine invertebrate taphonomy, I determined that the stranding record samples the living cetacean community with high fidelity, across fine and coarse taxonomic ranks, and at large geographic scales (>1000 km of coastline). The stranding record is also richer than the live surveys, with live-dead ratios between 1.1 and 1.3. The stranding record recovers similar rank-order relative abundances as live surveys, with statistical significance. Also, I applied sample-based rarefaction methods to generate collector's curves for strandings along the U.S. Pacific Coast to better evaluate the spatiotemporal characteristics of the stranding record. Results indicate that saturation (i.e., sampling >95% assemblage) at species, genus, and family levels occurs in less than five years of sampling, with families accumulating faster than species, and larger geographic regions (i.e., longer coastlines) accumulating taxa the most rapidly. The high fidelity of the stranding record, measured both in richness and by ranked relative abundance, implies that ecological structure from living cetacean communities is recorded in the death assemblage, a finding that parallels marine invertebrate assemblages, though at far larger spatial scales. These results have implications for studying cetacean ecology in both modern and ancient environments: first, these results imply that the stranding record, over sufficiently long time intervals, yields a richer assemblage than using line-transect methods, and faithfully records aspects of community structure; and second, these results imply that geochronologically well-constrained fossil cetacean assemblages might preserve ecologically relevant features of community structure, depending on depositional and taphonomic conditions. C1 [Pyenson, Nicholas D.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. RP Pyenson, ND (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM pyenson@zoology.ubc.ca FU National Science Foundation (NSF); NSF East Asia and Pacific Summer Institutes; Royal Society of New Zealand; New Zealand Ministry of Science and Technology; Natural Sciences and Engineering Research Council of Canada FX I am extremely grateful to the many volunteers of the U.S. Marine Mammal Stranding Network, who have spent hundreds of thousands of hours in the field and without whose efforts this study would not have been possible. I also thank J. Cordaro, B. Norberg, and S. A. Norman (all at the National Oceanic and Atmospheric Administration), who provided data, references, and valuable directions. Constructive and judicious reviews by K. Flessa and K. Parsons-Hubbard greatly improved the final manuscript, as did N. Atkins's careful copyediting. I am especially indebted to E. B. Davis, who provided timely and thoughtful advice throughout the course of this project, and J. A. Goldbogen, for encouragement, assistance, and helpful comments. I also thank R. E. Plotnick, for discussion and references about the fractal shape of coastlines, R. Lockwood, for help with fidelity metrics, and R. E. Fordyce, who provided a key reference on short notice. Lastly, numerous conversations in the field with R. E. Jones provided the original inspiration for writing this paper. This paper represents part of a doctoral dissertation completed in the Department of Integrative Biology and the Museum of Paleontology at the University of California, Berkeley. Comments from committee members D. R. Lindberg, A. D. Barnosky, J. H. Lipps, W. Alvarez, and G. J. Vermeij improved the quality of this paper. Portions of this manuscript were written with funding from a National Science Foundation (NSF) Graduate Research Fellowship, an NSF East Asia and Pacific Summer Institutes fellowship, co-sponsored by the Royal Society of New Zealand and the New Zealand Ministry of Science and Technology, and a postdoctoral research fellowship from the Natural Sciences and Engineering Research Council of Canada. NR 125 TC 28 Z9 30 U1 2 U2 19 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0094-8373 EI 1938-5331 J9 PALEOBIOLOGY JI Paleobiology PD SUM PY 2010 VL 36 IS 3 BP 453 EP 480 PG 28 WC Biodiversity Conservation; Ecology; Evolutionary Biology; Paleontology SC Biodiversity & Conservation; Environmental Sciences & Ecology; Evolutionary Biology; Paleontology GA 632TA UT WOS:000280450000006 ER PT J AU Weekes, TC AF Weekes, Trevor C. TI The Nineteenth-Century Spiral Nebula Whodunit SO PHYSICS IN PERSPECTIVE LA English DT Article DE William Parsons; Third Lord Rosse; Thomas Romney Robinson; James South; William Herschel; John Herschel; Birr Castle; reflecting telescopes; spiral nebulae; history of astronomy AB The discovery of the first spiral nebula was a milestone in the history of astronomy, but the initial observations of it are shrouded in mystery. The discovery came within months of the commissioning of the Third Earl of Rosse's very large 72-inch optical telescope at Birr Castle in the center of Ireland. Unfortunately, no observing records have survived, and while there is no doubt that the observations took place in the spring of 1845, there is some uncertainty as to whom was actually present when the discovery was made. The construction of the Earl's telescope (the Leviathan) was a magnificent achievement, since it was entirely of his design, built with his own funds, and constructed by his own workers who were literally taken "from the plough'' on his estate. The summer of 1845 saw the first appearance of the Irish Potato Famine of 1845-1848, which would seriously curtail astronomical activity when Lord Rosse's 72-inch telescope was in prime condition. C1 Harvard Smithsonian Ctr Astrophys, Whipple Observ, Amado, AZ 85645 USA. RP Weekes, TC (reprint author), Harvard Smithsonian Ctr Astrophys, Whipple Observ, 670 Mt Hopkins Rd, Amado, AZ 85645 USA. EM tweekes@cfa.harvard.edu NR 17 TC 1 Z9 1 U1 1 U2 1 PU BIRKHAUSER VERLAG AG PI BASEL PA VIADUKSTRASSE 40-44, PO BOX 133, CH-4010 BASEL, SWITZERLAND SN 1422-6944 J9 PHYS PERSPECT JI Phys. Perspect. PD JUN PY 2010 VL 12 IS 2 BP 146 EP 162 DI 10.1007/s00016-010-0018-5 PG 17 WC History & Philosophy Of Science SC History & Philosophy of Science GA 644SO UT WOS:000281400300003 ER PT J AU Braun, DR Harris, JWK Levin, NE Mccoy, JT Herries, AIR Bamford, MK Bishop, LC Richmond, BG Kibunjia, M AF Braun, David R. Harris, John W. K. Levin, Naomi E. McCoy, Jack T. Herries, Andy I. R. Bamford, Marion K. Bishop, Laura C. Richmond, Brian G. Kibunjia, Mzalendo TI Early hominin diet included diverse terrestrial and aquatic animals 1.95 Ma in East Turkana, Kenya SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Oldowan; Paleolithic; stone tools; paleomagnetism ID KOOBI-FORA-FORMATION; NORTHERN KENYA; SOUTH-AFRICA; EARLY HOMO; CUT MARKS; ETHIOPIA; PLIOCENE; BONES; BASIN; FISH AB The manufacture of stone tools and their use to access animal tissues by Pliocene hominins marks the origin of a key adaptation in human evolutionary history. Here we report an in situ archaeological assemblage from the Koobi Fora Formation in northern Kenya that provides a unique combination of faunal remains, some with direct evidence of butchery, and Oldowan artifacts, which are well dated to 1.95 Ma. This site provides the oldest in situ evidence that hominins, predating Homo erectus, enjoyed access to carcasses of terrestrial and aquatic animals that they butchered in a well-watered habitat. It also provides the earliest definitive evidence of the incorporation into the hominin diet of various aquatic animals including turtles, crocodiles, and fish, which are rich sources of specific nutrients needed in human brain growth. The evidence here shows that these critical brain-growth compounds were part of the diets of hominins before the appearance of Homo ergaster/erectus and could have played an important role in the evolution of larger brains in the early history of our lineage. C1 [Braun, David R.] Univ Cape Town, Dept Archaeol, ZA-7701 Rondebosch, South Africa. [Harris, John W. K.; McCoy, Jack T.] Rutgers State Univ, Dept Anthropol, New Brunswick, NJ 08901 USA. [Levin, Naomi E.] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA. [Herries, Andy I. R.] Univ New S Wales, Univ New S Wales Archaeomagnetism Lab, Sch Med Sci, Sydney, NSW 2052, Australia. [Bamford, Marion K.] Univ Witwatersrand, Bernard Price Inst Palaeontol, ZA-2050 Johannesburg, South Africa. [Bishop, Laura C.] Liverpool John Moores Univ, Sch Nat Sci & Psychol, Res Ctr Evolutionary Anthropol & Palaeoecol, Liverpool L3 3AF, Merseyside, England. [Richmond, Brian G.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20052 USA. [Kibunjia, Mzalendo] Natl Museums Kenya, Div Sites & Monuments, Nairobi 4065800100, Kenya. RP Braun, DR (reprint author), Univ Cape Town, Dept Archaeol, ZA-7701 Rondebosch, South Africa. EM david.braun@uct.ac.za RI Levin, Naomi/B-4124-2010; OI Levin, Naomi/0000-0001-5703-3717; Bishop, Laura/0000-0002-4216-8667 FU Liverpool University Geomagnetism Lab; National Museums of Kenya; Ministry of Education, Science and Technology of the Republic of Kenya [MOEST 13/001/31C 216]; National Science Foundation-International Research Fellowship [0602021]; Rutgers University (Center for Human Evolutionary Studies); University of Cape Town; Palaeontological Scientific Trust; University of New South Wales Faculty of Medicine; Australian Research Council [DP0877603] FX We thank J. Sealy, T. Plummer, B. Wood, and J. Parkington for constructive comments on our manuscript; the Ileret community that assisted us during this research; and the Archaeology Department of the National Museums of Kenya for support. We thank F. Brown for access to tephra geochemistry and T. Cerling for access to isotopic data and the support of the Liverpool University Geomagnetism Lab. This research was conducted by permission from the National Museums of Kenya and the Ministry of Education, Science and Technology of the Republic of Kenya (MOEST 13/001/31C 216). Research was funded by National Science Foundation-International Research Fellowship Program Grant 0602021, Rutgers University (Center for Human Evolutionary Studies), University of Cape Town (Emerging Researcher Program), Palaeontological Scientific Trust, a University of New South Wales Faculty of Medicine research grant, and Australian Research Council Discovery Grant DP0877603. NR 38 TC 97 Z9 98 U1 6 U2 81 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 JUN 1 PY 2010 VL 107 IS 22 BP 10002 EP 10007 DI 10.1073/pnas.1002181107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 603ZD UT WOS:000278246000020 PM 20534571 ER PT J AU Kemper, F Woods, PM Antoniou, V Bernard, JP Blum, RD Boyer, ML Chan, J Chen, CHR Cohen, M Dijkstra, C Engelbracht, C Galametz, M Galliano, F Gielen, C Gordon, KD Gorjian, V Harris, J Hony, S Hora, JL Indebetouw, R Jones, O Kawamura, A Lagadec, E Lawton, B Leisenring, JM Madden, SC Marengo, M Matsuura, M McDonald, I McGuire, C Meixner, M Mulia, AJ O'Halloran, B Oliveira, JM Paladini, R Paradis, D Reach, WT Rubin, D Sandstrom, K Sargent, BA Sewilo, M Shiao, B Sloan, GC Speck, AK Srinivasan, S Szczerba, R Tielens, AGGM van Aarle, E Van Dyk, SD van Loon, JT Van Winckel, H Vijh, UP Volk, K Whitney, BA Wilkins, AN Zijlstra, AA AF Kemper, F. Woods, Paul M. Antoniou, V. Bernard, J. -P. Blum, R. D. Boyer, M. L. Chan, J. Chen, C. -H. R. Cohen, M. Dijkstra, C. Engelbracht, C. Galametz, M. Galliano, F. Gielen, C. Gordon, Karl D. Gorjian, V. Harris, J. Hony, S. Hora, J. L. Indebetouw, R. Jones, O. Kawamura, A. Lagadec, E. Lawton, B. Leisenring, J. M. Madden, S. C. Marengo, M. Matsuura, M. McDonald, I. McGuire, C. Meixner, M. Mulia, A. J. O'Halloran, B. Oliveira, J. M. Paladini, R. Paradis, D. Reach, W. T. Rubin, D. Sandstrom, K. Sargent, B. A. Sewilo, M. Shiao, B. Sloan, G. C. Speck, A. K. Srinivasan, S. Szczerba, R. Tielens, A. G. G. M. van Aarle, E. Van Dyk, S. D. van Loon, J. Th. Van Winckel, H. Vijh, Uma P. Volk, K. Whitney, B. A. Wilkins, A. N. Zijlstra, A. A. TI The SAGE-Spec Spitzer Legacy Program: The Life Cycle of Dust and Gas in the Large Magellanic Cloud SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID YOUNG STELLAR OBJECTS; MULTIBAND IMAGING PHOTOMETER; POST-AGB STARS; MU-M SOURCES; AROMATIC-HYDROCARBON EMISSION; DWARF SPHEROIDAL GALAXY; RV TAURI STARS; SPACE-TELESCOPE; CARBON STARS; INFRARED SPECTROGRAPH AB The SAGE-Spec Spitzer Legacy program is a spectroscopic follow-up to the SAGE-LMC photometric survey of the Large Magellanic Cloud carried out with the Spitzer Space Telescope. We present an overview of SAGE-Spec and some of its first results. The SAGE-Spec program aims to study the life cycle of gas and dust in the Large Magellanic Cloud and to provide information essential to the classification of the point sources observed in the earlier SAGE-LMC photometric survey. We acquired 224.6 h of observations using the infrared spectrograph and the spectral energy distribution (SED) mode of the Multiband Imaging Photometer for Spitzer. The SAGE-Spec data, along with archival Spitzer spectroscopy of objects in the Large Magellanic Cloud, are reduced and delivered to the community. We discuss the observing strategy, the specific data-reduction pipelines applied, and the dissemination of data products to the scientific community. Initial science results include the first detection of an extragalactic 21 mu m feature toward an evolved star and elucidation of the nature of disks around RV Tauri stars in the Large Magellanic Cloud. Toward some young stars, ice features are observed in absorption. We also serendipitously observed a background quasar, at a redshift of z approximate to 0.14, which appears to be hostless. C1 [Kemper, F.; Woods, Paul M.; Jones, O.; Lagadec, E.; McDonald, I.; McGuire, C.; Zijlstra, A. A.] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Manchester M13 9PL, Lancs, England. [Antoniou, V.; Marengo, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA USA. [Bernard, J. -P.] Ctr Etud Spatiale Rayonnements, F-31028 Toulouse 4, France. [Blum, R. D.] Natl Opt Astron Observ, Tucson, AZ USA. [Boyer, M. L.; Gordon, Karl D.; Lawton, B.; Meixner, M.; Sargent, B. A.; Sewilo, M.; Shiao, B.; Volk, K.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Chan, J.; Mulia, A. J.; Speck, A. K.] Univ Missouri, Dept Phys & Astron, Columbia, MO 65211 USA. [Chen, C. -H. R.; Indebetouw, R.] Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. [Cohen, M.; Sandstrom, K.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Engelbracht, C.; Harris, J.] Univ Arizona, Steward Observ, Tucson, AZ USA. [Galametz, M.; Galliano, F.; Hony, S.; Madden, S. C.; Rubin, D.] Univ Paris Diderot, CEA Saclay, DAPNIA Serv Astrophys, CEA DSM CNRS,Lab AIM, F-91191 Gif Sur Yvette, France. [Gielen, C.; van Aarle, E.; Van Winckel, H.] Katholieke Univ Leuven, Inst Sterrenkunde, B-3001 Heverlee, Belgium. [Gorjian, V.] JPL Caltech, Pasadena, CA USA. [Hora, J. L.; Marengo, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Indebetouw, R.] Natl Radio Astron Observ, Charlottesville, VA USA. [Kawamura, A.] Nagoya Univ, Dept Astrophys, Chikusa Ku, Nagoya, Aichi 46401, Japan. [Lagadec, E.] ESO Headquarters Garching, D-85748 Garching, Germany. [Matsuura, M.] UCL, Dept Phys & Astron, Inst Origins, London WC1E 6BT, England. [Matsuura, M.] Univ Coll London, Mullard Space Sci Lab, Inst Origins, Dorking RH5 6NT, Surrey, England. [O'Halloran, B.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Oliveira, J. M.; van Loon, J. Th.] Univ Keele, Lennard Jones Labs, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Paladini, R.; Paradis, D.; Reach, W. T.; Van Dyk, S. D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Sandstrom, K.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Sloan, G. C.; Wilkins, A. N.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Srinivasan, S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Srinivasan, S.] Inst Astrophys Paris, F-75014 Paris, France. [Szczerba, R.] Nicholas Copernicus Astron Ctr, PL-87100 Torun, Poland. [Tielens, A. G. G. M.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Vijh, Uma P.] Univ Toledo, Ritter Astrophys Res Ctr, Toledo, OH 43606 USA. [Whitney, B. A.] Space Sci Inst, Boulder, CO USA. RP Kemper, F (reprint author), Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg,Oxford Rd, Manchester M13 9PL, Lancs, England. RI Woods, Paul/E-6926-2011; Van Winckel, Hans/I-7863-2013; Kemper, Francisca/D-8688-2011; OI Woods, Paul/0000-0003-4340-3590; Reach, William/0000-0001-8362-4094; Van Winckel, Hans/0000-0001-5158-9327; Kemper, Francisca/0000-0003-2743-8240; Hora, Joseph/0000-0002-5599-4650 FU NASA with UC Berkeley [1320707] FX M. Cohen thanks NASA for supporting his participation in SAGE-Spec through JPL grant 1320707 with UC Berkeley. B. Sargent, M. Meixner, and B. Shiao were supported for SAGE-Spec through JPL/SSC grant 1310534 with STScI. M. Meixner was additionally supported by NASA NAG5-12595. R. Szczerba acknowledges support from grant N203 393334 (MNiSW). NR 97 TC 57 Z9 57 U1 0 U2 0 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0004-6280 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2010 VL 122 IS 892 BP 683 EP 700 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600NK UT WOS:000277993400006 ER PT J AU High, FW Stubbs, CW Stalder, B Gilmore, DK Tonry, JL AF High, F. William Stubbs, Christopher W. Stalder, Brian Gilmore, David Kirk Tonry, John L. TI Sky Variability in the y Band at the LSST Site SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID HYDROXYL AIRGLOW; NIGHT-SKY; IMAGER; ATLAS; LINES AB We have measured spatial and temporal variability in the y-band sky brightness over the course of four nights above Cerro Tololo near Cerro Pachon, Chile, the planned site for the Large Synoptic Survey Telescope (LSST). Our wide-angle camera lens provided a 41 degrees field of view and a 145 ''. pixel scale. We minimized potential system throughput differences by deploying a deep-depletion CCD and a filter that matches the proposed LSST y(3) band (970 -1030 nm). Images of the sky exhibited coherent wave structure, attributable to atmospheric gravity waves at 90 km altitude, creating 3%-4% rms spatial sky flux variability on scales of about 2 degrees and larger. Over the course of a full night, the y(3) band additionally showed highly coherent temporal variability of up to a factor of 2 in flux. We estimate the mean absolute sky level to be approximately y(3) = 17.8 mag (Vega), or y(3) = 18.3 mag (AB). While our observations were made through a y(3) filter, the relative sky brightness variability should hold for all proposed y bands, whereas the absolute levels should more strongly depend on spectral response. The spatial variability presents a challenge to wide-field cameras that require illumination correction strategies that make use of stacked sky flats. The temporal variability may warrant an adaptive y band imaging strategy for LSST, to take advantage of times when the sky is darkest. C1 [High, F. William; Stubbs, Christopher W.; Stalder, Brian] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [High, F. William; Stubbs, Christopher W.; Stalder, Brian] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilmore, David Kirk] Stanford Linear Accelerator Ctr, Kavli Inst Particle Astrophys & Cosmol, Palo Alto, CA 94025 USA. [Tonry, John L.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. RP High, FW (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM high@physics.harvard.edu RI Stubbs, Christopher/C-2829-2012 OI Stubbs, Christopher/0000-0003-0347-1724 FU National Science Foundation [AST-0551161, AST-0132798]; Department of Energy laboratories; LSSTC; National Aeronautics and Space Administration and the National Science Foundation FX We thank the LSST Corporation, Harvard University, and the US Department of Energy Office of Science and the National Science Foundation for their support. The LSST design and development activity is supported by the National Science Foundation under Scientific Program Order No. 9 (AST-0551161) through Cooperative Agreement AST-0132798. Additional funding comes from private donations, in-kind support at Department of Energy laboratories, and other LSSTC Institutional Members. We thank the CTIO scientific and technical staff for their invaluable help in setting up these observations. We are also very grateful to the team that is establishing the astrometry. net online resource, which we used in its testing phase to determine the centers of the images we obtained. The authors gratefully acknowledge the referee for insightful comments and recommendations. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. NR 24 TC 5 Z9 5 U1 0 U2 0 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD JUN PY 2010 VL 122 IS 892 BP 722 EP 730 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 600NK UT WOS:000277993400009 ER PT J AU Lowery, DL O'Neal, MA Wah, JS Wagner, DP Stanford, DJ AF Lowery, Darrin L. O'Neal, Michael A. Wah, John S. Wagner, Daniel P. Stanford, Dennis J. TI Late Pleistocene upland stratigraphy of the western Delmarva Peninsula, USA SO QUATERNARY SCIENCE REVIEWS LA English DT Article ID LOESS; RECORD; CURVE AB New pedological, geological, archaeological, and geochronological data from the Miles Point site in eastern Maryland are compared with similar data from other nearby sites to develop a framework for interpreting the upland stratigraphy in the western Delmarva Peninsula. Our results indicate the presence of two different intervals of loess deposition. The earlier loess (Miles Point Loess) was deposited between 41 and 25 ka. A paleosol (Tilghman Soil) formed in this loess was initially developed in grasslands and boreal environments during a subsequent period of landscape stability between 25 and 18 ka. Between 18 and 12.8 ka, the Miles Point Loess and the Tilghman Soil were eroded in many areas as evidenced by diagnostic ca. 12.8 ka Clovis-age artifacts lying unconformably on the Tilghman Soil. Cores adjacent to the deep channel area of the Chesapeake Bay confirm this erosional unconformity prior to 12.7 ka. A relatively uniform terminal-Pleistocene loess (Paw Paw), deposited prior to the Early Archaic period, buried Clovis-age lag artifacts and other archaeological remains older than 13.2 ka. Stratigraphic evidence from the Late Pleistocene lower Susquehanna River Valley suggests that the Paw Paw Loess is the result of eolian redeposition and reworking of non-glacial eroded upland sediments that filled the valley between 12.7 and 11.5 ka. (C) 2010 Elsevier Ltd. All rights reserved. C1 [O'Neal, Michael A.] Univ Delaware, Dept Geog, Newark, DE 19716 USA. [Lowery, Darrin L.; O'Neal, Michael A.] Univ Delaware, Dept Geol Sci, Newark, DE 19716 USA. [Wah, John S.] Matapeake Soil & Environm Consultants, Shippensburg, PA 17257 USA. [Wagner, Daniel P.] Geosci Consultants, Hyattsville, MD 20782 USA. [Stanford, Dennis J.] Smithsonian Inst, Dept Anthropol, Museum Nat Hist, Washington, DC 20013 USA. RP O'Neal, MA (reprint author), Univ Delaware, Dept Geog, Newark, DE 19716 USA. EM michael@udel.edu RI O'Neal, Michael/B-2994-2012; O'Neal, Michael/K-1822-2015 OI O'Neal, Michael/0000-0002-2095-7454; O'Neal, Michael/0000-0002-6696-0106 NR 36 TC 14 Z9 14 U1 1 U2 7 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0277-3791 J9 QUATERNARY SCI REV JI Quat. Sci. Rev. PD JUN PY 2010 VL 29 IS 11-12 BP 1472 EP 1480 DI 10.1016/j.quascirev.2010.03.007 PG 9 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 610GU UT WOS:000278720500014 ER PT J AU Touwaide, A AF Touwaide, Alain TI The Books of Venice: Il libro veneziano SO RENAISSANCE QUARTERLY LA English DT Book Review C1 [Touwaide, Alain] Smithsonian Inst, Washington, DC 20560 USA. RP Touwaide, A (reprint author), Smithsonian Inst, 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 0034-4338 J9 RENAISSANCE QUART JI Renaiss. Q. PD SUM PY 2010 VL 63 IS 2 BP 548 EP U221 PG 2 WC Medieval & Renaissance Studies SC Arts & Humanities - Other Topics GA 638DP UT WOS:000280872100007 ER PT J AU Clough, GW AF Clough, G. Wayne TI Far Sighted 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 JUN PY 2010 VL 41 IS 3 BP 24 EP 24 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 599HO UT WOS:000277902200011 ER PT J AU Preminger, D Nandy, D Chapman, G Martens, PCH AF Preminger, Dora Nandy, Dibyendu Chapman, Gary Martens, Petrus C. H. TI Empirical Modeling of Radiative versus Magnetic Flux for the Sun-as-a-Star SO SOLAR PHYSICS LA English DT Article DE Cool stars; Irradiance; Magnetic flux; Solar variability ID SOLAR IRRADIANCE VARIATIONS; SPECTRAL IRRADIANCE; ACTIVE REGIONS; FIELD; VARIABILITY; RECONSTRUCTION; PARAMETERS; CYCLE-22 AB We study the relationship between full-disk solar radiative flux at different wavelengths and average solar photospheric magnetic-flux density, using daily measurements from the Kitt Peak magnetograph and other instruments extending over one or more solar cycles. We use two different statistical methods to determine the underlying nature of these flux -aEuro parts per thousand flux relationships. First, we use statistical correlation and regression analysis and show that the relationships are not monotonic for total solar irradiance and for continuum radiation from the photosphere, but are approximately linear for chromospheric and coronal radiation. Second, we use signal theory to examine the flux -aEuro parts per thousand flux relationships for a temporal component. We find that a well-defined temporal component exists and accounts for some of the variance in the data. This temporal component arises because active regions with high magnetic-field strength evolve, breaking up into small-scale magnetic elements with low field strength, and radiative and magnetic fluxes are sensitive to different active-region components. We generate empirical models that relate radiative flux to magnetic flux, allowing us to predict spectral-irradiance variations from observations of disk-averaged magnetic-flux density. In most cases, the model reconstructions can account for 85 -aEuro parts per thousand 90% of the variability of the radiative flux from the chromosphere and corona. Our results are important for understanding the relationship between magnetic and radiative measures of solar and stellar variability. C1 [Preminger, Dora] Calif State Univ Northridge, San Fernando Observ, Northridge, CA 91330 USA. [Nandy, Dibyendu] Indian Inst Sci Educ & Res, Dept Phys Sci, Mohanpur 741252, W Bengal, India. [Martens, Petrus C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Martens, Petrus C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59715 USA. RP Preminger, D (reprint author), Calif State Univ Northridge, San Fernando Observ, Northridge, CA 91330 USA. EM dora.preminger@csun.edu FU NASA [NNX07AT19G, NNX08AW53G]; NSF [ATM-0533511, ATM-0848518]; Department of Science and Technology, Government of India FX This research has been partially supported by NASA Living with a Star grant NNX07AT19G to Montana State University, by NASA grant NNX08AW53G to the Smithsonian Astrophysical Observatory, and by NSF grants ATM-0533511 and ATM-0848518 to the San Fernando Observatory. D.P. and G.C. would like to acknowledge the continuing support of CSUN for the program at the San Fernando Observatory. D.N. would like to acknowledge the Department of Science and Technology, Government of India, for support through the Ramanujan Fellowship. NR 37 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 EI 1573-093X J9 SOL PHYS JI Sol. Phys. PD JUN PY 2010 VL 264 IS 1 BP 13 EP 30 DI 10.1007/s11207-010-9560-1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610OM UT WOS:000278742600002 ER PT J AU Attrill, GDR Harra, LK van Driel-Gesztelyi, L Wills-Davey, MJ AF Attrill, G. D. R. Harra, L. K. van Driel-Gesztelyi, L. Wills-Davey, M. J. TI Revealing the Fine Structure of Coronal Dimmings and Associated Flows with Hinode/EIS SO SOLAR PHYSICS LA English DT Article ID ULTRAVIOLET IMAGING TELESCOPE; SOLAR ACTIVE REGIONS; CME-RELATED DIMMINGS; LARGE-SCALE ACTIVITY; X-RAY TELESCOPE; MASS EJECTION; EIT WAVES; MAGNETIC CLOUD; NUMERICAL-SIMULATION; SOHO MISSION AB We study two CME events on 13 and 14 December 2006 that were associated with large-scale dimmings. We study the eruptions from pre-event on 11 December through the recovery on 15 December, using a combination of Hinode/EIS, SOHO/EIT, SOHO/MDI, and MLSO H alpha data. The GOES X-class flares obscured the core dimmings, but secondary dimmings developed remote from the active region (AR) in both events. The secondary dimmings are found to be formed by a removal of bright coronal material from loops in the plage region to the East of the AR. Using Hinode/EIS data, we find that the outflows associated with the coronal-dimming regions are highly structured. The concentrated outflows are located at the footpoints of coronal loops (which exist before, and are re-established after, the eruptions), and these are correlated with regions of positive magnetic elements. Comparative study of the Hinode/EIS and SOHO/EIT data shows that the reduction in outflow velocity is consistent with the recovery in intensity of the studied regions. We find that concentrated downflows develop during the recovery phase of the dimmings and are also correlated with the same positive magnetic elements that were previously related to outflows. The local behaviour of the flows in and around the dimming regions following the eruptions is found to be dynamic and complex. Despite the global aspects of these events (widespread dimmings, CMEs, coronal waves) being largely homologous, there are significant local variations and distinct differences between the flows associated with the two events. We find that the secondary dimmings recover primarily by re-establishment of the bright coronal loops (the exact configuration changes between the eruptions, which is reflected by the complexity of the flows). C1 [Attrill, G. D. R.; Wills-Davey, M. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harra, L. K.; van Driel-Gesztelyi, L.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [van Driel-Gesztelyi, L.] Observ Paris, CNRS, UMR 8109, LESIA, F-92195 Meudon, France. [van Driel-Gesztelyi, L.] Hungarian Acad Sci, Konkoly Observ, Budapest, Hungary. RP Attrill, GDR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gattrill@cfa.harvard.edu OI Harra, Louise/0000-0001-9457-6200 FU NASA [NNX08BA97G]; Hungarian Science Foundation [OTKA K81421]; European Community [218816] FX We sincerely thank the referee for their comments and particularly for encouragement in developing the discussion. We thank Yingna Su for helpful discussion regarding the flare ribbons that developed in these events, and we acknowledge the hard work of the Hinode/EIS and SOHO/EIT teams for providing the data used in this study. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway). SOHO is a project of international co-operation between ESA and NASA. We acknowledge the PICS instrument at Mauna Loa for providing the H alpha data. The EIS Observing Timeline (http://solar-b.nrl.navy.mil/cgi-bin/timeline4.cgi), and the Hinode/EIS website hosted at MSSL (http://msslxr.mssl.ucl.ac.uk:8080/SolarB/) were used extensively in this work. GDRA and MWD gratefully acknowledge NASA grant NNX08BA97G. LvDG acknowledges funding through the Hungarian Science Foundation grant OTKA K81421 and the European Community's FP7/2007-2013 programme through the SOTERIA Network (EU FP7 Space Science Project No. 218816). NR 70 TC 15 Z9 15 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD JUN PY 2010 VL 264 IS 1 BP 119 EP 147 DI 10.1007/s11207-010-9558-8 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 610OM UT WOS:000278742600010 ER PT J AU Lenat, DR Ruiter, DE Parker, CR Robinson, JL Beaty, SR Flint, OS AF Lenat, David R. Ruiter, David E. Parker, Charles R. Robinson, Jason L. Beaty, Steven R. Flint, Oliver S., Jr. TI Caddisfly (Trichoptera) Records for North Carolina SO SOUTHEASTERN NATURALIST LA English DT Article ID MOUNTAINS-NATIONAL-PARK; AMERICA TRICHOPTERA; IMMATURE STAGES; RHYACOPHILIDAE; GENUS; LEPTOCERIDAE; HYDROPTILIDAE; LARVA; HYDROPSYCHIDAE; EPHEMEROPTERA AB Information is presented on 348 Trichoptera (caddisfly) species recorded from North Carolina, including 76 new state records. This information includes distribution across 4 ecoregions, occurrence by stream size, and the 1st published North Carolina record for each species. C1 [Lenat, David R.] Lenat Consulting Serv Inc, Raleigh, NC 27612 USA. [Parker, Charles R.] US Geol Survey, Gatlinburg, TN 37738 USA. [Robinson, Jason L.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Beaty, Steven R.] N Carolina Div Water Qual, Raleigh, NC 27609 USA. [Flint, Oliver S., Jr.] Smithsonian Inst, Washington, DC 20013 USA. RP Lenat, DR (reprint author), Lenat Consulting Serv Inc, 3607 Corbin St, Raleigh, NC 27612 USA. EM Lenatbks@mindspring.com NR 116 TC 1 Z9 2 U1 2 U2 5 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1528-7092 EI 1938-5412 J9 SOUTHEAST NAT JI Southeast. Nat. PD JUN PY 2010 VL 9 IS 2 BP 201 EP 236 DI 10.1656/058.009.0202 PG 36 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA V24FW UT WOS:000208397300002 ER PT J AU Graves, GR AF Graves, Gary R. TI Late 19th Century Abundance Trends of the Eskimo Curlew on Nantucket Island, Massachusetts SO WATERBIRDS LA English DT Article DE American Golden Plover; Eskimo Curlew; Nantucket Island; Numenius borealis; Pluvialis dominica AB The Eskimo Curlew (Numenius borealis), now near extinction, was intensively hunted during fall migration along the Atlantic coast from Labrador to Long Island through the late 195 century. Scores of post-1850 records from this region have been gleaned from the literature but the rate of population decline has never been assessed. George H. MacKay's shooting journal, which has been largely overlooked, includes quantitative data on curlew abundance trends from 1875 to 1897 on Nantucket Island, Massachusetts. MacKay observed 650 curlews and his party bagged 87 during 231 hunting days logged during the flight period (21 August-2 October) over 22 hunting seasons. The last major flights were observed in 1881. Although he continued to hunt enthusiastically through the early 1890s, annual totals of curlews observed by MacKay declined significantly (r(s) = 0.40, p <0.05) from 1875 to 1897, as did annual bag totals (r(s) = -0.41, p <0.05). Annual bag totals of American Golden Plovers (Pluvialis dominica), which often associated with Eskimo Curlews, also declined precipitously during the period (r(s) = 0.51, p < 0.01). Journal entries suggest that MacKay abandoned shorebird hunting after a string of disappointing seasons in the 1890s. MacKay's journal offers a unique historical perspective on the decline of the Eskimo Curlew, a species about which little additional historical information is likely to be learned. Received 26 August 2009, accepted 2 January 2010. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Graves, GR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, MRC 116,POB 37012, Washington, DC 20013 USA. EM gravesg@si.edu NR 17 TC 3 Z9 3 U1 0 U2 13 PU WATERBIRD SOC PI WASHINGTON PA NATL MUSEUM NATURAL HISTORY SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 1524-4695 J9 WATERBIRDS JI Waterbirds PD JUN PY 2010 VL 33 IS 2 BP 236 EP 241 DI 10.1675/063.033.0212 PG 6 WC Ornithology SC Zoology GA 683TM UT WOS:000284498100012 ER PT J AU Germain, RR Reudink, MW Marra, PP Ratcliffe, LM AF Germain, Ryan R. Reudink, Matthew W. Marra, Peter P. Ratcliffe, Laurene M. TI CAROTENOID-BASED MALE PLUMAGE PREDICTS PARENTAL INVESTMENT IN THE AMERICAN REDSTART SO WILSON JOURNAL OF ORNITHOLOGY LA English DT Article ID TIT PARUS-MAJOR; DIFFERENTIAL-ALLOCATION HYPOTHESIS; SEXUAL SELECTION; REPRODUCTIVE SUCCESS; SETOPHAGA-RUTICILLA; MATING SUCCESS; MIGRATORY BIRD; PATERNAL CARE; COLORATION; FEMALES AB We examined whether male plumage coloration signals parental quality in the American Redstart (Setophaga ruticilla). a highly ornamented. migratory warbler We measured the relationship between both adult male arrival date and phenotype (morphology, melanin- and carotenoid-based plumage), and parental care levels of both parents Males with brighter flank feathers made more visits to the nest and spent more time at the nest, consistent with the 'good-parent hypothesis' Female parental care (number of visits) was negatively correlated with intensity of red of her mate's tail feathers and positively associated with her mate's parental effort These data indicate offspring!, of brighter males receive more care front both parents Our results suggest carotenoid-based plumage trans of male American Redstarts may have an important role in intersexual signaling, and add to our understanding of the evolution of multiple ornaments Received 10 July 2009 Accepted 20 January 2010 C1 [Germain, Ryan R.; Reudink, Matthew W.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Reudink, Matthew W.; Marra, Peter P.] Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Germain, RR (reprint author), Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. FU Queen's University Biological Station; Natural Sciences and Engineering Research Council of Canada; Queen's University; National Science Foundation; Smithsonian Institution; Ontario Government (MTCU); American Ornuthologists' Union; Society of Canadian Ornithologists; Sigma Xi; American Museum of Natural History FX We thank the many field assistants who contributed to this study. and M M Osmond and T D Barran for assistance in video analysis V L Friesen, J J Nocera. J R Foote. C F Richter. and K E Delmore provided helpful comments on earlier versions of this manuscript We thank R D Montgomerie or use of color analysis equipment, and F J S Phelan and F L Connor or logistical support at Queen's University Biological Station This research was supported by the Natural Sciences and Engineering Research Council of Canada, Queen's University, National Science Foundation, Smithsonian Institution, Ontario Government (MTCU). American Ornithologists' Union, Society of Canadian Ornithologists, Sigma Xi, and the American Museum of Natural History NR 44 TC 18 Z9 18 U1 3 U2 15 PU WILSON ORNITHOLOGICAL SOC PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 1559-4491 J9 WILSON J ORNITHOL JI Wilson J. Ornithol. PD JUN PY 2010 VL 122 IS 2 BP 318 EP 325 DI 10.1676/09-107.1 PG 8 WC Ornithology SC Zoology GA 609SV UT WOS:000278678300012 ER PT J AU Stephens, CE AF Stephens, Carlene E. TI A Republic in Time: Temporality and Social Imagination in Nineteenth-Century America SO WINTERTHUR PORTFOLIO-A JOURNAL OF AMERICAN MATERIAL CULTURE LA English DT Book Review C1 [Stephens, Carlene E.] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Stephens, CE (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 6 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 0084-0416 J9 WINTERTHUR PORTFOLIO JI Winterthur Portfol.-J. Amer. Mater. Cult. PD SUM-FAL PY 2010 VL 44 IS 2-3 BP 256 EP 257 PG 3 WC Art SC Art GA 638BS UT WOS:000280865800012 ER PT J AU Sharp, KH Ritchie, KB Schupp, PJ Ritson-Williams, R Paul, VJ AF Sharp, Koty H. Ritchie, Kim B. Schupp, Peter J. Ritson-Williams, Raphael Paul, Valerie J. TI Bacterial Acquisition in Juveniles of Several Broadcast Spawning Coral Species SO PLOS ONE LA English DT Article ID BLACK BAND DISEASE; VERTICAL TRANSMISSION; REPRODUCTIVE ISOLATION; SCLERACTINIAN CORALS; MONTASTREA-ANNULARIS; SYMBIONTS; COMPLEX; LARVAE; REEFS; CYANOBACTERIA AB Coral animals harbor diverse microorganisms in their tissues, including archaea, bacteria, viruses, and zooxanthellae. The extent to which coral-bacterial associations are specific and the mechanisms for their maintenance across generations in the environment are unknown. The high diversity of bacteria in adult coral colonies has made it challenging to identify species-specific patterns. Localization of bacteria in gametes and larvae of corals presents an opportunity for determining when bacterial-coral associations are initiated and whether they are dynamic throughout early development. This study focuses on the early onset of bacterial associations in the mass spawning corals Montastraea annularis, M. franksi, M. faveolata, Acropora palmata, A. cervicornis, Diploria strigosa, and A. humilis. The presence of bacteria and timing of bacterial colonization was evaluated in gametes, swimming planulae, and newly settled polyps by fluorescence in situ hybridization (FISH) using general eubacterial probes and laser-scanning confocal microscopy. The coral species investigated in this study do not appear to transmit bacteria via their gametes, and bacteria are not detectable in or on the corals until after settlement and metamorphosis. This study suggests that mass-spawning corals do not acquire, or are not colonized by, detectable numbers of bacteria until after larval settlement and development of the juvenile polyp. This timing lays the groundwork for developing and testing new hypotheses regarding general regulatory mechanisms that control bacterial colonization and infection of corals, and how interactions among bacteria and juvenile polyps influence the structure of bacterial assemblages in corals. C1 [Sharp, Koty H.; Ritson-Williams, Raphael; Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA. [Ritchie, Kim B.] Mote Marine Lab, Sarasota, FL 34236 USA. [Schupp, Peter J.] Univ Guam, Univ Guam Stn, Mangilao, GU USA. RP Sharp, KH (reprint author), Ocean Genome Legacy, Ipswich, MA USA. EM kotysharp@gmail.com FU Mote Marine Laboratory; Smithsonian Marine Science Network; NIH MBRS SCORE [S06-GM-44796] FX This work was funded primarily by the Mote Marine Laboratory "Protect Our Reefs'' License Plate Research Grant. K. S. was supported by the Smithsonian Marine Science Network Postdoctoral Fellowship. P.J.S. acknowledges partial support by NIH MBRS SCORE grant S06-GM-44796. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 43 TC 27 Z9 27 U1 2 U2 33 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 MAY 28 PY 2010 VL 5 IS 5 AR e10898 DI 10.1371/journal.pone.0010898 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 603QC UT WOS:000278222100027 PM 20526374 ER PT J AU Schneps, MH Griswold, A Finkelstein, N McLeod, M Schrag, DP AF Schneps, Matthew H. Griswold, Alex Finkelstein, Nancy McLeod, Michele Schrag, Daniel P. TI Using Video to Build Learning Contexts Online SO SCIENCE LA English DT Editorial Material C1 [Schneps, Matthew H.; Griswold, Alex; Finkelstein, Nancy] Harvard Smithsonian Ctr Astrophys, Lab Visual Learning, Cambridge, MA 02138 USA. [McLeod, Michele] Annenberg Media, Washington, DC 20004 USA. [Schrag, Daniel P.] Harvard Univ, Dept Earth & Planetary Sci, Ctr Environm, Cambridge, MA 02138 USA. RP Schneps, MH (reprint author), Harvard Smithsonian Ctr Astrophys, Lab Visual Learning, 60 Garden St, Cambridge, MA 02138 USA. EM mschneps@cfa.harvard.edu NR 8 TC 3 Z9 3 U1 1 U2 7 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 MAY 28 PY 2010 VL 328 IS 5982 BP 1119 EP 1120 DI 10.1126/science.1186934 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 601YR UT WOS:000278104700033 PM 20508122 ER PT J AU Holt, JW Fishbaugh, KE Byrne, S Christian, S Tanaka, K Russell, PS Herkenhoff, KE Safaeinili, A Putzig, NE Phillips, RJ AF Holt, J. W. Fishbaugh, K. E. Byrne, S. Christian, S. Tanaka, K. Russell, P. S. Herkenhoff, K. E. Safaeinili, A. Putzig, N. E. Phillips, R. J. TI The construction of Chasma Boreale on Mars SO NATURE LA English DT Article ID NORTH POLAR-REGION; LAYERED DEPOSITS; GEOLOGIC HISTORY; STRATIGRAPHY; ORIGIN AB The polar layered deposits of Mars contain the planet's largest known reservoir of water ice(1,2) and the prospect of revealing a detailed Martian palaeoclimate record(3,4), but the mechanisms responsible for the formation of the dominant features of the north polar layered deposits (NPLD) are unclear, despite decades of debate. Stratigraphic analyses of the exposed portions of Chasma Boreale-a large canyon 500 km long, up to 100 km wide, and nearly 2 km deep-have led most researchers to favour an erosional process for its formation following initial NPLD accumulation. Candidate mechanisms include the catastrophic outburst of water(5), protracted basal melting(6), erosional undercutting(7), aeolian downcutting(7-9) and a combination of these processes(10). Here we use new data from the Mars Reconnaissance Orbiter to show that Chasma Boreale is instead a long-lived, complex feature resulting primarily from non-uniform accumulation of the NPLD. The initial valley that later became Chasma Boreale was matched by a second, equally large valley that was completely filled in by subsequent deposition, leaving no evidence on the surface to indicate its former presence. We further demonstrate that topography existing before the NPLD began accumulating influenced successive episodes of deposition and erosion, resulting in most of the present-day topography. Long-term and large-scale patterns of mass balance achieved through sedimentary processes, rather than catastrophic events, ice flow or highly focused erosion, have produced the largest geomorphic anomaly in the north polar ice of Mars. C1 [Holt, J. W.; Christian, S.] Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA. [Fishbaugh, K. E.] Smithsonian Natl Air & Space Museum, Washington, DC 20560 USA. [Byrne, S.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Christian, S.] Bryn Mawr Coll, Bryn Mawr, PA 19010 USA. [Tanaka, K.; Herkenhoff, K. E.] US Geol Survey, Astrogeol Sci Ctr, Flagstaff, AZ 86001 USA. [Russell, P. S.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Safaeinili, A.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Putzig, N. E.; Phillips, R. J.] SW Res Inst, Boulder, CO 80302 USA. RP Holt, JW (reprint author), Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA. EM jack@ig.utexas.edu RI Holt, John/C-4896-2009; Byrne, Shane/B-8104-2012 FU Institute for Geophysics of the Jackson School of Geosciences; NASA [NAG5-12693]; Mars Reconnaissance Orbiter (MRO); Italian Space Agency FX We thank P. Choudhary for assistance with radar data analysis. Work at the University of Texas was supported by the Institute for Geophysics of the Jackson School of Geosciences, a NASA grant (NAG5-12693) to J.W.H. and a Mars Reconnaissance Orbiter (MRO) Participating Scientist grant to J.W.H. MRO is operated for NASA by Caltech's Jet Propulsion Laboratory. SHARAD was provided to MRO by the Italian Space Agency through a contract with Thales Alenia Space Italia, and is operated by the INFOCOM Department, University of Rome. We thank the SHARAD Operations Center in Rome for their critical support. We honour the memory of our co-author and colleague A. S. This is UTIG contribution number 2186. NR 26 TC 19 Z9 19 U1 1 U2 14 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 MAY 27 PY 2010 VL 465 IS 7297 BP 446 EP 449 DI 10.1038/nature09050 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 601FM UT WOS:000278043700027 PM 20505721 ER PT J AU Ferreira, PSF Henry, TJ AF Ferreira, Paulo Sergio F. Henry, Thomas J. TI Revision of the genus Ambracius Stal, 1860 (Heteroptera: Miridae: Deraeocorinae: Clivinematini), with descriptions of three new species SO ZOOTAXA LA English DT Article DE Miridae; taxonomy; Deraeocorinae; Clivinematini; Ambracius; new species; distributions; hosts; key ID TRIBE CLIVINEMATINI; WORLD GENERA AB The clivinematine genus Ambracius Stal is revised and the three new species Ambracius alineae from Venezuela, A. liviae from the United States (Texas), and A. rudybuenoi from Panama are described and illustrated. The previously known species Ambracius capucinus (Reuter), A. dufouri Stal, A. mexicanus Carvalho, A. pallescens (Distant), A. rubricosus (Distant), and A. vittatus Carvalho are redescribed. A key to species is provided to aid in identification. C1 [Ferreira, Paulo Sergio F.] Univ Fed Vicosa, Dept Biol Anim, BR-36570000 Vicosa, MG, Brazil. [Henry, Thomas J.] Smithsonian Inst, Natl Museum Nat Hist, ARS, Systemat Entomol Lab,USDA, Washington, DC 20013 USA. RP Ferreira, PSF (reprint author), Univ Fed Vicosa, Dept Biol Anim, BR-36570000 Vicosa, MG, Brazil. EM pfiuza@ufv.br; thomas.henry@ars.usda.gov NR 38 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 27 PY 2010 IS 2485 BP 1 EP 15 PG 15 WC Zoology SC Zoology GA 603KY UT WOS:000278208700001 ER PT J AU Wikelski, M Moxley, J Eaton-Mordas, A Lopez-Uribe, MM Holland, R Moskowitz, D Roubik, DW Kays, R AF Wikelski, Martin Moxley, Jerry Eaton-Mordas, Alexander Lopez-Uribe, Margarita M. Holland, Richard Moskowitz, David Roubik, David W. Kays, Roland TI Large-Range Movements of Neotropical Orchid Bees Observed via Radio Telemetry SO PLOS ONE LA English DT Article ID EULAEMA-MERIANA HYMENOPTERA; EUGLOSSINE BEES; HARMONIC RADAR; POLLEN DISPERSAL; FORAGING RANGE; INSECT PESTS; FLIGHT; APIDAE; POLLINATORS; LANDSCAPE AB Neotropical orchid bees (Euglossini) are often cited as classic examples of trapline-foragers with potentially extensive foraging ranges. If long-distance movements are habitual, rare plants in widely scattered locations may benefit from euglossine pollination services. Here we report the first successful use of micro radio telemetry to track the movement of an insect pollinator in a complex and forested environment. Our results indicate that individual male orchid bees (Exaerete frontalis) habitually use large rainforest areas (at least 42-115 ha) on a daily basis. Aerial telemetry located individuals up to 5 km away from their core areas, and bees were often stationary, for variable periods, between flights to successive localities. These data suggest a higher degree of site fidelity than what may be expected in a free living male bee, and has implications for our understanding of biological activity patterns and the evolution of forest pollinators. C1 [Wikelski, Martin; Holland, Richard] Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. [Wikelski, Martin; Moxley, Jerry] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Eaton-Mordas, Alexander] Univ Arizona, Dept Ecol & Evolutionary Biol, Tucson, AZ USA. [Lopez-Uribe, Margarita M.] Cornell Univ, Dept Entomol, Ithaca, NY 14853 USA. [Moskowitz, David] EcolSciences Inc, Rockaway, NJ USA. [Wikelski, Martin; Roubik, David W.; Kays, Roland] Smithsonian Trop Res Inst, Balboa, Panama. [Kays, Roland] New York State Museum & Sci Serv, Albany, NY USA. RP Wikelski, M (reprint author), Max Planck Inst Ornithol, Dept Migrat & Immunoecol, Radolfzell am Bodensee, Germany. EM rkays@mail.nysed.gov RI Holland, Richard/A-6107-2010 OI Holland, Richard/0000-0003-4495-8061 FU US Environmental Protection Agency; New York State Museum; EcolSciences, Inc.; Smithsonian Tropical Research Institute; National Geographic Society FX The study was supported by the US Environmental Protection Agency, New York State Museum, EcolSciences, Inc., Smithsonian Tropical Research Institute and the National Geographic Society. EcolSciences, as the only commercial company among the funding organizations, had a role in the analysis, decision to publish, and preparation of the manuscript through the involvment of David Moskowitz. NR 53 TC 50 Z9 52 U1 7 U2 62 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 26 PY 2010 VL 5 IS 5 AR e10738 DI 10.1371/journal.pone.0010738 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 603PW UT WOS:000278221500005 PM 20520813 ER PT J AU McMahon, SM Parker, GG Miller, DR AF McMahon, Sean M. Parker, Geoffrey G. Miller, Dawn R. TI Reply to Foster et al.: Using a forest to measure trees: Determining which vital rates are responding to climate change SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Letter C1 [McMahon, Sean M.; Parker, Geoffrey G.; Miller, Dawn R.] Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. [McMahon, Sean M.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, APO, AA 34002 USA. RP McMahon, SM (reprint author), Smithsonian Environm Res Ctr, Edgewater, MD 21307 USA. EM mcmahons@si.edu OI Parker, Geoffrey/0000-0001-7055-6491 NR 4 TC 2 Z9 2 U1 0 U2 6 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 25 PY 2010 VL 107 IS 21 BP E88 EP E89 DI 10.1073/pnas.1003726107 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 601JP UT WOS:000278054700082 ER PT J AU Jander, KC Herre, EA AF Jander, K. Charlotte Herre, Edward Allen TI Host sanctions and pollinator cheating in the fig tree-fig wasp mutualism SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE mutualism; cooperation; exploitation; cheating; sanctions; fig ID LEGUME-RHIZOBIUM MUTUALISM; MOLECULAR PHYLOGENY; MONOECIOUS FIGS; YUCCA MOTHS; WORLD FIGS; EVOLUTION; COOPERATION; ECOLOGY; FICUS; MECHANISMS AB Theory predicts that mutualisms should be vulnerable to invasion by cheaters, yet mutualistic interactions are both ancient and diverse. What prevents one partner from reaping the benefits of the interaction without paying the costs? Using field experiments and observations, we examined factors affecting mutualism stability in six fig tree-fig wasp species pairs. We experimentally compared the fitness of wasps that did or did not perform their most basic mutualistic service, pollination. We found host sanctions that reduced the fitness of non-pollinating wasps in all derived, actively pollinated fig species (where wasps expend time and energy pollinating), but not in the basal, passively pollinated fig species (where wasps do not). We further screened natural populations of pollinators for wasp individuals that did not carry pollen ('cheaters'). Pollen-free wasps occurred only in actively pollinating wasp species, and their prevalence was negatively correlated with the sanction strength of their host species. Combined with previous studies, our findings suggest that (i) mutualisms can show coevolutionary dynamics analogous to those of 'arms races' in overtly antagonistic interactions; (ii) sanctions are critical for long-term mutualism stability when providing benefits to a host is costly, and (iii) there are general principles that help maintain cooperation both within and among species. C1 [Jander, K. Charlotte] Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. [Jander, K. Charlotte; Herre, Edward Allen] Smithsonian Trop Res Inst, Unit 9100, Dpo, AA 34002 USA. [Jander, K. Charlotte] Uppsala Univ, Dept Anim Ecol, Evolutionary Biol Ctr, S-75236 Uppsala, Sweden. RP Jander, KC (reprint author), Cornell Univ, Dept Neurobiol & Behav, Ithaca, NY 14853 USA. EM kcj4@cornell.edu FU Cornell University Graduate School; Smithsonian Tropical Research Institution FX We thank L. Berg, D. Castle, J. Coenen, J. Ek-Jander, A. Gomez, M. Lopez and Z. Maynard for help with fieldwork and laboratory work, and S. A. Mangan for extensive advice. M. Bjorklund, A. Dafoe, L. D. Harder, R. Lande, E. G. Leigh Jr, C. A. Machado, D. Molbo, T. D. Seeley, P. W. Sherman, E. L. Simms and the Simms laboratory, A. R. Smith, E. O. Suurmeyer, H. K. Reeve, S. A. Van Bael, M. J. West-Eberhard, and several anonymous reviewers provided helpful comments and suggestions. A. A. Agrawal, J. Booth, C. A. Machado, D. R. Nash and R. J. Rowe provided advice on the statistical and phylogenetic analyses. Special thanks to C. A. Machado for allowing us to use unpublished wasp phylogeny branch lengths. This study was part of K. C. J.'s PhD thesis at Cornell University. We thank Cornell University Graduate School for supporting K. C. J., and the Smithsonian Tropical Research Institution for providing funding (E. A. H. and K. C. J.) and maintaining the research facilities and intellectual environment that made this study possible. NR 55 TC 70 Z9 71 U1 13 U2 107 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 MAY 22 PY 2010 VL 277 IS 1687 BP 1481 EP 1488 DI 10.1098/rspb.2009.2157 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 581MT UT WOS:000276528500004 PM 20071379 ER PT J AU Temeles, EJ Kress, WJ AF Temeles, Ethan J. Kress, W. John TI Mate choice and mate competition by a tropical hummingbird at a floral resource SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE hummingbird; Eulampis jugularis; mate choice; mate competition; territoriality; foraging ID RUFOUS HUMMINGBIRDS; SEXUAL SELECTION; TERRITORIAL; ECONOMICS; QUALITY; PERFORMANCE; BEHAVIOR; DEFENSE; SIZE; TIME AB The influence of male territorial and foraging behaviours on female choice has received little attention in studies of resource-defence mating systems even though such male behaviours are thought to affect variation in their territory quality and mating success. Here we show that female purple-throated carib hummingbirds Eulampis jugularis preferred to mate with males that had high standing crops of nectar on their flower territories. A male's ability to maintain high nectar standing crops on his territory not only depended on the number of flowers in his territory, but also on his ability to enhance his territory through the prevention of nectar losses to intruders. We observed that males defended nectar supplies that were two to five times greater than their daily energy needs and consistently partitioned their territories in order to provide some resources to attract intruding females as potential mates. Such territorial behaviour resulted in males defending some flowers for their own food and other flowers as food for intruding females. Collectively, our results suggest that variation in mating success among males is driven primarily by variation in territory quality, which ultimately depends on a male's fighting ability and size. C1 [Temeles, Ethan J.] Amherst Coll, Dept Biol, Amherst, MA 01002 USA. [Kress, W. John] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Temeles, EJ (reprint author), Amherst Coll, Dept Biol, Amherst, MA 01002 USA. EM ejtemeles@amherst.edu FU Amherst College; Smithsonian Institution; NSF [DEB 0614218] FX We thank D. Williams, A. James, V. Gowda and E. Hypolite for field assistance, S. and A. Peyer Loerner and A. Jno Baptiste for accommodation on Dominica, and R. H. Wagner and two anonymous reviewers for comments. Our research was supported by Amherst College, the Smithsonian Institution, and NSF grant DEB 0614218. NR 35 TC 14 Z9 14 U1 6 U2 36 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 MAY 22 PY 2010 VL 277 IS 1687 BP 1607 EP 1613 DI 10.1098/rspb.2009.2188 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 581MT UT WOS:000276528500019 PM 20129990 ER PT J AU Churazov, E Tremaine, S Forman, W Gerhard, O Das, P Vikhlinin, A Jones, C Bohringer, H Gebhardt, K AF Churazov, E. Tremaine, S. Forman, W. Gerhard, O. Das, P. Vikhlinin, A. Jones, C. Boehringer, H. Gebhardt, K. TI Comparison of approximately isothermal gravitational potentials of elliptical galaxies based on X-ray and optical data SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: kinematics and dynamics; X-rays: galaxies: clusters ID LENS ACS SURVEY; INTRACLUSTER PLANETARY-NEBULAE; SIGHT VELOCITY DISTRIBUTIONS; VIRGO CLUSTER CORE; TO-LIGHT RATIO; DARK-MATTER; NGC 3379; XMM-NEWTON; LENTICULAR GALAXIES; SURFACE PHOTOMETRY AB We analyse six X-ray bright elliptical galaxies, observed with Chandra and XMM-Newton, and approximate their gravitational potentials by isothermal spheres phi = v2(c) log r over a range of radii from similar to 0.5 to similar to 25 kpc. We then compare the circular speed v(c) derived from X-ray data with the estimators available from optical data. In particular, we discuss two simple and robust procedures for evaluating the circular speed of the galaxy using the observed optical surface brightness and the line-of-sight velocity dispersion profiles. The best-fitting relation between the circular speeds derived from optical observations of stars and X-ray observations of hot gas is v(c,opt) similar or equal to eta v(c,X), where eta = 1.10-1.15 (depending on the method), suggesting, albeit with large statistical and systematic uncertainties, that non-thermal pressure on average contributes similar to 20-30 per cent of the gas thermal pressure. C1 [Churazov, E.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Churazov, E.; Vikhlinin, A.] Space Res Inst IKI, Moscow 117810, Russia. [Tremaine, S.] Inst Adv Study, Princeton, NJ 08540 USA. [Forman, W.; Vikhlinin, A.; Jones, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gerhard, O.; Das, P.; Boehringer, H.] MPI Extraterrestr Phys, D-85740 Garching, Germany. [Gebhardt, K.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. RP Churazov, E (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM churazov@mpa-garching.mpg.de RI Churazov, Eugene/A-7783-2013; Tremaine, Scott/M-4281-2015 OI Tremaine, Scott/0000-0002-0278-7180 FU DFG [CH389/3-2]; NASA [NAS8-38248, NAS8-01130, NAS8-03060, NNX08AH24G]; RAS; Chandra Science Center; Smithsonian Institution; MPI fur Astrophysik; MPI fur Extraterrestrische Physik; Cluster of Excellence 'Origin and Structure of the Universe; Humboldt Research Award FX We are grateful to Guinevere Kauffmann, Ben Metcalf and Glenn van de Ven for useful discussions. This work was supported by the DFG grant CH389/3-2; NASA contracts and grants NAS8-38248, NAS8-01130, NAS8-03060 and NNX08AH24G; the program 'Extended objects in the Universe' of the Division of Physical Sciences of the RAS; the Chandra Science Center; the Smithsonian Institution; MPI fur Astrophysik; MPI fur Extraterrestrische Physik and the Cluster of Excellence 'Origin and Structure of the Universe'. ST acknowledges support from a Humboldt Research Award. NR 70 TC 47 Z9 47 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2010 VL 404 IS 3 BP 1165 EP 1185 DI 10.1111/j.1365-2966.2010.16377.x PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 592MA UT WOS:000277381800008 ER PT J AU Dave, R Finlator, K Oppenheimer, BD Fardal, M Katz, N Keres, D Weinberg, DH AF Dave, Romeel Finlator, Kristian Oppenheimer, Benjamin D. Fardal, Mark Katz, Neal Keres, Dusan Weinberg, David H. TI The nature of submillimetre galaxies in cosmological hydrodynamic simulations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: N-body simulations; galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; submillimetre ID DEGREE EXTRAGALACTIC SURVEY; INITIAL MASS FUNCTION; STAR-FORMING GALAXIES; STELLAR POPULATION SYNTHESIS; HIGH-REDSHIFT GALAXIES; LYMAN BREAK GALAXY; DARK-MATTER HALOS; METALLICITY RELATION; GALACTIC OUTFLOWS; SURVEY SHADES AB We study the nature of rapidly star-forming galaxies at z = 2 in cosmological hydrodynamic simulations, and compare their properties to observations of submillimetre galaxies (SMGs). We identify simulated SMGs as the most rapidly star-forming systems that match the observed number density of SMGs. In our models, SMGs are massive galaxies sitting at the centres of large potential wells, being fed by smooth infall and gas-rich satellites at rates comparable to their star formation rates (SFRs). They are not typically undergoing major mergers that significantly boost their quiescent SFR, but they still often show complex gas morphologies and kinematics. Our simulated SMGs have stellar masses of M(*) similar to 1011-11.7 M(circle dot), SFRs of similar to 180-500 M(circle dot) yr-1, a clustering length of similar to 10 h-1 Mpc and solar metallicities. The SFRs are lower than those inferred from far-infrared (far-IR) data by similar to x3, which we suggest may owe to one or more systematic effects in the SFR calibrations. SMGs at z = 2 live in similar to 1013 M(circle dot) haloes, and by z = 0 they mostly end up as brightest group galaxies in similar to 1014 M(circle dot) haloes. We predict that higher M(*) SMGs should have on average lower specific SFRs, less disturbed morphologies and higher clustering. We also predict that deeper far-IR surveys will smoothly join SMGs on to the massive end of the SFR-M(*) relationship defined by lower mass z similar to 2 galaxies. Overall, our simulated rapid star-formers provide as good a match to available SMG data as merger-based scenarios, offering an alternative scenario that emerges naturally from cosmological simulations. C1 [Dave, Romeel; Finlator, Kristian; Oppenheimer, Benjamin D.] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Finlator, Kristian] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Oppenheimer, Benjamin D.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Fardal, Mark; Katz, Neal] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Keres, Dusan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. RP Dave, R (reprint author), Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. EM rad@as.arizona.edu RI Finlator, Kristian/M-4809-2014 OI Finlator, Kristian/0000-0002-0496-1656 FU NASA [IIST-AR-10946, NAS5-26555]; National Science Foundation [DMS-0619881] FX The simulations used here were run on University of Arizona's SGI cluster, ice. We thank Scott Chapman, Kristen Coppin, Reinhard Genzel, Desika Narayanan, Alex Pope, J.-D. Smith and Linda Tacconi for helpful conversations. We thank Rob Kennicutt and the Institute of Astronomy for their hospitality during much of the writing of this paper. Support for this work was provided by NASA through grant number IIST-AR-10946 from the Space Telescope Science Institute, which is operated by AURA, Inc. under NASA contract NAS5-26555. Support for this work, part of the Spitzer Space Telescope Theoretical Research Program, was also provided by NASA through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Computing resources were obtained through grant number DMS-0619881 from the National Science Foundation. NR 100 TC 121 Z9 121 U1 0 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2010 VL 404 IS 3 BP 1355 EP 1368 DI 10.1111/j.1365-2966.2010.16395.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 592MA UT WOS:000277381800022 ER PT J AU Degenaar, N Jonker, PG Torres, MAP Kaur, R Rea, N Israel, GL Patruno, A Trap, G Cackett, EM D'Avanzo, P Lo Curto, G Novara, G Krimm, H Holland, ST De Luca, A Esposito, P Wijnands, R AF Degenaar, N. Jonker, P. G. Torres, M. A. P. Kaur, R. Rea, N. Israel, G. L. Patruno, A. Trap, G. Cackett, E. M. D'Avanzo, P. Lo Curto, G. Novara, G. Krimm, H. Holland, S. T. De Luca, A. Esposito, P. Wijnands, R. TI Multiwavelength observations of 1RXH J173523.7-354013: revealing an unusual bursting neutron star SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; stars: neutron; X-rays: binaries; X-rays: bursts; X-rays: individual: 1RXH J173523; 7-354013; X-rays: individual: IGR J17353-3539 ID X-RAY-BURSTS; JEM-X; TELESCOPE; BINARY; EXTRACTION; SUPERBURST; EVOLUTION; SOFTWARE; MISSION; IMAGER AB On 2008 May 14, the Burst Alert Telescope onboard the Swift mission triggered on a type-I X-ray burst from the previously unclassified ROSAT object 1RXH J173523.7-354013, establishing the source as a neutron star X-ray binary. We report on X-ray, optical and near-infrared observations of this system. The X-ray burst had a duration of similar to 2 h and belongs to the class of rare, intermediately long type-I X-ray bursts. From the bolometric peak flux of similar to 3.5 x 10-8 erg cm-2 s-1, we infer a source distance of D less than or similar to 9.5 kpc. Photometry of the field reveals an optical counterpart that declined from R = 15.9 during the X-ray burst to R = 18.9 thereafter. Analysis of post-burst Swift/X-ray Telescope observations as well as archival XMM-Newton and ROSAT data suggests that the system is persistent at a 0.5-10 keV luminosity of similar to 2 x 1035 (D/9.5 kpc)2 erg s-1. Optical and infrared photometry together with the detection of a narrow H alpha emission line (full width at half maximum = 292 +/- 9 km s-1, equivalent width = -9.0 +/- 0.4 A) in the optical spectrum confirms that 1RXH J173523.7-354013 is a neutron star low-mass X-ray binary. The H alpha emission demonstrates that the donor star is hydrogen rich, which effectively rules out that this system is an ultracompact X-ray binary. C1 [Degenaar, N.; Kaur, R.; Rea, N.; Patruno, A.; Wijnands, R.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Jonker, P. G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rea, N.] ICE CSIC, IEEC, Fac Ciencias, Barcelona 08193, Spain. [Israel, G. L.] INAF Osservatorio Astron Roma, I-00040 Rome, Italy. [Trap, G.] CEA Saclay, DSM, IRFU, SAp, F-91191 Gif Sur Yvette, France. [Trap, G.] Univ Paris 07, CNRS, CEA, Observ Paris, F-75205 Paris 13, France. [Cackett, E. M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [D'Avanzo, P.; Lo Curto, G.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Novara, G.; De Luca, A.; Esposito, P.] INAF Ist Astrofis Spaziale & Fis Cosm Milano, I-20133 Milan, Italy. [Novara, G.] Univ Pavia, Dipartimento Fis Nucl & Teor, I-27100 Pavia, Italy. [Krimm, H.; Holland, S. T.] Univ Space Res Assoc, Columbia, MD 21044 USA. [Krimm, H.; Holland, S. T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Degenaar, N (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Postbus 94249, NL-1090 GE Amsterdam, Netherlands. EM degenaar@uva.nl RI Rea, Nanda/I-2853-2015; OI Rea, Nanda/0000-0003-2177-6388; Israel, GianLuca/0000-0001-5480-6438; De Luca, Andrea/0000-0001-6739-687X; Esposito, Paolo/0000-0003-4849-5092 FU Netherlands Organization for Scientific Research (NWO); Ramon y Cajal; NASA [PF8-90052] FX We are grateful to the referee, Craig Heinke, for useful comments that helped improve this manuscript. This work was based on observations made with ESO Telescopes at the Paranal and La Silla Observatories under programme IDs: 281.D-5030(A) and 60.A9700(D) and made use of the public data archive of Swift and INTEGRAL, as well as public data from the XMM-Newton slew survey. Support for this work was provided by the Netherlands Organization for Scientific Research (NWO). NR acknowledges support from a Ramon y Cajal Research position. EMC gratefully acknowledges support provided by NASA through the Chandra Fellowships Program, grant number PF8-90052. We acknowledge the use of the software package MOLLY written by Prof. Tom Marsh. NR 56 TC 19 Z9 19 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 21 PY 2010 VL 404 IS 3 BP 1591 EP 1602 DI 10.1111/j.1365-2966.2010.16388.x PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 592MA UT WOS:000277381800043 ER PT J AU Littler, MM Littler, DS Brooks, BL AF Littler, Mark M. Littler, Diane S. Brooks, Barrett L. TI Marine Macroalgal Diversity Assessment of Saba Bank, Netherlands Antilles SO PLOS ONE LA English DT Article AB Background: Located in the Dutch Windward Islands, Saba Bank is a flat-topped seamount (20-45 m deep in the shallower regions). The primary goals of the survey were to improve knowledge of biodiversity for one of the world's most significant, but little-known, seamounts and to increase basic data and analyses to promote the development of an improved management plan. Methodology/Principal Findings: Our team of three divers used scuba to collect algal samples to depths of 50 m at 17 dive sites. Over 360 macrophyte specimens (12 putative new species) were collected, more than 1,000 photographs were taken in truly exceptional habitats, and three astonishing new seaweed community types were discovered. These included: (1) "Field of Greens'' (N 17 degrees 30.620', W 63 degrees 27.707') dominated by green seaweeds as well as some filamentous reds, (2) "Brown Town'' (N 17 degrees 28.027', W 63 degrees 14.944') dominated by large brown algae, and (3) "Seaweed City'' (N 17 degrees 26.485', W 63 degrees 16.850') with a diversity of spectacular fleshy red algae. Conclusions/Significance: Dives to 30 m in the more two-dimensional interior habitats revealed particularly robust specimens of algae typical of shallower seagrass beds, but here in the total absence of any seagrasses (seagrasses generally do not grow below 20 m). Our preliminary estimate of the number of total seaweed species on Saba Bank ranges from a minimum of 150 to 200. Few filamentous and thin sheet forms indicative of stressed or physically disturbed environments were observed. A more precise number still awaits further microscopic and molecular examinations in the laboratory. The expedition, while intensive, has only scratched the surface of this unique submerged seamount/atoll. C1 [Littler, Mark M.; Littler, Diane S.; Brooks, Barrett L.] Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. RP Littler, MM (reprint author), Smithsonian Inst, Dept Bot, Washington, DC 20560 USA. EM littlerm@si.edu FU Department of Environment and Nature of the Netherlands Antilles; Conservation International; Smithsonian Marine Station at Ft. Pierce (SMSFP) FX Financial support for this study came from the Department of Environment and Nature of the Netherlands Antilles, Conservation International and the Smithsonian Marine Station at Ft. Pierce (SMSFP Contribution No. 810). The funding sources provided critical assistance in determining dive site locations but had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 13 TC 6 Z9 6 U1 0 U2 8 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 21 PY 2010 VL 5 IS 5 AR e10677 DI 10.1371/journal.pone.0010677 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 600VQ UT WOS:000278017400008 PM 20505757 ER PT J AU Williams, JT Carpenter, KE Van Tassell, JL Hoetjes, P Toller, W Etnoyer, P Smith, M AF Williams, Jeffrey T. Carpenter, Kent E. Van Tassell, James L. Hoetjes, Paul Toller, Wes Etnoyer, Peter Smith, Michael TI Biodiversity Assessment of the Fishes of Saba Bank Atoll, Netherlands Antilles SO PLOS ONE LA English DT Article AB Biodiversity surveys were conducted on Saba Bank, Netherlands Antilles, to assess ichthyofaunal richness and to compare with published surveys of other Caribbean localities. The primary objective was to estimate the total species richness of the Saba Bank ichthyofauna. A variety of sampling techniques was utilized to survey the fish species of both the visually accessible megafauna and the camouflaged and small-sized species comprising the cryptic ichthyofauna. Based on results presented herein, the number of species known on Saba Bank is increased from 42 previously known species to 270 species. Expected species-accumulation curves demonstrate that the current estimate of species richness of fishes for Saba Bank under represents the actual richness, and our knowledge of the ichthyofauna has not plateaued. The total expected fish-species richness may be somewhere between 320 and 411 species. The Saba Bank ichthyofaunal assemblage is compared to fish assemblages found elsewhere in the Caribbean. Despite the absence of shallow or emergent shore habitats like mangroves, Saba Bank ranks as having the eighth highest ichthyofaunal richness of surveyed localities in the Greater Caribbean. Some degree of habitat heterogeneity was evident. Fore-reef, patch-reef, and lagoonal habitats were sampled. Fish assemblages were significantly different between habitats. Species richness was highest on the fore reef, but 11 species were found only at lagoonal sites. A comprehensive, annotated list of the fishes currently known to occur on Saba Bank, Netherland Antilles, is provided and color photographs of freshly collected specimens are presented for 165 of the listed species of Saba Bank fishes to facilitate identification and taxonomic comparison with similar taxa at other localities. Coloration of some species is shown for the first time. Preliminary analysis indicates that at least six undescribed new species were collected during the survey and these are indicated in the annotated list. C1 [Williams, Jeffrey T.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Fish Div, Suitland, MD USA. [Carpenter, Kent E.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Van Tassell, James L.] Amer Museum Nat Hist, Dept Ichthyol, New York, NY 10024 USA. [Hoetjes, Paul] Minist Publ Hlth & Social Dev, Dept Environm & Nat, Curacao, Neth Antilles. [Toller, Wes] Saba Conservat Fdn, Ft Bay, Saba, Neth Antilles. [Etnoyer, Peter] Texas A&M Univ Corpus Christi, Harte Res Inst, Corpus Christi, TX USA. [Smith, Michael] Conservat Int Arlington, Ctr Appl Biodivers Sci, Arlington, VA USA. RP Williams, JT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Fish Div, Suitland, MD USA. EM williamsjt@si.edu FU Department of Environment and Nature of the Netherlands Antilles; Conservation International FX The Department of Environment and Nature of the Netherlands Antilles and Conservation International provided funding for this project. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 15 TC 11 Z9 11 U1 0 U2 7 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 21 PY 2010 VL 5 IS 5 AR e10676 DI 10.1371/journal.pone.0010676 PG 37 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 600VQ UT WOS:000278017400007 PM 20505760 ER PT J AU Uscanga, L Canto, J Gomez, JF Anglada, G Torrelles, JM Patel, NA Raga, AC Curiel, S AF Uscanga, L. Canto, J. Gomez, J. F. Anglada, G. Torrelles, J. M. Patel, N. A. Raga, A. C. Curiel, S. TI STATISTICAL ANALYSIS OF WATER MASERS IN STAR-FORMING REGIONS: CEPHEUS A AND W75 N SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cepheus A, W75 N); ISM: jets and outflows; masers; methods: statistical ID YOUNG STELLAR OBJECTS; THERMAL RADIO JET; H2O MASERS; W49N; OUTFLOW; TURBULENCE; HW2; AU AB We have done a statistical analysis of Very Long Baseline Array (VLBA) data of water masers in the starforming regions (SFRs) Cepheus A and W75 N, using correlation functions to study the spatial clustering and Doppler-velocity distribution of these masers. Two-point spatial correlation functions show a characteristic scale size for clusters of water maser spots less than or similar to 1 AU, similar to the values found in other SFRs. This suggests that the scale for water maser excitation tends to be less than or similar to 1 AU. Velocity correlation functions show power-law dependences with indices that can be explained by regular velocity fields, such as expansion and/or rotation. These velocity fields are similar to those indicated by the water maser proper-motion measurements; therefore, the velocity correlation functions appear to reveal the organized motion of water maser spots on scales larger than 1 AU. C1 [Uscanga, L.; Gomez, J. F.; Anglada, G.] Inst Astrofis Andalucia, CSIC, E-18080 Granada, Spain. [Canto, J.; Curiel, S.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Torrelles, J. M.] Univ Barcelona, Fac Fis, IEEC, Inst Ciencias Espacio,CSIC, E-08028 Barcelona, Spain. [Patel, N. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Raga, A. C.] Univ Nacl Autonoma Mexico, Inst Ciencias Nucl, Mexico City 04510, DF, Mexico. RP Uscanga, L (reprint author), Inst Astrofis Andalucia, CSIC, Apartado 3004, E-18080 Granada, Spain. EM lucero@iaa.es; jfg@iaa.es; guillem@iaa.es; torrelles@ieec.fcr.es; npatel@cfa.harvard.edu; raga@nucleares.unam.mx; scuriel@astroscu.unam.mx RI Uscanga, Lucero/C-5850-2014; Gomez, Jose Francisco/D-8392-2016; OI Gomez, Jose Francisco/0000-0002-7065-542X; Torrelles, Jose Maria/0000-0002-6896-6085 FU Secretaria de Estado de Universidades e Investigacion of MEC (Spain); Ministerio de Ciencia e Innovacion (Spain) [AYA 2008-06189-C03]; Consejeria de Innovacion, Ciencia y Empresa of Junta de Andalucia (Spain); CONACyT (Mexico) [61547, 60581] FX L.U. is supported by Secretaria de Estado de Universidades e Investigacion of MEC (Spain). G.A., J.F.G., J.M.T., and L.U. are partially supported by Ministerio de Ciencia e Innovacion (Spain), grant AYA 2008-06189-C03 (including FEDER funds), and by Consejeria de Innovacion, Ciencia y Empresa of Junta de Andalucia (Spain). J.C., A.C.R., and S.C. acknowledge the support of CONACyT (Mexico) grants 61547 and 60581. We are thankful to the referee for his/her useful comments that helped us to improve this paper. NR 26 TC 1 Z9 1 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 132 EP 142 DI 10.1088/0004-637X/715/1/132 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100012 ER PT J AU Hopkins, PF Bundy, K Croton, D Hernquist, L Keres, D Khochfar, S Stewart, K Wetzel, A Younger, JD AF Hopkins, Philip F. Bundy, Kevin Croton, Darren Hernquist, Lars Keres, Dusan Khochfar, Sadegh Stewart, Kyle Wetzel, Andrew Younger, Joshua D. TI MERGERS AND BULGE FORMATION IN Lambda CDM: WHICH MERGERS MATTER? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: theory; galaxies: active; galaxies: evolution; galaxies: formation ID STAR-FORMING GALAXIES; ULTRALUMINOUS INFRARED GALAXIES; SUPERMASSIVE BLACK-HOLES; ACTIVE GALACTIC NUCLEI; TULLY-FISHER RELATION; DIGITAL-SKY-SURVEY; HALO OCCUPATION DISTRIBUTION; SIMILAR-TO 2; HIERARCHICAL SATELLITE ACCRETION; BRIGHTEST CLUSTER GALAXIES AB We use a suite of semi-empirical models to predict the galaxy-galaxy merger rate and relative contributions to bulge growth as a function of mass (both halo and stellar), redshift, and mass ratio. The models use empirical constraints on the halo occupation distribution, evolved forward in time, to robustly identify where and when galaxy mergers occur. Together with the results of high-resolution merger simulations, this allows us to quantify the relative contributions of mergers with different properties (e. g., mass ratios, gas fractions, redshifts) to the bulge population. We compare with observational constraints, and find good agreement. We also provide useful fitting functions and make public a code to reproduce the predicted merger rates and contributions to bulge mass growth. We identify several robust conclusions. (1) Major mergers dominate the formation and assembly of similar to L(*) bulges and the total spheroid mass density, but minor mergers contribute a non-negligible similar to 30%. (2) This is mass dependent: bulge formation and assembly is dominated by more minor mergers in lower-mass systems. In higher-mass systems, most bulges originally form in major mergers near similar to L(*), but assemble in increasingly minor mergers. (3) The minor/major contribution is also morphology dependent: higher B/T systems preferentially form in more major mergers, with B/T roughly tracing the mass ratio of the largest recent merger; lower B/T systems preferentially form in situ from minor mergers. (4) Low-mass galaxies, being gas-rich, require more mergers to reach the same B/T as high-mass systems. Gas-richness dramatically suppresses the absolute efficiency of bulge formation, but does not strongly influence the relative contribution of major versus minor mergers. (5) Absolute merger rates at fixed mass ratio increase with galaxy mass. (6) Predicted merger rates agree well with those observed in pair and morphology-selected samples, but there is evidence that some morphology-selected samples include contamination from minor mergers. (7) Predicted rates also agree with the integrated growth in bulge mass density with cosmic time, but with a factor similar to 2 uncertainty in both-up to half the bulge mass density could come from non-merger processes. We systematically vary the model assumptions, totaling similar to 10(3) model permutations, and quantify the resulting uncertainties. Our conclusions regarding the importance of different mergers for bulge formation are very robust to these changes. The absolute predicted merger rates are systematically uncertain at the factor similar to 2 level; uncertainties grow at the lowest masses and high redshifts. C1 [Hopkins, Philip F.; Bundy, Kevin; Wetzel, Andrew] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Croton, Darren] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Hernquist, Lars; Keres, Dusan; Younger, Joshua D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Khochfar, Sadegh] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Stewart, Kyle] Univ Calif Irvine, Dept Phys & Astron, Ctr Cosmol, Irvine, CA 92697 USA. RP Hopkins, PF (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. FU NASA [HST-HF-01243.01, NAS 5-26555] FX We thank Andrew Benson, Owen Parry, Simon White, Volker Springel, Gabriella de Lucia, and Carlos Frenk for helpful discussions. Support for P. F. H. was provided by the Miller Institute for Basic Research in Science, University of California Berkeley. J. D. Y. acknowledges support from NASA through Hubble Fellowship grant HST-HF-01243.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 288 TC 189 Z9 189 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 202 EP 229 DI 10.1088/0004-637X/715/1/202 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100018 ER PT J AU Jorstad, SG Marscher, AP Larionov, VM Agudo, I Smith, PS Gurwell, M Lahteenmaki, A Tornikoski, M Markowitz, A Arkharov, AA Blinov, DA Chatterjee, R D'Arcangelo, FD Falcone, AD Gomez, JL Hagen-Thorn, VA Jordan, B Kimeridze, GN Konstantinova, TS Kopatskaya, EN Kurtanidze, O Larionova, EG Larionova, LV McHardy, IM Melnichuk, DA Roca-Sogorb, M Schmidt, GD Skiff, B Taylor, B Thum, C Troitsky, IS Wiesemeyer, H AF Jorstad, Svetlana G. Marscher, Alan P. Larionov, Valeri M. Agudo, Ivan Smith, Paul S. Gurwell, Mark Lahteenmaki, Anne Tornikoski, Merja Markowitz, Alex Arkharov, Arkadi A. Blinov, Dmitry A. Chatterjee, Ritaban D'Arcangelo, Francesca D. Falcone, Abe D. Gomez, Jose L. Hagen-Thorn, Vladimir A. Jordan, Brendan Kimeridze, Givi N. Konstantinova, Tatiana S. Kopatskaya, Evgenia N. Kurtanidze, Omar Larionova, Elena G. Larionova, Liudmilla V. McHardy, Ian M. Melnichuk, Daria A. Roca-Sogorb, Mar Schmidt, Gary D. Skiff, Brian Taylor, Brian Thum, Clemens Troitsky, Ivan S. Wiesemeyer, Helmut TI FLARING BEHAVIOR OF THE QUASAR 3C 454.3 ACROSS THE ELECTROMAGNETIC SPECTRUM SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; polarization; quasars: individual (3C 454.3); X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; EXTRAGALACTIC RADIO-SOURCES; GAMMA-RAY FLARE; BL-LACERTAE; POLARIMETRIC OBSERVATIONS; POLARIZATION VARIABILITY; RELATIVISTIC JETS; HIGH-FREQUENCIES; BLAZAR 3C-454.3; AGILE DETECTION AB We analyze the behavior of the parsec-scale jet of the quasar 3C 454.3 during pronounced flaring in 2005-2008. Three major disturbances propagated down the jet along different trajectories with Lorentz factors Gamma > 10. The disturbances show a clear connection with millimeter-wave outbursts, in 2005 May/June, 2007 July, and 2007 December. High-amplitude optical events in the R-band light curve precede peaks of the millimeter-wave outbursts by 15-50 days. Each optical outburst is accompanied by an increase in X-ray activity. We associate the optical outbursts with propagation of the superluminal knots and derive the location of sites of energy dissipation in the form of radiation. The most prominent and long lasting of these, in 2005 May, occurred closer to the black hole, while the outbursts with a shorter duration in 2005 autumn and in 2007 might be connected with the passage of a disturbance through the millimeter-wave core of the jet. The optical outbursts, which coincide with the passage of superluminal radio knots through the core, are accompanied by systematic rotation of the position angle of optical linear polarization. Such rotation appears to be a common feature during the early stages of flares in blazars. We find correlations between optical variations and those at X-ray and gamma-ray energies. We conclude that the emergence of a superluminal knot from the core yields a series of optical and high-energy outbursts, and that the millimeter-wave core lies at the end of the jet's acceleration and collimation zone. We infer that the X-ray emission is produced via inverse Compton scattering by relativistic electrons of photons both from within the jet (synchrotron self-Compton) and external to the jet (external Compton, or EC); which one dominates depends on the physical parameters of the jet. A broken power-law model of the gamma-ray spectrum reflects a steepening of the synchrotron emission spectrum from near-IR to soft UV wavelengths. We propose that the gamma-ray emission is dominated by the EC mechanism, with the sheath of the jet supplying seed photons for gamma-ray events that occur near the millimeter-wave core. C1 [Jorstad, Svetlana G.; Marscher, Alan P.; Chatterjee, Ritaban; D'Arcangelo, Francesca D.; Taylor, Brian] Boston Univ, Inst Astrophys Res, Boston, MA 02115 USA. [Jorstad, Svetlana G.; Larionov, Valeri M.; Blinov, Dmitry A.; Hagen-Thorn, Vladimir A.; Konstantinova, Tatiana S.; Kopatskaya, Evgenia N.; Larionova, Elena G.; Larionova, Liudmilla V.; Melnichuk, Daria A.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Larionov, Valeri M.; Hagen-Thorn, Vladimir A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Agudo, Ivan; Roca-Sogorb, Mar] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Smith, Paul S.; Schmidt, Gary D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lahteenmaki, Anne; Tornikoski, Merja] Helsinki Univ Technol TKK, Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Markowitz, Alex] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Arkharov, Arkadi A.] Russian Acad Sci, Main Pulkovo Astron Observ, St Petersburg 196140, Russia. [Falcone, Abe D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Jordan, Brendan] Dublin Inst Adv Studies, Sch Cosm Phys, Dublin, Ireland. [Kimeridze, Givi N.; Kurtanidze, Omar] Abastumani Astrophys Observ, Mt Kanobili, Abastumani, Rep of Georgia. [McHardy, Ian M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Skiff, Brian; Taylor, Brian] Lowell Observ, Flagstaff, AZ 86001 USA. [Thum, Clemens] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Wiesemeyer, Helmut] IRAM, E-18012 Granada, Spain. RP Jorstad, SG (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02115 USA. EM jorstad@bu.edu RI Larionov, Valeri/H-1349-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Larionova, Elena/H-7287-2013; Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Agudo, Ivan/G-1701-2015; Morozova, Daria/H-1298-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Kopatskaya, Evgenia/H-4720-2013 OI Larionov, Valeri/0000-0002-4640-4356; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Larionova, Elena/0000-0002-2471-6500; Blinov, Dmitry/0000-0003-0611-5784; Larionova, Liudmila/0000-0002-0274-1481; Agudo, Ivan/0000-0002-3777-6182; Morozova, Daria/0000-0002-9407-7804; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Kopatskaya, Evgenia/0000-0001-9518-337X FU NASA [NNX08AV65G, NNX08AV61G, NNX08AJ64G]; National Science Foundation (NSF) [AST-0907893]; RFBR [09-02-00092]; Spanish "Ministerio de Ciencia e Innovacion" [AYA2007-67626-C03-03]; Academy of Finland; NSF; BU; Lowell Observatory; UK Science and Technology Facilities Council; Smithsonian Institution; Academia Sinica; INSU/CNRS (France); MPG (Germany); IGN (Spain); Fermi GI [NNX09AU07G] FX The authors thank the referee for very useful comments. The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX08AV65G and NNX08AV61G, and through Astrophysical Data Analysis Program grant NNX08AJ64G, and by the National Science Foundation (NSF) through grant AST-0907893. The VLBA is an instrument of the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The St. Petersburg State University team acknowledges support from RFBR grant 09-02-00092. The research at the IAA-CSIC is supported in part by the Spanish "Ministerio de Ciencia e Innovacion" through grant AYA2007-67626-C03-03. The effort at Steward Observatory was funded in part by NASA through Fermi Guest Investigator grant NNX08AV65G. The Metsahovi team acknowledges support from the Academy of Finland. We are grateful to the IRAM Director for providing discretionary observing time at the 30 m telescope. 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 Calar Alto Observatory is jointly operated by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucia-CSIC. 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. Partly based on data taken and assembled by the WEBT collaboration and stored in the WEBT archive at the Osservatorio Astronomico di Torino-INAF (http://www.oato.inaf.it/blazars/webt/). The Sub-millimeter 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 IRAM 30 m telescope is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). We acknowledge the Swift team for providing the public archive of Swift-XRT data, and we acknowledge Fermi GI grant NNX09AU07G for supporting the public archive of processed data. NR 60 TC 98 Z9 98 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 362 EP 384 DI 10.1088/0004-637X/715/1/362 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100031 ER PT J AU Tripathi, A Winn, JN Johnson, JA Howard, AW Halverson, S Marcy, GW Holman, MJ de Kleer, KR Carter, JA Esquerdo, GA Everett, ME Cabrera, NE AF Tripathi, Anjali Winn, Joshua N. Johnson, John Asher Howard, Andrew W. Halverson, Sam Marcy, Geoffrey W. Holman, Matthew J. de Kleer, Katherine R. Carter, Joshua A. Esquerdo, Gilbert A. Everett, Mark E. Cabrera, Nicole E. TI A PROGRADE, LOW-INCLINATION ORBIT FOR THE VERY HOT JUPITER WASP-3b SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: activity; stars: individual (WASP-3); techniques: radial velocities ID LIGHT-CURVE PROJECT; SPIN-ORBIT; MAGNETIC ACTIVITY; PLANETARY SYSTEM; CONSECUTIVE TRANSITS; EXTRASOLAR PLANET; RETROGRADE ORBIT; TRES-1; STARS; MISALIGNMENT AB We present new spectroscopic and photometric observations of the transiting exoplanetary system WASP-3. Spectra obtained during two separate transits exhibit the Rossiter-McLaughlin (RM) effect and allow us to estimate the sky-projected angle between the planetary orbital axis and the stellar rotation axis, lambda = 3.3(-4.4)(+2.5) deg. This alignment between the axes suggests that WASP-3b has a low orbital inclination relative to the equatorial plane of its parent star. During our first night of spectroscopic measurements, we observed an unexpected redshift briefly exceeding the expected sum of the orbital and RM velocities by 140 m s(-1). This anomaly could represent the occultation of material erupting from the stellar photosphere, although it is more likely to be an artifact caused by moonlight scattered into the spectrograph. C1 [Tripathi, Anjali; Winn, Joshua N.; de Kleer, Katherine R.; Carter, Joshua A.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Tripathi, Anjali; Winn, Joshua N.; de Kleer, Katherine R.; Carter, Joshua A.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Johnson, John Asher; Cabrera, Nicole E.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Howard, Andrew W.; Halverson, Sam; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Holman, Matthew J.; Esquerdo, Gilbert A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Everett, Mark E.] Planetary Sci Inst, Tucson, AZ 85719 USA. RP Tripathi, A (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM tripathi@mit.edu; jwinn@mit.edu RI Carter, Joshua/A-8280-2013; Howard, Andrew/D-4148-2015 OI Howard, Andrew/0000-0001-8638-0320 FU W. M. Keck Foundation; MIT UROP Endowment Fund and Office; NASA [NNX09AD36G, NNX09AB33G]; MIT Class of 1942 for a Career Development Professorship; NSF [AST-0702821] 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 thank N. Madhusudhan, Michael L. Stevens, and Robert Noyes for helpful discussions. We are grateful to the anonymous referee for helping to clarify the interpretation of the RV spike. 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. A. T. and K.dK. thank the MIT UROP Endowment Fund and Office for financial support. J.N.W. is grateful to the NASA Origins program for support through grants NNX09AD36G and NNX09AB33G, and to the MIT Class of 1942 for a Career Development Professorship. J.A.J. is an NSF Astronomy and Astrophysics Postdoctoral Fellow with support from the NSF grant AST-0702821. NR 47 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 421 EP 428 DI 10.1088/0004-637X/715/1/421 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100035 ER PT J AU Torres, G Bakos, GA Hartman, J Kovacs, G Noyes, RW Latham, DW Fischer, DA Johnson, JA Marcy, GW Howard, AW Sasselov, DD Kipping, D Sipocz, B Stefanik, RP Esquerdo, GA Everett, ME Lazar, J Papp, I Sari, P AF Torres, G. Bakos, G. A. Hartman, J. Kovacs, Geza Noyes, R. W. Latham, D. W. Fischer, D. A. Johnson, J. A. Marcy, G. W. Howard, A. W. Sasselov, D. D. Kipping, D. Sipocz, B. Stefanik, R. P. Esquerdo, G. A. Everett, M. E. Lazar, J. Papp, I. Sari, P. TI HAT-P-14b: A 2.2 M-J EXOPLANET TRANSITING A BRIGHT F STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (HAT-P-14, GSC 3086-00152); techniques: photometric; techniques: spectroscopic ID EXTRASOLAR GIANT PLANETS; KEPLER FIELD; ECCENTRIC ORBIT; HOT JUPITERS; K-DWARF; STELLAR; CATALOG; TRES-2; 2MASS; MASS AB We report the discovery of HAT-P-14b, a fairly massive transiting extrasolar planet orbiting the moderately bright star GSC 3086-00152 (V = 9.98), with a period of P = 4.627669 +/- 0.000005 days. The transit is close to grazing (impact parameter 0.891(-0.008)(+0.007)) and has a duration of 0.0912 +/- 0.0017 days, with a reference epoch of mid-transit of T-c = 2,454,875.28938 +/- 0.00047 (BJD). The orbit is slightly eccentric (e = 0.107 +/- 0.013), and the orientation is such that occultations are unlikely to occur. The host star is a slightly evolved mid-F dwarf with a mass of 1.386 +/- 0.045 M-circle dot, a radius of 1.468 +/- 0.054 R-circle dot, effective temperature 6600 +/- 90 K, and a slightly metal-rich composition corresponding to [Fe/H] = +0.11 +/- 0.08. The planet has a mass of 2.232 +/- 0.059 M-J and a radius of 1.150 +/- 0.052 R-J, implying a mean density of 1.82 +/- 0.24 g cm(-3). Its radius is well reproduced by theoretical models for the 1.3 Gyr age of the system if the planet has a heavy-element fraction of about 50 M-circle plus (7% of its total mass). The brightness, near-grazing orientation, and other properties of HAT-P-14 make it a favorable transiting system to look for changes in the orbital elements or transit timing variations induced by a possible second planet, and also to place meaningful constraints on the presence of sub-Earth mass or Earth-mass exomoons, by monitoring it for transit duration variations. C1 [Torres, G.; Bakos, G. A.; Hartman, J.; Noyes, R. W.; Latham, D. W.; Sasselov, D. D.; Kipping, D.; Sipocz, B.; Stefanik, R. P.; Esquerdo, G. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kovacs, Geza] Konkoly Observ Budapest, Budapest, Hungary. [Fischer, D. A.] San Francisco State Univ, Dept Phys & Astron, San Francisco, CA 94132 USA. [Johnson, J. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Marcy, G. W.; Howard, A. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kipping, D.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Sipocz, B.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Everett, M. E.] Planetary Sci Inst, Tucson, AZ USA. [Lazar, J.] Hungarian Astron Assoc, Budapest, Hungary. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Hartman, Joel/0000-0001-8732-6166; Fischer, Debra/0000-0003-2221-0861 FU NASA [NNG04GN74G, NNX08AF23G, NNX09AF59G, N049Hr, N018Hr]; SAO IRD; NSF [AST-0702843, AST-0702821]; Kepler Mission under NASA [NCC2-1390]; Hungarian Scientific Research Foundation (OTKA) [K-81373]; NOAO [A264Hr, A146Hr] FX HATNet operations have been funded by NASA grants NNG04GN74G and NNX08AF23G, and SAO IR&D grants. G. T. acknowledges partial support from NASA grant NNX09AF59G. G.A.B. and J.A.J. were supported by Post-doctoral Fellowships of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (D. W. L., PI). G. K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. G.A.B. thanks Gabor Kovacs for his help in system management of the HATNet computers while the data analysis was carried out. We are grateful to the anonymous referee for helpful suggestions. This research has benefited from Keck telescope time allocations granted through NOAO (programs A264Hr, A146Hr) and NASA (N049Hr, N018Hr). This research has also made use of the SIMBAD database and the VizieR catalogue access tool, both operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System Abstract Service, and of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF. NR 64 TC 29 Z9 29 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 458 EP 467 DI 10.1088/0004-637X/715/1/458 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100037 ER PT J AU Howell, JH Armus, L Mazzarella, JM Evans, AS Surace, JA Sanders, DB Petric, A Appleton, P Bothun, G Bridge, C Chan, BHP Charmandaris, V Frayer, DT Haan, S Inami, H Kim, DC Lord, S Madore, BF Melbourne, J Schulz, B Vivian, U Vavilkin, T Veilleux, S Xu, K AF Howell, Justin H. Armus, Lee Mazzarella, Joseph M. Evans, Aaron S. Surace, Jason A. Sanders, David B. Petric, Andreea Appleton, Phil Bothun, Greg Bridge, Carrie Chan, Ben H. P. Charmandaris, Vassilis Frayer, David T. Haan, Sebastian Inami, Hanae Kim, Dong-Chan Lord, Steven Madore, Barry F. Melbourne, Jason Schulz, Bernhard Vivian, U. Vavilkin, Tatjana Veilleux, Sylvain Xu, Kevin TI THE GREAT OBSERVATORIES ALL-SKY LIRG SURVEY: COMPARISON OF ULTRAVIOLET AND FAR-INFRARED PROPERTIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: galaxies; ultraviolet: galaxies ID STAR-FORMATION HISTORY; NEARBY GALAXIES; LUMINOSITY FUNCTION; STARBURST GALAXIES; DUST ATTENUATION; FORMING GALAXIES; EVOLUTION; ABSORPTION; UNIVERSE; ATLAS AB The Great Observatories All-sky LIRG Survey (GOALS) consists of a complete sample of 202 luminous infrared galaxies (LIRGs) selected from the IRAS Revised Bright Galaxy Sample (RBGS). The galaxies span the full range of interaction stages, from isolated galaxies to interacting pairs to late stage mergers. We present a comparison of the UV and infrared properties of 135 galaxies in GOALS observed by GALEX and Spitzer. For interacting galaxies with separations greater than the resolution of GALEX and Spitzer (similar to 2 ''-6 ''), we assess the UV and IR properties of each galaxy individually. The contribution of the FUV to the measured star formation rate (SFR) ranges from 0.2% to 17.9%, with a median of 2.8% and a mean of 4.0% +/- 0.4%. The specific star formation rate (SSFR) of the GOALS sample is extremely high, with a median value (3.9 x 10(-10) yr(-1)) that is comparable to the highest SSFRs seen in the Spitzer Infrared Nearby Galaxies Survey sample. We examine the position of each galaxy on the IR excess-UV slope (IRX-beta) diagram as a function of galaxy properties, including IR luminosity and interaction stage. The LIRGs on average have greater IR excesses than would be expected based on their UV colors if they obeyed the same relations as starbursts with L(IR) < 10(11) L(circle dot) or normal late-type galaxies. The ratio of L(IR) to the value one would estimate from the IRX-beta relation published for lower luminosity starburst galaxies ranges from 0.2 to 68, with a median value of 2.7. A minimum of 19% of the total IR luminosity in the RBGS is produced in LIRGs and ultraluminous infrared galaxies with red UV colors (beta > 0). Among resolved interacting systems, 32% contain one galaxy which dominates the IR emission while the companion dominates the UV emission. Only 21% of the resolved systems contain a single galaxy which dominates both wavelengths. C1 [Howell, Justin H.; Armus, Lee; Surace, Jason A.; Petric, Andreea; Bridge, Carrie; Haan, Sebastian; Inami, Hanae] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Mazzarella, Joseph M.; Chan, Ben H. P.; Madore, Barry F.] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Evans, Aaron S.; Kim, Dong-Chan] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Evans, Aaron S.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Sanders, David B.; Vivian, U.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Appleton, Phil; Frayer, David T.; Lord, Steven; Schulz, Bernhard; Xu, Kevin] CALTECH, NASA Herschel Sci Ctr, IPAC, Pasadena, CA 91125 USA. [Bothun, Greg] Univ Oregon, Dept Phys, Eugene, OR 97403 USA. [Bridge, Carrie; Melbourne, Jason] CALTECH, Div Phys Math & Astron, Caltech Opt Observ, Pasadena, CA 91125 USA. [Charmandaris, Vassilis] Univ Crete, Dept Phys, Iraklion 71003, Greece. [Charmandaris, Vassilis] IESL Fdn Res & Technol Hellas, GR-71110 Iraklion, Greece. [Charmandaris, Vassilis] Observ Paris, Chercheur Assoc, F-75014 Paris, France. [Madore, Barry F.] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Vivian, U.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vavilkin, Tatjana] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. [Veilleux, Sylvain] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Howell, JH (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM jhhowell@ipac.caltech.edu RI Charmandaris, Vassilis/A-7196-2008; OI Charmandaris, Vassilis/0000-0002-2688-1956; Mazzarella, Joseph/0000-0002-8204-8619; Appleton, Philip/0000-0002-7607-8766 FU National Aeronautics and Space Administration [NAS5-98034]; EU ToK [39965, FP7-REGPOT 206469] FX This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made 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. Based on observations made with the NASA Galaxy Evolution Explorer. GALEX is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034. V. C. acknowledges partial support from the EU ToK grant 39965 and FP7-REGPOT 206469. We thank Ranga Chary, Brian Siana, and Harry Teplitz for helpful discussions. We thank Armando Gil de Paz for making his GALEX background subtraction code available, Danny Dale for providing the SINGS data points in Figure 3, and the anonymous referee for helpful comments. NR 39 TC 81 Z9 81 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 572 EP 588 DI 10.1088/0004-637X/715/1/572 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100048 ER PT J AU Wolk, SJ Winston, E Bourke, TL Gutermuth, R Megeath, ST Spitzbart, BD Osten, R AF Wolk, Scott J. Winston, Elaine Bourke, Tyler L. Gutermuth, Robert Megeath, S. Thomas Spitzbart, Bradley D. Osten, Rachel TI X-RAY AND INFRARED EMISSION FROM YOUNG STELLAR OBJECTS NEAR LkH alpha 101 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; stars: distances; stars: individual (LkH alpha 101); stars: pre-main sequence; stars: protostars; X-rays: stars ID HERBIG-AE/BE STARS; T-TAURI STARS; SPITZER-SPACE-TELESCOPE; LOW-MASS STARS; POINT-SOURCE IDENTIFICATION; MAIN-SEQUENCE STARS; RHO-OPHIUCHI CLOUD; ARRAY CAMERA IRAC; FORMING REGION; ORION-NEBULA AB We report on a multiwavelength study of a partially embedded region of star formation centered on the Herbig Be star LkH alpha 101. Using two 40 ks Chandra observations, we detect 213 X-ray sources in the approximate to 17' x 17' ACIS-I field. We combine the X-ray data with Two Micron All Sky Survey near-IR observations and Spitzer IRAC and MIPS 24 mu m observations to obtain a complete picture of the cluster. A total of 158 of the X-ray sources have infrared counterparts. Of these, we find nine protostars, 48 Class II objects, five transition objects, and 72 Class III objects. From the Spitzer data we identify an additional 10 protostars, 53 Class II objects, and four transition disk candidates which are not detected by Chandra. We obtained optical spectra of a sample of both X-ray-detected and non-X-ray-detected objects. Combining the X-ray, Spitzer, and spectral data, we obtain independent estimates of cluster distance and the total cluster size-excluding protostars. We obtain consistent distance estimates of 510(-40)(+ 100) pc and a total cluster size of 255(-25)(+50) stars. We find the Class II: III ratio is about 5: 7 with some evidence that the Class III sources are spatially more dispersed. The cluster appears very young with three sites of active star formation and a median age of about 1 Myr. C1 [Wolk, Scott J.; Bourke, Tyler L.; Spitzbart, Bradley D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winston, Elaine] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Gutermuth, Robert] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Gutermuth, Robert] Smith Coll, Coll Astron 5, Northampton, MA 01063 USA. [Megeath, S. Thomas] Univ Toledo, Dept Phys & Astron, Toledo, OH 43606 USA. [Osten, Rachel] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wolk, Scott/0000-0002-0826-9261 FU National Aeronautics and Space Administration; National Science Foundation; NASA [NAS8-03060, HF-01189.01, NAS5-26555]; Space Telescope Science Institute; [GO5-4618X] FX This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration and the National Science Foundation. CXC guest investigator program supported this work through grant GO5-4618X. S.J.W. was supported by NASA contract NAS8-03060. Support for R.A.O. was provided by NASA through Hubble Fellowship grant HF-01189.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. for NASA, under contract NAS5-26555. NR 104 TC 13 Z9 13 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 20 PY 2010 VL 715 IS 1 BP 671 EP 695 DI 10.1088/0004-637X/715/1/671 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590HM UT WOS:000277216100057 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Bautista, M Beilicke, M Benbow, W Bottcher, M Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Cui, W Dickherber, R Duke, C Falcone, A Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gibbs, K Gillanders, GH Godambe, S Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Hui, CM Humensky, TB Imran, A Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ Lamerato, A LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Moriarty, P Mukherjee, R Ong, RA Otte, AN Pandel, D Perkins, JS Petry, D Pichel, A Pohl, M Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Roustazadeh, P Schroedter, M Sembroski, GH Senturk, GD Smith, AW Steele, D Swordy, SP Tesic, G Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Williams, DA Wissel, S Wood, M Zitzer, B Ackermann, M Ajello, M Antolini, E Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Berenji, B Blandford, RD Bloom, ED Bonamente, E Borgland, AW Bouvier, A Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Carrigan, S Casandjian, JM Cavazzuti, E Cecchi, C Celik, O Charles, E Chekhtman, A Cheung, CC Chiang, J Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Dermer, CD de Palma, F Silva, EDE Drell, PS Dubois, R Dumora, D Farnier, C Favuzzi, C Fegan, SJ Fortin, P Frailis, M Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Gehrels, N Germani, S Giebels, B Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grove, JE Guiriec, S Hays, E Horan, D Hughes, RE Johannesson, G Johnson, AS Johnson, WN Kamae, T Katagiri, H Kataoka, J Knodlseder, J Kuss, M Lande, J Latronico, L Lee, SH Garde, ML Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Makeev, A Mazziotta, MN Michelson, PF Mitthumsiri, W Mizuno, T Moiseev, AA Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nolan, PL Norris, JP Nuss, E Ohno, M Ohsugi, T Omodei, N Orlando, E Ormes, JF Paneque, D Panetta, JH Pelassa, V Pepe, M Pesce-Rollins, M Piron, F Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Ripken, J Rodriguez, AY Roth, M Sadrozinski, HFW Sanchez, D Sander, A Scargle, JD Sgro, C Siskind, EJ Smith, PD Spandre, G Spinelli, P Strickman, MS Suson, DJ Takahashi, H Tanaka, T Thayer, JB Thayer, JG Thompson, DJ Tibaldo, L Torres, DF Tosti, G Tramacere, A Usher, TL Vasileiou, V Vilchez, N Vitale, V Waite, AP Wang, P Winer, BL Wood, KS Yang, Z Ylinen, T Ziegler, M AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Bautista, M. Beilicke, M. Benbow, W. Boettcher, M. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Cui, W. Dickherber, R. Duke, C. Falcone, A. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gibbs, K. Gillanders, G. H. Godambe, S. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Hui, C. M. Humensky, T. B. Imran, A. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. Lamerato, A. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Moriarty, P. Mukherjee, R. Ong, R. A. Otte, A. N. Pandel, D. Perkins, J. S. Petry, D. Pichel, A. Pohl, M. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Roustazadeh, P. Schroedter, M. Sembroski, G. H. Senturk, G. Demet Smith, A. W. Steele, D. Swordy, S. P. Tesic, G. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Williams, D. A. Wissel, S. Wood, M. Zitzer, B. Ackermann, M. Ajello, M. Antolini, E. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Berenji, B. Blandford, R. D. Bloom, E. D. Bonamente, E. Borgland, A. W. Bouvier, A. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Carrigan, S. Casandjian, J. M. Cavazzuti, E. Cecchi, C. Celik, Oe. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Dermer, C. D. de Palma, F. do Couto e Silva, E. Drell, P. S. Dubois, R. Dumora, D. Farnier, C. Favuzzi, C. Fegan, S. J. Fortin, P. Frailis, M. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Gehrels, N. Germani, S. Giebels, B. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grove, J. E. Guiriec, S. Hays, E. Horan, D. Hughes, R. E. Johannesson, G. Johnson, A. S. Johnson, W. N. Kamae, T. Katagiri, H. Kataoka, J. Knoedlseder, J. Kuss, M. Lande, J. Latronico, L. Lee, S. -H. Garde, M. Llena Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Makeev, A. Mazziotta, M. N. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Moiseev, A. A. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nolan, P. L. Norris, J. P. Nuss, E. Ohno, M. Ohsugi, T. Omodei, N. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Pelassa, V. Pepe, M. Pesce-Rollins, M. Piron, F. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Ripken, J. Rodriguez, A. Y. Roth, M. Sadrozinski, H. F. -W. Sanchez, D. Sander, A. Scargle, J. D. Sgro, C. Siskind, E. J. Smith, P. D. Spandre, G. Spinelli, P. Strickman, M. S. Suson, D. J. Takahashi, H. Tanaka, T. Thayer, J. B. Thayer, J. G. Thompson, D. J. Tibaldo, L. Torres, D. F. Tosti, G. Tramacere, A. Usher, T. L. Vasileiou, V. Vilchez, N. Vitale, V. Waite, A. P. Wang, P. Winer, B. L. Wood, K. S. Yang, Z. Ylinen, T. Ziegler, M. TI THE DISCOVERY OF gamma-RAY EMISSION FROM THE BLAZAR RGB J0710+591 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE BL Lacertae objects: individual (RGB J0710+591, VER J0710+591); gamma rays: galaxies ID BL-LACERTAE OBJECTS; ATMOSPHERIC CHERENKOV TELESCOPES; ACTIVE GALACTIC NUCLEI; HOST GALAXIES; BACKGROUND-RADIATION; LAC OBJECTS; SAMPLE; CONSTRAINTS; ASTRONOMY; VERITAS AB The high-frequency-peaked BL Lacertae object RGB J0710+591 was observed in the very high-energy (VHE; E > 100 GeV) wave band by the VERITAS array of atmospheric Cherenkov telescopes. The observations, taken between 2008 December and 2009 March and totaling 22.1 hr, yield the discovery of VHE gamma rays from the source. RGB J0710+591 is detected at a statistical significance of 5.5 standard deviations (5.5 sigma) above the background, corresponding to an integral flux of (3.9 +/- 0.8) x 10(-12) cm(-2) s(-1) (3% of the Crab Nebula's flux) above 300 GeV. The observed spectrum can be fit by a power law from 0.31 to 4.6 TeV with a photon spectral index of 2.69 +/- 0.26(stat) +/- 0.20(sys). These data are complemented by contemporaneous multiwavelength data from the Fermi Large Area Telescope, the Swift X-ray Telescope, the Swift Ultra-Violet and Optical Telescope, and the Michigan-Dartmouth-MIT observatory. Modeling the broadband spectral energy distribution (SED) with an equilibrium synchrotron self-Compton model yields a good statistical fit to the data. The addition of an external-Compton component to the model does not improve the fit nor brings the system closer to equipartition. The combined Fermi and VERITAS data constrain the properties of the high-energy emission component of the source over 4 orders of magnitude and give measurements of the rising and falling sections of the SED. C1 [Acciari, V. A.; Benbow, W.; Galante, N.; Gibbs, K.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. 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F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Sadrozinski, H. F. -W.; Ziegler, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Scargle, J. D.] NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. [Siskind, E. J.] NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA. [Suson, D. J.] Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA. [Torres, D. F.] ICREA, Barcelona, Spain. [Tramacere, A.] CIFS, I-10133 Turin, Italy. [Tramacere, A.] INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Ylinen, T.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Ylinen, T.] Univ Kalmar, Sch Pure & Appl Nat Sci, SE-39182 Kalmar, Sweden. RP Acciari, VA (reprint author), Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. EM jperkins@cfa.harvard.edu; fortin@llr.in2p3.fr RI Funk, Stefan/B-7629-2015; Thompson, David/D-2939-2012; Gehrels, Neil/D-2971-2012; Baldini, Luca/E-5396-2012; lubrano, pasquale/F-7269-2012; Morselli, Aldo/G-6769-2011; Nolan, Patrick/A-5582-2009; Kuss, Michael/H-8959-2012; giglietto, nicola/I-8951-2012; Reimer, Olaf/A-3117-2013; Tosti, Gino/E-9976-2013; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Johnson, Neil/G-3309-2014; Johannesson, Gudlaugur/O-8741-2015; Gargano, Fabio/O-8934-2015; Loparco, Francesco/O-8847-2015; Moskalenko, Igor/A-1301-2007; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; OI Funk, Stefan/0000-0002-2012-0080; Thompson, David/0000-0001-5217-9135; lubrano, pasquale/0000-0003-0221-4806; Morselli, Aldo/0000-0002-7704-9553; giglietto, nicola/0000-0002-9021-2888; Reimer, Olaf/0000-0001-6953-1385; Frailis, Marco/0000-0002-7400-2135; Ward, John E/0000-0003-1973-0794; Caraveo, Patrizia/0000-0003-2478-8018; Johannesson, Gudlaugur/0000-0003-1458-7036; Gargano, Fabio/0000-0002-5055-6395; Loparco, Francesco/0000-0002-1173-5673; Moskalenko, Igor/0000-0001-6141-458X; Mazziotta, Mario /0000-0001-9325-4672; Torres, Diego/0000-0002-1522-9065; Cesarini, Andrea/0000-0002-8611-8610; Sgro', Carmelo/0000-0001-5676-6214; Cui, Wei/0000-0002-6324-5772; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK; National Aeronautics and Space Administration; 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) and Japan; 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 FX The VERITAS Collaboration acknowledges support from the U.S. Department of Energy, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. 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.; 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. NR 44 TC 42 Z9 42 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 MAY 20 PY 2010 VL 715 IS 1 BP L49 EP L55 DI 10.1088/2041-8205/715/1/L49 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590NM UT WOS:000277233200011 ER PT J AU Kilic, M Munn, JA Williams, KA Kowalski, PM von Hippel, T Harris, HC Jeffery, EJ DeGennaro, S Brown, WR McLeod, B AF Kilic, Mukremin Munn, Jeffrey A. Williams, Kurtis A. Kowalski, P. M. von Hippel, Ted Harris, Hugh C. Jeffery, Elizabeth J. DeGennaro, Steven Brown, Warren R. McLeod, B. TI VISITORS FROM THE HALO: 11 Gyr OLD WHITE DWARFS IN THE SOLAR NEIGHBORHOOD SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: atmospheres; stars: evolution; white dwarfs ID DIGITAL-SKY-SURVEY; FINAL MASS RELATION; LUMINOSITY FUNCTION; COOLING SEQUENCE; ATMOSPHERE MODELS; GALACTIC HALO; STARS; EVOLUTION; END; CONSTRAINTS AB We report the discovery of three nearby old halo white dwarf (WD) candidates in the Sloan Digital Sky Survey (SDSS), including two stars in a common proper motion binary system. These candidates are selected from our 2800 deg(2) proper motion survey on the Bok and U. S. Naval Observatory Flagstaff Station 1.3 m telescopes, and they display proper motions of 0.'' 4-0 ''.5 yr(-1). Follow-up MMT spectroscopy and near-infrared photometry demonstrate that all three objects are hydrogen-dominated atmosphere WDs with T(eff) approximate to 3700-4100 K. For average mass WDs, these temperature estimates correspond to cooling ages of 9-10 Gyr, distances of 70-80 pc, and tangential velocities of 140-200 km s(-1). Based on the UVW space velocities, we conclude that they most likely belong to the halo. Furthermore, the combined main-sequence and WD cooling ages are 10-11 Gyr. Along with SDSS J1102+4113, they are the oldest field WDs currently known. These three stars represent only a small fraction of the halo WD candidates in our proper motion survey, and they demonstrate that deep imaging surveys like the Pan-STARRS and Large Synoptic Survey Telescope should find many old thick disk and halo WDs that can be used to constrain the age of the Galactic thick disk and halo. C1 [Kilic, Mukremin; Brown, Warren R.; McLeod, B.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Munn, Jeffrey A.; Harris, Hugh C.] USN Observ, Flagstaff, AZ 86002 USA. [Williams, Kurtis A.; DeGennaro, Steven] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Kowalski, P. M.] GFZ German Res Ctr Geosci, Helmholtz Ctr Potsdam, D-14473 Potsdam, Germany. [Kowalski, P. M.] Ruhr Univ Bochum, Lehrstuhl Theoret Chem, D-44780 Bochum, Germany. [von Hippel, Ted] Siena Coll, Dept Phys, Loudonville, NY 12211 USA. [Jeffery, Elizabeth J.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Kilic, M (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM mkilic@cfa.harvard.edu RI Kowalski, Piotr/L-7411-2013; OI Kowalski, Piotr/0000-0001-6604-3458; Williams, Kurtis/0000-0002-1413-7679 FU NASA, Caltech; National Science Foundation [AST-0607480, AST-0602288] FX Support for this work was provided by NASA through the Spitzer Space Telescope Fellowship Program, under an award from Caltech. This material is also based on work supported by the National Science Foundation under grants AST-0607480 and AST-0602288. We thank the MMIRS commissioning team for obtaining the near-infrared observations, and J. Liebert for extensive help with the Bok telescope imaging observations and for many useful discussions. We also thank E. Olszewski for building the 90Prime instrument and the Steward Observatory Time Allocation Committee for supporting our proper motion survey program. NR 42 TC 22 Z9 22 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 MAY 20 PY 2010 VL 715 IS 1 BP L21 EP L25 DI 10.1088/2041-8205/715/1/L21 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590NM UT WOS:000277233200005 ER PT J AU Liu, X Greene, JE Shen, Y Strauss, MA AF Liu, Xin Greene, Jenny E. Shen, Yue Strauss, Michael A. TI DISCOVERY OF FOUR kpc-SCALE BINARY ACTIVE GALACTIC NUCLEI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE black hole physics; galaxies: active; galaxies: interactions; galaxies: nuclei; galaxies: Seyfert; quasars: general ID SUPERMASSIVE BLACK-HOLES; DIGITAL-SKY-SURVEY; REDSHIFT SURVEY; ELLIPTIC GALAXIES; QUASARS; LINES; CLASSIFICATION; FRAMEWORK; MERGERS; SYSTEM AB We report the discovery of four kpc-scale binary active galactic nuclei (AGNs). These objects were originally selected from the Sloan Digital Sky Survey based on double-peaked [O III] lambda lambda 4959, 5007 emission lines in their fiber spectra. The double peaks could result from pairing active supermassive black holes (SMBHs) in a galaxy merger or could be due to bulk motions of narrow-line region gas around a single SMBH. Deep near-infrared (NIR) images and optical slit spectra obtained from the Magellan 6.5 m and the Apache Point Observatory 3.5 m telescopes strongly support the binary SMBH scenario for the four objects. In each system, the NIR images reveal tidal features and double stellar components with a projected separation of several kpc, while optical slit spectra show two Seyfert 2 nuclei spatially coincident with the stellar components, with line-of-sight velocity offsets of a few hundred km s(-1). These objects were drawn from a sample of only 43 objects, demonstrating the efficiency of this technique to find kpc-scale binary AGNs. C1 [Liu, Xin; Greene, Jenny E.; Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Shen, Yue] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, X (reprint author), Princeton Univ, Dept Astrophys Sci, Peyton Hall,Ivy Lane, Princeton, NJ 08544 USA. FU NSF [AST-0707266]; Clay Postdoctoral Fellowship; 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 FX We thank J. Krolik for interesting comments, and the anonymous referee for a prompt report. X.L. and M.A.S. acknowledge the support of NSF grant AST-0707266. Y.S. acknowledges support from a Clay Postdoctoral Fellowship through the Smithsonian Astrophysical Observatory.; Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 44 TC 73 Z9 73 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 MAY 20 PY 2010 VL 715 IS 1 BP L30 EP L34 DI 10.1088/2041-8205/715/1/L30 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590NM UT WOS:000277233200007 ER PT J AU Parenti, LR Hadiaty, RK AF Parenti, Lynne R. Hadiaty, Renny K. TI A New, Remarkably Colorful, Small Ricefish of the Genus Oryzias (Beloniformes, Adrianichthyidae) from Sulawesi, Indonesia SO COPEIA LA English DT Article AB Oryzlas woworae, a new species of ricefish, is described from a freshwater habitat on Muna Island off the southeastern coast of the main island of Sulawesi, Indonesia. The new species is distinguished from all other known ricefishes by a remarkable color pattern of both sexes in life: the ventral surface of head and body anterior to the pelvic fins, dorsal portion of pectoral fins, dorsal-fin base, posterior portion of anal-fin base, caudal peduncle, and dorsal and ventral portions of caudal fin are brilliant red; the midlateral scales from just posterior to the eye to the caudal-fin base and the body scales anterior to the anal fin and ventral to midlateral scales are steel blue; the blue coloration is most prominent In adult males. Oryzias woworae, the smallest known ricefish from Sulawesi, is hypothesized to be a member of an unnamed clade of ricefishes diagnosed by a truncate, rather than lunate or emarginate, caudal fin. Description of O. woworae brings the recognized number of species in the beloniform family Adrianichthyidae to 29, 13 of which are endemic to Sulawesi. Ricefishes, in particular the new species, may serve as icons to generate interest in conservation of the endemic freshwater biota of Sulawesi. C1 [Parenti, Lynne R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Hadiaty, Renny K.] Indonesian Inst Sci LIPI, Div Zool, Biol Res Ctr, Museum Zoologicum Bogoriense, Cibinong 16911, Indonesia. RP Parenti, LR (reprint author), Smithsonian Inst, Natl Museum Nat Hist, POB 37012,NHB MRC 159, Washington, DC 20013 USA. EM parentil@si.edu; renny_hadiaty@yahoo.com NR 20 TC 13 Z9 14 U1 0 U2 3 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 20 PY 2010 IS 2 BP 268 EP 273 DI 10.1643/CI-09-108 PG 6 WC Zoology SC Zoology GA 606MK UT WOS:000278428900011 ER PT J AU Hilton, EJ Johnson, GD Smith-Vaniz, WF AF Hilton, Eric J. Johnson, G. David Smith-Vaniz, William F. TI Osteology and Systematics of Parastromateus niger (Perciformes: Carangidae), with Comments on the Carangid Dorsal Gill-Arch Skeleton SO COPEIA LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; FISHES PERCIFORMES; FEEDING-HABITS; POMFRET; WATERS; FOOD AB The monotypic Indo-Pacific genus Parastromateus Bleeker, 1864 is morphologically peculiar among carangid fishes in its overall body form and has been difficult to place phylogenetically. This has been partly the result of a lack of detailed morphological data for this and other carangid fishes. Here, we describe and analyze the osteology of Parastromateus niger (Bloch, 1795), review its taxonomic history, and describe characters that are suggestive of its phylogenetic affinities. In addition, we made a broad survey of gill-arch skeletal characters for carangids. Previous studies have noted that a combination of features from the skeletal anatomy of Parastromateus firmly places it within the Carangidae (presence of a gap between the second and third anal-fin spine) and within the tribe Carangini (presence of scutes, inferior vertebral formina). Within the Carangini, however, its phylogenetic placement is less clear. In our survey of the gill arches of Carangidae, we found that only Parastromateus and Hemicaranx have an enlarged toothplate that bridges the epibranchial 4 ceratobranchial 4 joint. Additionally, these two genera have a superficially similar form of teeth on the pharyngeal toothplates (elongate and filamentous vs. conical and stout in other carangins). Although outside the scope of our study, these and other morphological aspects of Parastromateus need to be brought into a broad-based cladistic analysis of the Carangidae. C1 [Hilton, Eric J.] Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. [Johnson, G. David] Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Dept Zool, Washington, DC 20013 USA. [Smith-Vaniz, William F.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. RP Hilton, EJ (reprint author), Virginia Inst Marine Sci, Coll William & Mary, Gloucester Point, VA 23062 USA. EM ehilton@vims.edu; johnsond@si.edu; smithvaniz@gmail.com FU NSF [DEB-0414552] FX For access to specimens in their care, we thank S. Schaefer, B. Brown, and R. Arrindell (AMNH), K. Hartel (MCZ), J. Lundberg and M. Sabaj (ANSP), and M. Westneat and M. Rogers (FMNH). Photographs in Fig. 1D and Fig. 7 taken at FMNH by J. Weinstein. A draft of the manuscript was reviewed by V. Springer, for which we are grateful. This research was initiated while EJH was supported as a Smithsonian Institution Postdoctoral Fellow (2004-2005). Funds from NSF DEB-0414552 (to Hilton and Grande) helped to defray the costs of museum visits. This is contribution number 3065 of the Virginia Institute of Marine Science, College of William and Mary. NR 56 TC 10 Z9 11 U1 3 U2 8 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 20 PY 2010 IS 2 BP 312 EP 333 DI 10.1643/CI-09-118 PG 22 WC Zoology SC Zoology GA 606MK UT WOS:000278428900016 ER PT J AU Smith, D AF Smith, David TI Clarence Lavett Smith SO COPEIA LA English DT Biographical-Item C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Smith, D (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 159, Washington, DC 20013 USA. EM smithd@si.edu NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC ICHTHYOLOGISTS HERPETOLOGISTS PI CHARLESTON PA UNIV CHARLESTON, GRICE MARINE LABORATORY, 205 FORT JOHNSON RD, CHARLESTON, SC 29412 USA SN 0045-8511 J9 COPEIA JI Copeia PD MAY 20 PY 2010 IS 2 BP 334 EP 340 DI 10.1643/OT-09-192 PG 7 WC Zoology SC Zoology GA 606MK UT WOS:000278428900017 ER PT J AU Perets, HB Gal-Yam, A Mazzali, PA Arnett, D Kagan, D Filippenko, AV Li, W Arcavi, I Cenko, SB Fox, DB Leonard, DC Moon, DS Sand, DJ Soderberg, AM Anderson, JP James, PA Foley, RJ Ganeshalingam, M Ofek, EO Bildsten, L Nelemans, G Shen, KJ Weinberg, NN Metzger, BD Piro, AL Quataert, E Kiewe, M Poznanski, D AF Perets, H. B. Gal-Yam, A. Mazzali, P. A. Arnett, D. Kagan, D. Filippenko, A. V. Li, W. Arcavi, I. Cenko, S. B. Fox, D. B. Leonard, D. C. Moon, D. -S. Sand, D. J. Soderberg, A. M. Anderson, J. P. James, P. A. Foley, R. J. Ganeshalingam, M. Ofek, E. O. Bildsten, L. Nelemans, G. Shen, K. J. Weinberg, N. N. Metzger, B. D. Piro, A. L. Quataert, E. Kiewe, M. Poznanski, D. TI A faint type of supernova from a white dwarf with a helium-rich companion SO NATURE LA English DT Article ID CORE-COLLAPSE SUPERNOVAE; IA SUPERNOVA; GALAXIES; MODELS; STAR; TELESCOPE AB Supernovae are thought to arise from two different physical processes. The cores of massive, short-lived stars undergo gravitational core collapse and typically eject a few solar masses during their explosion. These are thought to appear as type Ib/c and type II supernovae, and are associated with young stellar populations. In contrast, the thermonuclear detonation of a carbon-oxygen white dwarf, whose mass approaches the Chandrasekhar limit, is thought to produce type Ia supernovae(1,2). Such supernovae are observed in both young and old stellar environments. Here we report a faint type Ib supernova, SN 2005E, in the halo of the nearby isolated galaxy, NGC 1032. The 'old' environment near the supernova location, and the very low derived ejected mass (similar to 0.3 solar masses), argue strongly against a core-collapse origin. Spectroscopic observations and analysis reveal high ejecta velocities, dominated by helium-burning products, probably excluding this as a subluminous(3,4) or a regular(1) type Ia supernova. We conclude that it arises from a low-mass, old progenitor, likely to have been a helium-accreting white dwarf in a binary. The ejecta contain more calcium than observed in other types of supernovae and probably large amounts of radioactive (44)Ti. C1 [Perets, H. B.; Gal-Yam, A.; Arcavi, I.; Kiewe, M.] Weizmann Inst Sci, Dept Particle Phys & Astrophys, Fac Phys, IL-76100 Rehovot, Israel. [Perets, H. B.; Sand, D. J.; Soderberg, A. M.; Foley, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzali, P. A.] Scuola Normale Super Pisa, I-56127 Pisa, Italy. [Mazzali, P. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Mazzali, P. A.] INAF Oss Astron Padova, I-35122 Padua, Italy. [Arnett, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Kagan, D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Filippenko, A. V.; Li, W.; Cenko, S. B.; Ganeshalingam, M.; Weinberg, N. N.; Metzger, B. D.; Piro, A. L.; Quataert, E.; Poznanski, D.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Leonard, D. C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Moon, D. -S.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sand, D. J.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Anderson, J. P.] Univ Chile, Dept Astron, Camino El Observ, Santiago, Chile. [Anderson, J. P.; James, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead CH41 1LD, Merseyside, England. [Ofek, E. O.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Bildsten, L.; Shen, K. J.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Bildsten, L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Nelemans, G.] Radboud Univ Nijmegen, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Poznanski, D.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Gal-Yam, A (reprint author), Weizmann Inst Sci, Dept Particle Phys & Astrophys, Fac Phys, IL-76100 Rehovot, Israel. EM hperets@cfa.harvard.edu; avishay.gal-yam@weizmann.ac.il RI Nelemans, Gijs/D-3177-2012; Perets, Hagai/K-9605-2015; OI Nelemans, Gijs/0000-0002-0752-2974; Perets, Hagai/0000-0002-5004-199X; James, Philip/0000-0003-4131-5183 FU ISF/FIRST Fellowship; Ilan Ramon-Fulbright Fellowship; Weizmann-Minerva grant; Israeli Science Foundation; EU; Benoziyo Center for Astrophysics; Peter and Patricia Gruber Awards; US National Science Foundation; US Department of Energy; Richard and Rhoda Goldman Fund; Sylvia & Jim Katzman Foundation; TABASGO Foundation FX We thank P. Podsiadlowski, E. Nakar and D. Maoz for comments. We acknowledge observations with the Liverpool Telescope, and various telescopes at the Lick, Palomar and Keck Observatories. We are grateful to the staffs of these observatories, as well as to the institutions, agencies and companies funding these facilities. This research also made use of the NASA/IPAC Extragalactic Database (NED). H. B. P. acknowledges the ISF/FIRST and Ilan Ramon-Fulbright Fellowships, and is a Harvard-Smithsonian Center for Astrophysics Fellow. The collaborative work of A.G.-Y. and P. A. M. is supported by a Weizmann-Minerva grant. A.G.-Y. acknowledges further support by the Israeli Science Foundation, an EU Seventh Framework Programme Marie Curie IRG Fellowship, the Benoziyo Center for Astrophysics, and the Peter and Patricia Gruber Awards. A. V. F. is grateful for the support of the US National Science Foundation, the US Department of Energy, Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. R.J.F. is a Clay Fellow. NR 28 TC 125 Z9 125 U1 2 U2 10 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD MAY 20 PY 2010 VL 465 IS 7296 BP 322 EP 325 DI 10.1038/nature09056 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 598IO UT WOS:000277829200034 PM 20485429 ER PT J AU Prohl, H Ron, SR Ryan, MJ AF Proehl, Heike Ron, Santiago R. Ryan, Michael J. TI Ecological and genetic divergence between two lineages of Middle American tungara frogs Physalaemus (=Engystomops) pustulosus SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; SPECIES GROUP; ALLELE FREQUENCIES; MITOCHONDRIAL-DNA; SEXUAL SELECTION; CONTROL REGION; CLIMATE-CHANGE; F-STATISTICS; EVOLUTIONARY AB Background: Uncovering how populations of a species differ genetically and ecologically is important for understanding evolutionary processes. Here we combine population genetic methods (microsatellites) with phylogenetic information (mtDNA) to define genetic population clusters of the wide-spread Neotropical tungara frog (Physalaemus pustulosus). We measure gene flow and migration within and between population clusters and compare genetic diversity between population clusters. By applying ecological niche modeling we determine whether the two most divergent genetic groups of the tungara frog (1) inhabit different habitats, and (2) are separated geographically by unsuitable habitat across a gap in the distribution. Results: Most population structure is captured by dividing all sample localities into two allopatric genetic lineages. The Northern genetic lineage (NW Costa Rica) is genetically homogenous while the Southern lineage (SW Costa Rica and Panama) is sub-divided into three population clusters by both microsatellite and mtDNA analyses. Gene flow is higher within the Northern lineage than within the Southern lineage, perhaps due to increased landscape heterogeneity in the South. Niche modeling reveals differences in suitable habitat between the Northern and Southern lineages: the Northern lineage inhabits dry/pine-oak forests, while the Southern lineage is confined to tropical moist forests. Both lineages seem to have had little movement across the distribution gap, which persisted during the last glacial maximum. The lack of movement was more pronounced for the Southern lineage than for the Northern lineage. Conclusions: This study confirms the finding of previous studies that tungara frogs diverged into two allopatric genetic lineages north and south of the gap in the distribution in central Costa Rica several million years ago. The allopatric distribution is attributed to unsuitable habitat and probably other unknown ecological factors present across the distribution gap. Niche conservatism possibly contributes to preventing movements across the gap and gene flow between both groups. Genetic and ecological data indicate that there is the potential for ecological divergence in allopatry between lineages. In this context we discuss whether the Northern and Southern lineages should be recognized as separate species, and we conclude that further studies of pre- and post-zygotic isolation are needed for a final assessment. Identified population clusters should motivate future behavioral and ecological research regarding within-species biodiversity and speciation mechanisms. C1 [Proehl, Heike] Univ Vet Med, Inst Zool, D-30559 Hannover, Germany. [Ron, Santiago R.] Pontificia Univ Catolica Ecuador, Escuela Biol, Museo Zool, Ctr Biodiversidad & Ambiente, Quito, Ecuador. [Proehl, Heike; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Proehl, Heike; Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Prohl, H (reprint author), Univ Vet Med, Inst Zool, Bunteweg 17, D-30559 Hannover, Germany. EM heike.proehl@tiho-hannover.de FU German Science Foundation [PR 626/2-1]; NSF [IBN-981654]; SENACYT [PI-C08-0000470] FX We thank the Costa Rican (MINAE) and Panamanian (ANAM) authorities for research permits (232-2000-OFAU, 160-2001-OFAU, 259-2002-OFAU, 169-2003-OFAU, DNAPVS-01-2000, DNPN-001-2002), the Smithsonian Tropical Research Institute for logistical help, C. Salaz, I. Meuche and C. Avila for help during field work and R. A. Koshy for help in the lab. R. Bruning prepared Figure 1 and Figure 5. HP was funded by a research grant from the German Science Foundation (PR 626/2-1), MJR by NSF IBN-981654, and SRR by SENACYT (PI-C08-0000470). NR 90 TC 14 Z9 14 U1 3 U2 20 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1471-2148 J9 BMC EVOL BIOL JI BMC Evol. Biol. PD MAY 18 PY 2010 VL 10 AR 146 DI 10.1186/1471-2148-10-146 PG 18 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 624OJ UT WOS:000279828100001 PM 20482771 ER PT J AU Newsome, SD Collins, PW Rick, TC Guthrie, DA Erlandson, JM Fogel, ML AF Newsome, Seth D. Collins, Paul W. Rick, Torben C. Guthrie, Daniel A. Erlandson, Jon M. Fogel, Marilyn L. TI Pleistocene to historic shifts in bald eagle diets on the Channel Islands, California SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE Haliaeetus leucocephalus; historic ecology; stable isotopes ID KELP FOREST COMMUNITIES; GOLDEN EAGLES; FERAL PIGS; FOOD WEBS; RESILIENCE; CARNIVORES; MATTER AB Studies of current interactions among species, their prey, and environmental factors are essential for mitigating immediate threats to population viability, but the true range of behavioral and ecological flexibility can be determined only through research on deeper time-scales. Ecological data spanning centuries to millennia provide important contextual information for long-term management strategies, especially for species that now are living in relict populations. Here we use a variety of methods to reconstruct bald eagle diets and local abundance of their potential prey on the Channel Islands from the late Pleistocene to the time when the last breeding pairs disappeared from the islands in the mid-20th century. Faunal and isotopic analysis of bald eagles shows that seabirds were important prey for immature/adult eagles for millennia before the eagles' local extirpation. In historic times (A.D. 1850-1950), however, isotopic and faunal data show that breeding bald eagles provisioned their chicks with introduced ungulates (e.g., sheep), which were locally present in high densities. Today, bald eagles are the focus of an extensive conservation program designed to restore a stable breeding population to the Channel Islands, but native and nonnative prey sources that were important for bald eagles in the past are either diminished (e.g., seabirds) or have been eradicated (e.g., introduced ungulates). In the absence of sufficient resources, a growing bald eagle population on the Channel Islands could expand its prey base to include carrion from local pinniped colonies, exert predation pressure on a recovering seabird population, and possibly prey on endangered island foxes. C1 [Newsome, Seth D.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82070 USA. [Newsome, Seth D.; Fogel, Marilyn L.] Carnegie Inst Washington, Geophys Lab, Washington, DC 20015 USA. [Collins, Paul W.] Santa Barbara Museum Nat Hist, Santa Barbara, CA 93105 USA. [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Archaeobiol Program, Washington, DC 20013 USA. [Guthrie, Daniel A.] Claremont Mckenna Coll, Joint Sci Dept, Claremont, CA 91711 USA. [Erlandson, Jon M.] Univ Oregon, Museum Nat & Cultural Hist, Eugene, OR 97403 USA. RP Newsome, SD (reprint author), Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82070 USA. EM snewsome@uwyo.edu RI Fogel, Marilyn/M-2395-2015; OI Fogel, Marilyn/0000-0002-1176-3818; Erlandson, Jon/0000-0002-4705-4319 FU National Science Foundation [ATM-0502491]; Carnegie Institution of Washington; W.M. Keck Foundation [07100] FX We thank collections managers and curators at the Academy of Natural Sciences, Philadelphia; the Field Museum of Natural History, Chicago; the Museum of Comparative Zoology, Harvard University, Cambridge; the Museum of Vertebrate Zoology, University of California, Berkeley; the Natural History Museum of Los Angeles County, Los Angeles; the San Diego Natural History Museum, San Diego; the Santa Barbara Museum of Natural History; the Slater Museum of Natural History, University of Puget Sound, Tacoma; the University of California, Los Angeles; the Ventura County Museum of History and Art, Ventura; and the Western Foundation of Vertebrate Zoology, Camarillo for providing historic eagle feather and bone samples. We thank E. A. Swarth, B. J. O'Connor, and N. M. Smith-Herman for laboratory assistance and A. C. Jakle for constructive reviews. The National Park Service provided funding that supported collection and identification of prey remains from the Ferrelo Point bald eagle nest. S. D. N. and M. L. F. was funded in part by National Science Foundation Grant ATM-0502491, by the Carnegie Institution of Washington, and by Grant 07100 from the W.M. Keck Foundation. NR 50 TC 20 Z9 21 U1 0 U2 28 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD MAY 18 PY 2010 VL 107 IS 20 BP 9246 EP 9251 DI 10.1073/pnas.0913011107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 598GH UT WOS:000277822600042 PM 20439737 ER PT J AU Williams, JT Bogorodsky, SV AF Williams, Jeffrey T. Bogorodsky, Sergey V. TI Entomacrodus solus, a new species of blenny (Perciformes, Blenniidae) from the Red Sea SO ZOOTAXA LA English DT Article DE Lonely blenny; fish; Ras Mohammed; Egypt AB Entomacrodus solus, new species, is described on the basis of 35 specimens collected by J.E. Randall on a shallow rocky shore at the end of a mangrove channel at Ras Mohammed, Red Sea. The new species belongs to the Nigricans Species Group, which is distinguished from all other blennies in having about the medial third of the ventral margin of the upper lip entire and the lateral thirds crenulate. Within the group, now consisting of 11 species, the new species is distinguished by having only single pores at each preopercular pore position, typically three predorsal commissural pores, and small white spots on lips, head and body. Entomacrodus solus is the only species of the circumtropical genus Entomacrodus known from the Red Sea. C1 [Williams, Jeffrey T.] Smithsonian Inst, Natl Museum Nat Hist, Museum Support Ctr, Dept Vertebrate Zool,Div Fishes, Suitland, MD USA. [Bogorodsky, Sergey V.] Stn Naturalists, Omsk, Russia. RP Williams, JT (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Museum Support Ctr, Dept Vertebrate Zool,Div Fishes, Suitland, MD USA. EM williamsjt@si.edu; ic187196@yandex.ru NR 18 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 17 PY 2010 IS 2475 BP 64 EP 68 PG 5 WC Zoology SC Zoology GA 598DZ UT WOS:000277814600005 ER PT J AU Davidson, EH Erwin, DH AF Davidson, Eric H. Erwin, Douglas H. TI Evolutionary Innovation and Stability in Animal Gene Networks SO JOURNAL OF EXPERIMENTAL ZOOLOGY PART B-MOLECULAR AND DEVELOPMENTAL EVOLUTION LA English DT Article ID REGULATORY NETWORKS; MORPHOLOGICAL DISPARITY; HOXD COMPLEX; BODY PLANS; DROSOPHILA; ULTRABITHORAX; SPECIFICATION; TRANSCRIPTION; ECHINODERMS; MECHANISMS C1 [Erwin, Douglas H.] Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. [Davidson, Eric H.] CALTECH, Div Biol 156 29, Pasadena, CA 91125 USA. [Erwin, Douglas H.] Santa Fe Inst, Santa Fe, NM 87501 USA. RP Erwin, DH (reprint author), Smithsonian Inst, Dept Paleobiol, MRC 121, Washington, DC 20013 USA. EM erwind@si.edu NR 41 TC 20 Z9 20 U1 1 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1552-5007 EI 1552-5015 J9 J EXP ZOOL PART B JI J. Exp. Zool. Part B PD MAY 15 PY 2010 VL 314B IS 3 BP 182 EP 186 DI 10.1002/jez.b.21329 PG 5 WC Evolutionary Biology; Developmental Biology; Zoology SC Evolutionary Biology; Developmental Biology; Zoology GA 584VA UT WOS:000276780300002 PM 19937660 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Cambridge Dictionary of Psychology SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 3 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000179 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The International Encyclopedia of Gambling, 2nd edition SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000185 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Inner Planets SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000181 ER PT J AU Guz, SS Jones, LV AF Guz, Savannah Schroll Jones, Lauren, V TI Stars and Galaxies SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000184 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI The Disney Song Encyclopedia SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000182 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Michael Jackson's Complete Guide to Single Malt Scotch: A Connoisseur's Guide to the Single Malt Whiskies of Scotland SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 5 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000183 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI America's Film Legacy: The Authoritative Guide to the Landmark Movies in the National Film Registry SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, 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 MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000180 ER PT J AU Guz, SS AF Guz, Savannah Schroll TI Handbook of Neuroscience for the Behavioral Sciences SO LIBRARY JOURNAL LA English DT Book Review C1 [Guz, Savannah Schroll] Smithsonian Lib, Washington, DC USA. NR 1 TC 0 Z9 0 U1 1 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 MAY 15 PY 2010 VL 135 IS 9 BP 100 EP 100 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 596OG UT WOS:000277694000178 ER PT J AU Carr, BJ Kohri, K Sendouda, Y Yokoyama, J AF Carr, B. J. Kohri, Kazunori Sendouda, Yuuiti Yokoyama, Junichi TI New cosmological constraints on primordial black holes SO PHYSICAL REVIEW D LA English DT Article ID GAMMA-RAY BURSTS; BIG-BANG NUCLEOSYNTHESIS; PARTICLE EMISSION RATES; COSMIC-STRING LOOPS; 1ST-ORDER PHASE-TRANSITIONS; RUNNING SPECTRAL INDEX; SELF-SIMILAR GROWTH; GLUON-JET EMISSION; DARK-MATTER; EARLY UNIVERSE AB We update the constraints on the fraction of the Universe going into primordial black holes in the mass range 10(9)-10(17) g associated with the effects of their evaporations on big bang nucleosynthesis and the extragalactic photon background. We include for the first time all the effects of quark and gluon emission by black holes on these constraints and account for the latest observational developments. We then discuss the other constraints in this mass range and show that these are weaker than the nucleosynthesis and photon background limits, apart from a small range 10(13)-10(14) g, where the damping of cosmic microwave background anisotropies dominates. Finally we review the gravitational and astrophysical effects of nonevaporating primordial black holes, updating constraints over the broader mass range 1-10(50) g. C1 [Carr, B. J.] Queen Mary Univ London, Astron Unit, London E1 4NS, England. [Carr, B. J.; Yokoyama, Junichi] Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan. [Carr, B. J.] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 1A1, Canada. [Kohri, Kazunori] Tohoku Univ, Dept Phys, Sendai, Miyagi 9808578, Japan. [Kohri, Kazunori] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England. [Kohri, Kazunori] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sendouda, Yuuiti] Kyoto Univ, Yukawa Inst Theoret Phys, Kyoto 6068502, Japan. [Sendouda, Yuuiti] Univ Tokyo, Grad Sch Sci, Dept Phys, Tokyo 1130033, Japan. [Yokoyama, Junichi] Univ Tokyo, Inst Phys & Math Universe, Chiba 2778568, Japan. RP Carr, BJ (reprint author), Queen Mary Univ London, Astron Unit, Mile End Rd, London E1 4NS, England. EM B.J.Carr@qmul.ac.uk; kohri@tuhep.phys.tohoku.ac.jp; sendouda@yukawa.kyoto-u.ac.jp; yokoyama@resceu.s.u-tokyo.ac.jp NR 305 TC 205 Z9 206 U1 0 U2 14 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 MAY 15 PY 2010 VL 81 IS 10 AR 104019 DI 10.1103/PhysRevD.81.104019 PG 33 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 602NS UT WOS:000278146700067 ER PT J AU Munari, L Mathis, WN AF Munari, Lorenzo Mathis, Wayne N. TI World Catalog of the Family Canacidae (including Tethinidae) (Diptera), with keys to the supraspecific taxa SO ZOOTAXA LA English DT Article DE Diptera; Canacidae; Tethinidae; world catalog ID SURGE FLIES DIPTERA; GULF-OF-MEXICO; SPECIES DIPTERA; HALIDAY DIPTERA; BEACH FLIES; SUBFAMILY APETAENINAE; NEARCTIC TETHINIDAE; ARABIAN PENINSULA; GENUS PROCANACE; NORTH-AMERICA AB All genera and species of the family Canacidae as well as all synonyms and the world distribution for each species are listed to form an updated world catalog. Since McAlpine's (2007) placement of the families Canacidae sensu stricto and Tethinidae into a single, inclusive family (Canacidae sensu lato, i.e. the older family-group name), a comprehensive world catalog has been needed to include the new taxonomic arrangement and the corpus of new entries published over the last fifteen years, that is since the preceding catalogs (Mathis, 1992; Mathis and Munari, 1996). Identification keys to all supraspecific taxa are also given for each taxonomic section. C1 [Munari, Lorenzo] Nat Hist Museum, Entomol Sect, I-30135 Venice, Italy. [Mathis, Wayne N.] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Munari, L (reprint author), Nat Hist Museum, Entomol Sect, S Croce 1730, I-30135 Venice, Italy. EM lormun@iol.it; mathisw@si.edu NR 399 TC 6 Z9 10 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 14 PY 2010 IS 2471 BP 1 EP 84 PG 84 WC Zoology SC Zoology GA 598DT UT WOS:000277814000001 ER PT J AU Lieb, B Gebauer, W Gatsogiannis, C Depoix, F Hellmann, N Harasewych, MG Strong, EE Markl, J AF Lieb, Bernhard Gebauer, Wolfgang Gatsogiannis, Christos Depoix, Frank Hellmann, Nadja Harasewych, Myroslaw G. Strong, Ellen E. Markl, Juergen TI Molluscan mega-hemocyanin: an ancient oxygen carrier tuned by a similar to 550 kDa polypeptide SO FRONTIERS IN ZOOLOGY LA English DT Article ID KEYHOLE LIMPET HEMOCYANIN; CRYO-EM STRUCTURE; QUATERNARY STRUCTURE; MOLECULAR-MODEL; CRYOELECTRON MICROSCOPY; GASTROPOD HEMOCYANIN; SUBUNIT ORGANIZATION; ELECTRON-MICROSCOPY; NAUTILUS-POMPILIUS; PROTEIN-STRUCTURE AB Background: The allosteric respiratory protein hemocyanin occurs in gastropods as tubular di-, tri- and multimers of a 35 x 18 nm, ring-like decamer with a collar complex at one opening. The decamer comprises five subunit dimers. The subunit, a 400 kDa polypeptide, is a concatenation of eight paralogous functional units. Their exact topology within the quaternary structure has recently been solved by 3D electron microscopy, providing a molecular model of an entire didecamer (two conjoined decamers). Here we study keyhole limpet hemocyanin (KLH2) tridecamers to unravel the exact association mode of the third decamer. Moreover, we introduce and describe a more complex type of hemocyanin tridecamer discovered in fresh/brackish-water cerithioid snails (Leptoxis, Melanoides, Terebralia). Results: The "typical" KLH2 tridecamer is partially hollow, whereas the cerithioid tridecamer is almost completely filled with material; it was therefore termed "meg-hemocyanin". In both types, the staggering angle between adjoining decamers is 36. The cerithioid tridecamer comprises two typical decamers based on the canonical 400 kDa subunit, flanking a central "meg-decamer" composed of ten unique similar to 550 kDa subunits. The additional similar to 150 kDa per subunit substantially enlarge the internal collar complex. Preliminary oxygen binding measurements indicate a moderate hemocyanin oxygen affinity in Leptoxis (p50 similar to 9 mmHg), and a very high affinity in Melanoides (similar to 3 mmHg) and Terebralia (similar to 2 mmHg). Species-specific and individual variation in the proportions of the two subunit types was also observed, leading to differences in the oligomeric states found in the hemolymph. Conclusions: In cerithioid hemocyanin tridecamers ("meg-hemocyanin") the collar complex of the central decamer is substantially enlarged and modified. The preliminary O-2 binding curves indicate that there are species-specific functional differences in the cerithioid meg-hemocyanins which might reflect different physiological tolerances of these gill-breathing animals. The observed differential expression of the two subunit types of meg-hemocyanin might allow individual respiratory acclimatization. We hypothesize that meg-hemocyanin is a key character supporting the adaptive radiation and invasive capacity of cerithioid snails. C1 [Lieb, Bernhard; Gebauer, Wolfgang; Gatsogiannis, Christos; Depoix, Frank; Markl, Juergen] Johannes Gutenberg Univ Mainz, Inst Zool, D-55099 Mainz, Germany. [Hellmann, Nadja] Johannes Gutenberg Univ Mainz, Inst Mol Biophys, D-55099 Mainz, Germany. [Harasewych, Myroslaw G.; Strong, Ellen E.] MRC, Natl Museum Nat Hist, Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Markl, J (reprint author), Johannes Gutenberg Univ Mainz, Inst Zool, D-55099 Mainz, Germany. EM markl@uni-mainz.de RI Depoix, s/E-5037-2011; Gatsogiannis, Christos/G-4433-2011 FU Deutsche Forschungsgemeinschaft [DFG-GK 1043] FX We thank Dr Jeffrey T. Garner (Alabama Fish & Game Division) for the samples of Leptoxis praerosa, Dr J. Robin Harris for critical reading of the manuscript, Christoph Kuhne for the Terebralia images, Prof. Dr Werner Kuhlbrandt and Deryck Mills (MPI Biophysics, Frankfurt, Germany) for kindly providing access to the FEI Polara microscope and the Deutsche Forschungsgemeinschaft (DFG-GK 1043 grant to JM) for financial support. NR 45 TC 14 Z9 14 U1 0 U2 7 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1742-9994 J9 FRONT ZOOL JI Front. Zool. PD MAY 13 PY 2010 VL 7 AR 14 DI 10.1186/1742-9994-7-14 PG 13 WC Zoology SC Zoology GA 611DV UT WOS:000278792100001 PM 20465844 ER PT J AU Lotz, JM Jonsson, P Cox, TJ Primack, JR AF Lotz, Jennifer M. Jonsson, Patrik Cox, T. J. Primack, Joel R. TI The effect of mass ratio on the morphology and time-scales of disc galaxy mergers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: structure ID DIGITAL-SKY-SURVEY; HIGH-REDSHIFT GALAXIES; SPIRAL GALAXIES; STAR-FORMATION; BLACK-HOLES; COSMOLOGICAL SIMULATIONS; ELLIPTIC GALAXIES; DUST ATTENUATION; ACCRETION EVENTS; MERGING GALAXIES AB The majority of galaxy mergers are expected to be minor mergers. The observational signatures of minor mergers are not well understood; thus, there exist few constraints on the minor merger rate. This paper seeks to address this gap in our understanding by determining if and when minor mergers exhibit disturbed morphologies and how they differ from the morphology of major mergers. We simulate a series of unequal-mass moderate gas-fraction disc galaxy mergers. With the resulting g-band images, we determine how the time-scale for identifying galaxy mergers via projected separation and quantitative morphology (the Gini coefficient G, asymmetry A and the second-order moment of the brightest 20 per cent of the light M(20)) depends on the merger mass ratio, relative orientations and orbital parameters. We find that G-M(20) is as sensitive to 9:1 baryonic mass ratio mergers as 1:1 mergers, with observability time-scales of similar to 0.2-0.4 Gyr. In contrast, asymmetry finds mergers with baryonic mass ratios between 4:1 and 1:1 (assuming local disc galaxy gas fractions). Asymmetry time-scales for moderate gas-fraction major disc mergers are similar to 0.2-0.4 Gyr and less than 0.06 Gyr for moderate gas-fraction minor mergers. The relative orientations and orbits have little effect on the time-scales for morphological disturbances. Observational studies of close pairs often select major mergers by choosing paired galaxies with similar luminosities and/or stellar masses. Therefore, the various ways of finding galaxy mergers (G-M(20), A, close pairs) are sensitive to galaxy mergers of different mass ratios. By comparing the frequency of mergers selected by different techniques, one may place empirical constraints on the major and minor galaxy merger rates. C1 [Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. [Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. RP Lotz, JM (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. EM lotz@noao.edu FU NASA [NAG5-11513, HST-AR-9998, HST-AR-10678, HST-AR-10958, HST-AR-11958, NAS5-26555, NNX07AG94G]; W. M. Keck Foundation; US Department of Energy FX JML acknowledges support from the NOAO Leo Goldberg Fellowship, NASA grants NAG5-11513 and HST-AR-9998 and would like to thank P. Madau for support during this project. PJ was supported by programmes HST-AR-10678, HST-AR-10958 and HST-AR-11958, provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and by the Spitzer Space Telescope Theoretical Research Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. TJC was supported by a grant from the W. M. Keck Foundation. JRP's research was supported by NASA ATP grant NNX07AG94G.; This research used computational resources of the NASA Advanced Supercomputing Division (NAS) and the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy. NR 57 TC 98 Z9 98 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2010 VL 404 IS 2 BP 575 EP 589 DI 10.1111/j.1365-2966.2010.16268.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591TZ UT WOS:000277329000002 ER PT J AU Lotz, JM Jonsson, P Cox, TJ Primack, JR AF Lotz, Jennifer M. Jonsson, Patrik Cox, T. J. Primack, Joel R. TI The effect of gas fraction on the morphology and time-scales of disc galaxy mergers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: structure ID STAR-FORMING GALAXIES; MASSIVE ELLIPTIC GALAXIES; LDSS REDSHIFT SURVEYS; MAJOR MERGERS; BLACK-HOLES; COSMOLOGICAL SIMULATIONS; FUNDAMENTAL PLANE; DUST ATTENUATION; SPIRAL GALAXIES; DWARF GALAXIES AB Gas-rich galaxy mergers are more easily identified by their disturbed morphologies than mergers with less gas. Because the typical gas fraction of galaxy mergers is expected to increase with redshift, the under-counting of low gas-fraction mergers may bias morphological estimates of the evolution of galaxy merger rate. To understand the magnitude of this bias, we explore the effect of gas fraction on the morphologies of a series of simulated disc galaxy mergers. With the resulting g-band images, we determine how the time-scale for identifying major and minor galaxy mergers via close projected pairs and quantitative morphology (the Gini coefficient G, the second-order moment of the brightest 20 per cent of the light M(20) and asymmetry A) depends on baryonic gas fraction f(gas). Strong asymmetries last significantly longer in high gas-fraction mergers of all mass ratios, with time-scales ranging from < 300 Myr for f(gas) similar to 20 per cent to >= 1 Gyr for f(gas) similar to 50 per cent. Therefore, the strong evolution with redshift observed in the fraction of asymmetric galaxies may reflect evolution in the gas properties of galaxies rather than the global galaxy merger rate. On the other hand, the time-scale for identifying a galaxy merger via G-M(20) is weakly dependent on gas fraction (similar to 200-400 Myr), consistent with the weak evolution observed for G-M(20) mergers. C1 [Lotz, Jennifer M.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Jonsson, Patrik] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cox, T. J.] Carnegie Observ, Pasadena, CA 91101 USA. [Primack, Joel R.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. RP Lotz, JM (reprint author), Natl Opt Astron Observ, 950 N Cherry Ave, Tucson, AZ 85719 USA. EM lotz@noao.edu FU NASA [NAG5-11513, HST-AR-9998, HST-AR-10678, HST-AR-10958, HST-AR-11958, NAS5-26555, NNX07AG94G]; W. M. Keck Foundation; US Department of Energy FX JML acknowledges support from the NOAO Leo Goldberg Fellowship, NASA grants NAG5-11513 and HST-AR-9998, and would like to thank P. Madau for support for this project. PJ was supported by programmes HST-AR-10678, HST-AR-10958 and HST-AR-11958 provided by NASA through grants from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and by the Spitzer Space Telescope Theoretical Research Program, through a contract issued by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. TJC was supported by a grant from the W. M. Keck Foundation. JRP was supported by NASA ATP grant NNX07AG94G.; This research used computational resources of the NASA Advanced Supercomputing Division (NAS) and the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy. NR 69 TC 79 Z9 79 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2010 VL 404 IS 2 BP 590 EP 603 DI 10.1111/j.1365-2966.2010.16269.x PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591TZ UT WOS:000277329000003 ER PT J AU Brocksopp, C Jonker, PG Maitra, D Krimm, HA Pooley, GG Ramsay, G Zurita, C AF Brocksopp, C. Jonker, P. G. Maitra, D. Krimm, H. A. Pooley, G. G. Ramsay, G. Zurita, C. TI Disentangling jet and disc emission from the 2005 outburst of XTE J1118+480 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; stars: individual: XTE J1118+480; X-rays: binaries ID X-RAY TRANSIENT; HOLE CANDIDATE XTE-J1118+480; ACCRETING BLACK-HOLES; LOW/HARD STATE; SYNCHROTRON EMISSION; HARD-STATE; BINARY; RADIO; SPECTRUM; MODEL AB The black hole X-ray transient, XTE J1118+480, has now twice been observed in outbursts - 2000 and 2005 - and on both occasions remained in the low/hard X-ray spectral state. Here we present radio, infrared, optical, soft X-ray and hard X-ray observations of the more recent outburst. We find that the light curves have very different morphologies compared with the 2000 event and the optical decay is delayed relative to the X-ray/radio. We attribute this lesser degree of correlation to contributions of emission from multiple components, in particular the jet and accretion disc. Whereas the jet seemed to dominate the broad-band spectrum in 2000, in 2005 the accretion disc seemed to be more prominent and we use an analysis of the light curves and spectra to distinguish between the jet and disc emission. There also appears to be an optically thin component to the radio emission in the 2005 data, possibly associated with multiple ejection events and decaying as the outburst proceeds. These results add to the discussion that the term 'low/hard state' covers a wider range of properties than previously thought, if it is to account for XTE J1118+480 during these two outbursts. C1 [Brocksopp, C.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Jonker, P. G.] Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Jonker, P. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Maitra, D.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. [Maitra, D.] Univ Amsterdam, Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. [Maitra, D.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Krimm, H. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Krimm, H. A.] Univ Space Res Assoc, Columbia, MD 20144 USA. [Pooley, G. G.] Univ Cambridge, Cavendish Lab, Mullard Radio Astron Observ, Cambridge CB3 0HE, England. [Ramsay, G.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Zurita, C.] Inst Astrofis Canarias, Tenerife 38200, Spain. RP Brocksopp, C (reprint author), Univ Coll London, Mullard Space Sci Lab, Holmbury St Mary, Dorking RH5 6NT, Surrey, England. EM cb4@mssl.ucl.ac.uk FU Netherlands Organization for Scientific Research; Swift project; UK Science and Technology Facilities Council; National Science Foundation FX We thank Sandy Leggett for help with the UKIRT data reduction, Jorn Wilms for advice regarding the HEXTE analysis and the anonymous referee for useful suggestions which improved the paper. PGJ acknowledges support from a VIDI grant from the Netherlands Organization for Scientific Research. HAK is supported by the Swift project. 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. The LT is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The United Kingdom Infrared Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the UK. The VLA is a facility of the National Radio Astronomy Observatory, which is operated by Associated Universities Inc., under cooperative agreement with the National Science Foundation. NR 49 TC 18 Z9 18 U1 0 U2 1 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 11 PY 2010 VL 404 IS 2 BP 908 EP 916 DI 10.1111/j.1365-2966.2010.16323.x PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591TZ UT WOS:000277329000022 ER PT J AU Staines, CL AF Staines, C. L. TI Type specimens of Chrysomelidae (Coleoptera) in the Academy of Natural Sciences in Philadelphia SO ZOOTAXA LA English DT Article DE types; Coleoptera; Chrysomelidae ID AMERICA NORTH; MEXICO AB Type specimens of 88 species of Chrysomelidae are housed in the Academy of Natural History of Philadelphia collection-5 holotypes, 60 syntypes, 13 paratypes, and 10 paralectotypes. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. RP Staines, CL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. EM stainesc@si.edu NR 56 TC 1 Z9 1 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 11 PY 2010 IS 2451 BP 26 EP 42 PG 17 WC Zoology SC Zoology GA 594UH UT WOS:000277563900002 ER PT J AU Mao, SA Gaensler, BM Haverkorn, M Zweibel, EG Madsen, GJ McClure-Griffiths, NM Shukurov, A Kronberg, PP AF Mao, S. A. Gaensler, B. M. Haverkorn, M. Zweibel, E. G. Madsen, G. J. McClure-Griffiths, N. M. Shukurov, A. Kronberg, P. P. TI A SURVEY OF EXTRAGALACTIC FARADAY ROTATION AT HIGH GALACTIC LATITUDE: THE VERTICAL MAGNETIC FIELD OF THE MILKY WAY TOWARD THE GALACTIC POLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; ISM: magnetic fields; polarization ID LOCAL INTERSTELLAR-MEDIUM; WARM IONIZED MEDIUM; HYBRID COSMIC-RAY; NORTH POLAR SPUR; DISTANT STARS; LINEAR-POLARIZATION; MAGELLANIC-CLOUD; INNER GALAXY; H-ALPHA; BUBBLE AB We present a study of the vertical magnetic field of the Milky Way toward the Galactic poles, determined from observations of Faraday rotation toward more than 1000 polarized extragalactic radio sources at Galactic latitudes vertical bar b vertical bar >= 77 degrees, using the Westerbork Radio Synthesis Telescope and the Australia Telescope Compact Array. We find median rotation measures (RMs) of 0.0 +/- 0.5 rad m(-2) and +6.3 +/- 0.7 rad m(-2) toward the north and south Galactic poles, respectively, demonstrating that there is no coherent vertical magnetic field in the Milky Way at the Sun's position. If this is a global property of the Milky Way's magnetism, then the lack of symmetry across the disk rules out pure dipole or quadrupole geometries for the Galactic magnetic field. The angular fluctuations in RM seen in our data show no preferred scale within the range approximate to 0 degrees.1 to approximate to 25 degrees. The observed standard deviation in RM of similar to 9 rad m(-2) then implies an upper limit of similar to 1 mu G on the strength of the random magnetic field in the warm ionized medium at high Galactic latitudes. 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. [Gaensler, B. M.; Madsen, G. J.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Haverkorn, M.] ASTRON, NL-7991 PD Dwingeloo, Netherlands. [Zweibel, E. G.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Shukurov, A.] Newcastle Univ, Sch Math & Stat, Newcastle Upon Tyne NE1 7RU, Tyne & Wear, England. [Kronberg, P. P.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Kronberg, P. P.] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. RP Mao, SA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM samao@cfa.harvard.edu RI Gaensler, Bryan/F-8655-2010; OI McClure-Griffiths, Naomi/0000-0003-2730-957X; Shukurov, Anvar/0000-0001-6200-4304; Gaensler, Bryan/0000-0002-3382-9558 FU Australian Research Council [FF0561298]; National Science Foundation; Netherlands Foundation for Scientific Research (NWO); Commonwealth of Australia FX We thank Eve Meyer and Gemma Anderson for helping to carry out the ATCA observations; Observer's friend Ger de Bruyn and Gyula Jozsa for helping with the preparation of the WSRT observations; Robert Braun for helping with the WSRT data calibration with AIPS, Douglas Finkbeiner for useful discussions, and Justin Kasper for detailed discussion on the ionospheric RM correction. This work was supported in part by an Australian Research Council Federation Fellowship (FF0561298) awarded to B. M. G. 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. The Westerbork Synthesis Radio Telescope is operated by the ASTRON (Netherlands Institute for Radio Astronomy) with support from the Netherlands Foundation for Scientific Research (NWO). The Australia Telescope Compact Array is part of the Australian Telescope, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. NR 100 TC 74 Z9 74 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2010 VL 714 IS 2 BP 1170 EP 1186 DI 10.1088/0004-637X/714/2/1170 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587ER UT WOS:000276973100016 ER PT J AU Belczynski, K Bulik, T Fryer, CL Ruiter, A Valsecchi, F Vink, JS Hurley, JR AF Belczynski, Krzysztof Bulik, Tomasz Fryer, Chris L. Ruiter, Ashley Valsecchi, Francesca Vink, Jorick S. Hurley, Jarrod R. TI ON THE MAXIMUM MASS OF STELLAR BLACK HOLES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; black hole physics; gravitational waves; stars: evolution; stars: neutron ID X-RAY SOURCES; LUMINOUS BLUE VARIABLES; ASYMPTOTIC GIANT BRANCH; METALLICITY DEPENDENCE; POPULATION SYNTHESIS; SOLAR METALLICITY; STAR EVOLUTION; NEUTRON-STAR; MODELS; PARAMETERS AB We present the spectrum of compact object masses: neutron stars and black holes (BHs) that originate from single stars in different environments. In particular, we calculate the dependence of maximum BH mass on metallicity and on some specific wind mass loss rates (e.g., Hurley et al. and Vink et al.). Our calculations show that the highest mass BHs observed in the Galaxy M(bh) similar to 15 M(circle dot) in the high metallicity environment (Z = Z(circle dot) = 0.02) can be explained with stellar models and the wind mass loss rates adopted here. To reach this result we had to set luminous blue variable mass loss rates at the level of similar to 10(-4) M(circle dot) yr(-1) and to employ metallicity-dependent Wolf-Rayet winds. With such winds, calibrated on Galactic BH mass measurements, the maximum BH mass obtained for moderate metallicity (Z = 0.3 Z(circle dot) = 0.006) is M(bh,max) = 30 M(circle dot). This is a rather striking finding as the mass of the most massive known stellar BH is M(bh) = 23-34 M(circle dot) and, in fact, it is located in a small star-forming galaxy with moderate metallicity. We find that in the very low (globular cluster-like) metallicity environment the maximum BH mass can be as high as M(bh,max) = 80 M(circle dot) (Z = 0.01 Z(circle dot) = 0.0002). It is interesting to note that X-ray luminosity from Eddington-limited accretion onto an 80 M(circle dot) BH is of the order of similar to 10(40) erg s(-1) and is comparable to luminosities of some known ultra-luminous X-ray sources. We emphasize that our results were obtained for single stars only and that binary interactions may alter these maximum BH masses (e.g., accretion from a close companion). This is strictly a proof-of-principle study which demonstrates that stellar models can naturally explain even the most massive known stellar BHs. C1 [Belczynski, Krzysztof; Fryer, Chris L.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Belczynski, Krzysztof; Bulik, Tomasz] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Bulik, Tomasz] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Fryer, Chris L.] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Ruiter, Ashley] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Ruiter, Ashley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Valsecchi, Francesca] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Vink, Jorick S.] Armagh Observ, Armagh BT61 9DG, North Ireland. [Hurley, Jarrod R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. RP Belczynski, K (reprint author), Los Alamos Natl Lab, POB 1663,MS 466, Los Alamos, NM 87545 USA. EM kbelczyn@nmsu.edu; tb@astrouw.edu.pl; clfreyer@lanl.gov; aruiter@nmsu.edu; francesca@u.northwestern.edu; jsv@arm.ac.uk; JHurley@groupwise.swin.edu.au FU KBN [N N203 302835]; U.S. Department of Energy at Los Alamos National Laboratory [DE-AC52-06NA25396] FX We express special thanks to Vicky Kalogera for critical comments. K. B. and T. B. acknowledge the support from KBN grant N N203 302835. This work was carried out in part under the auspices of the National Nuclear Security Administration of the U.S. Department of Energy at Los Alamos National Laboratory and supported by contract no. DE-AC52-06NA25396. NR 68 TC 163 Z9 163 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2010 VL 714 IS 2 BP 1217 EP 1226 DI 10.1088/0004-637X/714/2/1217 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587ER UT WOS:000276973100020 ER PT J AU Myers, PC AF Myers, Philip C. TI STAR-FORMING GAS IN YOUNG CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; stars: formation ID INITIAL MASS FUNCTION; EMBEDDED STELLAR CLUSTERS; MOLECULAR CLOUD; DENSE CORES; DARK CLOUDS; CO OUTFLOWS; LUMINOSITY FUNCTIONS; STRUCTURAL-ANALYSIS; LARGE-SCALE; EVOLUTION AB Initial conditions for star formation in clusters are estimated for protostars whose masses follow the initial mass function from 0.05 to 10 solar masses. Star-forming infall is assumed equally likely to stop at any moment, due to gas dispersal dominated by stellar feedback. For spherical infall, the typical initial condensation must have a steep density gradient, as in low-mass cores, surrounded by a shallower gradient, as in the clumps around cores. These properties match observed column densities in cluster-forming regions when the mean infall stopping time is 0.05 Myr and the accretion efficiency is 0.5. The infall duration increases with final protostar mass, from 0.01 to 0.3 Myr, and the mass accretion rate increases from 3 to 300 x 10(-6) solar masses yr(-1). The typical spherical accretion luminosity is similar to 5 solar luminosities, reducing the "luminosity problem" to a factor of similar to 3. The initial condensation density gradient changes from steep to shallow at radius 0.04 pc, enclosing 0.9 solar masses, with mean column density 2 x 10(22) cm(-2) and with effective central temperature 16 K. These initial conditions are denser and warmer than those for isolated star formation. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Myers, PC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM pmyers@cfa.harvard.edu NR 83 TC 10 Z9 10 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2010 VL 714 IS 2 BP 1280 EP 1289 DI 10.1088/0004-637X/714/2/1280 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587ER UT WOS:000276973100026 ER PT J AU Wang, JF Risaliti, G Fabbiano, G Elvis, M Zezas, A Karovska, M AF Wang, Junfeng Risaliti, G. Fabbiano, G. Elvis, M. Zezas, A. Karovska, M. TI REVISITING THE SHORT-TERM X-RAY SPECTRAL VARIABILITY OF NGC 4151 WITH CHANDRA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: individual (NGC 4151); galaxies: Seyfert; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT-GALAXY NGC-4151; SHORT-TIMESCALE VARIABILITY; CENTRAL BLACK-HOLE; IRON LINE; MULTIWAVELENGTH OBSERVATIONS; PHYSICAL CONDITIONS; SUZAKU OBSERVATIONS; COLUMN DENSITIES; DUST TORUS AB We present new X-ray spectral data for the Seyfert 1 nucleus in NGC 4151 observed with Chandra for similar to 200 ks. A significant ACIS pileup is present, resulting in a nonlinear count rate variation during the observation. With pileup corrected spectral fitting, we are able to recover the spectral parameters and find consistency with those derived from unpiled events in the ACIS readout streak and outer region from the bright nucleus. The absorption corrected 2-10 keV flux of the nucleus varied between 6 x 10(-11) erg s(-1) cm(-2) and 10(-10) erg s(-1) cm(-2) (L2-10 keV similar to 1.3-2.1x 10(42) erg s(-1)). Similar to earlier Chandra studies of NGC 4151 at a historical low state, the photon indices derived from the same absorbed power-law model are Gamma similar to 0.7-0.9. However, we show that Gamma is highly dependent on the adopted spectral models. Fitting the power-law continuum with a Compton reflection component gives Gamma similar to 1.1. By including passage of non-uniform X-ray obscuring clouds, we can reproduce the apparent flat spectral states with Gamma similar to 1.7, typical for Seyfert 1 active galactic nuclei. The same model also fits the hard spectra from previous ASCA "long look" observation of NGC 4151 in the lowest flux state. The spectral variability during our observation can be interpreted as variations in intrinsic soft continuum flux relative to a Compton reflection component that is from distant cold material and constant on short timescale, or variations of partially covering absorber in the line of sight toward the nucleus. An ionized absorber model with ionization parameter log xi similar to 0.8-1.1 can also fit the low-resolution ACIS spectra. If the partial covering model is correct, adopting a black hole mass M-BH similar to 4.6 x 10(7) M-circle dot we constrain the distance of the obscuring cloud from the central black hole to be r less than or similar to 9 It-day, consistent with the size of the broad emission line region of NGC 4151 from optical reverberation mapping. C1 [Wang, Junfeng; Risaliti, G.; Fabbiano, G.; Elvis, M.; Zezas, A.; Karovska, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Wang, JF (reprint author), INAF Arcetri Observ, Largo E,Fermi 5, I-50125 Florence, Italy. EM juwang@cfa.harvard.edu; risaliti@cfa.harvard.edu; pepi@cfa.harvard.edu; elvis@cfa.harvard.edu; azezas@cfa.harvard.edu; karovska@cfa.harvard.edu RI Wang, Junfeng/A-1476-2011; Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Risaliti, Guido/0000-0002-3556-977X FU NASA [GO8-9101X, NAS8-39073] FX We thank the anonymous referee for helpful comments that significantly improved the manuscript. This work is partially supported from NASA grant GO8-9101X and NASA Contract NAS8-39073 (CXC). J. W. thanks Michael McCollough for advice on ACIS readout streaks. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages CIAO and Sherpa. NR 93 TC 12 Z9 12 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 10 PY 2010 VL 714 IS 2 BP 1497 EP 1510 DI 10.1088/0004-637X/714/2/1497 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587ER UT WOS:000276973100043 ER PT J AU Elias-Rosa, N Van Dyk, SD Li, WD Miller, AA Silverman, JM Ganeshalingam, M Boden, AF Kasliwal, MM Vinko, J Cuillandre, JC Filippenko, AV Steele, TN Bloom, JS Griffith, CV Kleiser, IKW Foley, RJ AF Elias-Rosa, Nancy Van Dyk, Schuyler D. Li, Weidong Miller, Adam A. Silverman, Jeffrey M. Ganeshalingam, Mohan Boden, Andrew F. Kasliwal, Mansi M. Vinko, Jozsef Cuillandre, Jean-Charles Filippenko, Alexei V. Steele, Thea N. Bloom, Joshua S. Griffith, Christopher V. Kleiser, Io K. W. Foley, Ryan J. TI THE MASSIVE PROGENITOR OF THE TYPE II-LINEAR SUPERNOVA 2009kr SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: individual (NGC 1832); stars: evolution; supernovae: general; supernovae: individual (SN 2009kr) ID EXPANDING PHOTOSPHERE METHOD; INFRARED-EMISSION; P SUPERNOVAE; SN 1999EM; EVOLUTION; NGC-6946; SPECTRA; NOVAE; 1979C; PHOTOMETRY AB We present early-time photometric and spectroscopic observations of supernova (SN) 2009kr in NGC 1832. We find that its properties to date support its classification as Type II-linear (SN II-L), a relatively rare subclass of core-collapse supernovae (SNe). We have also identified a candidate for the SN progenitor star through comparison of pre-explosion, archival images taken with WFPC2 on board the Hubble Space Telescope with SN images obtained using adaptive optics plus NIRC2 on the 10 m Keck-II telescope. Although the host galaxy's substantial distance (similar to 26 Mpc) results in large uncertainties in the relative astrometry, we find that if this candidate is indeed the progenitor, it is a highly luminous (M(V)(0) = -7.8 mag) yellow supergiant with initial mass similar to 18-24 M(circle dot). This would be the first time that an SN II-L progenitor has been directly identified. Its mass may be a bridge between the upper initial mass limit for the more common Type II-plateau SNe and the inferred initial mass estimate for one Type II-narrow SN. C1 [Elias-Rosa, Nancy; Van Dyk, Schuyler D.] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Li, Weidong; Miller, Adam A.; Silverman, Jeffrey M.; Ganeshalingam, Mohan; Filippenko, Alexei V.; Steele, Thea N.; Bloom, Joshua S.; Griffith, Christopher V.; Kleiser, Io K. W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Boden, Andrew F.; Kasliwal, Mansi M.] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Vinko, Jozsef] Univ Szeged, Dept Opt & Quantum Elect, H-6720 Szeged, Hungary. [Vinko, Jozsef] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Cuillandre, Jean-Charles] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Elias-Rosa, N (reprint author), CALTECH, Spitzer Sci Ctr, 1200 E Calif Blvd, Pasadena, CA 91125 USA. EM nelias@ipac.caltech.edu RI Elias-Rosa, Nancy/D-3759-2014; OI Elias-Rosa, Nancy/0000-0002-1381-9125; Vinko, Jozsef/0000-0001-8764-7832; Van Dyk, Schuyler/0000-0001-9038-9950 FU Hungarian OTKA [K76816]; NSF [AST-0707769, AST-0908886]; Sylvia & Jim Katzman Foundation; TABASGO Foundation; NASA through STScI [AR-11248, GO-10877]; Harvard University; UC Berkeley; University of Virginia; NASA/Swift [NNX09AQ66G]; DOE FX We thank C. Blake, S. B. Cenko, B. Cobb, E. Falco, M. Kandrashoff, J. Kong, M. Modjaz, D. Starr, and T. Yuan for their assistance. J. V. received support from Hungarian OTKA Grant K76816, NSF Grant AST-0707769, and Texas Advanced Research Project grant ARP-0094. A.V.F.'s group and KAIT are supported by NSF grant AST-0908886, the Sylvia & Jim Katzman Foundation, the TABASGO Foundation, and NASA through grants AR-11248 and GO-10877 from STScI. PAIRITEL is operated by SAO with support from the Harvard University Milton Fund, UC Berkeley, University of Virginia, and NASA/Swift grant NNX09AQ66G. J. S. B. and his group are partially funded by a DOE SciDAC grant. NR 49 TC 39 Z9 39 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 MAY 10 PY 2010 VL 714 IS 2 BP L254 EP L259 DI 10.1088/2041-8205/714/2/L254 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590NA UT WOS:000277232000015 ER PT J AU Marshall, HL Hardcastle, MJ Birkinshaw, M Croston, J Evans, D Landt, H Lenc, E Massaro, F Perlman, ES Schwartz, DA Siemiginowska, A Stawarz, L Urry, CM Worrall, DM AF Marshall, H. L. Hardcastle, M. J. Birkinshaw, M. Croston, J. Evans, D. Landt, H. Lenc, E. Massaro, F. Perlman, E. S. Schwartz, D. A. Siemiginowska, A. Stawarz, L. Urry, C. M. Worrall, D. M. TI A FLARE IN THE JET OF PICTOR A SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual (Pictor A); galaxies: jets; X-rays: galaxies ID X-RAY-EMISSION; M87 JET; CHANDRA; HST-1 AB A Chandra X-ray imaging observation of the jet in Pictor A showed a feature that appears to be a flare that faded between 2000 and 2002. The feature was not detected in a follow-up observation in 2009. The jet itself is over 150 kpc long and about 1 kpc wide, so finding year-long variability is surprising. Assuming a synchrotron origin of the observed high-energy photons and a minimum energy condition for the outflow, the synchrotron loss time of the X-ray emitting electrons is of order 1200 years, which is much longer than the observed variability timescale. This leads to the possibility that the variable X-ray emission arises from a very small sub-volume of the jet, characterized by a magnetic field that is substantially larger than the average over the jet. C1 [Marshall, H. L.; Evans, D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Hardcastle, M. J.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Birkinshaw, M.; Massaro, F.; Schwartz, D. A.; Siemiginowska, A.; Worrall, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Birkinshaw, M.; Worrall, D. M.] Univ Bristol, Dept Phys, Bristol BS8 1TL, Avon, England. [Croston, J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Landt, H.] Univ Melbourne, Sch Phys, Melbourne, Vic 3010, Australia. [Lenc, E.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 2121, Australia. [Perlman, E. S.] Florida Inst Technol, Dept Phys & Space Sci, Melbourne, FL 32901 USA. [Stawarz, L.] JAXA ISAS, Sagamihara, Kanagawa 2298510, Japan. [Stawarz, L.] Jagiellonian Univ, Astron Observ, PL-30244 Krakow, Poland. [Urry, C. M.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. RP Marshall, HL (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM hermanm@space.mit.edu; m.j.hardcastle@herts.ac.uk; Mark.Birkinshaw@bristol.ac.uk; J.Croston@soton.ac.uk; devans@space.mit.edu; hlandt@unimelb.edu.au; Emil.Lenc@csiro.au; fmassaro@head.cfa.harvard.edu; eperlman@fit.edu; das@head-cfa.harvard.edu; aneta@head.cfa.harvard.edu; stawarz@slac.stanford.edu; meg.urry@yale.edu; D.Worrall@bristol.ac.uk RI Hardcastle, Martin/E-2264-2012; Urry, Claudia/G-7381-2011; Massaro, Francesco/L-9102-2016; OI Hardcastle, Martin/0000-0003-4223-1117; Urry, Claudia/0000-0002-0745-9792; Massaro, Francesco/0000-0002-1704-9850; Lenc, Emil/0000-0002-9994-1593 FU National Aeronautics and Space Administration (NASA) [SV3-73016, NAS8-03060, NAS 8-39073]; Polish MNiSW [N-N203-380336] FX Support for this work was provided in part by the National Aeronautics and Space Administration (NASA) through the Smithsonian Astrophysical Observatory (SAO) contract SV3-73016 to MIT for support of the Chandra X-Ray Center (CXC), which is operated by SAO for and on behalf of NASA under contract NAS8-03060. Support was also provided by NASA under contract NAS 8-39073 to SAO. 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. L. S. is grateful for the support from Polish MNiSW through the grant N-N203-380336. NR 14 TC 14 Z9 14 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 MAY 10 PY 2010 VL 714 IS 2 BP L213 EP L216 DI 10.1088/2041-8205/714/2/L213 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590NA UT WOS:000277232000007 ER PT J AU Pimiento, C Ehret, DJ MacFadden, BJ Hubbell, G AF Pimiento, Catalina Ehret, Dana J. MacFadden, Bruce J. Hubbell, Gordon TI Ancient Nursery Area for the Extinct Giant Shark Megalodon from the Miocene of Panama SO PLOS ONE LA English DT Article ID SPHYRNA-LEWINI GRIFFITH; OFFSHORE FORAGING AREA; CARCHARODON-CARCHARIAS; WHITE SHARK; ONTOGENIC CHANGES; SOUTH-CAROLINA; KANEOHE BAY; CALIFORNIA; MIGRATION; BEHAVIOR AB Background: As we know from modern species, nursery areas are essential shark habitats for vulnerable young. Nurseries are typically highly productive, shallow-water habitats that are characterized by the presence of juveniles and neonates. It has been suggested that in these areas, sharks can find ample food resources and protection from predators. Based on the fossil record, we know that the extinct Carcharocles megalodon was the biggest shark that ever lived. Previous proposed paleo-nursery areas for this species were based on the anecdotal presence of juvenile fossil teeth accompanied by fossil marine mammals. We now present the first definitive evidence of ancient nurseries for C. megalodon from the late Miocene of Panama, about 10 million years ago. Methodology/Principal Findings: We collected and measured fossil shark teeth of C. megalodon, within the highly productive, shallow marine Gatun Formation from the Miocene of Panama. Surprisingly, and in contrast to other fossil accumulations, the majority of the teeth from Gatun are very small. Here we compare the tooth sizes from the Gatun with specimens from different, but analogous localities. In addition we calculate the total length of the individuals found in Gatun. These comparisons and estimates suggest that the small size of Gatun's C. megalodon is neither related to a small population of this species nor the tooth position within the jaw. Thus, the individuals from Gatun were mostly juveniles and neonates, with estimated body lengths between 2 and 10.5 meters. Conclusions/Significance: We propose that the Miocene Gatun Formation represents the first documented paleo-nursery area for C. megalodon from the Neotropics, and one of the few recorded in the fossil record for an extinct selachian. We therefore show that sharks have used nursery areas at least for 10 millions of years as an adaptive strategy during their life histories. C1 [Pimiento, Catalina] Univ Florida, Dept Biol, Gainesville, FL 32610 USA. [Pimiento, Catalina; Ehret, Dana J.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Div Vertebrate Paleontol, Gainesville, FL 32611 USA. [Pimiento, Catalina] Smithsonian Trop Res Inst, Ctr Paleoecol & Archaeol, Panama City, Panama. [Ehret, Dana J.] Univ Florida, Sch Nat Resources & Environm, Gainesville, FL USA. [MacFadden, Bruce J.] Natl Sci Fdn, Div Res Learning Educ & Human Resources, Arlington, VA 22230 USA. [Hubbell, Gordon] Jaws Int, Gainesville, FL USA. RP Pimiento, C (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32610 USA. EM pimientoc@ufl.edu FU NSF [EAR 0418042]; Sigma [Xi G2009100426]; Florida Museum of Natural History; Smithsonian Tropical Research Institute; Mitchell Hope Scholarship; Ken Ericson Scholarship FX This project was funded by NSF EAR 0418042 (http://www.nsf.gov/funding), Sigma Xi G2009100426 (http://www.sigmaxi.org/programs/giar/index.shtml), The Florida Museum of Natural History (www.flmnh.ufl.edu), The Smithsonian Tropical Research Institute (www.stri.org), The Mitchell Hope Scholarship(http://www.southwestfloridafossilclub.com/) and the Ken Ericson Scholarship(http://www.flmnh.ufl.edu/vertpaleo/kenericsonscholarship.htm ). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 52 TC 24 Z9 26 U1 9 U2 72 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 MAY 10 PY 2010 VL 5 IS 5 AR e10552 DI 10.1371/journal.pone.0010552 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 593OJ UT WOS:000277467900008 PM 20479893 ER PT J AU Reasenberg, RD Phillips, JD AF Reasenberg, Robert D. Phillips, James D. TI A weak equivalence principle test on a suborbital rocket SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID SATELLITE; POINTS; STEP AB We describe a Galilean test of the weak equivalence principle, to be conducted during the free fall portion of a sounding rocket flight. The test of a single pair of substances is aimed at a measurement uncertainty of sigma(eta) < 10(-16) after averaging the results of eight separate drops. The weak equivalence principle measurement is made with a set of four laser gauges that are expected to achieve 0.1 pm Hz(-1/2). The discovery of a violation (eta not equal 0) would have profound implications for physics, astrophysics and cosmology. C1 [Reasenberg, Robert D.; Phillips, James D.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Reasenberg, RD (reprint author), Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM reasenberg@cfa.harvard.edu FU NASA SMD [NNC04GB30G, NNX08AO04G] FX This work was supported in part by the NASA SMD through grants NNC04GB30G (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 20 TC 12 Z9 12 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD MAY 7 PY 2010 VL 27 IS 9 AR 095005 DI 10.1088/0264-9381/27/9/095005 PG 14 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 575VK UT WOS:000276097200005 ER PT J AU Pawson, DL Pawson, DJ King, RA AF Pawson, David L. Pawson, Doris J. King, Rachael A. TI A taxonomic guide to the Echinodermata of the South Atlantic Bight, USA: 1. Sea cucumbers (Echinodermata: Holothuroidea) SO ZOOTAXA LA English DT Article DE Holothurians; sea cucumbers; South Atlantic Bight; SERTC ID HOLOTHURIANS AB A summary account is given of the 33 holothurian species known from the South Atlantic Bight, from Cape Hatteras, North Carolina, to Cape Canaveral, Florida, from the shore to a depth of 200 meters. Four of the six known orders of holothurians are represented in the study area. Each species is diagnosed and illustrated; citations of informative literature and brief discussions of distribution and general biology are included. Also included are dichotomous keys to aid in identification to the species level. A new genus is erected to accommodate Pseudocolochirus mysticus Deichmann, 1930. Ocnus pygmaeus (Theel, 1886b) and O. surinamensis (Semper, 1868) are referred to the genus Aslia Rowe, 1970. C1 [Pawson, David L.; Pawson, Doris J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [King, Rachael A.] SERTC, S Carolina Dept Nat Resources, Charleston, SC 29422 USA. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Mail Stop MRC163, Washington, DC 20013 USA. EM pawsond@si.edu RI King, Rachael/C-3821-2012 FU Southeast Regional Taxonomic Center FX We gratefully acknowledge support from the Southeast Regional Taxonomic Center (Dr. Elizabeth Wenner, Principal Investigator), for the study of echinoderms of the South Atlantic Bight. David M. Knott (data), and Susan Thornton-DeVictor (digital images of echinoderms), greatly facilitated our work on collections and in preparation of manuscripts for publication. Nadia Myers and Joe Cowan, formerly of SERTC, provided specimens and locality data. Joyce McCullough provided invaluable volunteer assistance. The reference collections of the Grice Marine Laboratory, College of Charleston, were made available to us through the courtesy of Dr. Antony Harold. The late Cynthia Ahearn, National Museum of Natural History, Smithsonian Institution, assisted us with collections databases. Most of the line illustrations of whole animals were prepared by Mary Ann Nelson. Susan Thornton-DeVictor photographed specimens, and prepared Figure 6. Jacqueline Paratore Lincoln edited the scanning electron microscope images. This is South Carolina Marine Resources Division Contribution No. 660, and Contribution No. 805 from the Smithsonian Marine Station at Fort Pierce, Florida. NR 69 TC 10 Z9 14 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 7 PY 2010 IS 2449 BP 1 EP 48 PG 48 WC Zoology SC Zoology GA 592LF UT WOS:000277379700001 ER PT J AU Mironov, AN Pawson, DL AF Mironov, Alexandr N. Pawson, David L. TI A new genus and species of Western Atlantic sea lily in the family Septocrinidae (Echinodermata: Crinoidea: Bourgueticrinida) SO ZOOTAXA LA English DT Article DE Rouxicrinus vestitus; Caribbean Sea; taxonomy; Crinoidea; Bourgueticrinida; Septocrinidae ID STALKED CRINOIDS; MORPHOLOGY AB Rouxicrinus vestitus new genus, new species, collected during submersible dives at depths of 421-887 m near Barbados, Colombia and the Bahamas is described, and notes on ecology are included. It is referred to the family Septocrinidae Mironov, 2000, which now comprises three genera, Zeuctocrinus A. M. Clark, 1973, Septocrinus Mironov, 2000, and Rouxicrinus new genus. This new genus differs significantly from both Septocrinus and Zeuctocrinus in having numerous low columnals in the proxistele, which tapers toward the crown, first pinnule arising more proximally, thorns on brachials and pinnulars, and a thick covering of soft tissue on arms and pinnules. C1 [Mironov, Alexandr N.] Russian Acad Sci, PP Shirshov Oceanol Inst, Moscow 117997, Russia. [Pawson, David L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Mironov, AN (reprint author), Russian Acad Sci, PP Shirshov Oceanol Inst, Nakhimovskyi Prospekt 36, Moscow 117997, Russia. EM miron@ocean.ru; pawsond@si.edu FU Harbor Branch Oceanographic Institution at Fort Pierce, Florida; Smithsonian Institution, Washington DC FX DLP wishes to acknowledge the collaboration and friendship of J. E. Miller, G. Hendler, and P. M. Kier during numerous manned submersible dives in the Caribbean, 1983-1989. The dives, in Johnson-Sea-Link submersibles, were made under the auspices of the Harbor Branch Oceanographic Institution at Fort Pierce, Florida, and Smithsonian Institution, Washington DC. Special thanks are due to the reviewers M. Roux and C. G. Messing, whose constructive comments and suggestions helped improve this paper. This paper is Contribution No. 782 from the Smithsonian Marine Station at Fort Pierce, Florida. NR 46 TC 4 Z9 4 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD MAY 7 PY 2010 IS 2449 BP 49 EP 68 PG 20 WC Zoology SC Zoology GA 592LF UT WOS:000277379700002 ER PT J AU Lind, EM Parker, JD AF Lind, Eric M. Parker, John D. TI Novel Weapons Testing: Are Invasive Plants More Chemically Defended than Native Plants? SO PLOS ONE LA English DT Article ID INCREASED COMPETITIVE ABILITY; ENEMY RELEASE HYPOTHESIS; BIOTIC RESISTANCE; NATURAL ENEMIES; GROWTH-RATE; LEAF-AREA; HERBIVORES; EVOLUTION; TRAITS; SUCCESS AB Background: Exotic species have been hypothesized to successfully invade new habitats by virtue of possessing novel biochemistry that repels native enemies. Despite the pivotal long-term consequences of invasion for native food-webs, to date there are no experimental studies examining directly whether exotic plants are any more or less biochemically deterrent than native plants to native herbivores. Methodology/Principal Findings: In a direct test of this hypothesis using herbivore feeding assays with chemical extracts from 19 invasive plants and 21 co-occurring native plants, we show that invasive plant biochemistry is no more deterrent (on average) to a native generalist herbivore than extracts from native plants. There was no relationship between extract deterrence and length of time since introduction, suggesting that time has not mitigated putative biochemical novelty. Moreover, the least deterrent plant extracts were from the most abundant species in the field, a pattern that held for both native and exotic plants. Analysis of chemical deterrence in context with morphological defenses and growth-related traits showed that native and exotic plants had similar trade-offs among traits. Conclusions/Significance: Overall, our results suggest that particular invasive species may possess deterrent secondary chemistry, but it does not appear to be a general pattern resulting from evolutionary mismatches between exotic plants and native herbivores. Thus, fundamentally similar processes may promote the ecological success of both native and exotic species. C1 [Lind, Eric M.; Parker, John D.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Lind, EM (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM linde@si.edu RI Parker, John/F-9761-2010; OI Parker, John/0000-0002-3632-7625; Lind, Eric/0000-0003-3051-7724 FU Earthwatch Institute/HSBC Climate Partnership; George P. and Caroline V. S. Hachenberg and Charles D. and Mary Vaux Walcott Endowment Funds FX Discussions with colleagues in the Global Invasions Network (NSF RCN DEB-0541673) inspired portions of this work. J.P.'s research on forest invasions is funded by the Earthwatch Institute/HSBC Climate Partnership, and the George P. and Caroline V. S. Hachenberg and Charles D. and Mary Vaux Walcott Endowment Funds to the Smithsonian Institution. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 60 TC 25 Z9 25 U1 3 U2 53 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD MAY 3 PY 2010 VL 5 IS 5 AR e10429 DI 10.1371/journal.pone.0010429 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 590PW UT WOS:000277240300007 PM 20454658 ER PT J AU Davis, JI Soreng, RJ AF Davis, Jerrold I. Soreng, Robert J. TI MIGRATION OF ENDPOINTS OF TWO GENES RELATIVE TO BOUNDARIES BETWEEN REGIONS OF THE PLASTID GENOME IN THE GRASS FAMILY (POACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE gene overlap; inverted-repeat region; ndhF; ndhH; nucleotide substitution rate; PACMAD clade; phylogenetics; plastid genome; Poaceae; small single-copy region ID CHLOROPLAST INVERTED REPEAT; SEQUENCE DATA; PHYLOGENETIC-RELATIONSHIPS; OVERLAPPING GENES; SINGLE-COPY; DATA SETS; DNA; EVOLUTION; INVERSIONS; TRIBE AB Overlapping genes occur widely in microorganisms and in some plastid genomes, but unique properties are observed when such genes span the boundaries between single-copy and repeat regions. The termini of ndhH and ndhF, situated near opposite ends of the small single-copy region (SSC) in the plastid genomes of grasses (Poaceae), have migrated repeatedly into and out of the adjacent inverted-repeat regions (IR). The two genes are transcribed in the same direction, and the 5' terminus of ndhH extends into the IR in some species, while the 3' terminus of ndhF extends into the IR in others. When both genes extend into the IR, portions of the genes overlap and are encoded by the same nucleotide positions. Fine-scale mapping of the SSC-IR junctions across a sample of 92 grasses and outgroups, integrated into a phylogenetic analysis, indicates that the earliest grasses resembled the related taxa Joinvillea (Joinvilleaceae) and Ecdeiocolea (Ecdeiocoleaceae), with ca. 180 nucleotides of ndhH extending into the IR, and with ndhF confined to the SSC. This structure is maintained in early-diverging grass lineages and in most species of the BEP clade. In the PACMAD clade, ndhH lies completely or nearly completely within the SSC, and ca. 20 nucleotides of ndhF extend into the IR. The nucleotide substitution rate has increased in the PACMAD clade in the portion of ndhH that has migrated into the SSC. C1 [Davis, Jerrold I.] Cornell Univ, Dept Plant Biol, Ithaca, NY 14853 USA. [Soreng, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, US Natl Herbarium, Washington, DC 20013 USA. RP Davis, JI (reprint author), Cornell Univ, Dept Plant Biol, 412 Mann Lib, Ithaca, NY 14853 USA. EM jid1@cornell.edu FU U.S. NSF [DEB-0318686] FX The authors thank K. Allred, C. Annable, P. Asimbaya, N. Barker, L. Clark, J. Conran, M. Crisp, J. Dransfield, G. Hui, S. Jacobs, S. Jones, E. Judziewicz, J. LaDuke, H. P. Linder, P. Peterson, E. Royl, P. Rudall, C. Schiers, N. Soreng, D. Stevenson, J. Wipff, W. Zhang, Fairchild Tropical Botanic Garden, Royal Botanic Gardens, Kew, and the USDA Plant Introduction Station for access to plant materials, M. Voionmaa for technical assistance, the U.S. NSF (grant #DEB-0318686) for funding in support of this research and Scot Kelchner and an anonymous referee for valuable comments. NR 83 TC 17 Z9 17 U1 0 U2 3 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 MAY PY 2010 VL 97 IS 5 BP 874 EP 892 DI 10.3732/ajb.0900228 PG 19 WC Plant Sciences SC Plant Sciences GA 589UO UT WOS:000277179900016 PM 21622452 ER PT J AU Kabat, SM Dick, CW Hunter, MD AF Kabat, Susan M. Dick, Christopher W. Hunter, Mark D. TI ISOLATION AND CHARACTERIZATION OF MICROSATELLITE LOCI IN THE COMMON MILKWEED, ASCLEPIAS SYRIACA (APOCYNACEAE) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Apocynaceae; Asclepias syriaca; microsatellite; milkweed ID HERBIVORE; SOUTHWARD AB Premise of the study: Microsatellite primers were developed for the common milkweed, Asclepias syriaca L., to assist in genet identification and the analysis of spatial genetic structure. Methods and Results: Using an enrichment cloning protocol, eight microsatellite loci were isolated and characterized in a Michigan population of A. syriaca. The primers amplified di- and trinucleotide repeats with 4-13 alleles per locus. Conclusions: The primers will be useful for studies of clonality and gene flow in natural populations. C1 [Kabat, Susan M.] Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. [Dick, Christopher W.; Hunter, Mark D.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Univ Michigan, Herbarium, Ann Arbor, MI 48109 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Kabat, SM (reprint author), Univ Michigan, Sch Nat Resources & Environm, Ann Arbor, MI 48109 USA. EM kabats@umich.edu RI Dick, Christopher/A-8744-2008 FU University of Michigan; National Science Foundation [DEB 0640379, DEB 0814340] FX The authors thank the University of Michigan Biological Station for logistical support. SMK thanks H. Draheim, S. Pereira, and R. Vannette for their support in the laboratory. CWD acknowledges financial support from the University of Michigan and the National Science Foundation (DEB 0640379). MDH acknowledges financial support from the National Science Foundation (DEB 0814340). NR 12 TC 8 Z9 8 U1 0 U2 4 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD MAY PY 2010 VL 97 IS 5 BP E37 EP E38 DI 10.3732/ajb.1000064 PG 2 WC Plant Sciences SC Plant Sciences GA 589UO UT WOS:000277179900023 PM 21622436 ER PT J AU Silva, MF Domenech-Carbo, MT Fuster-Lopez, L Mecklenburg, MF Martin-Rey, S AF Silva, Miguel F. Teresa Domenech-Carbo, Maria Fuster-Lopez, Laura Mecklenburg, Marion F. Martin-Rey, Susana TI Identification of additives in poly(vinylacetate) artist's paints using PY-GC-MS SO ANALYTICAL AND BIOANALYTICAL CHEMISTRY LA English DT Article; Proceedings Paper CT 15th European Conference on Analytical Chemistry (Euroanalysis) CY SEP 06-10, 2009 CL Innsbruck, AUSTRIA DE Paints; PVAc; Additives; PEG; Py-GC-MS; HMDS ID CHROMATOGRAPHY-MASS SPECTROMETRY; POLY(ETHYLENE GLYCOL) ADDITIVES; AMINE LIGHT STABILIZERS; BINDING MEDIA; MALDI-MS; ESI-MS; PYROLYSIS; SURFACTANTS; SILYLATION; ARTWORKS AB Commercial poly(vinyl acetate) (PVAc) paint formulations for artists include a number of compounds in addition to the PVAc polymer and pigments to improve the physical and chemical properties of the resulting product. Among the most common additives are surfactants, coalescing agents, defoamers, freeze-thaw agents and thickeners. These products significantly influence the behaviour of the dried film. Nevertheless, they are usually difficult to detect with conventional analytical methods given their low concentration. In order to identify these additives, present in the dried film as minor components, an analytical method based on in situ thermally assisted pyrolysis-silylation gas chromatography-mass spectrometry (GC-MS) using hexamethyldisilazane as a derivatisation reagent is proposed. This method improves the conventional GC-MS analysis performed by direct pyrolysis and enables the simultaneous identification of the PVAc binding medium and the additives included by the manufacturer in the commercial paint. Five different commercial PVAc paints have been analysed, namely, armour green, burnt umber, oriental red, raw umber and white from Flashe (R). Internal plasticiser VeoVa consisting of C-10 fatty acids with highly branched chains has been recognised from the MS spectra. On the other hand, the differences found in the additive content of the studied paints, in particular the poly(ethylene glycol)-type surfactant, are in good agreement with their mechanical properties. C1 [Silva, Miguel F.; Teresa Domenech-Carbo, Maria; Fuster-Lopez, Laura; Martin-Rey, Susana] Univ Politecn Valencia, Inst Restaurac Patrimonio, Valencia 46022, Spain. [Mecklenburg, Marion F.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. RP Domenech-Carbo, MT (reprint author), Univ Politecn Valencia, Inst Restaurac Patrimonio, Camino Vera S-N, Valencia 46022, Spain. EM tdomenec@crbc.upv.es RI FUSTER-LOPEZ, Laura/F-5503-2016 FU Ministerio de Ciencia e Innovacion (MICINN) [CTQ2008-06727-C03-01/BQU, ACOMP/2009/171, AP2006-3223] FX Financial support is gratefully acknowledged from the Spanish "I+D+I MICINN" project CTQ2008-06727-C03-01/BQU supported by ERDEF funds as well as the "Generalitat Valenciana" I+D project ACOMP/2009/171 and the AP2006-3223 project ascribed to the program of predoctoral stages of university professors and researchers in Spanish universities and research centres from the Ministerio de Ciencia e Innovacion (MICINN). Tensile strength testers of the Smithsonian Institution, Museum Conservation Institute are gratefully acknowledged. NR 36 TC 9 Z9 9 U1 2 U2 24 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1618-2642 EI 1618-2650 J9 ANAL BIOANAL CHEM JI Anal. Bioanal. Chem. PD MAY PY 2010 VL 397 IS 1 BP 357 EP 367 DI 10.1007/s00216-010-3505-2 PG 11 WC Biochemical Research Methods; Chemistry, Analytical SC Biochemistry & Molecular Biology; Chemistry GA 584GI UT WOS:000276738800038 PM 20177664 ER PT J AU Alvey, DC Morton, K Harmon, RS Gottfried, JL Remus, JJ Collins, LM Wise, MA AF Alvey, Daniel C. Morton, Kenneth Harmon, Russell S. Gottfried, Jennifer L. Remus, Jeremiah J. Collins, Leslie M. Wise, Michael A. TI Laser-induced breakdown spectroscopy-based geochemical fingerprinting for the rapid analysis and discrimination of minerals: the example of garnet SO APPLIED OPTICS LA English DT Article ID SENSOR TECHNOLOGY; REAL-TIME; GROSSULARITE; COLOR AB Laser-induced breakdown spectroscopy (LIBS) is an analytical technique real-time geochemical analysis that is being developed for portable use outside of the laboratory. In this study, statistical signal processing and classification techniques were applied to single-shot, broadband LIBS spectra, comprising measured plasma light intensities between 200 and 960 nm, for a suite of 157 garnets of different composition from 92 locations worldwide. Partial least squares discriminant analysis was applied to sets of 25 LIBS spectra for each garnet sample and used to classify the garnet samples based on composition and geographic origin. Careful consideration was given to the cross-validation procedure to ensure that the classification algorithm is robust to unseen data. The results indicate that broadband LIBS analysis can be used to discriminate garnets of different composition and has the potential to discern geographic origin. (C) 2010 C1 [Harmon, Russell S.] USA, Res Lab, Army Res Off, Durham, NC 27703 USA. [Alvey, Daniel C.] US Mil Acad, West Point, NY 10996 USA. [Morton, Kenneth; Remus, Jeremiah J.; Collins, Leslie M.] Duke Univ, Dept Elect & Comp Engn, Durham, NC 27708 USA. [Gottfried, Jennifer L.] USA, Res Lab, Aberdeen Proving Ground, MD 21005 USA. [Wise, Michael A.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20013 USA. RP Harmon, RS (reprint author), USA, Res Lab, Army Res Off, Durham, NC 27703 USA. EM russell.harmon@us.army.mil RI Gottfried, Jennifer/G-6333-2010 FU Argonne National Laboratory; ARL FX The analytical work reported here was undertaken by senior author D. Alvey as part of a U.S. Military Academy cadet summer research project with the US Army Research Laboratory (ARL), supported by the Argonne National Laboratory undergraduate student summer program. The signal processing and classification work was conducted in the SPACISS laboratory at Duke University. Additional support was provided by an ARL Fellow stipend to R. Harmon. NR 27 TC 33 Z9 35 U1 2 U2 16 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD MAY 1 PY 2010 VL 49 IS 13 BP C168 EP C180 DI 10.1364/AO.49.00C168 PG 13 WC Optics SC Optics GA 590HZ UT WOS:000277217400042 ER PT J AU Woods, DF Geller, MJ Kurtz, MJ Westra, E Fabricant, DG Dell'Antonio, I AF Woods, Deborah Freedman Geller, Margaret J. Kurtz, Michael J. Westra, Eduard Fabricant, Daniel G. Dell'Antonio, Ian TI TRIGGERED STAR FORMATION IN GALAXY PAIRS AT z=0.08-0.38 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: interactions; galaxies: stellar content ID DIGITAL SKY SURVEY; VLT DEEP SURVEY; ALPHA LUMINOSITY FUNCTION; FIBER-FED SPECTROGRAPH; CNOC2 REDSHIFT SURVEY; CLOSE PAIRS; INTERACTING GALAXIES; FORMING GALAXIES; MERGING GALAXIES; FORMATION RATES AB We measure the strength, frequency, and timescale of tidally triggered star formation at redshift z = 0.08-0.38 in a spectroscopically complete sample of galaxy pairs drawn from the magnitude-limited redshift survey of 9825 Smithsonian Hectospec Lensing Survey galaxies with R <20.3. To examine the evidence for tidal triggering, we identify a volume-limited sample of major (vertical bar Delta MR vertical bar < 1.75, corresponding to mass ratio > 1/5) pair galaxies with M(R) < -20.8 in the redshift range z = 0.08-0.31. The size and completeness of the spectroscopic survey allow us to focus on regions of low local density. The spectrophotometric calibration enables the use of the 4000 angstrom break (D(n)4000), the H alpha specific star formation rate (SSFR(H alpha)), and population models to characterize the galaxies. We show that D(n)4000 is a useful population classification tool; it closely tracks the identification of emission line galaxies. The sample of major pair galaxies in regions of low local density with low D(n)4000 demonstrates the expected anti-correlation between pairwise projected separation and a set of star formation indicators explored in previous studies. We measure the frequency of triggered star formation by comparing the SSFR(H alpha) in the volume-limited sample in regions of low local density: 32% +/- 7% of the major pair galaxies have SSFR(H alpha) at least double the median rate of the unpaired field galaxies. Comparison of stellar population models for pair and for unpaired field galaxies implies a timescale for triggered star formation of similar to 300-400 Myr. C1 [Woods, Deborah Freedman] Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. [Geller, Margaret J.; Kurtz, Michael J.; Westra, Eduard; Fabricant, Daniel G.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Dell'Antonio, Ian] Brown Univ, Dept Phys, Providence, RI 02912 USA. RP Woods, DF (reprint author), Harvard Univ, Dept Astron, Cambridge, MA 02138 USA. EM dwoods@cfa.harvard.edu RI KURTZ, Michael /B-3890-2009; OI Kurtz, Michael/0000-0002-6949-0090 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX This work benefited greatly from discussions with Elizabeth Barton, Nelson Caldwell, Scott Kenyon, and Lisa Kewley. We thank the members of D.F.W.'s PhD thesis committee for their comments that improved this work: Lars Hernquish, Robert Kirshner, and Andrew Szentgyorgyi. We thank the anonymous referee for a helpful and knowledgeable report. We gratefully acknowledge the contribution of the CfA's Telescope Data Center team, especially Doug Mink, Susan Tokarz, and William Wyatt for their work with the Hectospec data reduction pipeline. We thank the Hectospec engineering team, including Robert Fata, Tom Gauron, Edward Hertz, Mark Mueller, and Mark Lacasse, and the instrument specialists Perry Berlind and Michael Calkins, along with the rest of the staff at the MMT Observatory. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web site is http://www.sdss.org/. NR 97 TC 36 Z9 36 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2010 VL 139 IS 5 BP 1857 EP 1870 DI 10.1088/0004-6256/139/5/1857 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581HV UT WOS:000276513700010 ER PT J AU Evans, NR Guinan, E Engle, S Wolk, SJ Schlegel, E Mason, BD Karovska, M Spitzbart, B AF Evans, Nancy Remage Guinan, Edward Engle, Scott Wolk, Scott J. Schlegel, Eric Mason, Brian D. Karovska, Margarita Spitzbart, Bradley TI CHANDRA OBSERVATION OF POLARIS: CENSUS OF LOW-MASS COMPANIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; stars: variables: Cepheids; X-rays: stars ID X-RAY-PROPERTIES; ALPHA-PERSEI; CLASSICAL CEPHEIDS; OPEN CLUSTERS; EMISSION; SUPERGIANTS; PLEIADES; SEARCH; STARS; LINES AB We have observed Cepheid Polaris (alpha UMi A: F7 Ib [Aa] + F6 V [Ab]) with Chandra ACIS-I for 10 ks. An X-ray source was found at the location of Polaris with log L(X) = 28.89 erg s(-1) (0.3-8 keV) and kT = 0.6 keV. A spectrum this soft could come from either the supergiant or the dwarf, as shown by comparable coronal stars. Two resolved low-mass visual companions, "C" and "D," are not physical members of the system based on the lack of X-rays (indicating an age older than the Cepheid) and inconsistent proper motions. Polaris B is not an X-ray source, consistent with its early F spectral type, and probably does not have a lower mass companion itself. A possible more distant member is identified, and an additional less plausible one. This provides a complete census of companions out to 0.1 pc covering a mass ratio range of an order of magnitude and a Delta V of nearly 15 mag. C1 [Evans, Nancy Remage; Wolk, Scott J.; Karovska, Margarita; Spitzbart, Bradley] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Guinan, Edward; Engle, Scott] Villanova Univ, Dept Astron, Villanova, PA 19085 USA. [Engle, Scott] James Cook Univ, Ctr Astron, Townsville, Qld 4811, Australia. [Schlegel, Eric] Univ Texas San Antonio, Dept Phys & Astron, San Antonio, TX 78249 USA. [Mason, Brian D.] USN Observ, Washington, DC 20392 USA. RP Evans, NR (reprint author), Smithsonian Astrophys Observ, MS 4,60 Garden St, Cambridge, MA 02138 USA. EM nevans@cfa.harvard.edu OI Wolk, Scott/0000-0002-0826-9261 FU Chandra grants [GO6-711A]; Chandra X-ray Center NASA [NAS8-03060] FX We thank Fred Seward for valuable conversations and Howard Bond for providing a mosaicked WFPC2 image, as well as an estimate of the detection limit from the image. We also gratefully acknowledge financial support from Chandra grants GO6-711A and Chandra X-ray Center NASA Contract NAS8-03060 (N.R.E. and M.K.). NR 42 TC 8 Z9 8 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 MAY PY 2010 VL 139 IS 5 BP 1968 EP 1974 DI 10.1088/0004-6256/139/5/1968 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581HV UT WOS:000276513700018 ER PT J AU Wang, JH Protopapas, P Chen, WP Alcock, CR Burgett, WS Dombeck, T Grav, T Morgan, JS Price, PA Tonry, JL AF Wang, J. -H. Protopapas, P. Chen, W. -P. Alcock, C. R. Burgett, W. S. Dombeck, T. Grav, T. Morgan, J. S. Price, P. A. Tonry, J. L. TI SEARCHING FOR SUB-KILOMETER TRANS-NEPTUNIAN OBJECTS USING PAN-STARRS VIDEO MODE LIGHT CURVES: PRELIMINARY STUDY AND EVALUATION USING ENGINEERING DATA SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper belt: general; occultations; planets and satellites: solar system formation ID KUIPER-BELT OBJECTS; AMERICAN OCCULTATION SURVEY; STELLAR OCCULTATIONS; SOLAR-SYSTEM; SIZE DISTRIBUTION; BODIES; CATALOG; SCINTILLATION; ENCOUNTERS; ORIGIN AB We present a pre-survey study of using the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) high sampling rate video mode guide star images to search for trans-Neptunian objects (TNOs). Guide stars are primarily used by Pan-STARRS to compensate for image motion and hence improve the point-spread function. With suitable selection of the guide stars within the Pan-STARRS 7 deg(2) field of view, the light curves of these guide stars can also be used to search for occultations by TNOs. The best target stars for this purpose are stars with high signal-to-noise ratio (S/N) and small angular size. In order to do this, we compiled a catalog using the S/N calculated from stars with m(V) < 13 mag in the Tycho2 catalog, then cross matched these stars with the Two Micron All Sky Survey catalog, and estimated their angular sizes from (V - K) color. We also outlined a new detection method based on matched filter that is optimized to search for diffraction patterns in the light curves due to occultation by sub-kilometer TNOs. A detection threshold is set to compromise between real detections and false positives. Depending on the theoretical size distribution model used, we expect to find up to a hundred events during the three-year lifetime of the Pan-STARRS-1 project. The high sampling (30 Hz) of the project facilitates detections of small objects (as small as 400 m), which are numerous according to power-law size distribution, and thus allows us to verify various models and further constrain our understanding of the structure in the outer reach of the solar system. We have tested the detection algorithm and the pipeline on a set of engineering data (taken at 10 Hz instead of 30 Hz). No events were found within the engineering data, which is consistent with the small size of the data set and the theoretical models. Meanwhile, with a total of similar to 22 star-hours video mode data (vertical bar beta vertical bar < 10 degrees), we are able to set an upper limit of N(> 0.5 km) similar to 2.47 x 10(10) deg(-2) at 95% confidence limit. C1 [Wang, J. -H.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Wang, J. -H.; Chen, W. -P.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Protopapas, P.; Alcock, C. R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Protopapas, P.] Sch Engn & Appl Sci, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Burgett, W. S.; Morgan, J. S.; Price, P. A.; Tonry, J. L.] Univ Hawaii, Dept Phys, Honolulu, HI 96822 USA. [Dombeck, T.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Grav, T.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP Wang, JH (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM jhwang@asiaa.sinica.edu.tw; pprotopapas@cfa.harvard.edu FU NSC [96-2112-M-008-024-MY3]; NSF [AST-0501681]; NASA [NNG04G113G]; thematic research program [AS-88-TP-A02] FX Work at NCU was supported by the grant NSC 96-2112-M-008-024-MY3. Work at the CfA was supported in part by the NSF under grant AST-0501681 and by NASA under grant NNG04G113G. Work at ASIAA was supported in part by the thematic research program AS-88-TP-A02. And we also like to thank IIC for hosting J.-H.W. NR 43 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD MAY PY 2010 VL 139 IS 5 BP 2003 EP 2013 DI 10.1088/0004-6256/139/5/2003 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581HV UT WOS:000276513700022 ER PT J AU Kinman, TD Brown, WR AF Kinman, T. D. Brown, Warren R. TI LOW-AMPLITUDE VARIABLES: DISTINGUISHING RR LYRAE STARS FROM ECLIPSING BINARIES SO ASTRONOMICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: structure; stars: horizontal-branch; stars: individual (RR Lyrae) ID SKY VARIABILITY SURVEY; NORTH GALACTIC POLE; A-F STARS; HORIZONTAL-BRANCH; GLOBULAR-CLUSTERS; CONTACT BINARIES; AUTOMATED SURVEY; CATALOG; HALO; SUBSTRUCTURE AB It is not easy to identify and classify low-amplitude variables, but it is important that the classification is done correctly. We use photometry and spectroscopy to classify low-amplitude variables in a 246 deg(2) part of the Akerlof et al. field. Akerlof and Collaborators found that 38% of the RR Lyrae stars in their 2000 deg(2) test field were RR1 (type c). This suggests that these RR Lyrae stars belong to an Oosterhoff Type II population, while their period distribution is primarily Oosterhoff Type I. Our observations support their RR0 (type ab) classifications; however, six of the seven stars that they classified as RR1 (type c) are eclipsing binaries. Our classifications are supported by spectroscopic metallicities, line-broadening, and Galactic rotation measurements. Our 246 deg(2) field contains 16 RR Lyrae stars that are brighter than m(R) = 14.5; only four of these are RR1 (type c). This corresponds to an Oosterhoff Type I population in agreement with the period distribution. C1 [Kinman, T. D.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Kinman, TD (reprint author), Natl Opt Astron Observ, POB 26732, Tucson, AZ 85726 USA. FU NASA; NSF FX We thank the Director of the Lowell Observatory for allowing T. D. K. to use the Lowell 42 inch telescope for this work. We also thank Dr. David Schleicher (Lowell) both for help in using the Kron photometer and in the preliminary reduction of the data. We are also very grateful to Dr. Przemek Wozniak (LANL) for his help with the ROTSE1 catalog. This research has made use of both the SIMBAD database and the VizieR catalog access tool, operated at CDS Strasburg, France. We also used the Two Micron All Sky Survey. which is a joint project of the Univ. Massachusetts and IPAC (Cal. Tech.) and is funded by NASA and NSF. We also are grateful to Dr. Edward Schmidt for observing J123811.0+385028.0 and for allowing us to use his observations. We also thank the referee for comments that have helped us to make significant improvements to the paper. NR 62 TC 8 Z9 8 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 MAY PY 2010 VL 139 IS 5 BP 2014 EP 2025 DI 10.1088/0004-6256/139/5/2014 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581HV UT WOS:000276513700023 ER PT J AU Mondal, S Lin, CC Chen, WP Zhang, ZW Alcock, C Axelrod, T Bianco, FB Byun, YI Coehlo, NK Cook, KH Dave, R Kim, DW King, SK Lee, T Lehner, MJ Lin, HC Marshall, SL Protopapas, P Rice, JA Schwamb, ME Wang, JH Wang, SY Wen, CY AF Mondal, S. Lin, C. C. Chen, W. P. Zhang, Z. -W. Alcock, C. Axelrod, T. Bianco, F. B. Byun, Y. -I. Coehlo, N. K. Cook, K. H. Dave, R. Kim, D. -W. King, S. -K. Lee, T. Lehner, M. J. Lin, H. -C. Marshall, S. L. Protopapas, P. Rice, J. A. Schwamb, M. E. Wang, J. -H. Wang, S. -Y. Wen, C. -Y. TI THE TAIWANESE-AMERICAN OCCULTATION SURVEY PROJECT STELLAR VARIABILITY. II. DETECTION OF 15 VARIABLE STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE methods: data analysis; stars: imaging; stars: variables: Cepheids; stars: variables: delta Scuti; stars: variables: general; stars: variables: RR Lyrae; surveys ID LARGE-MAGELLANIC-CLOUD; KUIPER-BELT OBJECTS; SPACED DATA; CEPHEIDS; TAOS; INVENTORY; OVERTONE; CATALOG; BULGE; BAR AB The Taiwanese-American Occultation Survey (TAOS) project has collected more than a billion photometric measurements since 2005 January. These sky survey data-covering timescales from a fraction of a second to a few hundred days-are a useful source to study stellar variability. A total of 167 star fields, mostly along the ecliptic plane, have been selected for photometric monitoring with the TAOS telescopes. This paper presents our initial analysis of a search for periodic variable stars from the time-series TAOS data on one particular TAOS field, No. 151 (R. A. = 17(h)30(m)6(s).7, decl. = 27 degrees 17'30 '', J2000), which had been observed over 47 epochs in 2005. A total of 81 candidate variables are identified in the 3 deg(2) field, with magnitudes in the range 8 < R < 16. On the basis of the periodicity and shape of the light curves, 29 variables, 15 of which were previously unknown, are classified as RR Lyrae, Cepheid, delta Scuti, SX Phonencis, semi-regular, and eclipsing binaries. C1 [Mondal, S.; Lin, C. C.; Chen, W. P.; Zhang, Z. -W.; Lin, H. -C.; Wang, J. -H.] Natl Cent Univ, Inst Astron, Jhongli 32054, Taiwan. [Mondal, S.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, India. [Alcock, C.; Bianco, F. B.; Lehner, M. J.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bianco, F. B.; Lehner, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bianco, F. B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bianco, F. B.] Global Telescope Network Inc, Las Cumbres Observ, Santa Barbara, CA 93117 USA. [Byun, Y. -I.; Kim, D. -W.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Cook, K. H.; Marshall, S. L.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Dave, R.; Protopapas, P.] Harvard, Initiat Innovat Comp, Cambridge, MA 02138 USA. [King, S. -K.; Lee, T.; Lehner, M. J.; Wang, J. -H.; Wang, S. -Y.; Wen, C. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Mondal, S (reprint author), Natl Cent Univ, Inst Astron, 300 Jhongda Rd, Jhongli 32054, Taiwan. EM soumen@aries.res.in RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985; Schwamb, Megan/0000-0003-4365-1455 FU NSC [96-2112-M-008-024-MY3]; National Research Foundation of Korea [2009-0075376]; thematic research program [AS-88-TP-A02]; National Science Foundation [AST-0501681]; NASA [NNG04G113G]; U.S. Department of Energy by Lawrence Livermore National Laboratory [W-7405-Eng-48, DE-AC52-07NA27344]; Stanford Linear Accelerator Center [DE-AC02-76SF00515] FX The work at National Central University was supported by the grant NSC 96-2112-M-008-024-MY3. Y.I.B. acknowledges the support of the National Research Foundation of Korea through grant 2009-0075376. Work at Academia Sinica was supported in part by the thematic research program AS-88-TP-A02. Work at the Harvard College Observatory was supported in part by the National Science Foundation under grant AST-0501681 and by NASA under grant NNG04G113G. S.L.M.'s work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and by Stanford Linear Accelerator Center under Contract DE-AC02-76SF00515. K.H.C.'s work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory in part under Contract W-7405-Eng-48 and in part under Contract DE-AC52-07NA27344. NR 33 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD MAY PY 2010 VL 139 IS 5 BP 2026 EP 2033 DI 10.1088/0004-6256/139/5/2026 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581HV UT WOS:000276513700024 ER PT J AU Caballero-Garcia, MD Torres, G Ribas, I Risquez, D Montesinos, B Mas-Hesse, JM Domingo, A AF Caballero-Garcia, M. D. Torres, G. Ribas, I. Risquez, D. Montesinos, B. Mas-Hesse, J. M. Domingo, A. TI TYC 2675-663-1: a newly discovered W UMa system in an active state SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE binaries: close; stars: fundamental parameters; X-rays: stars ID MAIN-SEQUENCE STARS; LIGHT CURVES; BINARIES; CATALOG; OMC; EXTINCTION; ACCRETION; CAMERA AB Aims. The recently discovered eclipsing binary system TYC 2675-663-1 is an X-ray source and shows properties in the optical that are similar to the W UMa systems, but are somewhat unusual compared to what is seen in other contact binary systems. The goal of this work is to characterize its properties and investigate its nature by means of detailed photometric and spectroscopic observations. Methods. We have performed extensive V-band photometric measurements with the INTEGRAL satellite along with ground-based multi-band photometric observations, as well as high-resolution spectroscopic monitoring, from which we have measured the radial velocities of the components. These data have been analyzed to determine the stellar properties, including the absolute masses and radii. Additional low-resolution spectroscopy was obtained to investigate spectral features. Results. From the measured eclipse timings we determine an orbital period for the binary of P = 0.4223576 +/- 0.0000009 days. The light-curve and spectroscopic analyses reveal the observations to be well represented by a model of an overcontact system composed of main-sequence F5 and G7 stars (temperature difference of nearly 1000 K), with the possible presence of a third star. Low-resolution optical spectroscopy reveals a complex Ha emission and other features that are not yet understood. The unusually high mass ratio of q = 0.81 +/- 0.05 places it in the rare "H" (high mass ratio) subclass of the W UMa systems, which are presumably on their way to coalescence. C1 [Caballero-Garcia, M. D.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ribas, I.] IEEC, Barcelona 08034, Spain. [Risquez, D.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [Montesinos, B.; Mas-Hesse, J. M.; Domingo, A.] CAB LAEX CSIC INTA, Madrid 28691, Spain. RP Caballero-Garcia, MD (reprint author), Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England. EM mcaballe@ast.cam.ac.uk RI Mas-Hesse, J. Miguel /K-6805-2014; Domingo, Albert/L-9071-2014; Ribas, Ignasi/M-2134-2014; Montesinos, Benjamin/C-3493-2017; Caballero-Garcia, Maria/D-5659-2017 OI Mas-Hesse, J. Miguel /0000-0002-8823-9723; Domingo, Albert/0000-0001-9764-6411; Ribas, Ignasi/0000-0002-6689-0312; Montesinos, Benjamin/0000-0002-7982-2095; Caballero-Garcia, Maria/0000-0001-7920-4564 FU Spanish MCyT [ESP95-0389-C02-02, ESP2002-04124-C03-01, ESP2005-07714-C03-03, AYA2008-03467/ESP, PNE2003-04352]; ESA member states FX We are grateful to the referee, A. Prsa, for very helpful comments. M. C. G. thanks K. Yakut for very useful discussions and F. Vilardell for providing the table of the critical potentials. OMC has been funded by the Spanish MCyT under grants ESP95-0389-C02-02, ESP2002-04124-C03-01, ESP2005-07714-C03-03 and AYA2008-03467/ESP. We thank David Galadi and Teresa Eibe for the data taken at the CAB Giordano Bruno telescope. This research was partially supported by the MCyT under grant PNE2003-04352. This work is based on observations made with INTEGRAL, an ESA science mission with instruments and science data center funded by ESA member states and with the participation of Russia and the USA. We are grateful to the Calar Alto Observatory for allocation of Director's discretionary time to this program. NR 33 TC 1 Z9 1 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 MAY PY 2010 VL 514 AR A36 DI 10.1051/0004-6361/200913602 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 592VL UT WOS:000277409200036 ER PT J AU Mainieri, V Vignali, C Merloni, A Civano, F Puccetti, S Brusa, M Gilli, R Bolzonella, M Comastri, A Zamorani, G Aller, M Carollo, M Scarlata, C Elvis, M Aldcroft, TL Cappelluti, N Fabbiano, G Finoguenov, A Fiore, F Fruscione, A Koekemoer, AM Contini, T Kneib, JP Le Fevre, O Lilly, S Renzini, A Scodeggio, M Bardelli, S Bongiorno, A Caputi, K Coppa, G Cucciati, O de la Torre, S de Ravel, L Franzetti, P Garilli, B Iovino, A Kampczyk, P Knobel, C Kovac, K Lamareille, F Le Borgne, JF Le Brun, V Maier, C Mignoli, M Pello, R Peng, Y Montero, EP Ricciardelli, E Silverman, JD Tanaka, M Tasca, L Tresse, L Vergani, D Zucca, E Capak, P Ilbert, O Impey, C Salvato, M Scoville, N Taniguchi, Y Trump, J AF Mainieri, V. Vignali, C. Merloni, A. Civano, F. Puccetti, S. Brusa, M. Gilli, R. Bolzonella, M. Comastri, A. Zamorani, G. Aller, M. Carollo, M. Scarlata, C. Elvis, M. Aldcroft, T. L. Cappelluti, N. Fabbiano, G. Finoguenov, A. Fiore, F. Fruscione, A. Koekemoer, A. M. Contini, T. Kneib, J. -P. Le Fevre, O. Lilly, S. Renzini, A. Scodeggio, M. Bardelli, S. Bongiorno, A. Caputi, K. Coppa, G. Cucciati, O. de la Torre, S. de Ravel, L. Franzetti, P. Garilli, B. Iovino, A. Kampczyk, P. Knobel, C. Kovac, K. Lamareille, F. Le Borgne, J. -F. Le Brun, V. Maier, C. Mignoli, M. Pello, R. Peng, Y. Montero, E. Perez Ricciardelli, E. Silverman, J. D. Tanaka, M. Tasca, L. Tresse, L. Vergani, D. Zucca, E. Capak, P. Ilbert, O. Impey, C. Salvato, M. Scoville, N. Taniguchi, Y. Trump, J. TI Ultraluminous X-ray sources out to z similar to 0.3 in the COSMOS field SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: galaxies; X-rays: binaries; X-rays: general; surveys ID MASS BLACK-HOLES; EARLY-TYPE GALAXIES; STAR-FORMATION; CHANDRA OBSERVATIONS; LUMINOSITY FUNCTION; BINARIES; CATALOG; CLASSIFICATION; POPULATION; REDSHIFT AB Context. Using Chandra observations we identified a sample of seven off-nuclear X-ray sources in the redshift range z = 0.072-0.283, located within optically bright galaxies in the COSMOS Survey. All of them, if associated with their closest bright galaxy, would have L[0.5-7 keV] > 10(39) erg s(-1) and therefore can be classified as ultraluminous X-ray sources (ULXs). Aims. Using the multi-wavelength coverage available in the COSMOS field, we studied the properties of the host galaxies of these ULXs. In detail, we derived their star formation rate from Ha measurements and their stellar masses using SED fitting techniques with the aim to compute the probability to have an off-nuclear source based on the host galaxy properties. We divided the host galaxies in different morphological classes with the available ACS/HST imaging. Methods. We selected off-nuclear candidates with the following criteria: 1) the distance between the X-ray and the optical centroid has to be larger than 0.9 '', larger than 1.8 times the radius of the Chandra positional error circle and smaller than the Petrosian radius of the host galaxy; 2) the optical counterpart is a bright galaxy (R(AB) < 22); 3) the redshift of the counterpart is lower than z = 0.3; 4) the source has been observed in at least one Chandra pointing at an off-axis angle smaller than 5'; 5) the X-ray positional error is smaller than 0.8 ''. We verified each candidate super-imposing the X-ray contours on the optical/IR images. We expect less than one misidentified AGN due to astrometric errors and on average 1.3 serendipitous background source matches. Results. We find that our ULXs candidates are located in regions of the SFR versusM(*) plane where one or more off-nuclear detectable sources are expected. From a morphological analysis of the ACS imaging and the use of rest-frame colours, we find that our ULXs are hosted both in late and early type galaxies. Finally, we find that the fraction of galaxies hosting a ULX ranges from approximate to 0.5% to approximate to 0.2% going from L(0.5-2) (keV) = 3 x 10(39) erg s(-1) to L(0.5-2 keV) = 2 x 10(40) erg s(-1). C1 [Mainieri, V.; Tanaka, M.] ESO, D-85748 Garching, Germany. [Vignali, C.] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. [Vignali, C.; Gilli, R.; Bolzonella, M.; Comastri, A.; Zamorani, G.; Bardelli, S.; Coppa, G.; Mignoli, M.; Vergani, D.; Zucca, E.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Merloni, A.] TUM, D-85748 Garching, Germany. [Merloni, A.; Brusa, M.; Cappelluti, N.; Finoguenov, A.; Bongiorno, A.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Civano, F.; Elvis, M.; Aldcroft, T. L.; Fabbiano, G.; Fruscione, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Fiore, F.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Aller, M.; Carollo, M.; Scarlata, C.; Lilly, S.; Caputi, K.; Kampczyk, P.; Knobel, C.; Kovac, K.; Maier, C.; Peng, Y.; Silverman, J. D.] ETH Honggerberg, Swiss Fed Inst Technol, Inst Astron, CH-8093 Zurich, Switzerland. [Scarlata, C.] Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Koekemoer, A. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Contini, T.; Lamareille, F.; Le Borgne, J. -F.; Pello, R.; Montero, E. Perez] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Kneib, J. -P.; Le Fevre, O.; de la Torre, S.; de Ravel, L.; Le Brun, V.; Tasca, L.; Tresse, L.; Ilbert, O.] Lab Astrophys Marseille, Marseille, France. [Renzini, A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Scodeggio, M.; Franzetti, P.; Garilli, B.] INAF IASF Milano, Milan, Italy. [Cucciati, O.; Iovino, A.] INAF Osservatorio Astron Brera, Milan, Italy. [Ricciardelli, E.] Univ Padua, Dipartimento Astron, I-35122 Padua, Italy. [Impey, C.; Trump, J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Capak, P.; Salvato, M.; Scoville, N.] CALTECH, Pasadena, CA 91125 USA. [Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. RP Mainieri, V (reprint author), ESO, Karl Schwarzschild Str 2, D-85748 Garching, Germany. EM vmainier@eso.org RI Pello, Roser/G-4754-2010; Comastri, Andrea/O-9543-2015; Le Fevre, Olivier/G-7389-2011; Vignali, Cristian/J-4974-2012; Kneib, Jean-Paul/A-7919-2015; Mignoli, Marco/O-9426-2015; Gilli, Roberto/P-1110-2015; Zucca, Elena/O-9396-2015; Bardelli, Sandro/O-9369-2015; Bolzonella, Micol/O-9495-2015; OI Fiore, Fabrizio/0000-0002-4031-4157; Comastri, Andrea/0000-0003-3451-9970; Vignali, Cristian/0000-0002-8853-9611; Kneib, Jean-Paul/0000-0002-4616-4989; Mignoli, Marco/0000-0002-9087-2835; Gilli, Roberto/0000-0001-8121-6177; Scodeggio, Marco/0000-0002-2282-5850; Bongiorno, Angela/0000-0002-0101-6624; Zucca, Elena/0000-0002-5845-8132; Bardelli, Sandro/0000-0002-8900-0298; Bolzonella, Micol/0000-0003-3278-4607; Iovino, Angela/0000-0001-6958-0304; Franzetti, Paolo/0000-0002-6986-0127; Vergani, Daniela/0000-0003-0898-2216; Cappelluti, Nico/0000-0002-1697-186X; Garilli, Bianca/0000-0001-7455-8750; Koekemoer, Anton/0000-0002-6610-2048; Puccetti, Simonetta/0000-0002-2734-7835 FU [ASI/COFIS/WP3110 I/026/07/0]; [ASI/INAF I/023/05/0]; [ASI I/088/06/0]; [PRIN/MIUR 2006-02-5203] FX This work is based on observations made with ESO Telescopes at the La Silla or Paranal Observatories under programme ID 175. A-0839. We are grateful to the referee for detailed and extremely useful comments that improved the quality of the paper. We thank Piero Rosati and Bret Lehmer for useful scientific discussions. We are grateful to Bret Lehmer for providing the data points of the CDFs used in Fig. 9. This work has been supported in part by the grants: ASI/COFIS/WP3110 I/026/07/0, ASI/INAF I/023/05/0, ASI I/088/06/0, PRIN/MIUR 2006-02-5203. NR 40 TC 7 Z9 7 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 MAY PY 2010 VL 514 AR A85 DI 10.1051/0004-6361/200912544 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 633LQ UT WOS:000280504800052 ER PT J AU Acciari, VA Aliu, E Arlen, T Aune, T Bautista, M Beilicke, M Benbow, W Boltuch, D Bradbury, SM Buckley, JH Bugaev, V Butt, Y Byrum, K Cannon, A Cesarini, A Chow, YC Ciupik, L Cogan, P Cui, W Dickherber, R Duke, C Ergin, T Fegan, SJ Finley, JP Finnegan, G Fortin, P Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Grube, J Guenette, R Gyuk, G Hanna, D Holder, J Huang, D Hui, CM Humensky, TB Kaaret, P Karlsson, N Kertzman, M Kieda, D Konopelko, A Krawczynski, H Krennrich, F Lang, MJ LeBohec, S Maier, G McArthur, S McCann, A McCutcheon, M Millis, J Moriarty, P Ong, RA Pandel, D Perkins, JS Pohl, M Quinn, J Ragan, K Reynolds, PT Roache, E Rose, HJ Schroedter, M Sembroski, GH Smith, AW Smith, BR Steele, D Swordy, SP Theiling, M Thibadeau, S Varlotta, A Vassiliev, VV Vincent, S Wagner, RG Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Wissel, S Wood, M AF Acciari, V. A. Aliu, E. Arlen, T. Aune, T. Bautista, M. Beilicke, M. Benbow, W. Boltuch, D. Bradbury, S. M. Buckley, J. H. Bugaev, V. Butt, Y. Byrum, K. Cannon, A. Cesarini, A. Chow, Y. C. Ciupik, L. Cogan, P. Cui, W. Dickherber, R. Duke, C. Ergin, T. Fegan, S. J. Finley, J. P. Finnegan, G. Fortin, P. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Grube, J. Guenette, R. Gyuk, G. Hanna, D. Holder, J. Huang, D. Hui, C. M. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Kieda, D. Konopelko, A. Krawczynski, H. Krennrich, F. Lang, M. J. LeBohec, S. Maier, G. McArthur, S. McCann, A. McCutcheon, M. Millis, J. Moriarty, P. Ong, R. A. Pandel, D. Perkins, J. S. Pohl, M. Quinn, J. Ragan, K. Reynolds, P. T. Roache, E. Rose, H. J. Schroedter, M. Sembroski, G. H. Smith, A. W. Smith, B. R. Steele, D. Swordy, S. P. Theiling, M. Thibadeau, S. Varlotta, A. Vassiliev, V. V. Vincent, S. Wagner, R. G. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Wissel, S. Wood, M. TI OBSERVATIONS OF THE SHELL-TYPE SUPERNOVA REMNANT CASSIOPEIA A AT TeV ENERGIES WITH VERITAS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma rays: ISM; ISM: individual objects (Cassiopeia A); ISM: supernova remnants ID AIR CERENKOV TELESCOPES; GAMMA-RAY EMISSION; CRAB-NEBULA; A SUPERNOVA; MAGNETIC-FIELDS; PARTICLE-ACCELERATION; ELECTRON ACCELERATION; RX J1713.7-3946; MAGIC TELESCOPE; COSMIC-RAYS AB We report on observations of very high energy gamma rays from the shell-type supernova remnant (SNR) Cassiopeia A with the Very Energetic Radiation Imaging Telescope Array System stereoscopic array of four imaging atmospheric Cherenkov telescopes in Arizona. The total exposure time for these observations is 22 hr, accumulated between September and November of 2007. The gamma-ray source associated with the SNR Cassiopeia A was detected above 200 GeV with a statistical significance of 8.3 sigma. The estimated integral flux for this gamma-ray source is about 3% of the Crab-Nebula flux. The photon spectrum is compatible with a power law dN/dE proportional to E(-Gamma) with an index Gamma = 2.61 +/- 0.24(stat) +/- 0.2(sys). The data are consistent with a point-like source. We provide a detailed description of the analysis results and discuss physical mechanisms that may be responsible for the observed gamma-ray emission. C1 [Huang, D.; Konopelko, A.; Smith, B. R.] Pittsburg State Univ, Dept Phys, Pittsburg, KS 66762 USA. [Acciari, V. A.; Benbow, W.; Galante, N.; Perkins, J. S.; Roache, E.; Theiling, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Aliu, E.; Boltuch, D.; Holder, J.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Arlen, T.; Chow, Y. C.; Fegan, S. J.; Ong, R. A.; Vassiliev, V. V.; Weinstein, A.; Wood, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Aune, T.; Furniss, A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Aune, T.; Furniss, A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bautista, M.; Cogan, P.; Guenette, R.; Hanna, D.; Maier, G.; McCann, A.; McCutcheon, M.; Ragan, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; McArthur, S.; Thibadeau, S.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Butt, Y.; Ergin, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Byrum, K.; Smith, A. W.; Wagner, R. G.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cannon, A.; Grube, J.; Quinn, J.; Ward, J. E.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Cesarini, A.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland, Sch Phys, Galway, Ireland. [Ciupik, L.; Fortson, L.; Gyuk, G.; Karlsson, N.; Steele, D.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Finley, J. P.; Gall, D.; Millis, J.; Sembroski, G. H.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Finnegan, G.; Hui, C. M.; Kieda, D.; LeBohec, S.; Vincent, S.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Fortin, P.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Humensky, T. B.; Swordy, S. P.; Wakely, S. P.; Weisgarber, T.; Wissel, S.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Kaaret, P.; Pandel, D.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Kertzman, M.] DePauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Pohl, M.; Schroedter, M.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Konopelko, A (reprint author), Pittsburg State Univ, Dept Phys, 1701 South Broadway, Pittsburg, KS 66762 USA. EM akonopel@pittstate.edu OI Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201 FU U.S. Department of Energy; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland; STFC in the UK; NASA [NNX08AV62G] FX This research was supported by grants from the U.S. Department of Energy, the U.S. National Science Foundation, and the Smithsonian Institution, by NSERC in Canada, by Science Foundation Ireland, and by STFC in the UK. The VERITAS collaboration acknowledges the NASA support on the Fermi GST LAT grant No. NNX08AV62G. NR 61 TC 48 Z9 49 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2010 VL 714 IS 1 BP 163 EP 169 DI 10.1088/0004-637X/714/1/163 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583SV UT WOS:000276701000014 ER PT J AU Lawrence, A Elvis, M AF Lawrence, Andy Elvis, Martin TI MISALIGNED DISKS AS OBSCURERS IN ACTIVE GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars: general ID NARROW-LINE REGION; ABSORBING COLUMN DENSITIES; RAY SPECTRAL PROPERTIES; SEYFERT 2 GALAXIES; SWIFT BAT SURVEY; GALACTIC NUCLEI; RADIO GALAXIES; UNIFIED SCHEMES; MOLECULAR GAS; BLACK-HOLE AB We critically review the evidence concerning the fraction of active galactic nuclei (AGNs) that appear as Type 2 AGNs, carefully distinguishing strict Type 2 AGNs from both more lightly reddened Type 1 AGNs, and from low excitation narrow line AGNs, which may represent a different mode of activity. Low-excitation AGNs occur predominantly at low luminosities; after removing these, true Type 2 AGNs represent 58% +/- 5% of all AGNs, and lightly reddened Type 1 AGNs a further similar to 15%. Radio, IR, and volume-limited samples all agree in showing no change of Type 2 fraction with luminosity. X-ray samples do show a change with luminosity; we discuss possible reasons for this discrepancy. We test a very simple picture which produces this Type 2 fraction with minimal assumptions. In this picture, infall from large scales occurs in random directions, but must eventually align with the inner accretion flow, producing a severely warped disk on parsec scales. If the re-alignment is dominated by tilt, with minimal twist, a wide range of covering factors is predicted in individual objects, but with an expected mean fraction of Type 2 AGNs of exactly 50%. This "tilted disk" picture predicts reasonable alignment of observed nuclear structures on average, but with distinct misalignments in individual cases. Initial case studies of the few well-resolved objects show that such misalignments are indeed present. C1 [Lawrence, Andy] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Elvis, Martin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lawrence, A (reprint author), Stanford Univ, KIPAC, Stanford, CA 94309 USA. NR 113 TC 82 Z9 82 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2010 VL 714 IS 1 BP 561 EP 570 DI 10.1088/0004-637X/714/1/561 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583SV UT WOS:000276701000044 ER PT J AU Warren, BE Wilson, CD Israel, FP Serjeant, S Bendo, GJ Brinks, E Clements, DL Irwin, JA Knapen, JH Leech, J Matthews, HE Muhle, S Mortimer, AMJ Petitpas, G Sinukoff, E Spekkens, K Tan, BK Tilanus, RPJ Usero, A van der Werf, PP Vlahakis, C Wiegert, T Zhu, M AF Warren, B. E. Wilson, C. D. Israel, F. P. Serjeant, S. Bendo, G. J. Brinks, E. Clements, D. L. Irwin, J. A. Knapen, J. H. Leech, J. Matthews, H. E. Muhle, S. Mortimer, A. M. J. Petitpas, G. Sinukoff, E. Spekkens, K. Tan, B. K. Tilanus, R. P. J. Usero, A. van der Werf, P. P. Vlahakis, C. Wiegert, T. Zhu, M. TI THE JAMES CLERK MAXWELL TELESCOPE NEARBY GALAXIES LEGACY SURVEY. II. WARM MOLECULAR GAS AND STAR FORMATION IN THREE FIELD SPIRAL GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 628, NGC 3521, NGC 3627); galaxies: ISM; galaxies: kinematics and dynamics; galaxies: spiral; galaxies: star formation; ISM: molecules ID CO OBSERVATIONS; BIMA SURVEY; H-ALPHA; KINEMATICS; ROTATION; NGC-3627; SCHMIDT; CLUSTER; CLOUDS; THINGS AB We present the results of large-area (12)CO J = 3-2 emission mapping of three nearby field galaxies, NGC 628, NGC 3521, and NGC 3627, completed at the James Clerk Maxwell Telescope as part of the Nearby Galaxies Legacy Survey. These galaxies all have moderate to strong (12)CO J = 3-2 detections over large areas of the fields observed by the survey, showing resolved structure and dynamics in their warm/dense molecular gas disks. All three galaxies were part of the Spitzer Infrared Nearby Galaxies Survey sample, and as such have excellent published multiwavelength ancillary data. These data sets allow us to examine the star formation properties, gas content, and dynamics of these galaxies on sub-kiloparsec scales. We find that the global gas depletion time for dense/warm molecular gas in these galaxies is consistent with other results for nearby spiral galaxies, indicating this may be independent of galaxy properties such as structures, gas compositions, and environments. Similar to the results from The Hi Nearby Galaxy Survey, we do not see a correlation of the star formation efficiency with the gas surface density consistent with the Schmidt-Kennicutt law. Finally, we find that the star formation efficiency of the dense molecular gas traced by (12)CO J = 3-2 is potentially flat or slightly declining as a function of molecular gas density, the (12)CO J = 3-2/J = 1-0 ratio (in contrast to the correlation found in a previous study into the starburst galaxy M83), and the fraction of total gas in molecular form. C1 [Warren, B. E.; Wilson, C. D.; Sinukoff, E.] McMaster Univ, Dept Phys & Astron, Hamilton, ON L8S 4M1, Canada. [Israel, F. P.; van der Werf, P. P.; Vlahakis, C.] Leiden Univ, Sterrewacht Leiden, NL-2300 RA Leiden, Netherlands. [Serjeant, S.] Open Univ, Dept Phys & Astron, Milton Keynes MK7 6AA, Bucks, England. [Bendo, G. J.; Clements, D. L.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Brinks, E.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Irwin, J. A.] Queens Univ, Dept Phys Engn Phys & Astron, Kingston, ON, Canada. [Knapen, J. H.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Leech, J.; Tan, B. K.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Matthews, H. E.] DRAO, Herzberg Inst Astrophys, Natl Res Council Canada, Penticton, BC V2A 6J9, Canada. [Muhle, S.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Mortimer, A. M. J.] Scottish Univ Phys Alliance, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spekkens, K.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 4B4, Canada. [Tilanus, R. P. J.] Joint Astron Ctr, Hilo, HI 96720 USA. [Tilanus, R. P. J.] Netherlands Org Sci Res, The Hague, Netherlands. [Usero, A.] Observ Astron Nacl, Madrid 28014, Spain. [Wiegert, T.] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada. [Zhu, M.] Chinese Acad Sci, Natl Astron Observ, Beijing, Peoples R China. RP Warren, BE (reprint author), Univ Western Australia, Int Ctr Radio Astron Res, M468,35 Stirling Highway, Crawley, WA 6009, Australia. EM sinukoej@muss.cis.mcmaster.ca; wilson@physics.mcmaster.ca; israel@strw.leidenuniv.nl; g.bendo@imperial.ac.uk; E.Brinks@herts.ac.uk; d.clements@imperial.ac.uk; irwin@astro.queensu.ca; jhk@iac.es; jxl@astro.ox.ac.uk; henry.matthews@nrc-cnrc.gc.ca; muehle@jive.nl; ajm@roe.ac.uk; gpetitpa@cfa.harvard.edu; sinukoej@muss.cis.mcmaster.ca; Kristine.Spekkens@rmc.ca; tanbk@astro.ox.ac.uk; r.tilanus@jach.hawaii.edu; a.usero@oan.es; pvdwerf@strw.leidenuniv.nl; vlahakis@strw.leidenuniv.nl; wiegert@physics.umanitoba.ca; mz@bao.ac.cn OI Brinks, Elias/0000-0002-7758-9699 FU NSERC (Canada) FX We thank the anonymous referee for helping to clarify several issues in this paper. We thank Fabian Walter for making the THINGS Hi data cube for NGC 3521 available to our survey after we initially experienced trouble obtaining it from the Web site. The JCMT 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 J.I., K. S., and C.D.W. is supported by grants from NSERC (Canada). Travel funding for observatory trips by B.E.W. and T.W. was supplied by the National Research Council (Canada). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyon1.fr). This work made use of THINGS, "The Hi Nearby Galaxy Survey" (Walter et al. 2008). NR 39 TC 30 Z9 31 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2010 VL 714 IS 1 BP 571 EP 588 DI 10.1088/0004-637X/714/1/571 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583SV UT WOS:000276701000045 ER PT J AU Seth, AC Cappellari, M Neumayer, N Caldwell, N Bastian, N Olsen, K Blum, RD Debattista, VP McDermid, R Puzia, T Stephens, A AF Seth, Anil C. Cappellari, Michele Neumayer, Nadine Caldwell, Nelson Bastian, Nate Olsen, Knut Blum, Robert D. Debattista, Victor P. McDermid, Richard Puzia, Thomas Stephens, Andrew TI THE NGC 404 NUCLEUS: STAR CLUSTER AND POSSIBLE INTERMEDIATE-MASS BLACK HOLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: elliptical and lenticular, cD; galaxies: formation; galaxies: individual (NGC 404); galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: structure ID HUBBLE-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; EARLY-TYPE GALAXIES; MULTI-GAUSSIAN EXPANSION; DWARF SPHEROIDAL GALAXY; GIANT BRANCH STARS; TP-AGB MODELS; SPIRAL GALAXIES; SEYFERT-GALAXIES; STELLAR POPULATIONS AB We examine the nuclear morphology, kinematics, and stellar populations in nearby S0 galaxy NGC 404 using a combination of adaptive optics assisted near-IR integral-field spectroscopy, optical spectroscopy, and Hubble Space Telescope imaging. These observations enable study of the NGC 404 nucleus at a level of detail possible only in the nearest galaxies. The surface brightness profile suggests the presence of three components: a bulge, a nuclear star cluster (NSC), and a central light excess within the cluster at radii < 3 pc. These components have distinct kinematics with modest rotation seen in the NSC and counter-rotation seen in the central excess. Molecular hydrogen emission traces a disk with rotation nearly orthogonal to that of the stars. The stellar populations of the three components are also distinct, with half of the mass of the NSC having ages of similar to 1 Gyr (perhaps resulting from a galaxy merger), while the bulge is dominated by much older stars. Dynamical modeling of the stellar kinematics gives a total NSC mass of 1.1 x 10(7) M(circle dot). Dynamical detection of a possible intermediate-mass black hole (BH) is hindered by uncertainties in the central stellar mass profile. Assuming a constant mass-to-light ratio, the stellar dynamical modeling suggests a BH mass of < 1 x 10(5) M(circle dot), while the molecular hydrogen gas kinematics are best fitted by a BH with a mass of 4.5(-2.0)(+3.5) x 10(5) M(circle dot). Unresolved and possibly variable dust emission in the near-infrared and active galactic nucleus-like molecular hydrogen emission-line ratios do suggest the presence of an accreting BH in this nearby LINER galaxy. C1 [Seth, Anil C.; Caldwell, Nelson] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cappellari, Michele] Univ Oxford, Sub Dept Astrophys, Oxford OX1 3RH, England. [Neumayer, Nadine] European So Observ, D-85748 Garching, Germany. [Bastian, Nate] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Olsen, Knut; Blum, Robert D.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Debattista, Victor P.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [McDermid, Richard; Stephens, Andrew] Gemini Observ, Hilo, HI 96720 USA. [Puzia, Thomas] Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Seth, AC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM aseth@cfa.harvard.edu OI Neumayer, Nadine/0000-0002-6922-2598; Cappellari, Michele/0000-0002-1283-8420 FU STFC; Cluster of Excellence; Association of Universities for Research in Astronomy, Inc.; [GN-2008B-Q-74] FX We thank the referee, Jenny Greene, for helpful comments, Stephane Charlot for sharing his models, Christy Tremonti for sharing her code, the staff at Gemini and MMT, NED, and ADS. A. S. acknowledges support from the Harvard-Smithsonian CfA as a CfA and OIR fellow, and helpful conversations with Margaret Geller, Pat Cote, and Davor Krajnovic. M.C. and N.B. acknowledge support from STFC Advanced Fellowships. N.N. acknowledges support from the Cluster of Excellence "Origin and Evolution of the Universe." Partially based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc.. Gemini data was taken as part of program GN-2008B-Q-74. NR 130 TC 69 Z9 69 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2010 VL 714 IS 1 BP 713 EP 731 DI 10.1088/0004-637X/714/1/713 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583SV UT WOS:000276701000057 ER PT J AU Gitti, M O'Sullivan, E Giacintucci, S David, LP Vrtilek, J Raychaudhury, S Nulsen, PEJ AF Gitti, Myriam O'Sullivan, Ewan Giacintucci, Simona David, Laurence P. Vrtilek, Jan Raychaudhury, Somak Nulsen, Paul E. J. TI CAVITIES AND SHOCKS IN THE GALAXY GROUP HCG 62 AS REVEALED BY CHANDRA, XMM-NEWTON, AND GIANT METREWAVE RADIO TELESCOPE DATA SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: clusters: general; galaxies: clusters: individual (HCG 62); intergalactic medium; X-rays: galaxies: clusters ID X-RAY CAVITIES; AGN FEEDBACK; HOT GAS; STATISTICAL-ANALYSIS; COOLING CLUSTERS; COMPACT GROUP; DARK-MATTER; CORE; BUBBLES; TEMPERATURE AB We report on the results of an analysis of Chandra, XMM-Newton, and new Giant Metrewave Radio Telescope (GMRT) data of the X-ray bright compact group of galaxies HCG 62, which is one of the few groups known to possess clear, small X-ray cavities in the inner regions. This is part of an ongoing X-ray/low-frequency radio study of 18 groups, initially chosen for the availability of good-quality X-ray data and evidence for active galactic nucleus/hot gas interaction. At higher frequency (1.4 GHz), the HCG 62 cavity system shows minimal if any radio emission, but the new GMRT observations at 235 MHz and 610 MHz clearly detect extended low-frequency emission from radio lobes corresponding to the cavities. By means of the synergy of X-ray and low-frequency radio observations, we compare and discuss the morphology, luminosity, and pressure of the gas and of the radio source. We find that the radio source is radiatively inefficient, with a ratio of radio luminosity to mechanical cavity power of similar to 10(-4), and that the radio pressure of the lobes is about 1 order of magnitude lower than the X-ray pressure of the surrounding thermal gas. Thanks to the high spatial resolution of the Chandra surface brightness and temperature profiles, we also identify a shock front located at 36 kpc to the southwest of the group center, close to the southern radio lobe, with a Mach number similar to 1.5 and a total power which is about 1 order of magnitude higher than the cavity power. Such a shock may have heated the gas in the southern region, as indicated by the temperature map. The shock may also explain the arc-like region of enriched gas seen in the iron abundance map, as this may be produced by a non-Maxwellian electron distribution near its front. C1 [Gitti, Myriam; O'Sullivan, Ewan; Giacintucci, Simona; David, Laurence P.; Vrtilek, Jan; Nulsen, Paul E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gitti, Myriam] INAF, Astron Observ Bologna, I-40127 Bologna, Italy. [O'Sullivan, Ewan; Raychaudhury, Somak] Univ Birmingham, Birmingham B15 2TT, W Midlands, England. [Giacintucci, Simona] INAF, Inst Radioastron, I-40129 Bologna, Italy. RP Gitti, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI O'Sullivan, Ewan/0000-0002-5671-6900; Gitti, Myriam/0000-0002-0843-3009; Nulsen, Paul/0000-0003-0297-4493 FU European Community; [ASI-INAF I/088/06/0]; [GO0-11003X] FX We thank the anonymous referee for constructive suggestions that improved the presentation of the results. We thank S. Ettori for providing the software required to produce the XMM-Newton color map in Figure 7 (right) and M. Markevitch for useful discussions. M. Gitti also thanks T. Ponman and F. Brighenti for comments on the original manuscript. M. Gitti acknowledges support by grant ASI-INAF I/088/06/0. E. O'Sullivan acknowledges the support of the European Community under the Marie Curie Research Training Network. This research is supported by Chandra grant GO0-11003X. NR 58 TC 51 Z9 51 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD MAY 1 PY 2010 VL 714 IS 1 BP 758 EP 771 DI 10.1088/0004-637X/714/1/758 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 583SV UT WOS:000276701000060 ER PT J AU Launhardt, R Nutter, D Ward-Thompson, D Bourke, TL Henning, T Khanzadyan, T Schmalzl, M Wolf, S Zylka, R AF Launhardt, R. Nutter, D. Ward-Thompson, D. Bourke, T. L. Henning, Th. Khanzadyan, T. Schmalzl, M. Wolf, S. Zylka, R. TI LOOKING INTO THE HEARTS OF BOK GLOBULES: MILLIMETER AND SUBMILLIMETER CONTINUUM IMAGES OF ISOLATED STAR-FORMING CORES SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE dust, extinction; infrared: stars; ISM: clouds; stars: formation; submillimeter: ISM ID YOUNG STELLAR OBJECTS; TRANSLUCENT MOLECULAR CLOUDS; INITIAL MASS FUNCTION; NEAR-INFRARED OBSERVATIONS; CLERK-MAXWELL-TELESCOPE; SMALL DARK CLOUDS; MAGNETIC-FIELD; SCUBA SURVEY; DENSE CORES; ATMOSPHERIC LIMITATIONS AB We present the results of a comprehensive infrared, submillimeter, and millimeter continuum emission study of isolated low-mass star-forming cores in 32 Bok globules, with the aim to investigate the process of star formation in these regions. The submillimeter and millimeter dust continuum emission maps together with the spectral energy distributions are used to model and derive the physical properties of the star-forming cores, such as luminosities, sizes, masses, densities, etc. Comparisons with ground-based near-infrared and space-based mid-and far-infrared images from Spitzer are used to reveal the stellar content of the Bok globules, association of embedded young stellar objects (YSOs) with the submillimeter dust cores, and the evolutionary stages of the individual sources. Submillimeter dust continuum emission was detected in 26 out of the 32 globule cores observed. For 18 globules with detected (sub) millimeter cores, we derive evolutionary stages and physical parameters of the embedded sources. We identify nine starless cores, most of which are presumably prestellar, nine Class 0 protostars, and twelve Class I YSOs. Specific source properties like bolometric temperature, core size, and central densities are discussed as a function of evolutionary stage. We find that at least two thirds (16 out of 24) of the star-forming globules studied here show evidence of forming multiple stars on scales between 1000 and 50,000 AU. However, we also find that most of these small prototstar and star groups are comprised of sources with different evolutionary stages, suggesting a picture of slow and sequential star formation in isolated globules. C1 [Launhardt, R.; Henning, Th.; Khanzadyan, T.; Schmalzl, M.; Wolf, S.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Nutter, D.; Ward-Thompson, D.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Bourke, T. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zylka, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. RP Launhardt, R (reprint author), Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany. EM rl@mpia.de FU Canadian Space Agency; NASA [1279198, 1288806]; National Science Foundation FX The authors thank the staff at all of the telescopes where data for this paper were obtained. The JCMT is operated by the JAC, Hawaii, on behalf of the UK STFC, the Netherlands OSR, and the National Research Council (NRC) of Canada. This research used the facilities of the Canadian Astronomy Data Centre (CADC) operated by the NRC of Canada with the support of the Canadian Space Agency. This paper is partially based on observations collected at the European Southern Observatory, La Silla, Chile. 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 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. Partial support for T. L. B. was provided by NASA through contracts 1279198 and 1288806 issued by the Jet Propulsion Laboratory, California Institute of Technology, to the Smithsonian Astronomical Observatory. We also thank J. Steinacker, A. Stutz, and C. KenKnight for helpful discussions and critical reading of the manuscript. Last, but not least, we also acknowledge helpful comments by the referee, G. A. Racca, which helped to improve the clarity of the paper. NR 155 TC 37 Z9 37 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2010 VL 188 IS 1 BP 139 EP 177 DI 10.1088/0067-0049/188/1/139 PG 39 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591LQ UT WOS:000277302500006 ER PT J AU Kenyon, SJ Bromley, BC AF Kenyon, Scott J. Bromley, Benjamin C. TI VARIATIONS ON DEBRIS DISKS. II. ICY PLANET FORMATION AS A FUNCTION OF THE BULK PROPERTIES AND INITIAL SIZES OF PLANETESIMALS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; planetary systems; planets and satellites: formation; protoplanetary disks; stars: formation; zodiacal dust ID SUN-LIKE STARS; MAIN-SEQUENCE STARS; TURBULENT PROTOPLANETARY DISKS; SPITZER-MIPS OBSERVATIONS; CIRCUMSTELLAR DUST DISKS; LATE HEAVY BOMBARDMENT; EARLY KUIPER-BELT; SOLAR-TYPE STARS; LOW-MASS STARS; T-TAURI STARS AB We describe comprehensive calculations of the formation of icy planets and debris disks at 30-150 AU around 1-3 M(circle dot) stars. Disks composed of large, strong planetesimals produce more massive planets than disks composed of small, weak planetesimals. The maximum radius of icy planets ranges from similar to 1500 km to 11,500 km. The formation rate of 1000 km objects-"Plutos"-is a useful proxy for the efficiency of icy planet formation. Plutos form more efficiently in massive disks, in disks with small planetesimals, and in disks with a range of planetesimal sizes. Although Plutos form throughout massive disks, Pluto production is usually concentrated in the inner disk. Despite the large number of Plutos produced in many calculations, icy planet formation is inefficient. At the end of the main sequence lifetime of the central star, Plutos contain less than 10% of the initial mass in solid material. This conclusion is independent of the initial mass in the disk or the properties of the planetesimals. Debris disk formation coincides with the formation of planetary systems containing Plutos. As Plutos form, they stir leftover planetesimals to large velocities. A cascade of collisions then grinds the leftovers to dust, forming an observable debris disk. In disks with small (less than or similar to 1-10 km) planetesimals, collisional cascades produce luminous debris disks with maximum luminosity similar to 10(-2) times the stellar luminosity. Disks with larger planetesimals produce debris disks with maximum luminosity similar to 5 x 10(-4) (10 km) to 5 x 10(-5) (100 km) times the stellar luminosity. Following peak luminosity, the evolution of the debris disk emission is roughly a power law, f alpha t(-n) with n approximate to 0.6-0.8. Observations of debris disks around A-type and G-type stars strongly favor models with small planetesimals. In these models, our predictions for the time evolution and detection frequency of debris disks agree with published observations. We suggest several critical observations that can test key features of our calculations. C1 [Kenyon, Scott J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Bromley, Benjamin C.] Univ Utah, Dept Phys, Salt Lake City, UT 84112 USA. RP Kenyon, SJ (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM skenyon@cfa.harvard.edu; bromley@physics.utah.edu OI Kenyon, Scott/0000-0003-0214-609X FU NASA Offices of Mission to Planet Earth, Aeronautics, and Space Science; NASA [NAG5-13278]; NASA TPF Foundation [NNG06GH25G]; Spitzer [20132] FX We acknowledge a generous allotment, similar to 10 cpu years, of computer time on the 1024 cpu Dell Xeon cluster "cosmos" at the Jet Propulsion Laboratory through funding from the NASA Offices of Mission to Planet Earth, Aeronautics, and Space Science. We thank M. Werner for his strong support of this project. We also acknowledge use of similar to 2 cpu years on the CfA cluster "hydra." Advice and comments from J. Carpenter, C. Chen, T. Currie, M. Geller, G. Kennedy, M. Meyer, G. Rieke, K. Su, and an anonymous referee greatly improved our presentation. Portions of this project were supported by the NASA Astrophysics Theory Program, through grant NAG5-13278, the NASA TPF Foundation Science Program, through grant NNG06GH25G, and the Spitzer Guest Observer Program, through grant 20132. NR 162 TC 45 Z9 45 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD MAY PY 2010 VL 188 IS 1 BP 242 EP 279 DI 10.1088/0067-0049/188/1/242 PG 38 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 591LQ UT WOS:000277302500010 ER PT J AU Derevianko, A Porsev, SG Babb, JF AF Derevianko, Andrei Porsev, Sergey G. Babb, James F. TI Electric dipole polarizabilities at imaginary frequencies for hydrogen, the alkali-metal, alkaline-earth, and noble gas atoms SO ATOMIC DATA AND NUCLEAR DATA TABLES LA English DT Article ID MANY-BODY CALCULATIONS; VAN-DER-WAALS; COEFFICIENTS; CONSTANTS; HE AB The electric dipole polarizabilities evaluated at imaginary frequencies for hydrogen, the alkali-metal atoms, the alkaline-earth atoms, and the noble gases are tabulated along with the resulting values of the atomic static polarizabilities, the atom-surface interaction constants, and the dispersion (or van der Waals) constants for the homonuclear and the heteronuclear diatomic combinations of the atoms. (C) 2009 Elsevier Inc. All rights reserved. C1 [Babb, James F.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Porsev, Sergey G.] Petersburg Nucl Phys Inst, Gatchina 188300, Russia. [Derevianko, Andrei; Porsev, Sergey G.] Univ Nevada, Dept Phys, Reno, NV 89557 USA. RP Babb, JF (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM andrei@unr.edu; sporsev@gmail.com; jbabb@cfa.harvard.edu RI Derevianko, Andrei/G-8356-2011; OI Babb, James/0000-0002-3883-9501 NR 36 TC 69 Z9 69 U1 2 U2 24 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0092-640X J9 ATOM DATA NUCL DATA JI Atom. Data Nucl. Data Tables PD MAY PY 2010 VL 96 IS 3 BP 323 EP 331 DI 10.1016/j.adt.2009.12.002 PG 9 WC Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Physics GA 568HV UT WOS:000275514100005 ER PT J AU Boyle, SA Smith, AT AF Boyle, Sarah A. Smith, Andrew T. TI Can landscape and species characteristics predict primate presence in forest fragments in the Brazilian Amazon? SO BIOLOGICAL CONSERVATION LA English DT Article DE Brazil; Conservation; Forest fragmentation; Land cover; Matrix; Primate ID TROPICAL RAIN-FOREST; MONKEYS ALOUATTA-SENICULUS; HABITAT FRAGMENTATION; SEED DISPERSAL; FRENCH-GUIANA; SPIDER MONKEYS; CHIROPOTES-SATANAS; CONSERVATION VALUE; RANGING PATTERNS; BEARDED SAKIS AB Habitat loss and fragmentation are global conservation concerns, but animal species do not respond to these threats in the same manner. At the Biological Dynamics of Forest Fragments Project (BDFFP), located 80 km north of Manaus, Amazonas, Brazil, the distribution and persistence of six native primate species differ among fragments that were isolated in 1980s. We identified both landscape and species characteristics predicting the presence of primates in these forest fragments. Fragment size positively and distance to nearest forested area negatively predicted primate species richness in the fragments; however, these relationships were not straightforward because these two variables were correlated. The proportion of fruit in a species' diet was the most important factor predicting its presence in the forest fragments, with species relying primarily on frugivory faring poorly. Home range size was the second-best predictor of a species' presence; however, some species with large home ranges were present in the 10-ha forest fragments. The extent to which the individual primate species traveled in and out of the fragments varied, suggesting that further research is necessary to determine the primary factors that lead to the animals' use of the matrix. We conclude that in addition to conserving large tracts of habitat, reducing the isolation of the forest fragments through the creation of forest corridors and through the presence of additional forest fragments within the agricultural matrix may increase animal movement across the landscape. Such changes to the matrix may be critical for those species that do not readily traverse non-forested areas. (C) 2010 Elsevier Ltd. All rights reserved. C1 [Boyle, Sarah A.; Smith, Andrew T.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. [Boyle, Sarah A.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Boyle, Sarah A.] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. RP Boyle, SA (reprint author), Rhodes Coll, Dept Biol, 2000 N Pkwy, Memphis, TN 38112 USA. EM boyles@rhodes.edu; a.smith@asu.edu FU Biological Dynamics of Forest Fragments Project (BDFFP); Smithsonian Tropical Research Institute; Arizona State University; Primate Conservation, Inc.; Organization for Tropical Studies, American Society of Primatologists FX We thank Brazil's Conselho Nacional de Desenvolvimento Cientifico e Tecnologico - CNPq, the Instituto Brasileiro do Meio Ambiente e dos Recursos Naturais Renovaveis - IBAMA, and the Instituto Nacional de Pesquisas da Amazonia - INPA for permission to conduct this research. The Biological Dynamics of Forest Fragments Project (BDFFP), Smithsonian Tropical Research Institute, and Arizona State University provided further logistical and financial support, and the Fulbright/Institute of International Education, Margot Marsh Biodiversity Foundation, Providing Educational Opportunities (PEO), Primate Conservation, Inc., Organization for Tropical Studies, American Society of Primatologists provided additional funding. We thank A. M. dos Reis, O. F. da Silva, W. C. Lourenco, L R. da Silva, and W. R. Spironello for assistance in Brazil. V. Arroyo-Rodriguez and two anonymous reviewers provided comments that improved the manuscript. This is publication number 545 in the BDFFP technical series. NR 108 TC 33 Z9 34 U1 5 U2 51 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD MAY PY 2010 VL 143 IS 5 BP 1134 EP 1143 DI 10.1016/j.biocon.2010.02.008 PG 10 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 606LY UT WOS:000278427700014 ER PT J AU Bravo, A Harms, KE Emmons, LH AF Bravo, Adriana Harms, Kyle E. Emmons, Louise H. TI Preference for Collpa Water by Frugivorous Bats (Artibeus): An Experimental Approach SO BIOTROPICA LA English DT Article DE licks; Peruvian Amazon; Phyllostomidae; sodium; Stenodermatinae ID SOUTHEASTERN PERU; LICK; PHYLLOSTOMIDAE; GEOPHAGY; ALOUATTA; AMAZON; SODIUM; FIGS AB Several species of stenodermatine bats congregate in large numbers at collpas in southeastern Peru to drink water. We conducted the first experimental tests of preference for collpa water by representative bats. Artibeus species preferred mineral-rich collpa water over water from other sources, supporting the hypothesis that they seek resources (especially sodium) at collpas. 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), Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. EM adrianabravo1@gmail.com FU Amazon Conservation Association; American Society of Mammalogists; Bat Conservation International; Graduate Student Association-Biograds of Louisiana State University (LSU); Idea Wild; Louisiana Office of Environmental Education; LSU Graduate School; Rufford Small Grants; U. S. National Science Foundation FX We extend our gratitude to the Peruvian Institute of Natural Resources (INRENA) for providing the research permits to conduct this study. For help in the field, we thank the ACCA rangers, Y. Arteaga, M. Bravo, S. Claramunt, M. Cruz, Z. Ordonez, A. L. Rodales, M. Rodriguez, and W. Torres. We also thank E. Kalko, R. Page, N. Pitman, J. Ramos, and K. Salas for their insights on flight cage experiments or for help with logistics of the study. We are grateful to L. Aguirre, S. Claramunt, J. Cronin, L. Hooper-Bui, V. Remsen, R. Stevens, P. Stouffer, M. Williams, and an anonymous reviewer 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 (LSU), Idea Wild, Louisiana Office of Environmental Education, LSU Graduate School, Rufford Small Grants, and the U. S. National Science Foundation (to KEH). NR 33 TC 5 Z9 5 U1 1 U2 9 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2010 VL 42 IS 3 BP 276 EP 280 DI 10.1111/j.1744-7429.2010.00639.x PG 5 WC Ecology SC Environmental Sciences & Ecology GA 591GY UT WOS:000277289400002 ER PT J AU DeWalt, SJ Schnitzer, SA Chave, J Bongers, F Burnham, RJ Cai, ZQ Chuyong, G Clark, DB Ewango, CEN Gerwing, JJ Gortaire, E Hart, T Ibarra-Manriquez, G Ickes, K Kenfack, D Macia, MJ Makana, JR Martinez-Ramos, M Mascaro, J Moses, S Muller-Landau, HC Parren, MPE Parthasarathy, N Perez-Salicrup, DR Putz, FE Romero-Saltos, H Thomas, D AF DeWalt, Saara J. Schnitzer, Stefan A. Chave, Jerome Bongers, Frans Burnham, Robyn J. Cai, Zhiquan Chuyong, Georges Clark, David B. Ewango, Corneille E. N. Gerwing, Jeffrey J. Gortaire, Esteban Hart, Terese Ibarra-Manriquez, Guillermo Ickes, Kalan Kenfack, David Macia, Manuel J. Makana, Jean-Remy Martinez-Ramos, Miguel Mascaro, Joseph Moses, Sainge Muller-Landau, Helene C. Parren, Marc P. E. Parthasarathy, Narayanaswamy Perez-Salicrup, Diego R. Putz, Francis E. Romero-Saltos, Hugo Thomas, Duncan TI Annual Rainfall and Seasonality Predict Pan-tropical Patterns of Liana Density and Basal Area SO BIOTROPICA LA English DT Article DE abundance; climate; liana communities; tropical forest ID DRY EVERGREEN FORESTS; FLORISTIC COMPOSITION; NEOTROPICAL FORESTS; COMMUNITY STRUCTURE; SPECIES-DIVERSITY; NATIONAL-PARK; TREE; ABUNDANCE; DYNAMICS; INDIA AB We test the hypotheses proposed by Gentry and Schnitzer that liana density and basal area in tropical forests vary negatively with mean annual precipitation (MAP) and positively with seasonality. Previous studies correlating liana abundance with these climatic variables have produced conflicting results, warranting a new analysis of drivers of liana abundance based on a different dataset. We compiled a pan-tropical dataset containing 28,953 lianas (>= 2.5 cm diam.) from studies conducted at 13 Neotropical and 11 Paleotropical dry to wet lowland tropical forests. The ranges in MAP and dry season length (DSL) (number of months with mean rainfall < 100 mm) represented by these datasets were 860-7250 mm/yr and 0-7 mo, respectively. Pan-tropically, liana density and basal area decreased significantly with increasing annual rainfall and increased with increasing DSL, supporting the hypotheses of Gentry and Schnitzer. Our results suggest that much of the variation in liana density and basal area in the tropics can be accounted for by the relatively simple metrics of MAP and DSL. C1 [DeWalt, Saara J.; Ickes, Kalan] Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. [Schnitzer, Stefan A.; Mascaro, Joseph] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53211 USA. [Schnitzer, Stefan A.; Muller-Landau, Helene C.; Thomas, Duncan] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Chave, Jerome] CNRS, Lab Evolut & Diversite Biol, Toulouse, France. [Chave, Jerome] Univ Toulouse 3, F-31062 Toulouse, France. [Bongers, Frans; Ewango, Corneille E. N.; Parren, Marc P. E.] Wageningen Univ, Dept Environm Sci, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Burnham, Robyn J.; Kenfack, David] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 48109 USA. [Cai, Zhiquan] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Mengla 666303, Peoples R China. [Chuyong, Georges] Univ Buea, Dept Anim & Plant Sci, Buea, Southwest Prov, Cameroon. [Clark, David B.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Ewango, Corneille E. N.] Ctr Format & Rech Conservat Forestiere, Ituri Forest, Congo. [Gerwing, Jeffrey J.] Inst Homem & Meio Ambiente Amazonia IMAZON, Belem, Para, Brazil. [Gerwing, Jeffrey J.] Portland State Univ, Univ Studies, Portland, OR 97207 USA. [Gortaire, Esteban; Romero-Saltos, Hugo] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Herbario QCA, Quito, Ecuador. [Hart, Terese; Makana, Jean-Remy] Wildlife Conservat Soc, Kinshasa, Zaire. [Ibarra-Manriquez, Guillermo; Martinez-Ramos, Miguel; Perez-Salicrup, Diego R.] Univ Nacl Autonoma Mexico, Ctr Invest Ecosistemas, Morelia 58190, Michoacan, Mexico. [Macia, Manuel J.] Univ Autonoma Madrid, Dept Biol, Area Bot, E-28049 Madrid, Spain. [Moses, Sainge] Korup Forest Dynam Plot Programme, Mundemba, Southwest Prov, Cameroon. [Parren, Marc P. E.] Tropenbos Int Congo Basin Programme, Yaounde, Cameroon. [Parthasarathy, Narayanaswamy] Pondicherry Univ, Dept Ecol & Environm Sci, Pondicherry 605014, India. [Putz, Francis E.] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Romero-Saltos, Hugo] Univ Miami, Dept Biol, Coral Gables, FL 33124 USA. [Thomas, Duncan] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. RP DeWalt, SJ (reprint author), Clemson Univ, Dept Biol Sci, Clemson, SC 29634 USA. EM saarad@clemson.edu RI Macia, Manuel/H-4631-2012; OI Macia, Manuel/0000-0002-4676-612X; Schnitzer, Stefan/0000-0002-2715-9455 FU NCEAS; NSF [EF-0553768]; University of California; Santa Barbara; State of California; HSBC Climate Partnership; NSF, National Science Foundation of China; Wageningen University; Department of Science and Technology of the Government of India; World Wildlife Fund (Brazil); USAID; Organization for Tropical Studies, British Ecological Society; CONACyT (Mexico); European Commission; Fondo Mexicano para la Conservacion de la Naturaleza; BOLFOR; PAPIIT-UNAM; Center for Tropical Forest Science; Smithsonian Tropical Research Institute; University of Wisconsin-Milwaukee Graduate School; International Cooperative Biodiversity Groups; Bioresources Development and Conservation Programme-Cameroon; Ministry of Environment and Forests-Cameroon; Centre National de la Recherche Scientifique; UNESCO; University of Miami; Pontificia Universidad Catolica del Ecuador; REPSOL-YPF; Andrew W. Mellon Foundation FX This work was conducted as a part of the Lianas and Tropical Forest Dynamics Working Group supported by the NCEAS, a Center funded by NSF ( Grant #EF-0553768), the University of California, Santa Barbara, and the State of California. Data collection and management were funded by many organizations including the HSBC Climate Partnership, NSF, National Science Foundation of China, Wageningen University, Department of Science and Technology of the Government of India, World Wildlife Fund (Brazil), USAID, Organization for Tropical Studies, British Ecological Society, CONACyT (Mexico), European Commission, Fondo Mexicano para la Conservacion de la Naturaleza, BOLFOR, PAPIIT-UNAM, Center for Tropical Forest Science, Smithsonian Tropical Research Institute, University of Wisconsin-Milwaukee Graduate School, International Cooperative Biodiversity Groups, Bioresources Development and Conservation Programme-Cameroon, Ministry of Environment and Forests-Cameroon, Centre National de la Recherche Scientifique, UNESCO, University of Miami, Pontificia Universidad Catolica del Ecuador, REPSOL-YPF, and the Andrew W. Mellon Foundation. D. Zoellner helped create the map of study sites. We appreciate comments on the manuscript by M. Pena-Claros, G. van der Heijden, and an anonymous reviewer and discussions with L. Poorter. NR 55 TC 62 Z9 66 U1 5 U2 54 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2010 VL 42 IS 3 BP 309 EP 317 DI 10.1111/j.1744-7429.2009.00589.x PG 9 WC Ecology SC Environmental Sciences & Ecology GA 591GY UT WOS:000277289400006 ER PT J AU Raboy, BE Neves, LG Zeigler, S Saraiva, NA Cardoso, N dos Santos, GR Ballou, JD Leimgruber, P AF Raboy, Becky E. Neves, Leonardo G. Zeigler, Sara Saraiva, Nicholas A. Cardoso, Nayara dos Santos, Gabriel Rodrigues Ballou, Jonathan D. Leimgruber, Peter TI Strength of Habitat and Landscape Metrics in Predicting Golden-Headed Lion Tamarin Presence or Absence in Forest Patches in Southern Bahia, Brazil SO BIOTROPICA LA English DT Article DE Atlantic forest; fragmentation; Leontopithecus chrysomelas; lion tamarins; logistic regression; Monte Carlo methods; predictive models ID ATLANTIC FOREST; LEONTOPITHECUS-CHRYSOMELAS; SMALL MAMMALS; BIODIVERSITY; FRAGMENTATION; CONSERVATION; EXTINCTION; POPULATIONS; ECOLOGY AB We investigated the effects of forest fragmentation on golden-headed lion tamarins (Leontopithecus chrysomelas) by qualitatively and quantitatively characterizing the landscape throughout the species range, conducting surveys, and exploring predictive models of presence and absence. We identified 784 forest patches that varied in size, shape, core area, habitat composition, elevation, and distance to neighboring patches and towns. We conducted 284 interviews with local residents and 133 playback experiments in 98 patches. Results indicated a reduction in the western portions of the former species range. We tested whether L. chrysomelas presence or absence was related to the aforementioned fragmentation indices using Monte Carlo logistic regression techniques. The analysis yielded a majority of iterations with a one-term final model of which Core Area Index (percent of total area that is core) was the only significant type. Model concordance ranged between 65 and 90 percent. Area was highlighted for its potential predictive ability. Although final models for area lacked significance, their failure to reach significance was marginal and we discuss potential confounding factors weakening the term's predictive ability. We conclude that lower Core Area Index scores are useful indicators of forest patches at risk for not supporting L. chrysomelas. Taken together, our analyses of the landscape, survey results, and logistic regression modeling indicated that the L. chrysomelas metapopulation is facing substantial threat. The limited vagility of lion tamarins in nonforest matrix may lead to increasingly smaller and inbred populations subject to significant impact from edge effects and small population size. Local extinction is imminent in many forest patches in the L. chrysomelas range. C1 [Raboy, Becky E.; Saraiva, Nicholas A.; Ballou, Jonathan D.; Leimgruber, Peter] Smithsonian Inst, Natl Zool Pk, Dept Conservat & Sci, Washington, DC 20013 USA. [Raboy, Becky E.; Neves, Leonardo G.; Cardoso, Nayara; dos Santos, Gabriel Rodrigues] Inst Estudos Socioambientais Sul Bahia, BR-45653145 Ilheus, BA, Brazil. [Neves, Leonardo G.; Cardoso, Nayara] Univ Estadual Santa Cruz, Dept Ciencias Biol, BR-45662000 Ilheus, BA, Brazil. [Zeigler, Sara] Univ Maryland, Dept Geog, College Pk, MD 20742 USA. [Saraiva, Nicholas A.] ONG Pivot Maranhao, BR-65585000 Paulino Neves, MA, Brazil. RP Raboy, BE (reprint author), Smithsonian Inst, Natl Zool Pk, Dept Conservat & Sci, POB 37012 MRC 5503, Washington, DC 20013 USA. EM raboyb@si.edu RI Leimgruber, Peter/O-1304-2015 OI Leimgruber, Peter/0000-0002-3682-0153 FU Association of Zoos and Aquariums/Disney Worldwide; Critical Ecosystem Partnership Fund; International Primatological Society; Lion Tamarins of Brazil FX The Association of Zoos and Aquariums/Disney Worldwide Conservation Fund, the Critical Ecosystem Partnership Fund, the International Primatological Society, and the Lion Tamarins of Brazil Fund funded this project with additional institutional support from the Smithsonian Institution and the Institute for Social and Environmental Studies of Southern Bahia. G. Canale was instrumental in helping design our interview methods. We thank C. Guidorizzi and L. Oliveira for assisting during the interviews and playbacks. We are especially grateful to the survey participants and landowners for their cooperation in this study. B. Raboy had a CNPq permit (Portaria No-82, February 8, 2002 and No-187, March 28, 2007) to conduct this research. S. Hankerson produced the SAS code for the randomization trials. We thank S. Hankerson, K. De Vleeschouwer, and J. Dietz for comments on earlier versions of the manuscript. NR 46 TC 13 Z9 13 U1 4 U2 28 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD MAY PY 2010 VL 42 IS 3 BP 388 EP 397 DI 10.1111/j.1744-7429.2009.00595.x PG 10 WC Ecology SC Environmental Sciences & Ecology GA 591GY UT WOS:000277289400016 ER PT J AU Linder, HP Hardy, CR AF Linder, H. P. Hardy, C. R. TI A generic classification of the Restioneae (Restionaceae), southern Africa SO BOTHALIA LA English DT Article DE Africa; generic classification; Restionaceae; Restioneae; taxonomy ID CAPE FLORISTIC REGION; ORCHID GENUS DISA; RHODOCOMA RESTIONACEAE; MOLECULAR PHYLOGENY; FLAVONOID PATTERNS; SPECIES TREES; DELIMITATION; MORPHOLOGY; TAXONOMY; POALES AB We propose a new generic classification of the African Restionaceae, tribe Restioneae (subfamily Restionoideae), based on the phylogeny and on extensive morphological data. The phylogeny is based on both plastid sequence data and morphological data. We delimit the genera to be monophyletic, to minimize the nomenclatural changes, and to maximize the ability to diagnose the genera. We recognize eight genera, one of which with nine subgenera, in the tribe. Of the currently accepted genera, only three need changes. We provide descriptions for all genera and subgenera, and include a key to them. In this paper we erect one new genus. Soroveta, redelimit Platycaulos and Restio. and reduce Calopsis and Ischyrolepis to synonomy under Restio. We list the species which we recognize under each genus, make 37 new combinations, propose eight new names, and also describe eight new species that belong in these genera. C1 [Linder, H. P.] Univ Zurich, Inst Systemat Bot, CH-8008 Zurich, Switzerland. [Hardy, C. R.] Millersville Univ Pennsylvania, James C Parks Herbarium, Dept Biol, Millersville, PA 17551 USA. [Hardy, C. R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Linder, HP (reprint author), Univ Zurich, Inst Systemat Bot, CH-8008 Zurich, Switzerland. RI Linder, Hans Peter/F-5316-2010 FU Swiss Science Foundation [SNF 31-66594-01]; Claraz Foundation; National Geographic Society [7289-02] FX This study was funded by the Swiss Science Foundation grant SNF 31-66594-01, and the field work was supported by the Claraz Foundation and National Geographic Society Grant 7289-02. CapeNature provided collecting permission. We particularly want to thank Philip Moline (field work, collaboration on the Elegia complex), the Bolus Herbarium and Terry Trinder-Smith for handling our collections in Cape Town. Peter Goldblatt, Barbara Briggs and Nick Helme are thanked for critical input into the paper, and Peter Wilson and Otto Leistner for checking the Latin. NR 80 TC 8 Z9 8 U1 0 U2 1 PU NATL BOTANICAL INST PI PRETORIA PA PRIVATE BAG X101, PRETORIA 0001, SOUTH AFRICA SN 0006-8241 J9 BOTHALIA JI Bothalia PD MAY PY 2010 VL 40 IS 1 BP 1 EP 35 PG 35 WC Plant Sciences SC Plant Sciences GA 628RM UT WOS:000280138300001 ER PT J AU Baugh, AT Ryan, MJ AF Baugh, Alexander T. Ryan, Michael J. TI Ambient light alters temporal-updating behaviour during mate choice in a Neotropical frog SO CANADIAN JOURNAL OF ZOOLOGY LA English DT Article ID PREDATION RISK; PHYSALAEMUS-PUSTULOSUS; TUNGARA FROGS; BUSH-CRICKETS; FEMALES; SIGNALS; CALLS; PREFERENCES; ORTHOPTERA; SELECTION AB It is well known that animal decision-making can be influenced by environmental variables, such as the risk of predation. During the breeding season, nocturnal amphibians encounter a range of environmental conditions at breeding aggregations, including variable ambient light conditions. For nocturnal frogs, illumination is expected to minimize conspicuous movement that might increase predator detection. Previous work has shown that female Physalaemus pustulosus (Cope, 1864) (= Engystomops pustulosus (Cope, 1864)) are sensitive to variation in light levels during mate choice. Here we use an acoustic playback design in which stimuli are adjusted for intensity and complexity during female phonotaxis to show that choosiness is influenced by light level. Frogs were more likely to commit to an initial mate choice despite a dynamic reduction in mate attractiveness under dim light conditions compared with darkness. These results suggest that females are trading off the attractiveness of potential mates with the perceived costs of executing mate choice by committing to an initial decision and thereby reducing assessment time and movement. The dynamic playback design used here provides an approach that could be applied in other systems in which context-dependent decision-making is thought to be important. C1 [Baugh, Alexander T.; Ryan, Michael J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, Michael J.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Baugh, AT (reprint author), Max Planck Inst Ornithol Migrat & Immunoecol, Schlossallee 2, D-78315 Radolfzell am Bodensee, Germany. EM alex.baugh@gmail.com RI Baugh, Alexander/E-4777-2010; OI Baugh, Alexander/0000-0003-2032-892X FU National Science Foundation [IOB 0544096] FX We thank A. Lea and L. Ziegler for their assistance with data collection. The Smithsonian Tropical Research Institute provided logistical support for this study and Autoridad Nacional del Ambiente approved scientific permits in the Republic of Panama. Funding was contributed by National Science Foundation grant No. IOB 0544096 to M.J.R. NR 45 TC 7 Z9 7 U1 1 U2 8 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 65 AURIGA DR, SUITE 203, OTTAWA, ON K2E 7W6, CANADA SN 0008-4301 EI 1480-3283 J9 CAN J ZOOL JI Can. J. Zool. PD MAY PY 2010 VL 88 IS 5 BP 448 EP 453 DI 10.1139/Z10-018 PG 6 WC Zoology SC Zoology GA 610KP UT WOS:000278731900003 ER PT J AU Ahlering, MA Arlt, D Betts, MG Fletcher, RJ Nocera, JJ Ward, MP AF Ahlering, Marissa A. Arlt, Debora Betts, Matthew G. Fletcher, Robert J., Jr. Nocera, Joseph J. Ward, Michael P. TI RESEARCH NEEDS AND RECOMMENDATIONS FOR THE USE OF CONSPECIFIC-ATTRACTION METHODS IN THE CONSERVATION OF MIGRATORY SONGBIRDS SO CONDOR LA English DT Article DE avian conservation techniques; conspecific attraction; endangered and threatened species; habitat selection; playbacks; social information ID INADVERTENT SOCIAL INFORMATION; BREEDING HABITAT SELECTION; EXTRA-PAIR PATERNITY; PUBLIC INFORMATION; SITE SELECTION; HETEROSPECIFIC ATTRACTION; SPATIAL AUTOCORRELATION; EMPIDONAX-MINIMUS; RESIDENT BIRDS; HIDDEN LEKS AB Numerous studies have confirmed that when selecting habitat birds can use social information acquired from observing other individuals, and many aspects of this social information can be capitalized upon to manage bird populations. The conservation implications of attraction to conspecifics are especially promising for management, and as research progresses it is important to consider how this behavior can be applied to conservation practice. The biological underpinnings of conspecific attraction and the repercussions of manipulating species' distributions with attraction methods are not well understood, but conservation decisions often cannot wait for scientific research. Here we synthesize the current research on manipulation of songbirds by conspecific-attraction methods and review our knowledge gaps critically. We reviewed the published literature on conspecific-attraction experiments in songbirds and found that of 24 studies in which they were attempted, 20 were successful in attracting birds. Although many experiments have been successful in attracting conspecifics with various cues, we outline issues to be considered before songbirds are manipulated by attraction methods, and we highlight areas of research necessary to enhance the understanding of conspecific attraction and its use in conservation. C1 [Ahlering, Marissa A.] Univ Missouri, Columbia, MO 65211 USA. [Arlt, Debora] Swedish Univ Agr Sci, Dept Ecol, S-75007 Uppsala, Sweden. [Betts, Matthew G.] Oregon State Univ, Dept Forest Ecosyst & Soc, Corvallis, OR 97331 USA. [Fletcher, Robert J., Jr.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Nocera, Joseph J.] Trent Univ, Ontario Minist Nat Resources, Peterborough, ON K9J 7B8, Canada. [Ward, Michael P.] Univ Illinois, Illinois Nat Hist Survey, Champaign, IL 61820 USA. RP Ahlering, MA (reprint author), Smithsonian Inst, Natl Zool Pk, Washington, DC 20008 USA. EM mahlering@tnc.org OI Fletcher, Robert/0000-0003-1717-5707 NR 95 TC 34 Z9 36 U1 4 U2 40 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 EI 1938-5129 J9 CONDOR JI Condor PD MAY PY 2010 VL 112 IS 2 BP 252 EP 264 DI 10.1525/cond.2010.090239 PG 13 WC Ornithology SC Zoology GA 614OO UT WOS:000279069700008 ER PT J AU Wiley, AE Ostrom, PH Stricker, CA James, HF Gandhi, H AF Wiley, Anne E. Ostrom, Peggy H. Stricker, Craig A. James, Helen F. Gandhi, Hasand TI ISOTOPIC CHARACTERIZATION OF FLIGHT FEATHERS IN TWO PELAGIC SEABIRDS: SAMPLING STRATEGIES FOR ECOLOGICAL STUDIES SO CONDOR LA English DT Article DE carbon; feather; hydrogen; nitrogen; seabird; stable isotopes ID STABLE-ISOTOPES; TEMPORAL VARIATION; MASS-SPECTROMETRY; BONE-COLLAGEN; AMINO-ACIDS; HYDROGEN; RATIOS; CARBON; NITROGEN; DIETS AB We wish to use stable-isotope analysis of flight feathers to understand the feeding behavior of pelagic seabirds, such as the Hawaiian Petrel (Pterodroma sandwichensis) and Newell's Shearwater (Puffinus auricularis newelli). Analysis of remiges is particularly informative because the sequence and timing of remex molt are often,known. The initial step, reported here, is to obtain accurate isotope values from whole remiges by means of a minimally invasive protocol appropriate for live birds or museum specimens. The high variability observed in delta(13)C and delta(15)N values within a feather precludes the use of a small section of vane. We found the average range within 42 Hawaiian Petrel remiges to be 1.3 parts per thousand for both delta(13)N and delta(15)N and that within 10 Newell's Shearwater remiges to be 1.3 parts per thousand and 0.7 parts per thousand for delta(13)N and delta(15)N, respectively. The delta(13)N of all 52 feathers increased from tip to base, and the majority of Hawaiian Petrel feathers showed an analogous trend in delta(15)N. Although the average range of delta D in 21 Hawaiian Petrel remiges was 11 parts per thousand, we found no longitudinal trend. We discuss influences of trophic level, foraging location, metabolism, and pigmentation on isotope values and compare three methods of obtaining isotope averages of whole feathers. Our novel barb-sampling protocol requires only 1.0 mg of feather and minimal preparation time. Because it leaves the feather nearly intact, this protocol will likely facilitate obtaining isotope values from remiges of live birds and museum specimens. As a consequence, it will help expand the understanding of historical trends in foraging behavior. C1 [Wiley, Anne E.; Ostrom, Peggy H.; Gandhi, Hasand] Michigan State Univ, Dept Zool, E Lansing, MI 48824 USA. [Stricker, Craig A.] US Geol Survey, Denver Fed Ctr, Lakewood, CO 80225 USA. [James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. RP Wiley, AE (reprint author), Michigan State Univ, Dept Zool, 203 Nat Sci Bldg, E Lansing, MI 48824 USA. EM wileyann@msu.edu FU National Science Foundation [DEB 0745604] FX We thank Nick Holmes, Darcy Hu, Jay Penniman, Fern Duvall, and all those in the Hawaii Department of Land and Natural Resources and National Park Service who have graciously provided samples from the field, and Andreanna Welch, Megan Spitzer, Christina Gebhard, and Alison Yoshida for collecting samples at the National Museum of Natural History. We also thank Cayce Gulbransen of the U.S. Geological Survey for analyzing hydrogen isotopes and Mary Bremigan, Jefferey Kelly, Alan Brush, Eric Hegg, and Peter Pyle for their helpful comments on our manuscript. This work was supported by funds from the National Science Foundation DEB 0745604. The use of any trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U.S. government. NR 53 TC 10 Z9 11 U1 2 U2 31 PU COOPER ORNITHOLOGICAL SOC PI LAWRENCE PA ORNITHOLOGICAL SOC NORTH AMER PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0010-5422 J9 CONDOR JI Condor PD MAY PY 2010 VL 112 IS 2 BP 337 EP 346 DI 10.1525/cond.2010.090186 PG 10 WC Ornithology SC Zoology GA 614OO UT WOS:000279069700017 ER PT J AU Latrubesse, EM Cozzuol, M da Silva-Caminha, SAF Rigsby, CA Absy, ML Jaramillo, C AF Latrubesse, Edgardo M. Cozzuol, Mario da Silva-Caminha, Silane A. F. Rigsby, Catherine A. Absy, Maria Lucia Jaramillo, Carlos TI The Late Miocene paleogeography of the Amazon Basin and the evolution of the Amazon River system SO EARTH-SCIENCE REVIEWS LA English DT Review DE Amazon basin; Amazon River; Late Miocene; Paleogeography; Paleoecology; fossil vertebrates; palinology; Solimoes Formation ID HIMALAYAN FORELAND BASIN; SEA-LEVEL FLUCTUATIONS; SOUTH-AMERICA; PLIOCENE SEDIMENTATION; SOUTHWESTERN AMAZONIA; EASTERN CORDILLERA; OVERBANK DEPOSITS; TROPICAL RIVERS; LATE QUATERNARY; YECUA FORMATION AB On the basis of paleontological content (vertebrates and palynology) and facies analysis from river banks, road cuts, and three wells, we have assigned the uppermost levels of the Solimoes Formation in western Amazonia, Brazil, to the Late Miocene. The vertebrate fossil record from outcropping sediments is assigned to the Huayquerian-Mesopotamian mammalian biozones, spanning 9-6.5 Ma. Additionally, we present results that demonstrate that deposits in Peruvian Amazonia attributed to Miocene tidal environments are actually fluvial sediments that have been misinterpreted (both environmentally and chronologically) by several authors. The entire Late Miocene sequence was deposited in a continental environment within a subsiding basin. The facies analysis, fossil fauna content, and palynological record indicate that the environment of deposition was dominated by avulsive rivers associated with megafan systems, and avulsive rivers in flood basins (swamps, lakes, internal deltas, and splays). Soils developed on the flatter, drier areas, which were dominated by grasslands and gallery forest in a tropical to subtropical climate. These Late Miocene sediments were deposited from westward of the Purus arch up to the border of Brazil with Peru (Divisor Ranges) and Bolivia (Pando block). Eastward of the Iquitos structural high, however, more detailed studies, including vertebrate paleontology, need to be performed to calibrate with more precision the ages of the uppermost levels of the Solimiies Formation. The evolution of the basin during the late Miocene is mainly related to the tectonic behavior of the Central Andes (-3 -15 S). At approximately 5 Ma, a segment of low angle of subduction was well developed in the Nazca Plate, and the deformation in the Subandean foreland produced the inland reactivation of the Divisor/ Contamana Ranges and tectonic arrangements in the Eastern Andes. During the Pliocene southwestern Brazilian Amazonia ceased to be an effective sedimentary basin, and became instead an erosional area that contributed sediments to the Amazon fluvial system. At that time, the lowland fluvial systems of southwestern Amazonia (the Purus, Jurua and Javari basins) become isolated from the Andes by the newly formed northflowing Ucayali system and south-east flowing Madre de Dios System. It was during the early Pliocene that the Amazon fluvial system integrated regionally and acquired its present appearance, and also when it started to drain water and sediments on a large scale to the Atlantic Ocean. (C) 2010 Elsevier B.V. All rights reserved. C1 [Latrubesse, Edgardo M.] Univ Texas Austin, Dept Geog & Environm, Austin, TX 78712 USA. [Cozzuol, Mario] Univ Fed Minas Gerais, Dept Zool, ICB, Belo Horizonte, MG, Brazil. [da Silva-Caminha, Silane A. F.; Absy, Maria Lucia] Univ Fed Mato Grosso, Dept Geol, BR-78060900 Cuiaba, MT, Brazil. [Rigsby, Catherine A.] E Carolina Univ, Dept Geol Sci, Greenville, NC USA. [Jaramillo, Carlos] Smithsonian Trop Res Inst, Balboa, Panama. RP Latrubesse, EM (reprint author), Univ Texas Austin, Dept Geog & Environm, A3100, Austin, TX 78712 USA. EM latrubesse@austin.utexas.edu RI Cozzuol, Mario/H-8302-2012 OI Cozzuol, Mario/0000-0003-3645-0401 NR 120 TC 112 Z9 118 U1 3 U2 45 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 MAY PY 2010 VL 99 IS 3-4 BP 99 EP 124 DI 10.1016/j.earscirev.2010.02.005 PG 26 WC Geosciences, Multidisciplinary SC Geology GA 608UV UT WOS:000278612400001 ER PT J AU Uriarte, M Bruna, EM Rubim, P Anciaes, M Jonckheere, I AF Uriarte, Maria Bruna, Emilio M. Rubim, Paulo Anciaes, Marina Jonckheere, Inge TI Effects of forest fragmentation on the seedling recruitment of a tropical herb: assessing seed vs. safe-site limitation SO ECOLOGY LA English DT Article DE Amazonian forest; Heliconia acuminata; landscape modification; safe-cite limitation; seed limitation; seedling recruitment ID AMAZONIAN UNDERSTORY HERB; NEOTROPICAL RAIN-FOREST; ATLANTIC FOREST; TREE SEEDLINGS; POSTAGRICULTURAL FORESTS; MESOSCALE DISTRIBUTION; HELICONIA-ACUMINATA; PLANT-POPULATIONS; SHADE TOLERANCE; WOODLAND HERBS AB Studies simultaneously evaluating the importance of safe-site and seed limitation for plant establishment are rare, particularly in human-modified landscapes. We used spatially,explicit neighborhood models together with data from 10 0.5-ha mapped census plots in a fragmented landscape spanning 1000 km(2) to (1) evaluate the relative importance of seed production, dispersal, and safe-site limitation for the recruitment of the understory herb Heliconia acuminata; and (2) determine how these processes differ between fragments and continuous forests. Our analyses demonstrated a large degree of variation in seed production, dispersal, and establishment among and within the 10 study plots. Seed production limitation was strong but only at small spatial scales. Average dispersal distance was less than 4 m, leading to severe dispersal limitation at most sites. Overall, safe-site limitation was the most important constraint on seedling establishment. Fragmentation led to a more heterogeneous light environment with negative consequences for seedling establishment but had little effect on seed production or dispersal. These results suggest that the effects of fragmentation on abiotic processes may be more important than the disruption of biotic interactions in driving biodiversity loss in tropical forests, at least for some functional groups. These effects May be common when the matrix surrounding fragments contains enough tree cover to enable movement of dispersers and pollinators. C1 [Uriarte, Maria] Columbia Univ, Dept Ecol Evolut & Environm Biol, New York, NY 10027 USA. [Bruna, Emilio M.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Bruna, Emilio M.] Univ Florida, Ctr Latin Amer Studies, Gainesville, FL 32611 USA. [Bruna, Emilio M.; Rubim, Paulo; Anciaes, Marina] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Bruna, Emilio M.; Rubim, Paulo; Anciaes, Marina] Smithsonian Trop Res Inst, BR-69011970 Manaus, Amazonas, Brazil. [Jonckheere, Inge] Katholieke Univ Leuven, Biosyst Dept, Geomat Grp, B-3001 Louvain, Belgium. RP Uriarte, M (reprint author), Columbia Univ, Dept Ecol Evolut & Environm Biol, 1200 Amsterdam Ave, New York, NY 10027 USA. EM mu2126@columbia.edu RI Bruna, Emilio/H-2769-2012; Uriarte, Maria/L-8944-2013 OI Bruna, Emilio/0000-0003-3381-8477; FU U.S. National Science Foundation [DEB-0614339, DEB-0614149, INT 98-06351]; Institute for Food and Agricultural Sciences; Center for Latin American Studies; College of Agricultural and Life Sciences at the University of Florida FX We thank Liza Comita, Kathryn Flinn, and an anonymous reviewer for helpful comments on the manuscript. We also thank the technicians and students who helped conduct the censuses and are grateful for the logistical support of the BDFFP and its stall. Financial support was provided by the U.S. National Science Foundation (award DEB-0614339 to M. Uriarte and DEB-0614149 and INT 98-06351 to E. M. Bruna) and the Institute for Food and Agricultural Sciences, Center for Latin American Studies, and College of Agricultural and Life Sciences at the University of Florida. This is publication number 548 in the BDFFP Technical Series. NR 75 TC 26 Z9 26 U1 4 U2 54 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 MAY PY 2010 VL 91 IS 5 BP 1317 EP 1328 DI 10.1890/09-0785.1 PG 12 WC Ecology SC Environmental Sciences & Ecology GA 598VQ UT WOS:000277867600009 PM 20503865 ER PT J AU Parker, JD Salminen, JP Agrawal, AA AF Parker, John D. Salminen, Juha-Pekka Agrawal, Anurag A. TI Herbivory enhances positive effects of plant genotypic diversity SO ECOLOGY LETTERS LA English DT Letter DE Biodiversity and ecosystem functioning; community genetics; diffuse selection; genetic diversity and herbivory; Oenothera biennis; phenotypic plasticity; plant-insect interactions ID PRIMROSE OENOTHERA-BIENNIS; GENETIC DIVERSITY; NATURAL-SELECTION; SPECIES RICHNESS; ECOSYSTEM FUNCTION; TROPHIC LEVELS; BIODIVERSITY; COMMUNITY; RESISTANCE; CONSEQUENCES AB P>Both plant diversity and vertebrate herbivores can impact plant fitness and ecosystem functioning, however their interactions have not been explicitly tested. We manipulated plant genotypic diversity of the native plant Oenothera biennis and monitored its survivorship and lifetime fitness with and without one of its major vertebrate consumers, white-tailed deer Odocoileus virginianus. Intense but unmanipulated herbivory by meadow voles Microtus pennsylvanicus killed over 70% of nearly 4000 experimental plants. However, plants grown in genotypically diverse patches suffered fewer vole attacks and had higher survival and reproductive output than plants in monoculture. Moreover, positive effects of genotypic diversity were enhanced by the presence of deer, indicating a non-additive interaction between diversity and trophic-level complexity. Genetic selection analyses showed that the selective value of ecologically important traits depended on plant diversity and exposure to deer, demonstrating that community complexity can promote fitness through multiple ecologically and evolutionarily important feedbacks. C1 [Parker, John D.; Agrawal, Anurag A.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14850 USA. [Salminen, Juha-Pekka] Univ Turku, Dept Chem, Lab Organ Chem & Chem Biol, FI-20014 Turku, Finland. 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 NR 50 TC 30 Z9 31 U1 1 U2 59 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2010 VL 13 IS 5 BP 553 EP 563 DI 10.1111/j.1461-0248.2010.01452.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 584YJ UT WOS:000276790200004 PM 20298460 ER PT J AU Miller, MJ Bermingham, E Klicka, J Escalante, P Winker, K AF Miller, Matthew J. Bermingham, Eldredge Klicka, John Escalante, Patricia Winker, Kevin TI Neotropical birds show a humped distribution of within-population genetic diversity along a latitudinal transect SO ECOLOGY LETTERS LA English DT Letter DE Centre-marginal hypothesis; genetic diversity; gradient; latitude; mid-domain effect; tropics ID SPECIES RICHNESS; HISTORICAL DIVERSIFICATION; ENVIRONMENTAL GRADIENTS; GEOMETRIC CONSTRAINTS; PATTERNS; DEMOGRAPHY; AMERICA; MODEL; PHYLOGEOGRAPHY; CONSEQUENCES AB P>The latitudinal gradient in species richness is a nearly universal ecological phenomenon. Similarly, conspecific genetic diversity often increases towards the equator - usually explained as the consequence of post-glacial range expansion or due to the shared response of genetic diversity to processes that promote species richness. However, no study has yet examined the relationship between latitude and within-population genetic diversity in exclusively tropical species. We surveyed genetic variation in nine resident bird species co-occurring in tropical lowlands between southern Mexico and western Ecuador, where avian species richness increases with decreasing latitude. Within-population genetic variation was always highest at mid-range latitudes, and not in the most equatorial populations. Differences in demography and gene flow across species' ranges may explain some of our observations; however, much of the pattern may be due simply to geometric constraints. Our findings have implications for conservation planning and for understanding how biodiversity scales from genes to communities. C1 [Miller, Matthew J.; Winker, Kevin] Univ Alaska Museum, Fairbanks, AK 99775 USA. [Miller, Matthew J.; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama. [Klicka, John] Univ Nevada, Barrick Museum Nat Hist, Las Vegas, NV 89154 USA. [Escalante, Patricia] Univ Nacl Autonoma Mexico, Inst Biol, Mexico City 04511, DF, Mexico. RP Miller, MJ (reprint author), Univ Alaska Museum, 907 Yukon Dr, Fairbanks, AK 99775 USA. EM millerma@si.edu RI Miller, Matthew/B-4560-2008; Winker, Kevin/M-2042-2014; Escalante, Patricia/B-8704-2014 OI Miller, Matthew/0000-0002-2939-0239; Winker, Kevin/0000-0002-8985-8104; Escalante, Patricia/0000-0002-5531-263X FU FIC NIH HHS [U01TW006634] NR 50 TC 17 Z9 18 U1 1 U2 19 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1461-023X J9 ECOL LETT JI Ecol. Lett. PD MAY PY 2010 VL 13 IS 5 BP 576 EP 586 DI 10.1111/j.1461-0248.2010.01454.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 584YJ UT WOS:000276790200006 PM 20529101 ER PT J AU Mozdzer, TJ Zieman, JC McGlathery, KJ AF Mozdzer, Thomas J. Zieman, Joseph C. McGlathery, Karen J. TI Nitrogen Uptake by Native and Invasive Temperate Coastal Macrophytes: Importance of Dissolved Organic Nitrogen SO ESTUARIES AND COASTS LA English DT Article DE Phragmites; Spartina; Amino acids; Urea; DON; N uptake ID AUSTRALIS COMMON REED; VESICULAR-ARBUSCULAR MYCORRHIZAE; BRACKISH TIDAL MARSH; ENGLAND SALT-MARSH; FREE AMINO-ACIDS; PHRAGMITES-AUSTRALIS; SPARTINA-ALTERNIFLORA; UPTAKE KINETICS; NORTH-AMERICA; MARINE BASIN AB We investigated if the success of the invasive common reed Phragmites australis could be attributed to a competitive ability to use dissolved organic nitrogen (DON) when compared to the dominant macrophyte Spartina alterniflora in tidal wetlands. Short-term nutrient uptake experiments were performed in the laboratory on two genetic lineages of Phragmites (native and introduced to North America) and S. alterniflora. Our results provide the first evidence for direct assimilation of DON by temperate marsh plants and indicate that amino acids are assimilated intact by all plant types at similar rates. Both Phragmites lineages had significantly greater urea-N assimilation rates than S. alterniflora, and the affinity for dissolved inorganic nitrogen (DIN) species was the greatest in native Phragmites > introduced Phragmites > S. alterniflora. Field studies demonstrated uptake of both DON and DIN in similar proportion as those determined in the laboratory experiments. Based on these uptake rates, we estimate that DON has the potential to account for up to 47% of N demand for Phragmites plants, and up to 24% for S. alterniflora plants. Additionally, we suggest that differences in N uptake between native and introduced Phragmites lineages explain one mechanism for the success of the introduced type under increasingly eutrophic conditions. C1 [Mozdzer, Thomas J.; Zieman, Joseph C.; McGlathery, Karen J.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. RP Mozdzer, TJ (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM mozdzert@si.edu RI Mozdzer, Thomas/G-4372-2011; Mozdzer, Thomas/A-3599-2014 OI Mozdzer, Thomas/0000-0002-1053-0967 FU National Science Foundation [DEB 0080381, DEB 0621014] FX We would like to thank the LTER Grants DEB 0080381 and DEB 0621014 from the National Science Foundation for funding, John Snyder and Maria Takahashi for assistance in conducting the laboratory experiments, and Aaron Mills for helpful advice. Additionally, two anonymous reviews comments greatly helped improve the manuscript. NR 69 TC 32 Z9 36 U1 3 U2 49 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1559-2723 J9 ESTUAR COAST JI Estuaries Coasts PD MAY PY 2010 VL 33 IS 3 BP 784 EP 797 DI 10.1007/s12237-009-9254-9 PG 14 WC Environmental Sciences; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 606HI UT WOS:000278413100016 ER PT J AU Carnevale, G Tyler, JC AF Carnevale, Giorgio Tyler, James C. TI Review of the fossil pufferfish genus Archaeotetraodon (Teleostei, Tetraodontidae), with description of three new taxa from the Miocene of Italy SO GEOBIOS LA English DT Review DE Teleostei; Tetraodontidae; Archaeotetraodon; New species; Paleoecology; Fossil record ID MESSINIAN TRIPOLI FORMATION; GENOME SIZE EVOLUTION; PHYLOGENETIC-RELATIONSHIPS; ASTRONOMICAL CALIBRATION; FISHES ACANTHOMORPHA; MITOCHONDRIAL GENOME; MEDITERRANEAN BASIN; NORTH-CAROLINA; SP-NOV; FUGU AB Three new species of the extinct pufferfish genus Archaeotetraodon are described from the Middle to Upper Miocene of Italy A. bannikovi nov. sp., A. dicarloi nov. sp. and A. zafaranai nov. sp.), and compared in detail with the three previously described taxa of the genus [A. jamestyleri (Bannikov), A. winterbottomi Tyler and Bannikov and A. cerrinaferoni Carnevale and Santini], which are known, respectively, from the Miocene of Ukraine, the Oligocene of Russia, and the Miocene of Algeria. The three new species described herein bring the number of known Archaeotetraodon species to six, thereby making it by far the most speciose extinct genus of the order Tetraodontiformes. The monophyly of Archaeotetraodon is supported by two derived conditions: bifid scale spinules (versus single spinules in all other tetraodontids), and the fusion of the haemal spine of the penultimate vertebra to the centrum (versus autogenous in all other tetraodontids). We compare a large suite of morphological features of Archaeotetraodon to those found within the group of more basal tetraodontid genera to which we believe it belongs, but we are unable to determine the closest relationships of Archaeotetraodon within that group. Morphofunctional and paleoenvironmental considerations suggest that the species of the genus Archaeotetraodon were adapted to a pelagic or deep-sea lifestyle and were probably able to tolerate relatively low oxygen concentrations. The entire fossil record of the family Tetraodontidae is discussed. (C) 2010 Elsevier Masson SAS. All rights reserved. C1 [Carnevale, Giorgio] Univ Pisa, Dipartimento Sci Terra, I-56126 Pisa, Italy. [Carnevale, Giorgio] Univ Pisa, Museo Storia Nat & Terr, I-56011 Calci, PI, Italy. [Tyler, James C.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. RP Carnevale, G (reprint author), Univ Pisa, Dipartimento Sci Terra, Via Santa Maria 53, I-56126 Pisa, Italy. EM carnevale@dst.unipi.it NR 110 TC 9 Z9 9 U1 1 U2 8 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 0016-6995 J9 GEOBIOS-LYON JI Geobios PD MAY-JUN PY 2010 VL 43 IS 3 BP 283 EP 304 DI 10.1016/j.geobios.2009.10.005 PG 22 WC Paleontology SC Paleontology GA 615WR UT WOS:000279169300002 ER PT J AU Allen, SR Fiske, RS Tamura, Y AF Allen, Sharon R. Fiske, Richard S. Tamura, Yoshihiko TI Effects of water depth on pumice formation in submarine domes at Sumisu, Izu-Bonin arc, western Pacific SO GEOLOGY LA English DT Article ID EFFUSIVE SILICIC VOLCANISM; PYROCLASTIC VOLCANISM; ERUPTIONS; CALDERA; MEXICO; JAPAN; MODEL AB Domes of the Sumisu volcanic complex (western Pacific), having summits at ocean depths of 1100, 600, 245, and 95 m, are mantled with compositionally identical rhyolitic pumice that has similar vesicularity, but that varies systematically in distribution, size, and surface texture-suggesting that facies and morphology can serve as useful indicators of eruption depth. At depths >500 m, the pumice formed a thick carapace on dense rhyolite and dis-integrated by quench fracture and mechanical failure into a jumble of giant (meters to tens of meters) polyhedral blocks with smooth curviplanar surfaces that display a single quenched margin. Vesiculation was arrested on eruption in seawater in all but the interior of the thickest carapace. At <500 m depths, the pumice occurs as an apron of blocky giant and smaller rough-textured clasts enclosed by quenched margins and pockmarked by coarse (cm) vesicles. No carapace pumice occurs, and the summit is composed of craggy dense dome rock. These shallower water pumice clasts resemble those spalled from historic submarine dome-forming eruptions that buoyed to the sea surface. We interpret spalling to result from vent-derived, weak volatile-driven explosions that take place at water depths <500 m. Our study shows that an increase in hydrostatic pressures over a range of 12 MPa reduces volatile-driven explosivity for subaqueous, rhyolitic, dome-forming eruptions, but does not affect vesicularity. We conclude that meter-size, highly vesicular pumice is diagnostic of subaqueous dome eruptions in water depths of at least 1300 m, and its morphology can be used to distinguish between explosive and effusive origins. C1 [Allen, Sharon R.] Univ Tasmania, ARC Ctr Excellence Ore Deposits, Hobart, Tas 7001, Australia. [Allen, Sharon R.] Univ Tasmania, Sch Earth Sci, Hobart, Tas 7001, Australia. [Fiske, Richard S.] Smithsonian Inst, Washington, DC 20560 USA. [Tamura, Yoshihiko] Japan Agcy Marine Earth Sci & Technol, Yokosuka, Kanagawa 2370061, Japan. RP Allen, SR (reprint author), Univ Tasmania, ARC Ctr Excellence Ore Deposits, Hobart, Tas 7001, Australia. NR 31 TC 18 Z9 18 U1 0 U2 10 PU GEOLOGICAL SOC AMER, INC PI BOULDER PA PO BOX 9140, BOULDER, CO 80301-9140 USA SN 0091-7613 J9 GEOLOGY JI Geology PD MAY PY 2010 VL 38 IS 5 BP 391 EP 394 DI 10.1130/G30500.1 PG 4 WC Geology SC Geology GA 590JE UT WOS:000277220900002 ER PT J AU Crew, SR AF Crew, Spencer R. TI Learning from Greensboro: Truth and Reconciliation in the United States SO HUMAN RIGHTS QUARTERLY LA English DT Book Review C1 [Crew, Spencer R.] George Mason Univ, Fairfax, VA 22030 USA. [Crew, Spencer R.] Smithsonian Inst, Natl Museum Amer Hist, Innovat & Inclus Exhibit Program, Washington, DC 20560 USA. [Crew, Spencer R.] Smithsonian Inst, Natl Museum Amer Hist, Publ Program, Washington, DC 20560 USA. RP Crew, SR (reprint author), George Mason Univ, Fairfax, VA 22030 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 0275-0392 J9 HUM RIGHTS QUART JI Hum. Rights Q. PD MAY PY 2010 VL 32 IS 2 BP 451 EP 454 PG 4 WC Political Science; Social Issues SC Government & Law; Social Issues GA 592BD UT WOS:000277348700010 ER PT J AU Stiling, P Forkner, R Drake, B AF Stiling, Peter Forkner, Rebecca Drake, Bert TI Long-term exposure to elevated CO2 in a Florida scrub-oak forest increases herbivore densities but has no effect on other arthropod guilds SO INSECT CONSERVATION AND DIVERSITY LA English DT Article DE Detritivores; elevated CO2; herbivores; insect abundance; insectivores; Kennedy Space Center; long-term effects; scrub-oak forest ID ATMOSPHERIC CARBON-DIOXIDE; FOLIAR QUALITY; PLANT; ECOSYSTEM; ABUNDANCE; RESPONSES; INSECTS AB 1. This study uses pitfall traps and sticky traps to examine the effects of elevated CO2 on the densities of insect herbivores, insectivores, and detritivores. 2. Pitfall trapping for the last 3 years of 11 years of continuously elevated CO2 revealed increases of insect herbivore species such as Thysanoptera (thrips), Hemiptera, and Lepidoptera, but no effects on insectivores such as spiders, parasitic wasps, and ants; or on detritivores such as Diptera (flies), Psocoptera (book lice), Blattodea (cockroaches), Collembola (spring tails), Orthoptera (crickets), and Coleoptera (beetles). 3. As the bottom-up effects of elevated CO2 are transmitted through plants to herbivores, they do not appear to reach insect natural enemies or decomposers. C1 [Stiling, Peter] Univ S Florida, Dept Integrat Biol, Tampa, FL 33620 USA. [Forkner, Rebecca] George Mason Univ, Fairfax, VA 22030 USA. [Drake, Bert] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Stiling, P (reprint author), Univ S Florida, Dept Integrat Biol, SCA 110,4202 E Fowler Ave, Tampa, FL 33620 USA. EM pstiling@cas.usf.edu FU Office of Science (BER), U.S. Department of Energy, through the Southeast Regional Center of the National Institute for Global Environmental Change; Department of Energy [DE-FGO2-95ER61993] FX This research was supported by the Office of Science (BER), U.S. Department of Energy, through the Southeast Regional Center of the National Institute for Global Environmental Change grants to Peter Stiling and by Department of Energy grant (DE-FGO2-95ER61993) to Bert Drake. Daniel Moon, Anthony Rossi, and Jamie Colson-Moon helped collect the pitfall traps. Thanks to Sylvia Lukasiewicz, Terri Albarricin, Kara Winston, Christina Harris, Georgina Johnson, Heather Faulkner, Toni Gordon, Arnaldo Villafranca, Ciro Vasquez, Samvid Owivedi, Shawn Simmons, Andy Paluch, Matt Dumouchel, Crystal Bernarducci, Shalane Ponsell, Pauline Thai, Jessica Allen, Amanda Ditson, Hamid Hoveida, Carl Franconi, Caitlyn Palmby, and Dianne Harshberger for help in sorting pitfall samples. Thanks also to the editor and a reviewer for useful suggestions. We acknowledge the support and encouragement of NASA Kennedy Space Center and Dynamac Corporation, especially Ross Hinkle. NR 28 TC 3 Z9 3 U1 0 U2 15 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1752-458X J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD MAY PY 2010 VL 3 IS 2 BP 152 EP 156 DI 10.1111/j.1752-4598.2010.00080.x PG 5 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 579VK UT WOS:000276404300010 ER PT J AU Mueller, UG Ortiz, A Bacci, M AF Mueller, U. G. Ortiz, A. Bacci, M., Jr. TI Planting of fungus onto hibernating workers of the fungus-growing ant Mycetosoritis clorindae (Attini, Formicidae) SO INSECTES SOCIAUX LA English DT Article DE Hibernation; Leucocoprini; Insect-fungus mutualism; Fungus-coat; Symbiosis ID MYCOCEPURUS-SMITHII HYMENOPTERA; NEST ARCHITECTURE; EMERY HYMENOPTERA; FORAGING ECOLOGY; SOUTHERN BRAZIL; AGRICULTURE; EVOLUTION; VEGETATION; DIVERSITY; PREDATION AB We describe a peculiar fungus-coating behavior of the attine ant Mycetosoritis clorindae, where workers plant fungal mycelium on hibernating nestmates. Hibernating nestmates become ultimately enveloped in a live mycelial coat, remain motionless in this coated state, and essentially become integrated into the garden matrix. The shallow nest architecture of M. clorindae (depth of main garden is 15-30 cm) in southern Brazil forces the ants to overwinter at relatively low temperatures in the topmost soil layer. Fungal coating may help the ants to survive the prolonged periods of immobility during winter. Fungus-planting on attine adults is so far unknown from other attine species, but the behavior parallels the planting of mycelium on larvae and pupae occurring in many attine species. Planting of mycelium on adult nestmates may have been overlooked so far in attine ants because this behavior may occur only in dormant nests, which are least frequently collected. The possible adaptive functions of fungus coatings of hibernating adults and developing brood are likely similar, including for example physical protection, prevention of desiccation, shielding against parasites and predators (e.g., army ants), or defense against diseases. C1 [Mueller, U. G.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Mueller, U. G.] Smithsonian Trop Res Inst, Balboa, Panama. [Ortiz, A.; Bacci, M., Jr.] Univ Estadual Paulista, Inst Biociencias, Ctr Estudos Insetos Sociais, BR-13506900 Rio Claro, SP, Brazil. [Ortiz, A.] Univ Nacl Colombia, Fac Ciencias, Medellin, Colombia. [Bacci, M., Jr.] Univ Estadual Paulista, Inst Biociencias, Dept Bioquim & Microbiol, BR-13506900 Rio Claro, SP, Brazil. RP Mueller, UG (reprint author), Univ Texas Austin, Sect Integrat Biol, 1 Univ Stn,C0930, Austin, TX 78712 USA. EM umueller@mail.utexas.edu; aortizr@unalmed.edu.co; mbacci@rc.unesp.br FU CAPES-UT [05/02]; FAPESP [2003/08112-0]; NSF [DEB-0639879] FX We thank the CAPES-UT Cooperation Program (Proc. 05/02, to MB), FAPESP (Proc. 2003/08112-0, to MB), and the NSF (DEB-0639879, to UGM) for financial support. We thank S. Amador-Vargas, N. Biani, H. Ishak, R. Sen, C. Rabeling, and particularly two anonymous reviewers for constructive comments; and J.R. Somera for drawing Figure 1. NR 43 TC 6 Z9 6 U1 0 U2 12 PU SPRINGER BASEL AG PI BASEL PA PICASSOPLATZ 4, BASEL, 4052, SWITZERLAND SN 0020-1812 EI 1420-9098 J9 INSECT SOC JI Insect. Soc. PD MAY PY 2010 VL 57 IS 2 BP 209 EP 215 DI 10.1007/s00040-010-0072-7 PG 7 WC Entomology SC Entomology GA 570CJ UT WOS:000275648900012 ER PT J AU Herrera, F Manchester, SR Jaramillo, C MacFadden, B da Silva-Caminha, SA AF Herrera, Fabiany Manchester, Steven R. Jaramillo, Carlos MacFadden, Bruce da Silva-Caminha, Silane A. TI PHYTOGEOGRAPHIC HISTORY AND PHYLOGENY OF THE HUMIRIACEAE SO INTERNATIONAL JOURNAL OF PLANT SCIENCES LA English DT Article DE fossils; Humiriaceae; phylogeny; morphology; Miocene; Panama ID LOWER MIOCENE COMMUNITIES; NEOTROPICAL PALEOBOTANY; CULEBRA FORMATION; FRENCH-GUIANA; RAIN-FORESTS; PANAMA; COLOMBIA; DISPERSAL; ECOLOGY; AMERICA AB To place a new fossil occurrence of Sacoglottis in a broader context, we surveyed the fruit morphology of all extant genera of the Humiriaceae, conducted a cladistic analysis, and critically reviewed the fossil record for this family. Living and fossil fruits of Humiriaceae are recognized by a woody endocarp, germination valves, and, in some genera, wall cavities. The phylogenetic analysis based on 40 morphological characters yielded two most parsimonious trees indicating Vantanea as sister taxon to all genera among Humiriaceae. Schistostemon is indistinguishable from Sacoglottis in fruit morphology and is recovered as sister to Sacoglottis in the topology; we recommend restoring Schistostemon to the rank of subgenus within Sacoglottis. A review of prior published reports of fossil fruits attributed to Humiriaceae led to the rejection and/or reattribution of some records but supports recognition of Vantanea, Humiria, Humiriastrum, and Sacoglottis. The available characters do not support recognition of multiple fossil species of Sacoglottis. We recognize the occurrence of Sacoglottis tertiaria Berry emend. Herrera from Peru, Ecuador, Colombia, and a newly collected Miocene site from Panama. The Cenozoic fossil record of Humiriaceae in South and Central America, together with discreditation of former reports from Europe, strongly supports a Neotropical origin for this family. C1 [Herrera, Fabiany; Manchester, Steven R.; MacFadden, Bruce] Univ Florida, Florida Museum Nat Hist, Dept Biol, Gainesville, FL 32611 USA. [Herrera, Fabiany; Jaramillo, Carlos; da Silva-Caminha, Silane A.] Smithsonian Trop Res Inst, Panama City, Panama. [MacFadden, Bruce] Natl Sci Fdn, Div Res Learning, EHR DRL, Arlington, VA 22031 USA. RP Herrera, F (reprint author), Univ Florida, Florida Museum Nat Hist, Dept Biol, Gainesville, FL 32611 USA. EM fherrera@flmnh.ufl.edu FU Autoridad del Canal de Panama; University of Florida (UF); National Science Foundation (NSF) [0824299, EF-0431266, OISE-0638810, EAR-0642528, EAR-0824299]; Paleobiology STRI endowment; UF 2007 Research Opportunity Grant FX This research was made possible through the collaboration and funding of the Autoridad del Canal de Panama and R. Perez for donating the Toyota vehicles used in the fieldwork. The work was also supported by a graduate research fellowship of the University of Florida (UF) to F. Herrera; the M. Tupper Fellowship, the National Science Foundation (NSF; grant 0824299), and the Paleobiology STRI endowment to C. Jaramillo; NSF grant EF-0431266 to S. R. Manchester; and a UF 2007 Research Opportunity Grant and NSF grants OISE-0638810, EAR-0642528, and EAR-0824299 to B. MacFadden. We thank C. Montes, N. Strong, M. Carvalho, A. Rincon, and the paleontology team at STRI for help with fieldwork; J. Bloch and J. Chen for help with the cladistic analysis; S. Wing (SI) and V. Wijninga and H. Hooghiemstra (UA) for providing access to the fossil collections; D. Bell (US), C. Galdames (STRI), K. Perkins (FLAS), and F. Gonzalez (UN) for access to modern Humiriaceae collections; D. Jarzen, T. Lott, and E. Moreno for helpful discussions about the systematics of the fossils; and N. Atkins for improving the grammar. F. Herrera thanks B. Himschoot, M. I. Barreto, and family for support. Any opinions, findings, conclusions, or recommendations expressed in this article are those of the authors and do not necessarily reflect the views of the NSF. NR 66 TC 13 Z9 15 U1 1 U2 7 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 MAY PY 2010 VL 171 IS 4 BP 392 EP 408 DI 10.1086/651229 PG 17 WC Plant Sciences SC Plant Sciences GA 583AB UT WOS:000276642000005 ER PT J AU Wilson, S Martin, K AF Wilson, Scott Martin, Kathy TI Variable reproductive effort for two ptarmigan species in response to spring weather in a northern alpine ecosystem SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID LIFE-HISTORY EVOLUTION; WHITE-TAILED PTARMIGAN; WILLOW PTARMIGAN; CLIMATE-CHANGE; CLUTCH SIZE; DIFFERENTIAL MORTALITY; PHENOTYPIC PLASTICITY; GEOGRAPHIC VARIATION; POPULATION-DENSITY; NEST PREDATION AB Predicting how animal populations respond to climate change requires knowledge of how species traits influence the response of individuals to variation in anuual weather. Over a four-year study with two warm and two cold years, we examined how sympatric rock ptarmigan Lagopus muta and white-tailed ptarmigan L. leucura in the southern Yukon Territory respond to spring weather in terms of breeding phenology and the allocation of reproductive effort. The onset of breeding was approximately synchronous; for each one-degree rise in spring temperature, mean breeding dates of rock and white-tailed ptarmigan advanced by about 2.7 and 4 days respectively. Although onset of breeding was similar, the two species differed in their reproductive effort. As breeding was delayed, average first clutch sizes of rock ptarmigan declined from 9.4 to 5.8 eggs over the breeding period, while those of white-tailed ptarmigan only declined from an average of 7.8 to 6.8. Rock ptarmigan were also less likely to re-nest if their first clutch was lost to predators and as a consequence they had shorter breeding seasons. White-tailed ptarmigan produced about 25% more offspring annually than rock ptarmigan and contributed more young through re-nesting. While white-tailed ptarmigan had higher annual reproductive output, adult rock ptarmigan had a 20-25% higher annual survival rate, which may indicate a reproduction-survival trade-off for the two species. These results show that even within the same location, closely related species can differ in how they allocate effort as environmental conditions fluctuate. C1 [Wilson, Scott; Martin, Kathy] Univ British Columbia, Dept Forest Sci, Vancouver, BC V6T 1Z4, Canada. [Martin, Kathy] Environm Canada, Delta, BC V4K 3N2, Canada. RP Wilson, S (reprint author), Smithsonian Migr Bird Ctr, Natl Zool Pk, Washington, DC USA. EM wilsonsd@si.edu FU Pika Camp; Kluane Lake; Natural Sciences and Engineering Research Council of Canada (NSERC) FX We thank P. Arcese, S. Morrison and A. G. Wilson for providing valuable comments on earlier drafts of this manuscript and D. Chalmers, A. Clason, O. Davies, E. Gillis, S. Nouvet, G. Pelchat, S. Trefry and M. Wong for assistance in the field. We also thank D. S. Hik, A. and S. Williams, and L. Goodwin for providing logistical support at Pika Camp and the Arctic Inst. of North America at Kluane Lake. Funding for this research was provided by Natural Sciences and Engineering Research Council of Canada (NSERC; Discovery Grant, Northern Research Supplement, Int. Polar Year) and Environment Canada support to KM, and NSERC Postgraduate Scholarship, Northern Scientific Training Program, British Columbia Upland Birds Society, Calgary Bird Banding Society, UBC Dept of Forestry, and Izaak Walton Killam and Univ. Graduate Fellowships to SW. The use of animals in this research adheres to the ethical standards of Canada as approved by the Univ. of British Columbia Animal Care Committee (permit no. A05-0450). NR 60 TC 14 Z9 15 U1 2 U2 41 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 EI 1600-048X J9 J AVIAN BIOL JI J. Avian Biol. PD MAY PY 2010 VL 41 IS 3 BP 319 EP 326 DI 10.1111/j.1600-048X.2009.04945.x PG 8 WC Ornithology SC Zoology GA 614RI UT WOS:000279077000012 ER PT J AU ter Hofstede, HM Kalko, EKV Fullard, JH AF ter Hofstede, Hannah M. Kalko, Elisabeth K. V. Fullard, James H. TI Auditory-based defence against gleaning bats in neotropical katydids (Orthoptera: Tettigoniidae) SO JOURNAL OF COMPARATIVE PHYSIOLOGY A-NEUROETHOLOGY SENSORY NEURAL AND BEHAVIORAL PHYSIOLOGY LA English DT Article DE Antipredator behaviour; Acoustic startle response; Calling song; Tettigoniidae; Chiroptera ID BUSHCRICKET REQUENA-VERTICALIS; NEOCONOCEPHALUS-ENSIGER; MACROPHYLLUM-MACROPHYLLUM; FEMALE PHONOTAXIS; GUILD STRUCTURE; SONG CESSATION; ACOUSTIC CUES; BUSH-CRICKETS; BEHAVIOR; INSECT AB Neotropical katydids (Orthoptera: Tettigoniidae) are preyed on by gleaning bats, which are known to use male calling songs to locate them. At least one katydid species has been reported to stop singing in response to bat echolocation calls. To investigate the relationship between this behavioural defence and ecological and sensory factors, we surveyed calling song characteristics, song cessation in response to the echolocation calls of a sympatric gleaning bat (Trachops cirrhosus), and T-cell responses (an auditory interneuron sensitive to ultrasound) in five katydid species from Panama. The two katydid species that stopped singing in response to bat calls (Balboa tibialis and Ischnomela gracilis, Pseudophyllinae) also had the highest T-cell spike number and rate in response to these stimuli. The third pseudophylline species (Docidocercus gigliotosi) did not reliably cease singing and had low T-cell spiking activity. Neoconocephalus affinis (Copiphorinae) produced continuous calling song, possibly preventing males from hearing the bat during singing, and did not show a behavioural response despite high T-cell activity in response to bat calls. Steirodon rufolineatum (Phaneropterinae) did not cease singing and differed in T-cell activity compared to the other species. T-cell function might not be conserved in katydids, and evidence for this idea is discussed. C1 [ter Hofstede, Hannah M.] Univ Bristol, Sch Biol Sci, Bristol BS8 1UG, Avon, England. [Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Fullard, James H.] Univ Toronto, Dept Biol, Mississauga, ON L5L 1C6, Canada. RP ter Hofstede, HM (reprint author), Univ Bristol, Sch Biol Sci, Woodland Rd, Bristol BS8 1UG, Avon, England. EM bzhmth@bristol.ac.uk FU Natural Sciences and Engineering Research Council of Canada; Smithsonian Tropical Research Institute FX We thank the staff at the Smithsonian Tropical Research Institute facilities at Barro Colorado Island for their logistical support and assistance, especially Oris Acevedo and Belkys Jimenez. Thanks also to Rachel Page for joint work on the foraging behaviour of Trachops cirrhosus, from which we obtained the echolocation recordings, Peter Wall for the custom MATLAB application, and Negin Amin for data analysis. Funding for this study was provided by the Natural Sciences and Engineering Research Council of Canada (discovery grant to J.H.F and postgraduate scholarship to H.M.tH.) and the Smithsonian Tropical Research Institute (short term fellowship to H.M.tH.). Holger Goerlitz and Brock Fenton provided helpful comments on the manuscript. Experiments described here comply with the "Principles of animal care" publication No. 86-23, revised 1985, of the National Institute of Health, and also with the current laws of the country in which the experiments were performed. NR 55 TC 12 Z9 13 U1 0 U2 15 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0340-7594 J9 J COMP PHYSIOL A JI J. Comp. Physiol. A -Neuroethol. Sens. Neural Behav. Physiol. PD MAY PY 2010 VL 196 IS 5 BP 349 EP 358 DI 10.1007/s00359-010-0518-4 PG 10 WC Behavioral Sciences; Neurosciences; Physiology; Zoology SC Behavioral Sciences; Neurosciences & Neurology; Physiology; Zoology GA 587CL UT WOS:000276964800003 PM 20237786 ER PT J AU Lemaitre, R AF Lemaitre, Rafael TI DARRYL L. FELDER ANNOUNCEMENT RECIPIENT OF THE CRUSTACEAN SOCIETY EXCELLENCE IN RESEARCH AWARD SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Biographical-Item C1 Smithsonian Inst, Dept Invertebrate Zool, Museum Support Ctr, Natl Museum Nat Hist, Suitland, MD 20746 USA. RP Lemaitre, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Museum Support Ctr, Natl Museum Nat Hist, 4210 Silver Hill Rd, Suitland, MD 20746 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU CRUSTACEAN SOC PI SAN ANTONIO PA 840 EAST MULBERRY, SAN ANTONIO, TX 78212 USA SN 0278-0372 J9 J CRUSTACEAN BIOL JI J. Crustac. Biol. PD MAY PY 2010 VL 30 IS 2 BP 340 EP 342 DI 10.1651/09-3238.1 PG 3 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 586MH UT WOS:000276913200021 ER PT J AU Kane, AS Song, J Halvorsen, MB Miller, DL Salierno, JD Wysocki, LE Zeddies, D Popper, AN AF Kane, A. S. Song, J. Halvorsen, M. B. Miller, D. L. Salierno, J. D. Wysocki, L. E. Zeddies, D. Popper, A. N. TI Exposure of fish to high-intensity sonar does not induce acute pathology SO JOURNAL OF FISH BIOLOGY LA English DT Article DE anthropogenic sound; ear; noise; sonar ID ATLANTIC SALMON; RAINBOW-TROUT; SOUND; HEARING; EARS AB This study investigated immediate effects of intense sound exposure associated with low-frequency (170-320 Hz) or with mid-frequency (2.8-3.8 kHz) sonars on caged rainbow trout Oncorhynchus mykiss, channel catfish Ictalurus punctatus and hybrid sunfish Lepomis sp. in Seneca Lake, New York, U. S. A. This study focused on potential effects on inner ear tissues using scanning electron microscopy and on non-auditory tissues using gross and histopathology. Fishes were exposed to low-frequency sounds for 324 or 628 s with a received peak signal level of 193 dB re 1 mu Pa (root mean square, rms) or to mid-frequency sounds for 15 s with a received peak signal level of 210 dB re 1 mu Pa (rms). Although a variety of clinical observations from various tissues and organ systems were described, no exposure-related pathologies were observed. This study represents the first investigation of the effects of high-intensity sonar on fish tissues in vivo. Data from this study indicate that exposure to low and midfrequency sonars, as described in this report, might not have acute effects on fish tissues. (C) 2010 The Authors Journal compilation (C) 2010 The Fisheries Society of the British Isles C1 [Song, J.; Halvorsen, M. B.; Miller, D. L.; Wysocki, L. E.; Zeddies, D.; Popper, A. N.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Song, J.; Halvorsen, M. B.; Miller, D. L.; Wysocki, L. E.; Zeddies, D.; Popper, A. N.] Univ Maryland, Ctr Comparat & Evolutionary Biol Hearing, College Pk, MD 20742 USA. [Song, J.] Smithsonian Inst, Natl Museum Amer Hist, Div Fishes, Washington, DC 20013 USA. [Salierno, J. D.] Fairleigh Dickinson Univ, Dept Biol, Madison, NJ 07940 USA. [Kane, A. S.] Univ Florida, Emerging Pathogens Inst, Gainesville, FL 32610 USA. [Kane, A. S.] Univ Florida, Coll Vet Med, Ctr Environm & Human Toxicol, Gainesville, FL 32611 USA. [Kane, A. S.] Univ Florida, Coll Publ Hlth & Hlth Profess, Dept Environm & Global Hlth, Gainesville, FL 32611 USA. RP Popper, AN (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM apopper@umd.edu FU U.S. Chief of Naval Operations (Undersea Surveillance Branch); U.S. Chief of Naval Operations (Environmental Readiness Division) FX We thank B. Casper and J. Mayer for review of the MS. We are grateful to K. White, J. Michalec and N. Elias and his staff at the U.S. Navy Sonar Test Facility at Seneca Lake for logistic and technical support. We also thank P. Stein, A. Bahlavouni, A. Philips and M. Poston of Scientific Solutions, Inc. for acoustic analyses, design of the test tanks and facilitating the complex operational procedures. Invaluable assistance was provided by individuals from Marine Acoustics, Inc. (MAI), including G. Sisson who provided on-site technical support, C. Spikes who provided logistical support and guidance, and W. Ellison who gave critical insight on underwater acoustics and experimental design. LFA work was supported by the U.S. Chief of Naval Operations (Undersea Surveillance Branch), while MFA work was supported by the U.S. Chief of Naval Operations (Environmental Readiness Division). We are also grateful to J. S. Johnson and V. F. Stone of the Office of the U.S. Chief of Naval Operations for their support of these projects and their trust in the scientific process that resulted in their permitting us to design and conduct the experiments independently, with minimal involvement other than providing the necessary funding. NR 35 TC 12 Z9 12 U1 1 U2 14 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0022-1112 J9 J FISH BIOL JI J. Fish Biol. PD MAY PY 2010 VL 76 IS 7 BP 1825 EP 1840 DI 10.1111/j.1095-8649.2010.02626.x PG 16 WC Fisheries; Marine & Freshwater Biology SC Fisheries; Marine & Freshwater Biology GA 592WU UT WOS:000277413300020 PM 20557634 ER PT J AU DeSilva, JM Zipfel, B Van Arsdale, AP Tocheri, MW AF DeSilva, Jeremy M. Zipfel, Bernhard Van Arsdale, Adam P. Tocheri, Matthew W. TI The Olduvai Hominid 8 foot: Adult or subadult? SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Metatarsals; Epiphyseal fusion; Homo habilis ID HOMO-HABILIS; GENUS HOMO; GORGE; MORPHOLOGY; SKELETON; REMAINS; DMANISI; GEORGIA; BONES AB Olduvai Hominid 8 (OH 8), an articulating set of fossil hominin tarsal and metatarsal bones, is critical to interpretations of the evolution of hominin pedal morphology and bipedal locomotion. It has been suggested that OH 8 may represent the foot of a subadult and may be associated with the OH 7 mandible, the type specimen of Homo habilis. This assertion is based on the presence of what may be unfused distal metatarsal epiphyses. Accurately assessing the skeletal maturity of the OH 8 foot is important for interpretations of the functional morphology and locomotor behavior of Plio-Pleistocene hominins. In this study, we compare metatarsal fusion patterns and internal bone morphology of the lateral metatarsals among subadult hominines (85 modern humans, 48 Pan, and 25 Gorilla) to assess the likelihood that OH 8 belonged to either an adult or subadult hominin. Our results suggest that if OH 8 is indeed from a subadult, then it displays a metatarsal developmental pattern that is unobserved in our comparative sample. In OH 8, the fully fused base of the first metatarsal and the presence of trabecular bone at the distal ends of the second and third metatarsal shafts make it highly improbable that it belonged to a subadult, let alone a subadult that matches the developmental age of the OH 7 mandible. In total, the results of this study suggest that the OH 8 foot most likely belonged to an adult hominin. (C) 2010 Elsevier Ltd. All rights reserved. C1 [DeSilva, Jeremy M.] Boston Univ, Dept Anthropol, Boston, MA 02215 USA. [Zipfel, Bernhard] Univ Witwatersrand, Bernard Price Inst Palaeontol Res, Sch Geosci, Inst Human Evolut, ZA-2050 Wits, South Africa. [Van Arsdale, Adam P.] Wellesley Coll, Dept Anthropol, Wellesley, MA 02181 USA. [Tocheri, Matthew W.] Smithsonian Inst, Human Origins Program, Dept Anthropol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP DeSilva, JM (reprint author), Boston Univ, Dept Anthropol, Boston, MA 02215 USA. EM jdesilva@bu.edu OI Tocheri, Matthew/0000-0001-7600-8998 FU Palaeontological Scientific Trust (PAST); Leakey Foundation FX The authors thank the Tanzanian Commission for Science and Technology, A. Kwekason and P. Msemwa at the National Museum and House of Culture for permission to study the OH 8 foot. We are grateful to D. Lordkipanidze, C. Zollikofer, M. Ponce de Leon, and R. Quam for providing photographs of the Dmanisi and Valdegoba metatarsals. We thank W. Jungers, W.E.H. Harcourt-Smith, J. Njau and B. Pobiner for helpful discussions. Thanks also to the University of the Witwatersrand Fossil Primate Access Committee for permission to study Sterkfontein metatarsals and N. Pather for access to the Raymond Dart collection of human skeletons. Study of original and cast material was made possible thanks to E. Mbua, Y. Haile-Selassie, and M. Morgan. Study of extant material was made possible by J. Chupasko, M. Morgan, C. Zollikofer, M. Ponce de Leon, L Jellema, O. Lovejoy, W. Wendelen, E. Gilissen (RMCA), L Gordon, and R. Thorington (NMNH). Comments by two reviewers and an associate editor helped to improve this paper. Funding was provided by the Palaeontological Scientific Trust (PAST) and the Leakey Foundation. NR 32 TC 6 Z9 6 U1 0 U2 8 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0047-2484 J9 J HUM EVOL JI J. Hum. Evol. PD MAY PY 2010 VL 58 IS 5 BP 418 EP 423 DI 10.1016/j.jhevol.2010.03.004 PG 6 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 608DY UT WOS:000278564000004 PM 20416928 ER PT J AU Zhang, XM Wen, J Dao, ZL Motley, TJ Long, CL AF Zhang, Xue-Mei Wen, Jun Dao, Zhi-Ling Motley, Timothy J. Long, Chun-Lin TI Genetic variation and conservation assessment of Chinese populations of Magnolia cathcartii (Magnoliaceae), a rare evergreen tree from the South-Central China hotspot in the Eastern Himalayas SO JOURNAL OF PLANT RESEARCH LA English DT Article DE Breeding system; Conservation; Fragmentation; Magnolia cathcartii; Gene flow; Genetic diversity ID ALLOZYME VARIATION; EXTINCTION DEBT; NORTH-AMERICA; DIVERSITY; PLANTS; FOREST; DEFORESTATION; CONSEQUENCES; PHYLOGEOGRAPHY; MANAGEMENT AB Nine natural populations of the rare evergreen tree Magnolia cathcartii (Magnoliaceae) were sampled across its natural range, and amplified fragment length polymorphism (AFLP) markers were used to assess genetic variation within and among populations. Three ex situ populations were also surveyed to determine whether conservation plantings include the entire genetic diversity of the species. Genetic diversity within the natural populations was very low (0.122 for Nei's gene diversity), and the southeast populations had the highest diversity. The ex situ populations had a lower diversity than the mean diversity for all populations, and none of the ex situ populations reached the levels of diversity found in their source populations. Genetic differentiation was high among natural populations (G (st) = 0.247), and an isolation-by-distance pattern was detected. Habitat fragmentation, restricted gene flow, and geitonogamy are proposed to be the primary reasons for the low genetic diversity and high genetic differentiation. More protection is needed, especially for the southeast populations, which possess the highest numbers of unique alleles according to AFLP fragment analyses. The ex situ program was a good first step towards preserving this species, but the current ex situ populations preserve only a limited portion of its genetic diversity. Future ex situ efforts should focus on enhancing the plantings with individuals from southeastern Yunnan. C1 [Zhang, Xue-Mei; Dao, Zhi-Ling; Long, Chun-Lin] Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. [Zhang, Xue-Mei] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Amer Hist, Dept Bot, Washington, DC 20013 USA. [Motley, Timothy J.] Old Dominion Univ, Dept Biol Sci, Norfolk, VA 23529 USA. [Motley, Timothy J.; Long, Chun-Lin] Cent Univ Nationalities, Coll Life & Environm Sci, Beijing 100081, Peoples R China. RP Long, CL (reprint author), Chinese Acad Sci, Kunming Inst Bot, Kunming 650204, Yunnan, Peoples R China. EM long@mail.kib.ac.cn OI Long, Chunlin/0000-0002-6573-6049 FU Ministry of Education of China [B08044, CUN 985-3-3]; Ministry of Science and Technology of China [2005DKA21006]; USA National Science Foundation [DEB-0103795]; Chinese Academy of Sciences FX This work was supported by the Ministry of Education of China through its 111 Project (B08044, CUN 985-3-3), the Ministry of Science and Technology of China (2005DKA21006), the USA National Science Foundation (DEB-0103795), and the Knowledge Innovation Program of the Chinese Academy of Sciences. The authors thank Dr. Hong-Guang Zha and Dr. Yong-Hong Zhang for helpful suggestions during the experiments, Dr. Hong-Tao Li and Dr. Ying-Xiong Qiu for assistance in data analysis, and Dr. Xue-Fei Yang for providing the base map for Fig. 1. NR 82 TC 5 Z9 6 U1 0 U2 21 PU SPRINGER TOKYO PI TOKYO PA 1-11-11 KUDAN-KITA, CHIYODA-KU, TOKYO, 102-0073, JAPAN SN 0918-9440 J9 J PLANT RES JI J. Plant Res. PD MAY PY 2010 VL 123 IS 3 BP 321 EP 331 DI 10.1007/s10265-009-0278-9 PG 11 WC Plant Sciences SC Plant Sciences GA 587WE UT WOS:000277025000009 PM 20037748 ER PT J AU Baird, KE Funk, VA Wen, J Weeks, A AF Baird, Kristen E. Funk, Vicki A. Wen, Jun Weeks, Andrea TI Molecular phylogenetic analysis of Leibnitzia Cass. (Asteraceae: Mutisieae: Gerbera-complex), an Asian-North American disjunct genus SO JOURNAL OF SYSTEMATICS AND EVOLUTION LA English DT Article DE Beringia; biogeography; Gerbera-complex; Mutisieae ID NUCLEAR RIBOSOMAL DNA; COMPOSITAE; HISTORY; PLANTS; EVOLUTION; TAXONOMY AB Leibnitzia comprises six species of perennial herbs that are adapted to high elevation conditions and is one of only two Asteraceae genera known to have an exclusively disjunct distribution spanning central to eastern Asia and North America. Molecular phylogenetic analysis of Leibnitzia and other Gerbera-complex members indicates that Leibnitzia is monophyletic, which is in contrast with our expectation that the American Leibnitzia species L. lyrata and L. occimadrensis would be more closely related to another American member of the Gerbera-complex, namely Chaptalia. Ancestral area reconstructions show that the historical biogeography of the Gerbera-complex mirrors that of the entire Asteraceae, with early diverging lineages located in South America that were followed by transfers to Africa and Eurasia and, most recently, to North America. Intercontinental transfer of Leibnitzia appears to have been directed from Asia to North America. Independent calibrations of nuclear (ribosomal DNA internal transcribed spacer region) and chloroplast (trnL-rpl32 intron) DNA sequence data using relaxed clock methods and either mean rate or fossil-based priors unanimously support Miocene and younger divergence times for Gerbera-complex taxa. The ages are not consistent with most Gondwanan vicariance episodes and, thus, the global distribution of Gerbera-complex members must be explained in large part by long-distance dispersal. American species of Leibnitzia are estimated to have diverged from their Asian ancestor during the Quaternary (ca. 2 mya) and either migrated overland to North America via Beringia and retreated southwards along high elevation corridors to their present location in southwestern North America or were dispersed long distance. C1 [Baird, Kristen E.; Weeks, Andrea] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Funk, Vicki A.; Wen, Jun] US Natl Herbarium, Smithsonian Inst, MRC 166, Washington, DC 20013 USA. RP Weeks, A (reprint author), George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. EM aweeks3@gmu.edu OI Weeks, Andrea/0000-0002-0000-4541 NR 42 TC 15 Z9 15 U1 1 U2 4 PU WILEY PERIODICALS, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN STREET, MALDEN, MA 02148-529 USA SN 1674-4918 J9 J SYST EVOL JI J. Syst. Evol. PD MAY PY 2010 VL 48 IS 3 BP 161 EP 174 DI 10.1111/j.1759-6831.2010.00077.x PG 14 WC Plant Sciences SC Plant Sciences GA 601SW UT WOS:000278085400002 ER PT J AU Thompson, JR Spies, TA AF Thompson, Jonathan R. Spies, Thomas A. TI Factors associated with crown damage following recurring mixed-severity wildfires and post-fire management in southwestern Oregon SO LANDSCAPE ECOLOGY LA English DT Article DE Burn mosaic; Reburn; Salvage logging; Burn severity; Biscuit Fire ID SUB-ALPINE FORESTS; KLAMATH MOUNTAINS; FIRE SEVERITY; EVERGREEN FOREST; BURN SEVERITY; LANDSAT TM; CALIFORNIA; LANDSCAPE; FUELS; USA AB Wildfires and post-fire logging and planting have a lasting influence on the quantity and arrangement of live and dead vegetation, which can, in turn, affect the behavior of future fires. In 2002, the Biscuit Fire re-burned 38,000 ha of mixed-conifer/evergreen hardwood forest in southwestern Oregon that had burned heterogeneously during the 1987 Silver Fire and then was subject, in part, to post-fire logging and planting. We measured vegetation cover and crown damage from at temporal sequence (1987, 2000, and 2002) of digital aerial photo-plots (plot size = 6.25 ha) within managed and unmanaged portions of the twice-burned landscape. We estimated the strength and nature of relationships between crown damage in the two fires while also accounting for the influence of several vegetation, topographic, weather, and management variables. On average, unmanaged plots within the reburn area had 58% of their live crown cover scorched or consumed by the Biscuit Fire (median = 64%). The level of re-burn crown damage was strongly related to the level of crown damage during the Silver Fire. Typically, the areas that burned severely in the Silver Fire succeeded to a mix of shrubs and tree regeneration (i.e. shrub-stratum vegetation), which then experienced high levels of Biscuit Fire damage. In contrast, the level of tree-stratum damage in the Biscuit Fire was largely independent of Silver Fire damage. Within plots that were salvage-logged then planted after the Silver Fire, on average 98% of the vegetation cover was damaged by the Biscuit Fire (median = 100%). Within the plots that experienced complete crown damage in the Silver Fire but were left unmanaged, on average 91% of the vegetation cover was damaged by the Biscuit Fire (median = 95%). Our findings suggest that in productive fire-prone landscapes, a post-fire mosaic of young regenerating vegetation can influence the pattern of crown damage in future wildfires. C1 [Thompson, Jonathan R.] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Thompson, Jonathan R.] Oregon State Univ, Dept Forest Sci, Corvallis, OR 97331 USA. [Spies, Thomas A.] US Forest Serv, Pacific NW Res Stn, USDA, Corvallis, OR 97330 USA. RP Thompson, JR (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM thompsonjr@si.edu; tspies@fs.fed.us FU Joint Fire Science Program FX This project was funded by the Joint Fire Science Program. We thank Keith Olsen and Duck Creek Inc for technical help and Jessica Halofsky, Tom Atzet, Warren Cohen, and Rick Miller for helpful comments on an earlier draft. NR 57 TC 30 Z9 30 U1 2 U2 29 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0921-2973 J9 LANDSCAPE ECOL JI Landsc. Ecol. PD MAY PY 2010 VL 25 IS 5 BP 775 EP 789 DI 10.1007/s10980-010-9456-3 PG 15 WC Ecology; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 582PK UT WOS:000276609800009 ER PT J AU Bullock, ES McKeegan, KD Gounelle, M Grady, MM Russell, SS AF Bullock, Emma S. McKeegan, Kevin D. Gounelle, Matthieu Grady, Monica M. Russell, Sara S. TI Sulfur isotopic composition of Fe-Ni sulfide grains in CI and CM carbonaceous chondrites SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MASS-INDEPENDENT SULFUR; AQUEOUS ALTERATION; ALLENDE METEORITE; MINERALOGY; ABUNDANCE; SULFATE; MATRIX; CONSTRAINTS; COMPONENTS; ASTEROIDS AB In situ secondary ion mass spectrometry analyses of 32S, 33S, and 34S in iron-nickel sulfide grains in two CI1 chondrites and six CM chondrites were performed. The results show a wider range of both enrichment and depletion in delta 34S relative to troilite from the Canyon Diablo meteorite (CDT) than has been observed in previous studies. All data points lie within error of a single mass dependent fractionation line. Sulfides from CI1 chondrites show delta 34S(CDT) from -0.7 to 6.8 parts per thousand, while sulfide grains in the CM1 chondrite are generally depleted in heavy sulfur relative to CDT (delta 34S from -2.9 to 1.8 parts per thousand). CM2 chondrites contain sulfide grains that show enrichment and depletion in 34S (delta 34S(CDT) from -7.0 to 6.8 parts per thousand). Sulfates forming from sulfide grains during aqueous alteration on the chondrite parent body are suggested to concentrate light sulfur, leaving the remaining sulfide grains enriched in the heavy isotopes of sulfur. The average degree of enrichment in 34S in CM chondrite sulfides is broadly consistent with previously suggested alteration sequences. C1 [Bullock, Emma S.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [McKeegan, Kevin D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [Gounelle, Matthieu] CNRS, LMCM, F-75005 Paris, France. [Gounelle, Matthieu] Museum Natl Hist Nat, UMR 7202, F-75005 Paris, France. [Grady, Monica M.] Open Univ, Milton Keynes MK7 7AA, Bucks, England. [Grady, Monica M.; Russell, Sara S.] Nat Hist Museum, Dept Mineral, London SW7 5BD, England. RP Bullock, ES (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM bullocke@si.edu RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011; OI McKeegan, Kevin/0000-0002-1827-729X; Grady, Monica/0000-0002-4055-533X FU STFC; NASA; NSF FX The authors would like to thank Dr. Adrian Brearley and an anonymous reviewer for their thoughtful and thorough reviews, which greatly improved the manuscript. Financial assistance was provided by STFC (formerly PPARC) and NASA. The UCLA ion microprobe laboratory is partially supported by a grant from the NSF Instrumentation and Facilities Program. NR 53 TC 16 Z9 16 U1 0 U2 7 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD MAY PY 2010 VL 45 IS 5 BP 885 EP 898 DI 10.1111/j.1945-5100.2010.01052.x PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 648TB UT WOS:000281715900010 ER PT J AU Miller, SE Helgen, LE Hebert, PDN AF Miller, Scott E. Helgen, Lauren E. Hebert, Paul D. N. TI Clarification of the identity of Homona salaconis (Lepidoptera: Tortricidae) (vol 7, pg 549, 2007) SO MOLECULAR ECOLOGY RESOURCES LA English DT Correction C1 [Miller, Scott E.; Helgen, Lauren E.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Hebert, Paul D. N.] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. RP Miller, SE (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RI Hebert, Paul/C-4161-2013; OI Hebert, Paul/0000-0002-3081-6700; Miller, Scott/0000-0002-4138-1378 FU FIC NIH HHS [U01 TW006671-05] NR 6 TC 0 Z9 0 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD MAY PY 2010 VL 10 IS 3 BP 580 EP 580 DI 10.1111/j.1755-0998.2010.02836.x PG 1 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 579WI UT WOS:000276407300024 PM 25152771 ER PT J AU Han, KL Robbins, MB Braun, MJ AF Han, Kin-Lan Robbins, Mark B. Braun, Michael J. TI A multi-gene estimate of phylogeny in the nightjars and nighthawks (Caprimulgidae) SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Caprimulgidae; Nightjars; Nighthawks; Molecular phylogeny; Cytochrome b; c-myc; Growth hormone; Convergence; Sexual selection; Evolution; Indels; Non-coding DNA ID LENGTH DIFFERENCE TEST; MYC GENE; C-MYC; INCONGRUENCE; SEQUENCE; AVES; VERTEBRATES; EVOLUTION; BIRDS; CONSERVATION AB Caprimulgidae is a cosmopolitan family of nocturnal and crepuscular insectivorous birds comprising the nightjars, nighthawks, and relatives. Sexual selection and convergence or parallelism in plumage and behavior have made it difficult to discern evolutionary relationships in this group. In order to provide a framework for comparative studies of this family, a molecular phylogeny was reconstructed using mitochondrial cytochrome b, and nuclear c-myc and growth hormone DNA sequences. Likelihood, parsimony and Bayesian analyses agree in placing Eurostopodus species and Caprimulgus enarratus, a Malagasy endemic, as the earliest branches of the tree. The remaining taxa are divided among four well-supported clades, three in the New World and one in the Old World. Insertion/deletion events, common in non-coding sequences, provide additional support in resolving the phylogeny. Neither of the traditional subfamilies, Caprimulginae (nightjars) and Chordeilinae (nighthawks), is monophyletic, suggesting that the morphological specializations characterizing "nighthawks" evolved multiple times and the "nightjar" body plan is an old and conservative one. The large genus Caprimulgus is polyphyletic with respect to many other genera in the family, which are often defined by derived plumage traits that likely reflect sexual selection or ecological specialization. A taxonomic revision of the family is proposed based on the combined tree, including naming a new genus for C. enarratus. (C) 2010 Elsevier Inc. All rights reserved. C1 [Han, Kin-Lan] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Han, Kin-Lan; Braun, Michael J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Suitland, MD 20746 USA. [Han, Kin-Lan; Braun, Michael J.] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20740 USA. [Robbins, Mark B.] Univ Kansas, Nat Hist Museum, Div Ornithol, Lawrence, KS 66045 USA. [Robbins, Mark B.] Biodivers Inst, Lawrence, KS 66045 USA. RP Han, KL (reprint author), Univ Florida, Dept Biol, POB 118525, Gainesville, FL 32611 USA. EM hankin@ufl.edu RI Han, Kin-Lan/G-7121-2011 FU US National Science Foundation [DEB-0228675, DEB-0228682] FX We thank J. Hunt, C. Huddleston, and T. Yuri for assistance in the laboratory, E. Braun, R. Kimball and an anonymous reviewer for constructive comments on early drafts of this manuscript, G. Barrowclough for access to the AMNH skin collection, the institutions and collectors listed in Appendix A for providing tissue samples and S. Birks, R. Brumfield, J. Dean, D. Dittman, L. Joseph, S. Hackett, J. Hinshaw, C. Huddleston, J. Klicka, D. Mindell, J. Norman, S. Reddy, F. Sheldon, A. Navarro-Sigtienza, P. Sweet, and D. Willard who facilitated their transfer. C. Mitter and R. Highton provided advice and insight throughout the course of the study. D.W. Steadman provided advice on caprimulgiform fossils, made comments on the manuscript and suggested the name Gactornis. Computer resources were provided by the Lattice Project at University of Maryland and the Fisher Bioinformatics Cluster at the University of Florida Genetics Institute. This work was supported by the US National Science Foundation Assembling the Tree of Life Program Grants DEB-0228675 (Smithsonian) and DEB-0228682 (University of Florida). NR 59 TC 15 Z9 16 U1 1 U2 19 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 MAY PY 2010 VL 55 IS 2 BP 443 EP 453 DI 10.1016/j.ympev.2010.01.023 PG 11 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 586BH UT WOS:000276875300009 PM 20123032 ER PT J AU Peterson, PM Romaschenko, K Johnson, G AF Peterson, Paul M. Romaschenko, Konstantin Johnson, Gabriel TI A classification of the Chloridoideae (Poaceae) based on multi-gene phylogenetic trees SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Biogeography; Classification; Chloridoideae; Grasses; Molecular systematics; Phylogenetic trees; Poaceae ID GRASS FAMILY POACEAE; C-4 PHOTOSYNTHESIS; SEQUENCE DATA; MATK SEQUENCES; NEW-WORLD; MOLECULAR PHYLOGENY; ERAGROSTIS POACEAE; 1ST RECORD; NUCLEAR; DNA AB We conducted a molecular phylogenetic study of the subfamily Chloridoideae using six plastid DNA sequences (ndhA intron, ndhF, rps16-trnK, rps16 intron, rps3, and rpl32-trnL) and a single nuclear ITS DNA sequence. Our large original data set includes 246 species (17.3%) representing 95 genera (66%) of the grasses currently placed in the Chloridoideae. The maximum likelihood and Bayesian analysis of DNA sequences provides strong support for the monophyly of the Chloridoideae; followed by, in order of divergence: a Triraphideae clade with Neyraudia sister to Triraphis; an Eragrostideae clade with the Cotteinae (includes Cottea and Enneapogon) sister to the Uniolinae (includes Entoplocamia, Tetrachne, and Uniola), and a terminal Eragrostidinae clade of Ectrosia, Harpachne, and Psammagrostis embedded in a polyphyletic Eragrostis; a Zoysieae clade with Urochondra sister to a Zoysiinae (Zoysia) clade, and a terminal Sporobolinae clade that includes Spartina, Calamovilfa, Pogoneura, and Crypsis embedded in a polyphyletic Sporobolus: and a very large terminal Cynodonteae clade that includes 13 monophyletic subtribes. The Cynodonteae includes, in alphabetical order: Aeluropodinae (Aeluropus); Boutelouinae (Bouteloua); Eleusininae (includes Apochiton, Astrebla with Schoenefeldia embedded, Austrochloris, Brachyachne, Chloris, Cynodon with Brachyachne embedded in part, Eleusine, Enteropogon with Eustachys embedded in part, Eustachys, Chrysochloa, Coelachyrum, Leptochloa with Dinebra embedded, Lepturus, Lintonia, Microchloa, Saugetia, Schoenefeldia, Sclerodactylon, Tetrapogon, and Trichloris); Hilariinae (Hilaria); Monanthochloinae (includes Distichlis, Monanthochloe, and Reederochloa); Muhlenbergiinae (Muhlenbergia with Aegopogon, Bealia, Blepharoneuron, Chaboissaea, Lycurus, Pereilema, Redfieldia, Schaffnerella, and Schedonnardus all embedded); Orcuttiinae (includes Orcuttia and Tuctoria); Pappophorinae (includes Neesiochloa and Pappophorum); Scleropogoninae (includes Blepharidachne, Dasyochloa, Erioneuron, Munroa, Scleropogon, and Swallenia); Traginae (Tragus with Monelytrum, Polevansia, and Willkommia all embedded); Tridentinae (includes Gouinia, Tridens, Triplasis, and Vaseyochloa); Triodiinae (Triodia); and the Tripogoninae (Melanocenchris and Tripogon with Eragrostiella embedded). In our study the Cynodonteae still include 19 genera and the Zoysieae include a single genus that are not yet placed in a subtribe. The tribe Triraphideae and the subtribe Aeluropodinae are newly treated at that rank. We propose a new tribal and subtribal classification for all known genera in the Chloridoideae. The subfamily might have originated in Africa and/or Asia since the basal lineage, the Triraphideae, includes species with African and Asian distribution. Published by Elsevier Inc. C1 [Peterson, Paul M.] Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, Washington, DC 20013 USA. [Romaschenko, Konstantin] CSIC ICUB, Bot Inst Barcelona, Barcelona 08038, Spain. [Johnson, Gabriel] Smithsonian Inst, Dept Bot, Suitland, MD 20746 USA. [Johnson, Gabriel] Smithsonian Inst, Labs Analyt Biol, Suitland, MD 20746 USA. RP Peterson, PM (reprint author), Smithsonian Inst, Natl Museum Nat Hist, MRC 166, Dept Bot, 10th & Constitut Ave NW, Washington, DC 20013 USA. EM peterson@si.edu RI Romaschenko, Konstantin/K-3096-2014 OI Romaschenko, Konstantin/0000-0002-7248-4193 FU National Geographic Society Committee for Research and Exploration [8087-06]; Smithsonian Institution's, Restricted Endowments Fund; Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation; Biodiversity Surveys and Inventories Program; Laboratory of Analytical Biology FX We thank the National Geographic Society Committee for Research and Exploration(Grant No. 8087-06) for field and laboratory support; the Smithsonian Institution's, Restricted Endowments Fund, the Scholarly Studies Program, Research Opportunities, Atherton Seidell Foundation, Biodiversity Surveys and Inventories Program, Small Grants Program, and the Laboratory of Analytical Biology, all for financial support. We would also like to acknowledge Lee Weigt, Jeffery Hunt, and David Erickson for help in the laboratory; Robert J. Soreng, Jeffery M. Saarela, Carol R. Annable, and Nancy F. Refulio Rodriguez for accompanying the first author on numerous field expeditions; Robert J. Soreng for many extended discussions pertinent to the manuscript; and Robert J. Soreng and an anonymous reviewer for providing helpful comments on the manuscript. NR 98 TC 73 Z9 81 U1 2 U2 34 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 MAY PY 2010 VL 55 IS 2 BP 580 EP 598 DI 10.1016/j.ympev.2010.01.018 PG 19 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 586BH UT WOS:000276875300020 PM 20096795 ER PT J AU Zanol, J Halanych, KM Struck, TH Fauchald, K AF Zanol, Joana Halanych, Kenneth M. Struck, Torsten H. Fauchald, Kristian TI Phylogeny of the bristle worm family Eunicidae (Eunicida, Annelida) and the phylogenetic utility of noncongruent 16S, COI and 18S in combined analyses SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Eunicidae; Annelida; 16S; COI; 18S; Combined analyses; Phylogenetic utility; Phylogenetic signal; PABA; Bootstrap variation; Heterochrony; Antennae; Palps ID MULTIPLE SEQUENCE ALIGNMENT; MOLECULAR PHYLOGENY; INCOMPLETE TAXA; BAYES FACTORS; EVOLUTION; RECONSTRUCTION; POLYCHAETA; BOOTSTRAP; ACCURACY; PROGENESIS AB The bristleworm family Eunicidae is distributed worldwide and well-known for the large size of many of its species, its hard jaws and its economic importance in the bait industry. Monophyly of Eunicidae has been contradicted in previous molecular and morphological phylogenetic analyses focusing on Eunicida or on its type genus, Eunice. The current study focused on the phylogeny of the family per se combining mitochondrial and nuclear genes in different analyses. It recovered well-resolved phylogenetic hypotheses supporting the monophyly of Eunicidae and Palola, the only monophyletic genus among the genera for which we tested their monophyly (Eunice, Marphysa, Palola, Lysidice and Nematonereis). Four other stable clades containing the type species of different genera, or species deemed very similar to them, were recovered within Eunicidae. These clades may represent monophyletic redefinitions of current genera, except for Eunice, and of previous synonymized genera. Evolution of the number of peristomial cirri and prostomial appendages in Eunicidae happened by independent step-by-step reduction in the opposite order of their ontogenetic development, suggestive of sequential heterochrony. All three genes were informative, however, at different levels within the combined trees. 16S and COI were important in recovering a monophyletic Eunicidae and relationships within the family, while 18S was important in the resolution of basal eunicidan relationships, monophyly of Onuphidae and basal relationships within this family. Moreover, results of congruence tests (SH and WRST using PABA) indicate that hidden support is picked up in the combined analyses, which is not revealed in the single gene analyses. Further supporting the idea that congruence is not a requirement for combining different partitions. (C) 2009 Elsevier Inc. All rights reserved. C1 [Zanol, Joana] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Zanol, Joana; Fauchald, Kristian] Natl Museum Nat Hist, Dept Invertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. [Halanych, Kenneth M.] Auburn Univ, Dept Life Sci, Auburn, AL 36849 USA. [Struck, Torsten H.] Univ Osnabruck, AG Zool, Biol Chem FB05, D-49076 Osnabruck, Germany. RP Zanol, J (reprint author), Univ Fed Rio de Janeiro, Inst Biol, Dept Genet, Ilha Fundao, Av Prof Rodolpho Paulo Rocco S-N CCS,Bloco A,A2-0, BR-21941617 Rio De Janeiro, Brazil. EM jzanol@gwmail.gwu.edu; halankm@auburn.edu; Struck@biologie.uni-osnabrueck.de; Fauchald@si.edu RI Halanych, Ken/A-9480-2009; Zanol, Joana/J-6263-2016 OI Halanych, Ken/0000-0002-8658-9674; Zanol, Joana/0000-0002-2178-791X FU NSF [0508819, EAR-0120646]; Cosmos Club FX We are greatly thankful to Diana L. Lipscomb, Allen G. Collins, Sheri A. Church, James M. Clark, Gustavo Hormiga, Fernando Alvarez, M. Rosario Castaneda, Vinita Gowda, Lara Lopardo, Dimitar Dimitrov, Christoph Bleidorn, Tiago B. Quental, Omar Torres-Carvajal and Kevin de Queiroz for their contribution at different phases of this study. Many thanks to all the staff in Invertebrate Zoology Department (NMNH, Smithsonian Institution), Heather Blasczyk, all other members of Halanych's lab in the Spring 2005, Lee Weight, Jeff Hunt, Jeff Bates and all other members of the LAB (NMNH, Smithsonian Institution) for the help with lab work; M. Teresa Aguado, Christos Arvanitidis, Nicola Bettoso, Luis F. Carre-ra-Parra, Maria Cristina Gambi, Chris Glasby, Stephane Hourdez, Ceri Lewis, Eduardo Lopez, Anderson E.S. Oliveira, Julio Parapar, Fredrik Pleijel and Anja Schulze for the donation of specimens; and Leslie H. Harris, Bruno Pernet, Shelly Walther, David E. Montagne, John, all the staff in the July 2004 monitoring cruise of the County Sanitation District of Los Angeles County, Rosebel C. Nales-so, Wilson Franklin Junior, Rossana Sousa, Tatiane Martins Garcia, Flavia Mochel, Jane, Luiz, other UFMA undergraduate students, Martin Christoffersen, Andre Souza, Geoff Keel for the help during field work. This research was funded by a NSF Doctoral Dissertation Improvement Grant (Award #0508819), NSF-WormNet grant (EAR-0120646) and a Cosmos Club Grants-in-Aid of research. Contribution #61 to the AU Marine Biology Program. NR 72 TC 27 Z9 32 U1 1 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD MAY PY 2010 VL 55 IS 2 BP 660 EP 676 DI 10.1016/j.ympev.2009.12.024 PG 17 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 586BH UT WOS:000276875300027 PM 20040377 ER PT J AU den Tex, RJ Thorington, R Maldonado, JE Leonard, JA AF den Tex, Robert-Jan Thorington, Richard Maldonado, Jesus E. Leonard, Jennifer A. TI Speciation dynamics in the SE Asian tropics: Putting a time perspective on the phylogeny and biogeography of Sundaland tree squirrels, Sundasciurus SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cytochrome b; Fib6; c-myc; FTH; POR; GBG; HMG1; Sunda shelf; Pleistocene species pump; Molecular dating; RY coding ID CYTOCHROME-B GENE; MOLECULAR PHYLOGENY; SOUTHEAST-ASIA; BIODIVERSITY HOTSPOTS; FRUIT BATS; EVOLUTION; ARCHIPELAGO; POPULATION; SEQUENCES; HISTORY AB Tropical rainforests are well known for their extraordinarily high levels of biodiversity. The origin of this species richness is still debated. For instance, the museum hypothesis states that over evolutionary time more and more species will accumulate with relatively few extinctions. In contrast, the Pleistocene diversification model argues that during the last 2 million years, climatic factors (glaciations) caused environmental changes that drove isolation and vicariant speciation events. In this study, we construct a molecular phylogeny of the Sundaland (Malay Peninsula, Sumata, Borneo, Palawan) and Greater Mindanao (Mindanao, Samar, Leyte) tree squirrels (genus Sundasciurus). Our results show that most speciation events in this forest dependent taxon occurred before the Pleistocene and that even the timing of intra-specific splits among populations from different landmasses are relatively old. Additionally, we found unexpectedly high divergence within and between highland populations of S. tenuis on Sumatra and the Malay Peninsula, highlighting the importance of Pliocene events in both speciation and within species divergences in this region. (C) 2010 Elsevier Inc. All rights reserved. C1 [den Tex, Robert-Jan; Leonard, Jennifer A.] Uppsala Univ, Dept Evolutionary Biol, S-75236 Uppsala, Sweden. [Thorington, Richard; Maldonado, Jesus E.] Natl Museum Nat Hist, Dept Vertebrate Zool, Smithsonian Inst, Washington, DC 20013 USA. [Maldonado, Jesus E.; Leonard, Jennifer A.] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Leonard, Jennifer A.] Estac Biol Donana CSIC, Seville 41092, Spain. RP Leonard, JA (reprint author), Uppsala Univ, Dept Evolutionary Biol, Norbyvagen 18D, S-75236 Uppsala, Sweden. EM JLeonard@ebd.csic.es RI CSIC, EBD Donana/C-4157-2011; Leonard, Jennifer/A-7894-2010 OI CSIC, EBD Donana/0000-0003-4318-6602; Leonard, Jennifer/0000-0003-0291-7819 FU Smithsonian Restricted Endowment Walcott Fund; Swedish Research Council FX The authors thank Larry Heaney for providing tissue samples and advice. Andrew Rivara and Lauren Helgen helped with DNA sequencing of tissue samples. Dr. Tabitha Viner, The National Zoological Park (Smithsonian Institution), Department of Pathology, provided zoo tissue samples. Samples were kindly provided by The National Museum of Natural History, Smithsonian Institution, Washington DC; The Field Museum, Chicago; The Museum of Vertebrate Zoology, Berkeley; The British Museum of Natural History, London; and NNM 'Naturalis' (formerly Rijksmuseum van Natuurlijke Historie), Leiden, The Netherlands. This project was funded by the Smithsonian Restricted Endowment Walcott Fund and the Swedish Research Council. Logistical support was provided by the Center for Conservation and Evolutionary Genetics, National Zoological Park, Smithsonian Institution, USA. NR 48 TC 24 Z9 24 U1 0 U2 32 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 MAY PY 2010 VL 55 IS 2 BP 711 EP 720 DI 10.1016/j.ympev.2009.12.023 PG 10 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 586BH UT WOS:000276875300031 PM 20040379 ER PT J AU Wildt, DE Comizzoli, P Pukazhenthi, B Songsasen, N AF Wildt, David E. Comizzoli, Pierre Pukazhenthi, Budhan Songsasen, Nucharin TI Lessons From Biodiversity-The Value of Nontraditional Species to Advance Reproductive Science, Conservation, and Human Health SO MOLECULAR REPRODUCTION AND DEVELOPMENT LA English DT Review ID IN-VITRO FERTILIZATION; ARTIFICIAL-INSEMINATION; YELLOW SEAHORSE; DOMESTIC CAT; CANIS-LUPUS; OOCYTES; IMPACT; SPERM; TECHNOLOGIES; VERTEBRATES AB Reproduction is quintessential to species survival But what is underappreciated for this discipline is the wondrous array of reproductive mechanisms among species-variations as diverse as the morphology of the species themselves (more than 55,000 vertebrate and 1 1 million invertebrate types) We have investigated only a tiny fraction of these species in reproductive science. Besides the need to fill enormous gaps in a scholarly database, this knowledge has value for recovering and genetically managing rare species as well as addressing certain reproductive issues in humans This article provides examples, first to advise against oversimplifying reproduction and then to show how such knowledge can have practical use for managing whole animals, populations, or even saving an entire species We also address the expected challenges and opportunities that could lead to creative shifts in philosophy and effective actions to benefit more species as well as a future generation of reproductive scientists C1 [Wildt, David E.; Comizzoli, Pierre; Pukazhenthi, Budhan; Songsasen, Nucharin] Conservat & Res Ctr, Ctr Species Survival, Dept Reprod Sci, Front Royal, VA 22630 USA. RP Wildt, DE (reprint author), Conservat & Res Ctr, Ctr Species Survival, Dept Reprod Sci, Smithsonians Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. FU NIH HHS [R01 OD010948] NR 91 TC 41 Z9 41 U1 2 U2 17 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1040-452X J9 MOL REPROD DEV JI Mol. Reprod. Dev. PD MAY PY 2010 VL 77 IS 5 BP 397 EP 409 DI 10.1002/mrd.21137 PG 13 WC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology SC Biochemistry & Molecular Biology; Cell Biology; Developmental Biology; Reproductive Biology GA 580FU UT WOS:000276433900005 PM 19967718 ER PT J AU Miller, AA Silverman, JM Butler, NR Bloom, JS Chornock, R Filippenko, AV Ganeshalingam, M Klein, CR Li, W Nugent, PE Smith, N Steele, TN AF Miller, A. A. Silverman, J. M. Butler, N. R. Bloom, J. S. Chornock, R. Filippenko, A. V. Ganeshalingam, M. Klein, C. R. Li, W. Nugent, P. E. Smith, N. Steele, T. N. TI SN 2008iy: an unusual Type IIn Supernova with an enduring 400-d rise time SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE circumstellar matter; stars: mass-loss; supernovae: general; supernovae: individual: SN 2008iy; supernovae: individual: SN 1988Z ID MASSIVE STAR; ETA-CARINAE; SKY SURVEY; P-CYGNI; CIRCUMSTELLAR INTERACTION; LUMINOUS SUPERNOVA; INFRARED-EMISSION; OPTICAL-SPECTRA; DATA RELEASE; CLUMPY WIND AB We present spectroscopic and photometric observations of the Type IIn supernova (SN) 2008iy. SN 2008iy showed an unprecedentedly long rise time of similar to 400 d, making it the first known SN to take significantly longer than 100 d to reach peak optical luminosity. The peak absolute magnitude of SN 2008iy was M-r approximate to -19.1 mag, and the total radiated energy over the first similar to 700 d was similar to 2 x 1050 erg. Spectroscopically, SN 2008iy is very similar to the Type IIn SN 1988Z at late times and, like SN 1988Z, it is a luminous X-ray source (both SNe had an X-ray luminosity L-X > 10(41) erg s(-1)). SN 2008iy has a growing near-infrared excess at late times similar to several other SNe IIn. The Ha emission-line profile of SN 2008iy shows a narrow P Cygni absorption component, implying a pre-SN wind speed of similar to 100 km s(-1). We argue that the luminosity of SN 2008iy is powered via the interaction of the SN ejecta with a dense, clumpy circumstellar medium. The similar to 400-d rise time can be understood if the number density of clumps increases with distance over a radius similar to 1.7 x 10(16) cm from the progenitor. This scenario is possible if the progenitor experienced an episodic phase of enhanced mass loss <1 century prior to explosion or if the progenitor wind speed increased during the decades before core collapse. We favour the former scenario, which is reminiscent of the eruptive mass-loss episodes observed for luminous blue variable (LBV) stars. The progenitor wind speed and increased mass-loss rates serve as further evidence that at least some, and perhaps all, Type IIn SNe experience LBV-like eruptions shortly before core collapse. We also discuss the host galaxy of SN 2008iy, a subluminous dwarf galaxy, and offer a few reasons why the recent suggestion that unusual, luminous SNe preferentially occur in dwarf galaxies may be the result of observational biases. C1 [Miller, A. A.; Silverman, J. M.; Butler, N. R.; Bloom, J. S.; Chornock, R.; Filippenko, A. V.; Ganeshalingam, M.; Klein, C. R.; Li, W.; Smith, N.; Steele, T. N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nugent, P. E.] Univ Calif Berkeley, Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Miller, AA (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. EM amiller@astro.berkeley.edu NR 97 TC 27 Z9 28 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2010 VL 404 IS 1 BP 305 EP 317 DI 10.1111/j.1365-2966.2010.16280.x PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 584ZU UT WOS:000276794600052 ER PT J AU Richard, J Smith, GP Kneib, JP Ellis, RS Sanderson, AJR Pei, L Targett, TA Sand, DJ Swinbank, AM Dannerbauer, H Mazzotta, P Limousin, M Egami, E Jullo, E Hamilton-Morris, V Moran, SM AF Richard, Johan Smith, Graham P. Kneib, Jean-Paul Ellis, Richard S. Sanderson, A. J. R. Pei, L. Targett, T. A. Sand, D. J. Swinbank, A. M. Dannerbauer, H. Mazzotta, P. Limousin, M. Egami, E. Jullo, E. Hamilton-Morris, V. Moran, S. M. TI LoCuSS: first results from strong-lensing analysis of 20 massive galaxy clusters at z=0.2 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gravitational lensing; galaxies: clusters: general ID HUBBLE-SPACE-TELESCOPE; DARK-MATTER HALOS; X-RAY MEASUREMENTS; TO-LIGHT RATIOS; SCALING RELATIONS; LENSED GALAXIES; CHANDRA SAMPLE; COOL CORES; FIELD; GAS AB We present a statistical analysis of a sample of 20 strong lensing clusters drawn from the Local Cluster Substructure Survey, based on high-resolution Hubble Space Telescope imaging of the cluster cores and follow-up spectroscopic observations using the Keck-I telescope. We use detailed parametrized models of the mass distribution in the cluster cores, to measure the total cluster mass and fraction of that mass associated with substructures within R = 250 kpc. These measurements are compared with the distribution of baryons in the cores, as traced by the old stellar populations and the X-ray emitting intracluster medium. Our main results include: (i) the distribution of Einstein radii is lognormal, with a peak and 1 sigma width of < log(10)theta(E)(z = 2)> = 1.16 +/- 0.28; (ii) we detect an X-ray/lensing mass discrepancy of < M(SL)/M(X)> = 1.3 at 3 sigma significance-clusters with larger substructure fractions displaying greater mass discrepancies, and thus greater departures from hydrostatic equilibrium and (iii) cluster substructure fraction is also correlated with the slope of the gas density profile on small scales, implying a connection between cluster-cluster mergers and gas cooling. Overall our results are consistent with the view that cluster-cluster mergers play a prominent role in shaping the properties of cluster cores, in particular causing departures from hydrostatic equilibrium, and possibly disturbing cool cores. Our results do not support recent claims that large Einstein radius clusters present a challenge to the cold dark matter paradigm. C1 [Richard, Johan; Swinbank, A. M.] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Smith, Graham P.; Sanderson, A. J. R.; Hamilton-Morris, V.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Kneib, Jean-Paul; Limousin, M.] Univ Aix Marseille, Lab Astrophys Marseille, CNRS, F-13388 Marseille 13, France. [Ellis, Richard S.; Pei, L.] CALTECH, Pasadena, CA 91125 USA. [Targett, T. A.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Sand, D. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dannerbauer, H.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Mazzotta, P.] Univ Roma Tor Vergata, Dept Phys, I-00133 Rome, Italy. [Limousin, M.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Egami, E.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Jullo, E.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Moran, S. M.] Johns Hopkins Dept Phys & Astron, Baltimore, MD 21218 USA. RP Richard, J (reprint author), Univ Durham, Inst Computat Cosmol, Dept Phys, South Rd, Durham DH1 3LE, England. EM johan.richard@durham.ac.uk RI Kneib, Jean-Paul/A-7919-2015; Mazzotta, Pasquale/B-1225-2016 OI Kneib, Jean-Paul/0000-0002-4616-4989; Mazzotta, Pasquale/0000-0002-5411-1748 NR 91 TC 88 Z9 88 U1 0 U2 2 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2010 VL 404 IS 1 BP 325 EP 349 DI 10.1111/j.1365-2966.2009.16274.x PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 584ZU UT WOS:000276794600054 ER PT J AU Muxlow, TWB Beswick, RJ Garrington, ST Pedlar, A Fenech, DM Argo, MK van Eymeren, J Ward, M Zezas, A Brunthaler, A AF Muxlow, T. W. B. Beswick, R. J. Garrington, S. T. Pedlar, A. Fenech, D. M. Argo, M. K. van Eymeren, J. Ward, M. Zezas, A. Brunthaler, A. TI Discovery of an unusual new radio source in the star-forming galaxy M82: faint supernova, supermassive black hole or an extragalactic microquasar? SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; galaxies: individual: M82; galaxies: nuclei; galaxies: starburst; radio continuum: stars ID REMNANTS; NUCLEUS; POPULATION; MESSIER-82; STARBURST; EMISSION; SCALE; BURST; JET AB A faint new radio source has been detected in the nuclear region of the starburst galaxy M82 using Multi-Element Radio-Linked Interferometer Network radio observations designed to monitor the flux density evolution of the recent bright supernova SN 2008iz. This new source was initially identified in observations made between 2009 May 1 and 5 but had not been present in observations made 1 week earlier, or in any previous observations of M82. In this Letter, we report the discovery of this new source and monitoring of its evolution over its first 9 months of existence. The true nature of this new source remains unclear, and we discuss whether this source is an unusual and faint supernova, a supermassive black hole associated with the nucleus of M82 or intriguingly the first detection of radio emission from an extragalactic microquasar. C1 [Muxlow, T. W. B.; Beswick, R. J.; Garrington, S. T.; Pedlar, A.; van Eymeren, J.] Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Manchester M13 9PL, Lancs, England. [Fenech, D. M.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Argo, M. K.] Curtin Univ Technol, Curtin Inst Radio Astron, ICRAR, Perth, WA 6845, Australia. [Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Zezas, A.] Fdn Res & Technol Hellas, IESL, Iraklion 71110, Crete, Greece. [Zezas, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brunthaler, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Muxlow, TWB (reprint author), Univ Manchester, Sch Phys & Astron, Ctr Astrophys, Jodrell Bank, Oxford Rd, Manchester M13 9PL, Lancs, England. EM twbm@jb.man.ac.uk RI Zezas, Andreas/C-7543-2011; OI Zezas, Andreas/0000-0001-8952-676X; Muxlow, Thomas/0000-0001-5797-8796; Argo, Megan/0000-0003-3594-0214 NR 34 TC 15 Z9 15 U1 0 U2 0 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD MAY 1 PY 2010 VL 404 IS 1 BP L109 EP L113 DI 10.1111/j.1745-3933.2010.00845.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 584ZU UT WOS:000276794600023 ER PT J AU Weldon, PJ AF Weldon, Paul J. TI Nuisance arthropods, nonhost odors, and vertebrate chemical aposematism SO NATURWISSENSCHAFTEN LA English DT Review DE Aposematism; Arthropod; Ectoparasite; Host; Nonhost; Odor; Semiochemical ID GLOSSINA-MORSITANS-MORSITANS; TSETSE FLIES DIPTERA; RHIPICEPHALUS-SANGUINEUS ACARI; NONPREFERRED WATERBUCK HOSTS; L-LACTIC ACID; ANOPHELES-GAMBIAE; OVIPOSITION SITE; CARBON-DIOXIDE; PREFERRED BUFFALO; RESPONSES AB Mosquitoes, ticks, and other ectoparasitic arthropods use chemoreception to avoid vertebrates that are known or presumed to be dangerous or otherwise unprofitable hosts. Nonhosts may belong to a species that is regularly unaccepted or one that includes both accepted and unaccepted individuals. A diverse array of qualities including immunocompetence, vigilant grooming behavior, mechanical inaccessibility, and toxicity have been proposed as the features that render vertebrate chemical emitters unsuitable as hosts for arthropods. In addition to advantages accrued by ectoparasitic arthropods that avoid nonhosts, vertebrates that are not accepted as hosts benefit by evading injurious ectoparasites and the infectious agents they transmit. The conferral of advantages to both chemical receivers (ectoparasitic arthropods) and emitters (unpreferred vertebrates) in these interactions renders nonhost odors aposematic. Chemical aposematism involving ectoparasites selects for vertebrates that emit distinctive odors. In addition, chemical mimicry, where vulnerable organisms benefit when misidentified as nonhosts, may be accommodated by duped ectoparasites. C1 Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Weldon, PJ (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM weldonp@si.edu NR 51 TC 11 Z9 11 U1 1 U2 18 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0028-1042 EI 1432-1904 J9 NATURWISSENSCHAFTEN JI Naturwissenschaften PD MAY PY 2010 VL 97 IS 5 BP 443 EP 448 DI 10.1007/s00114-010-0665-z PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 591QX UT WOS:000277318800001 PM 20376425 ER PT J AU Medianero, E Ibanez, A Nieves-Aldrey, JL AF Medianero, Enrique Ibanez, Alicia Nieves-Aldrey, Jose L. TI The Importance of Beta Diversity in Local Gall-Inducing Arthropod Distribution SO NEOTROPICAL ENTOMOLOGY LA English DT Article DE Coiba Island; geographic distribution; Panama; plant community ID INSECT SPECIES RICHNESS; RAINFALL GRADIENT; TROPICAL FORESTS; FORMING INSECTS; SOUTH-AFRICA; COMMUNITY; PATTERNS; REGION AB Many studies over the past twenty years have documented the richness of arthropod galling species around the world, and some have proposed hypotheses to explain local and global patterns of galling species richness. However, few studies have been directed toward understanding how the gall-inducing species are locally distributed. The aim of this study was to determine the distribution of gall-inducing arthropods species at Coiba National Park, a tropical habitat on the Pacific coast of Panama. Our results suggest that more gall-inducing species had an aggregated distribution, and gall-inducing arthropod diversity shows a strong beta diversity component. Geographic distance was not correlated with similarity in gall-inducing species composition between the studied sites. This fact has important implications when trying to estimate gall-inducing arthropod richness and general patterns, and could cause contradictory results for hypotheses that attempt to explain the local and global patterns of galling species richness. C1 [Medianero, Enrique] Univ Panama, Programa Centroamer Maestria Entomol Vicerrectori, Panama City, Panama. [Ibanez, Alicia] Smithsonian Trop Res Inst, Balboa, Panama. [Nieves-Aldrey, Jose L.] CSIC, Museo Nacl Ciencias Nat, E-28006 Madrid, Spain. RP Medianero, E (reprint author), Univ Panama, Programa Centroamer Maestria Entomol Vicerrectori, Panama City, Panama. EM emedianero@ancon.up.ac.pa; ibaneza@si.edu; aldrey@mncn.csic.es RI Nieves-Aldrey, Jose Luis/K-2544-2012 OI Nieves-Aldrey, Jose Luis/0000-0002-4711-7455 FU Republic of Panama (IFARHU-SENACYT); Spanish Agency of International Cooperation (AECI); Spanish Ministry of Education and Culture [DGES PB97-1241] FX Special thanks to Dr Santiago Castroviejo who was directly responsible for conceiving and initiating the Coiba Inventory Research Project and to O Diaserud for his help with the multiple-site similarity measure. Thanks to the Panamanian Authority of the Environment (ANAM) for collecting permits. We thank all the staff of A ECI in Panama and ANAM at the Biological Research Station of Coiba, as well as many colleagues from The Natural Sciences Museum and the Royal Botanical Garden in Madrid; their friendly help and support in several ways made this research possible. Enrique Medianero was supported by a scholarship granted by the Republic of Panama (IFARHU-SENACYT). This work was supported by the Spanish Agency of International Cooperation (AECI) and was also partially funded by a grant to JLNA from the research project DGES PB97-1241 of the Spanish Ministry of Education and Culture. NR 35 TC 3 Z9 3 U1 2 U2 17 PU ENTOMOLOGICAL SOC BRASIL PI LONDRINA, PA C POSTAL 481, 86001-970 LONDRINA,, PR, BRAZIL SN 1519-566X J9 NEOTROP ENTOMOL JI Neotrop. Entomol. PD MAY-JUN PY 2010 VL 39 IS 3 BP 365 EP 370 DI 10.1590/S1519-566X2010000300009 PG 6 WC Entomology SC Entomology GA 628OZ UT WOS:000280131200009 PM 20676509 ER PT J AU Calderon, AI Romero, LI Ortega-Barria, E Solis, PN Zacchino, S Gimenez, A Pinzon, R Caceres, A Tamayo, G Guerra, C Espinosa, A Correa, M Gupta, MP AF Calderon, Angela I. Romero, Luz I. Ortega-Barria, Eduardo Solis, Pablo N. Zacchino, Susana Gimenez, Alberto Pinzon, Roberto Caceres, Armando Tamayo, Giselle Guerra, Carlos Espinosa, Alex Correa, Mireya Gupta, Mahabir P. TI Screening of Latin American plants for antiparasitic activities against malaria, Chagas disease, and leishmaniasis SO PHARMACEUTICAL BIOLOGY LA English DT Article DE Malaria; Chagas disease; leishmaniasis; Latin America; screening; antiparasitic activity ID VITRO ANTIPLASMODIAL ACTIVITY; NORCASSANE-TYPE DITERPENES; TRYPANOCIDAL ACTIVITY; ANTIMALARIAL ACTIVITY; TRADITIONAL MEDICINE; CAESALPINIA-CRISTA; TRYPANOSOMA-CRUZI; CASSANE-TYPE; DERIVATIVES AB In order to explore rationally the medical potential of the plant biodiversity of the Central and South American region as a source of novel antiparasitic molecules, a multinational Organization of American States (OAS) project, which included the participation of multidisciplinary research centers from Argentina, Bolivia, Colombia, Costa Rica, Guatemala, Nicaragua and Panama, was carried out during the period 2001-2004. This project aimed at screening organic plant extracts for antitrypanosomal, antileishmanial and antimalarial activities and subsequently isolating and characterizing bioactive molecules. Plants for antiparasitic screening were selected from a database of ethnomedical uses of Latin American plants (PlanMedia) based on the amount of biological and chemical information available in the literature. We report here the evaluation of 452 extracts from 311 plant species in vitro screens against Plasmodium falciparum, Leishmania mexicana, and Trypanosoma cruzi. Out of 311 species tested, 17 plants (5.4%) showed antiparasitic activities at IC(50) values < 10 mu g/mL. The most active plants were Acnistus arborescens (L.) Schltdl. (Solanaceae) (leaf, EtOH, IC(50): 4 mu g/mL) Monochaetum myrtoideum Naudin (Melastomataceae) (leaf, MeOH, IC(50): 5 mu g/mL) and Bourreria huanita (Lex.) Hemsl. (Boraginaceae) (branch, EtOH, IC(50): 6 mu g/mL). These were selectively active against P. falciparum, L. mexicana and T. cruzi, respectively.2 potentials. This work was supported by the Natural Sciences and Engineering Research Council of Canada, the Austrian Science Foundation (Grant No. FWF-Z 118-N16), the European Community (projects SCALA, CHIMONO), and the Chemical Science, Geoscience, and Bioscience Division of the Office of Basic Energy Science, Office of Science, US Department of Energy and National Science Foundation grants to the Harvard-MIT Center for Ultracold Atoms and Institute for Theoretical Atomic and Molecular Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 37 TC 24 Z9 24 U1 1 U2 8 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD MAY PY 2010 VL 81 IS 5 AR 050701 DI 10.1103/PhysRevA.81.050701 PG 4 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 602LF UT WOS:000278140000005 ER PT J AU Evangelista, D Fernandez, MJ Berns, MS Hoover, A Dudley, R AF Evangelista, Dennis Fernandez, Maria Jose Berns, Madalyn S. Hoover, Aaron Dudley, Robert TI Hovering Energetics and Thermal Balance in Anna's Hummingbirds (Calypte anna) SO PHYSIOLOGICAL AND BIOCHEMICAL ZOOLOGY LA English DT Article ID INSECT FLIGHT; RUFOUS HUMMINGBIRDS; AERODYNAMICS; TEMPERATURE; SELECTION; MUSCLE; COST; THERMOGENESIS; PERFORMANCE; EFFICIENCY AB We studied the energetics of hover-feeding Anna's hummingbirds, using three different simultaneous techniques: heat loss as estimated via thermal imaging, metabolic rate as measured at a feeder mask using flow-through respirometry, and aerodynamic power estimated from wingbeat kinematic data. These three methods yielded comparable estimates of power output at ambient air temperatures ranging from 18 degrees to 26 degrees C, whereas heat imbalance at higher air temperatures (up to 34 degrees C) suggested loss by mechanisms other than convection and radiation from the body, such as evaporative cooling and enthalpy rise associated with exhaled air and excreted water and convective heat loss from the patagia. Hummingbirds increased wingbeat frequency and decreased stroke amplitude as air temperature increased, but overall muscle efficiency was found to be approximately constant over the experimental range of air temperatures. C1 [Evangelista, Dennis; Fernandez, Maria Jose; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Berns, Madalyn S.] Univ Calif Berkeley, Dept Bioengn, Berkeley, CA 94720 USA. [Hoover, Aaron] Univ Calif Berkeley, Dept Mech Engn, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Evangelista, D (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM devangel@berkeley.edu RI Evangelista, Dennis/E-2741-2010; Evangelista, Dennis/N-4434-2013 OI Evangelista, Dennis/0000-0002-6565-8300 FU National Science Foundation (NSF) [DEB-0543556]; Fulbright fellowship FX We thank C. Clark for capturing birds and providing a skin specimen for the construction of the thermal model. We also thank R. Full, M. Koehl, Y. Munk, S. Sponberg, and T. Libby for assistance, equipment, and comments as a part of Berkeley's Mechanics of Organisms Lab class (IB 135L) within the Center for Integrative Biomechanics Education and Research (CIBER). Several anonymous reviewers provided comments that were helpful. D. E. was supported by a National Science Foundation (NSF) graduate fellowship. M.J.F. was supported by a Fulbright fellowship. Y. Munk provided useful comments on the manuscript. Laboratory support was provided by NSF grant DEB-0543556. NR 38 TC 7 Z9 7 U1 1 U2 15 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 1522-2152 J9 PHYSIOL BIOCHEM ZOOL JI Physiol. Biochem. Zool. PD MAY-JUN PY 2010 VL 83 IS 3 BP 406 EP 413 DI 10.1086/651460 PG 8 WC Physiology; Zoology SC Physiology; Zoology GA 583HL UT WOS:000276664400002 PM 20350142 ER PT J AU Merrill, WL AF Merrill, William L. TI Landscapes of Origin in the Americas: Creation Narratives Linking Ancient Places and Present Communities SO PLAINS ANTHROPOLOGIST LA English DT Book Review C1 [Merrill, William L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Merrill, WL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU PLAINS ANTHROPOLOGICAL SOC PI LINCOLN PA 3201 SOUTH STREET, PO BOX 152, LINCOLN, NE 68506-3266 USA SN 0032-0447 J9 PLAINS ANTHROPOL JI Plains Anthropol. PD MAY PY 2010 VL 55 IS 214 BP 183 EP 184 PG 2 WC Anthropology SC Anthropology GA 813OG UT WOS:000294376200007 ER PT J AU Ma, Y Wang, DY Lin, J Dai, S Zhang, XF AF Ma, Yuan Wang, De-Yu Lin, Jun Dai, Shuo Zhang, Xue-Fei TI Associations of decimetric type III bursts with coronal mass ejections and H alpha flares SO RESEARCH IN ASTRONOMY AND ASTROPHYSICS LA English DT Article DE Sun: magnetic fields; Sun: flares; Sun: radio bursts; Sun: coronal mass ejections ID RADIO-BURSTS; SOLAR-FLARES; ACCELERATION; EMISSION; RECONNECTION; TRANSIENTS; MODEL; SHOCK; CMES AB We present a statistical study of decimetric type III radio bursts, coronal mass ejections (CMEs), and H alpha flares observed in the period from July 2000 to March 2005. In total, we investigated 395 decimetric type HI radio burst events, 21% of which showed apparent correlation to CMEs that were associated with Ha flares. We noticed that the Ha flares which were strongly associated with CMEs were gradual events, and 82% of them took place before CMEs appeared in the field of view of LASCO C2; that most of the CME-associated radio bursts started in the frequency range around 750 MHz with a frequency drifting rate of several hundred MHz s(-1), of which both positive and negative ones were recognized; and that the correlation of type III radio bursts to CMEs without associated flares is fairly vague, less than 9%. C1 [Ma, Yuan; Lin, Jun; Dai, Shuo; Zhang, Xue-Fei] Chinese Acad Sci, Yunnan Astron Observ, Natl Astron Observ China, Kunming 650011, Peoples R China. [Wang, De-Yu] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Lin, Jun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ma, Y (reprint author), Chinese Acad Sci, Yunnan Astron Observ, Natl Astron Observ China, Kunming 650011, Peoples R China. EM jlin@ynao.ac.cn RI LIN, JUN/B-9890-2017 FU Ministry of Science and Technology of China [2006CB806301, 2006CB806303]; National Natural Science Foundation of China [10473020, 10333030, 10873030]; Chinese Academy of Sciences [KJCX2-YW-T04]; NASA [NNX07AL72G] FX This work was supported by the Ministry of Science and Technology of China under the 973 Program grants 2006CB806301 and 2006CB806303, by the National Natural Science Foundation of China (Grant Nos. 10473020, 10333030 and 10873030), and by the Chinese Academy of Sciences under the grant KJCX2-YW-T04 to YNAO. IL acknowledges NASA grant NNX07AL72G for supporting his visit to CfA. NR 32 TC 0 Z9 0 U1 0 U2 3 PU NATL ASTRONOMICAL OBSERVATORIES, CHIN ACAD SCIENCES PI BEIJING PA 20A DATUN RD, CHAOYANG, BEIJING, 100012, PEOPLES R CHINA SN 1674-4527 J9 RES ASTRON ASTROPHYS JI Res. Astron. Astrophys. PD MAY PY 2010 VL 10 IS 5 BP 484 EP 494 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 601VJ UT WOS:000278093100008 ER PT J AU Clough, GW AF Clough, G. Wayne TI Antarctica! SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD MAY PY 2010 VL 41 IS 2 BP 22 EP 22 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 587ED UT WOS:000276971400011 ER PT J AU Drohan, PJ Havlin, JL Megonigal, JP Cheng, HH AF Drohan, Patrick J. Havlin, John L. Megonigal, J. Patrick Cheng, H. H. TI The "Dig It!" Smithsonian Soils Exhibition: Lessons Learned and Goals for the Future SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article AB The opening of "Dig It!: The Secrets of Soil," a 5000-ft(2) exhibit on soil at the Smithsonian National Museum of Natural History in Washington, DC, presented an opportunity to reflect on the development process. The project generated important and new ways of thinking about soils education, and taught the SSSA much about itself and how to manage a project of this size and scope. While early struggles in organization and financing of the exhibit presented challenges never before faced by SSSA at this scale, persistence, flexibility, and some unconventional thinking won out in the end, and SSSA achieved its most significant educational success to date. Most importantly, the process taught many soil scientists that achieving greater visibility for soil science meant partnering with professionals outside of soil science, and trusting that they could convey the message delivered by the exhibit with the same enthusiasm they might have in the classroom. The lessons learned from the project, in the scope of its history, can help others further SSSA, soils education, and soil science as a respected, scientific field. We suggest six goals for the future of soil science that, if embraced with whole-heart dedication and support, can help to embed the importance of soil in world thinking and policy. Our suggested goals are unconventional, like the experiences we faced in creating the exhibit, and thus perhaps will seem beyond the capability of most soil scientists. Hence our reminder: unconventional and bold thinking are what helped create the exhibit and will be what leads SSSA forward as a society best serving the world. C1 [Drohan, Patrick J.] Penn State Univ, Dep Crop & Soil Sci, University Pk, PA 16802 USA. [Havlin, John L.] N Carolina State Univ, Dep Soil Sci, Raleigh, NC 27695 USA. [Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Cheng, H. H.] Univ Minnesota, Dep Soil Water & Climate, St Paul, MN 55108 USA. RP Drohan, PJ (reprint author), Penn State Univ, Dep Crop & Soil Sci, 452 ASI Bldg, University Pk, PA 16802 USA. EM pjd7@psu.edu NR 6 TC 5 Z9 6 U1 1 U2 2 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD MAY-JUN PY 2010 VL 74 IS 3 BP 697 EP 705 DI 10.2136/sssaj2009.0017 PG 9 WC Soil Science SC Agriculture GA 593YZ UT WOS:000277500600001 ER PT J AU Megonigal, JP Stauffer, B Starrs, S Pekarik, A Drohan, P Havlin, J AF Megonigal, J. Patrick Stauffer, Barbara Starrs, Siobhan Pekarik, Andrew Drohan, Patrick Havlin, John TI "Dig It!": How an Exhibit Breathed Life into Soils Education SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID OCEAN; DUST AB We propose that the primary goal of public soils education should not be to teach, but to inspire. The goal to inspire guided the design of "Dig It! The Secrets of Soil:" a large exhibit in the Smithsonian's National Museum of Natural History, Washington, DC, for 18 mo beginning in June 2008. The "Dig It!" exhibit was designed from an ecosystem perspective, in which agriculture the traditional context for soils education is considered to be just one of many ecosystem types. For visitors inspired primarily by art and culture, there were objects chosen to surprise and expand the imagination about soils. The exhibit was designed to communicate to wide range of ages, centered on 12-14 yr olds. As such, it was rich in audiovisual media that included a cartoon, a movie, two looping videos, a kiosk for exploring the state soils, a quiz game, and a role-playing game. It also included scale models and actual soil monoliths. The exhibit addressed the full spectrum of issues that concern contemporary soil scientists climate change, aquatic eutrophication, soil degradation, sustainable farming, and others by organizing the content according to scale (global, regional, and local). Interviews with visitors indicated that the exhibit had the potential to effectively alter the preconceived notions of more than 2 million visitors about soils. We fully expect the exhibit to continue inspiring the public about soils through the richness of the exhibit website (www.forces.si.edu/soils; verified 6 Mar. 2010), which includes videos, games, and interactive content. C1 [Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Stauffer, Barbara; Starrs, Siobhan] Natl Museum Nat Hist, Washington, DC 20013 USA. [Pekarik, Andrew] Smithsonian Off Policy & Anal, Washington, DC 20560 USA. [Drohan, Patrick] Penn State Univ, Dep Crop & Soil Sci, University Pk, PA 16802 USA. [Havlin, John] N Carolina State Univ, Dep Soil Sci, Raleigh, NC 27695 USA. RP Megonigal, JP (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM megonigalp@si.edu FU NASA REASoN; Soil Science Society of America; The Nutrients for Life Foundation; USDA; Department of the Interior; National Science Foundation [DEB-0516400] FX The "Dig It! The Secrets of Soil" web site was developed under the Forces of Change Program at the National Museum of Natural History and was made possible by support from a NASA REASoN Grant. The "Dig It! The Secrets of Soil" exhibit was developed under the Forces of Change Program at the National Museum of Natural History and was made possible by support from the founding sponsor, the Soil Science Society of America; the lead sponsor, The Nutrients for Life Foundation; the USDA; and the Department of the Interior. This contribution was supported by National Science Foundation Grant DEB-0516400 to J.P. Megonigal. NR 15 TC 3 Z9 4 U1 0 U2 6 PU SOIL SCI SOC AMER PI MADISON PA 677 SOUTH SEGOE ROAD, MADISON, WI 53711 USA SN 0361-5995 J9 SOIL SCI SOC AM J JI Soil Sci. Soc. Am. J. PD MAY-JUN PY 2010 VL 74 IS 3 BP 706 EP 716 DI 10.2136/sssaj2009.0409 PG 11 WC Soil Science SC Agriculture GA 593YZ UT WOS:000277500600002 ER PT J AU Yeates, AR Constable, JA Martens, PCH AF Yeates, A. R. Constable, J. A. Martens, P. C. H. TI Solar Cycle Variation of Magnetic Flux Ropes in a Quasi-Static Coronal Evolution Model SO SOLAR PHYSICS LA English DT Article DE Coronal mass ejections, theory; Magnetic fields, corona; Magnetic fields, models; Solar cycle, models ID MASS EJECTIONS; FIELD; PROMINENCES; FILAMENTS; HELICITY; REGIONS; LASCO; SUN AB The structure of electric current and magnetic helicity in the solar corona is closely linked to solar activity over the 11-year cycle, yet is poorly understood. As an alternative to traditional current-free "potential-field" extrapolations, we investigate a model for the global coronal magnetic field which is non-potential and time-dependent, following the build-up and transport of magnetic helicity due to flux emergence and large-scale photospheric motions. This helicity concentrates into twisted magnetic flux ropes, which may lose equilibrium and be ejected. Here, we consider how the magnetic structure predicted by this model - in particular the flux ropes - varies over the solar activity cycle, based on photospheric input data from six periods of cycle 23. The number of flux ropes doubles from minimum to maximum, following the total length of photospheric polarity inversion lines. However, the number of flux rope ejections increases by a factor of eight, following the emergence rate of active regions. This is broadly consistent with the observed cycle modulation of coronal mass ejections, although the actual rate of ejections in the simulation is about a fifth of the rate of observed events. The model predicts that, even at minimum, differential rotation will produce sheared, non-potential, magnetic structure at all latitudes. C1 [Yeates, A. R.; Martens, P. C. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Constable, J. A.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [Martens, P. C. H.] Montana State Univ, Dept Phys, Bozeman, MT 59717 USA. RP Yeates, AR (reprint author), Univ Dundee, Div Math, Dundee DD1 4HN, Scotland. EM anthony@maths.dundee.ac.uk RI Yeates, Anthony/D-1338-2014 OI Yeates, Anthony/0000-0002-2728-4053 FU NASA [NNM07AB07C, NNX08AW53]; UK STFC; NSF [ATM-0851866] FX We thank A. A. van Ballegooijen, D. H. Mackay, A. N. Wilmot-Smith, D. I. Pontin and an anonymous referee for useful suggestions, and D. H. Mackay also for the use of parallel computing facilities obtained through a Royal Society research grant. ARY acknowledges financial support from NASA contract NNM07AB07C at SAO, and from the UK STFC at Dundee. The visit of JAC to SAO was supported by NASA grant NNX08AW53 and by NSF grant ATM-0851866 for "REU site: Solar Physics at the Harvard-Smithsonian Center for Astrophysics." Magnetogram data from NSO/Kitt Peak were produced cooperatively by NSF/NOAO, NASA/GSFC and NOAA/SEL. SOLIS data used here are produced cooperatively by NSF/NSO and NASA/LWS. NR 40 TC 5 Z9 5 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2010 VL 263 IS 1-2 BP 121 EP 134 DI 10.1007/s11207-010-9546-z PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 589LD UT WOS:000277148200009 ER PT J AU Cranmer, SR Gardner, LD Kohl, JL AF Cranmer, S. R. Gardner, L. D. Kohl, J. L. TI A Model for the Stray-Light Contamination of the UVCS Instrument on SOHO SO SOLAR PHYSICS LA English DT Article DE Instrumental effects; Spectrum, ultraviolet ID ULTRAVIOLET CORONAGRAPH SPECTROMETER; SCATTERED-LIGHT; FAR-ULTRAVIOLET; LINE-PROFILES; SOLAR CORONA; PERFORMANCE; CORONOGRAPH; UVCS/SOHO; SPECTRA; MIRRORS AB We present a detailed model of stray-light suppression in the spectrometer channels of the Ultraviolet Coronagraph Spectrometer (UVCS) on the SOHO spacecraft. The control of diffracted and scattered stray light from the bright solar disk is one of the most important tasks of a coronagraph. We compute the fractions of light that diffract past the UVCS external occulter and non-specularly pass into the spectrometer slit. The diffracted component of the stray light depends on the finite aperture of the primary mirror and on its figure. The amount of non-specular scattering depends mainly on the micro-roughness of the mirror. For reasonable choices of these quantities, the modeled stray-light fraction agrees well with measurements of stray light made both in the laboratory and during the UVCS mission. The models were constructed for the bright H i Ly alpha emission line, but they are applicable to other spectral lines as well. C1 [Cranmer, S. R.; Gardner, L. D.; Kohl, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM scranmer@cfa.harvard.edu; lgardner@cfa.harvard.edu; jkohl@cfa.harvard.edu NR 41 TC 4 Z9 4 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD MAY PY 2010 VL 263 IS 1-2 BP 275 EP 291 DI 10.1007/s11207-010-9521-8 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 589LD UT WOS:000277148200019 ER PT J AU Ward, PS Brady, SG Fisher, BL Schultz, TR AF Ward, Philip S. Brady, Sean G. Fisher, Brian L. Schultz, Ted R. TI Phylogeny and Biogeography of Dolichoderine Ants: Effects of Data Partitioning and Relict Taxa on Historical Inference SO SYSTEMATIC BIOLOGY LA English DT Article DE Base composition; biogeography; data partitioning; Dolichoderinae; Formicidae; fossil record; outgroup; phylogenetic inference; relict taxa ID MOLECULAR CLOCK; SUBFAMILY DOLICHODERINAE; DIVERGENCE TIMES; MODEL SELECTION; HYMENOPTERA-FORMICIDAE; FOSSIL CALIBRATIONS; BAYESIAN ANALYSES; FUNCTIONAL-GROUPS; SPECIES TREES; MIXED MODELS AB Ants (Hymenoptera: Formicidae) are conspicuous organisms in most terrestrial ecosystems, often attaining high levels of abundance and diversity. In this study, we investigate the evolutionary history of a major clade of ants, the subfamily Dolichoderinae, whose species frequently achieve ecological dominance in ant communities. This group has also produced some of the world's most successful invasive ants. We use an extensive molecular data set (similar to 9 kb of sequence data from 10 nuclear genes, covering 48 dolichoderine species and 6 outgroup taxa) to infer the phylogenetic relationships, divergence dates, and biogeographic history of these ants. We evaluate the effects of data partitioning and outgroup composition on phylogenetic inference by estimating relationships under a series of increasingly partitioned data sets and by running analyses both with and without Aneuretus simoni, a rare and localized species that is the nearest living relative of Dolichoderinae. We also examine the effects of excluding 2 data partitions with significant base composition heterogeneity. Our results reveal 4 well-supported and mutually exclusive clades of dolichoderines, corresponding to 4 newly defined tribes: Bothriomyrmecini (B), Dolichoderini (D), Leptomyrmecini (L), and Tapinomini (T). All Bayesian and likelihood analyses yield the same unrooted (ingroup-only) topology, ((D,L),(B,T)), with the outgroups attaching either on the Dolichoderini branch or on the Tapinomini branch. Placement of the root is highly sensitive to choice of model partition and to inclusion/exclusion of Aneuretus. Bayes' factors strongly favor the more partitioned models, and in these Tapinomini is recovered as sister to the remaining dolichoderines, but only if Aneuretus is included. Exclusion of Aneuretus precludes recovery of this topology in all but the most highly partitioned Bayesian analyses and then only with nonsignificant support, underscoring the importance of relict, taxonomically isolated taxa for phylogenetic inference. Removal of 2 partitions with heterogeneous base composition also markedly increases support for placement of the root on the Tapinomini branch. Our divergence date estimates and biogeographic analyses indicate that crown-group dolichoderines arose about 65 million years ago (Ma), although this was preceded by a substantial period (30 million years) of stem group evolution. The 4 extant tribes are estimated to have crown-group origins in the late Paleocene or Eocene (40-60 Ma). Tapinomini and Bothriomyrmecini originated in the Paleotropics and subsequently dispersed to other biogeographic regions. Crown-group Leptomyrmecini arose and diversified in the Neotropics, but they also gave rise to one clade that colonized Australia about 30 Ma and subsequently experienced a massive radiation on that continent. This event occurred later than the diversification of dolichoderines in the northern hemisphere, so that by the time dolichoderines came to dominate the Australian fauna they had already declined in abundance in the Holarctic region. C1 [Ward, Philip S.] Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. [Brady, Sean G.; Schultz, Ted R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Fisher, Brian L.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. RP Ward, PS (reprint author), Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. EM psward@ucdavis.edu OI Fisher, Brian/0000-0002-4653-3270 FU National Science Foundation [EF-0431330] FX This work was supported by the National Science Foundation Ant AToL (Assembling the Tree of Life) grant EF-0431330. NR 106 TC 85 Z9 92 U1 2 U2 25 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 EI 1076-836X J9 SYST BIOL JI Syst. Biol. PD MAY PY 2010 VL 59 IS 3 BP 342 EP 362 DI 10.1093/sysbio/syq012 PG 21 WC Evolutionary Biology SC Evolutionary Biology GA 581MR UT WOS:000276528300008 PM 20525640 ER PT J AU Hacker, BC Vining, M AF Hacker, Barton C. Vining, Margaret TI Cutting a New Pattern: Uniforms and Women's Mobilization for War 1854-1919 SO TEXTILE HISTORY LA English DT Article ID WORLD-WAR; AMERICAN WOMEN; MEDICAL WOMEN; CITIZENSHIP; BRITAIN; 1ST-WORLD-WAR; SISTERS; GENDER; CROSS AB Hundreds of thousands of women donned uniforms in World War I. Some actually became part of the armed forces as members of women's auxiliaries and nurse corps, while others were hired under contract. But many more wore military-style uniforms as volunteers in civilian war relief and support organizations, both secular and religious. And still more donned uniforms of other kinds on the home front as factory workers, trolley conductors, police, and a host of others. Uniforms gave women a symbolic claim to full citizenship and their war service provided them a moral claim to suffrage widely recognized after the war. C1 [Hacker, Barton C.; Vining, Margaret] Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. RP Hacker, BC (reprint author), Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. NR 197 TC 0 Z9 0 U1 0 U2 2 PU MANEY PUBLISHING PI LEEDS PA STE 1C, JOSEPHS WELL, HANOVER WALK, LEEDS LS3 1AB, W YORKS, ENGLAND SN 0040-4969 J9 TEXT HIST JI Text. Hist. PD MAY PY 2010 VL 41 SU 1 BP 108 EP 143 DI 10.1179/174329510X12646114289707 PG 36 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 603CB UT WOS:000278184400010 ER PT J AU De Santana, CD Vari, RP AF De Santana, Carlos David Vari, Richard P. TI Electric fishes of the genus Sternarchorhynchus (Teleostei, Ostariophysi, Gymnotiformes); phylogenetic and revisionary studies SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE adaptive radiation; Apteronotidae; cladistics; convergence; key innovation; new species; osteology; South America ID ADAPTIVE RADIATION; GHOST KNIFEFISH; AMAZON BASIN; VENEZUELA GYMNOTIFORMES; SEXUAL-DIMORPHISM; INCOMPLETE TAXA; SOUTH-AMERICA; MISSING DATA; RIVER-BASIN; APTERONOTIDAE AB Analysis of 88 characters of external and internal body systems yielded a phylogenetic reconstruction of the Neotropical electric knifefish genus Sternarchorhynchus (Apteronotidae; Gymnotiformes). The results support a hypothesis of Sternarchorhynchus as the sister group to Platyurosternarchus. A series of synapomorphies, many involving major innovations of the neurocranium, jaws, suspensorium, and associated systems that permit an unusual mode of graspsuction feeding, support the monophyly of both genera. Synapomorphies largely resolve relationships within Sternarchorhynchus with basal nodes strongly supported by characters pertinent to prey capture and initial processing of food items These possible key innovations may provide Sternarchorhynchus with a competitive advantage over other clades of the Apteronotidae and account for the species diversity of the genus in Neotropical rivers. Adaptive radiation in Sternarchorhynchus was analysed. Habitat preference transitions repeatedly occurred in the genus between deepriver channel dwelling species and rheophilic species with preferences for higher energy setting including rapids and swift flowing fluviatile settings. Twenty-two species of Sternarchorhynchus are described as new based on samples that originated in the smaller rivers draining into the Golfo de Paria, the Marowijne and Essequiho River basins, the Rio Orinoco and in particular the Amazon River basin. The 32 species in Sternarchorhynchus make it the most speciose genus in the Apteronotidae. No claim to original US government works. Journal compilation (C) 2010 The Linnean Society of London, Zoological Journal of the Linnean Society, 2010, 159, 223-371. C1 [De Santana, Carlos David; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. 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 varir@SI.edu FU National Museum of Natural History; National Museum of Natural History of the Smithsonian Institution FX Research associated with this study was supported by a Predoctoral Fellowship from the Smithsonian Institution in the Division of Fishes of the National Museum of Natural History and by funding from the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology in the Division of Fishes, National Museum of Natural History of the Smithsonian Institution. We are indebted to the following individuals and institutions for the loan and exchange of specimens: Barbara Brown, Radford Arrindell, and Scott Schaeffer (AMNH), John Lundberg, Mark Sabaj Perez, and Kyle Luckenbill (ANSP), Jonathan Armbruster and David Werneke (AUM), Ralf Britz and Oliver Crimmen (BMNH), David Catania and Tomio Iwamoto (CAS), John Friel (CU), Mary Anne Rogers (FMNH), Javier Maldonado-Ocampo (IAVHP), Michael Retzer (INHS), Lucia Rapp Py-Daniel (INPA), Georges Lenglet (IRScNB), Jeffrey Siegel and Richard Fenney (LACM), Francisco Provenzano (MBUCV), Donald Taphorn (MCNG), Luiz Malabarba and Roberto Reis (MCP), Karsten Hartel (MCZ), Sonia Fisch-Muller and Alain Merguin (MHNG), Paulo Buckup (MNRJ), Hernan Ortega (MUSM), Osvaldo Oyakawa and Mario de Pinna (MZUSP), Erling Holm (ROM), Robert Robins (UF), Douglas Nelson (UMMZ), Ronald Vonk (ZMA), Peter Bartsch (ZMB), and William Crampton, University of Central Florida. Peter Bartsch (ZMB) provided a photograph and radiograph of the holotype of Sternarchus oxyrhynchus and meristic and morphometric data from that specimen. Ernst Mikschi and Helmut Wellendorf (NMW) arranged for radiographs of the two syntypes of S. mormyrus and hospitality during a visit by the second author. Mark Sabaj Perez and Kyle Luckenbill (ANSP) provided a photograph of one of the syntypes of S. mormyrus. Most of the photographs in this paper were prepared by T. Britt Griswold. The anatomical drawings were prepared by Tamara L. Clark. Drawings were labelled by Sandra J. Raredon (USNM) who also prepared the distribution maps and provided diverse invaluable technical assistance at the National Museum of Natural History throughout the course of the project. NR 164 TC 18 Z9 22 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0024-4082 EI 1096-3642 J9 ZOOL J LINN SOC-LOND JI Zool. J. Linn. Soc. PD MAY PY 2010 VL 159 IS 1 BP 223 EP 371 DI 10.1111/j.1096-3642.2009.00588.x PG 149 WC Zoology SC Zoology GA 589RE UT WOS:000277169700004 ER PT J AU Onofrio, R AF Onofrio, Roberto TI MACROSCOPIC QUANTUM VACUUM AND MICROSCOPIC GRAVITATION SO INTERNATIONAL JOURNAL OF MODERN PHYSICS A LA English DT Article; Proceedings Paper CT 9th Conference on Quantum Field Theory under the Influence of External Conditions CY SEP 21-25, 2009 CL Univ Oklahoma, Oklahoma City, OK HO Univ Oklahoma DE Casimir forces; non-Newtonian gravitation; Higgs particle; compact astrophysical object ID SAGITTARIUS A-ASTERISK; MODEL HIGGS-BOSON; CASIMIR FORCE; PROPER-MOTION; RANGE; RESTRICTIONS; GALAXY; LEADS; FIELD; MASS AB Macroscopic quantum vacuum and modern theories of gravitation share the strong int erplay between geometry and physical phenomena. We review selected issues related to the accuracy of the measurement of Casimir forces with particular emphasis on the implications for the search of non-Newtonian gravitational forces in the micrometer range. We then discuss the interplay of the Higgs particle with gravitation, arguing that spectroscopic shifts in atomic transitions due to the modifications of the vacuum expect ation value of the Higgs field in regions with strong curvature of space-time may be of conceptual and observational relevance. C1 [Onofrio, Roberto] Univ Padua, Dipartimento Fis Galileo Galilei, I-35131 Padua, Italy. [Onofrio, Roberto] Dartmouth Coll, Dept Phys & Astron, Lebanon, NH 03766 USA. [Onofrio, Roberto] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02139 USA. RP Onofrio, R (reprint author), Univ Padua, Dipartimento Fis Galileo Galilei, I-35131 Padua, Italy. EM onofrior@gmail.com NR 51 TC 7 Z9 7 U1 0 U2 3 PU WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA 5 TOH TUCK LINK, SINGAPORE 596224, SINGAPORE SN 0217-751X J9 INT J MOD PHYS A JI Int. J. Mod. Phys. A PD APR 30 PY 2010 VL 25 IS 11 BP 2260 EP 2269 DI 10.1142/S0217751X10049530 PG 10 WC Physics, Nuclear; Physics, Particles & Fields SC Physics GA 595MK UT WOS:000277614500010 ER PT J AU Lee, CF Bezdek, J Staines, CL AF Lee, Chi-Feng Bezdek, Jan Staines, Charles L. TI A review of the genus Agetocera (Coleoptera: Chrysomelidae: Galerucinae) in Taiwan-are there only two species? SO ZOOTAXA LA English DT Review DE Coleoptera; Chrysomelidae; Galerucinae; Agetocera; new species; speciation; Taiwan; Palaearctic Region ID HOPE COLEOPTERA AB The Taiwanese species of Agetocera (Coleoptera: Chrysomelidae) are reviewed. Three new species, A. yuae, A. choui, and A. huatungensis are described and A. discedens Weise and A. taiwana Chujo are redescribed. Agetocera taiwana together with the new species form a group of four sibling species. The Agetocera taiwana species group is defined and a key to Taiwanese Agetocera species is provided. C1 [Lee, Chi-Feng] Agr Res Inst Taiwan, Appl Zool Div, Taichung 413, Taiwan. [Bezdek, Jan] Mendel Univ Brno, Dept Zool, Brno 61300, Czech Republic. [Staines, Charles L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, MRC 187, Washington, DC 20013 USA. RP Lee, CF (reprint author), Agr Res Inst Taiwan, Appl Zool Div, Taichung 413, Taiwan. EM chifeng@tari.gov.tw; bezdek@mendelu.cz; stainesc@si.edu FU Ministry of Education, Youth and Sports of the Czech Republic [MSM6215648905] FX This study was supported by the Research plan No. MSM6215648905, Biological and technological aspects of sustainability of controlled ecosystems and their adaptability to climate change, which is financed by the Ministry of Education, Youth and Sports of the Czech Republic. NR 22 TC 5 Z9 5 U1 0 U2 0 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD APR 30 PY 2010 IS 2441 BP 1 EP 19 PG 19 WC Zoology SC Zoology GA 589WT UT WOS:000277185600001 ER PT J AU Pulupa, MP Bale, SD Kasper, JC AF Pulupa, M. P. Bale, S. D. Kasper, J. C. TI Langmuir waves upstream of interplanetary shocks: Dependence on shock and plasma parameters SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID EARTHS BOW SHOCK; PERPENDICULAR COLLISIONLESS SHOCKS; RANKINE-HUGONIOT PROBLEM; SOLAR-WIND ELECTRONS; II RADIO-EMISSION; ENERGETIC ELECTRONS; ACCELERATION; SIMULATIONS; SPACECRAFT; FORESHOCK AB We have examined 178 interplanetary shocks observed by the Wind spacecraft to establish which shock and plasma parameters are favorable for the production of upstream Langmuir waves and therefore to determine which shocks are likely to generate interplanetary Type II radio bursts. Of the 178 shocks included in this study, 43 produced upstream Langmuir waves, as evinced by enhancements in wave power near the plasma frequency. The large number of observed shocks permits the use of statistical tests to determine which parameters control the upstream activity. The best predictor of activity is the de Hoffmann-Teller speed, a result consistent with the fast Fermi model of electron acceleration. Several other parameters, including the magnetic field strength and the level of solar activity (but not the Mach number), are also correlated with upstream activity. These additional parameters may be associated with an increased level of shock front curvature or upstream structure, leading to the formation of upstream foreshock regions, or with the generation of an upstream electron population favorable for shock reflection. C1 [Pulupa, M. P.; Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94708 USA. [Pulupa, M. P.; Bale, S. D.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94708 USA. [Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pulupa, MP (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94708 USA. EM pulupa@ssl.berkeley.edu; bale@ssl.berkeley.edu; jkasper@cfa.harvard.edu RI Bale, Stuart/E-7533-2011; Kasper, Justin/D-1152-2010; OI Bale, Stuart/0000-0002-1989-3596; Kasper, Justin/0000-0002-7077-930X; Pulupa, Marc/0000-0002-1573-7457 FU NASA [NNX08AE34G] FX Work at UC Berkeley is sponsored by the NASA grant NNX08AE34G. Wind/MFI data are courtesy of the MFI team (PI: R. P. Lepping) at Goddard Space Flight Center. NR 48 TC 13 Z9 13 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD APR 29 PY 2010 VL 115 AR A04106 DI 10.1029/2009JA014680 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 590YZ UT WOS:000277265800002 ER PT J AU Rawlinson, KA AF Rawlinson, Kate A. TI Embryonic and post-embryonic development of the polyclad flatworm Maritigrella crozieri; implications for the evolution of spiralian life history traits SO FRONTIERS IN ZOOLOGY LA English DT Article ID LARVAL NERVOUS-SYSTEM; ANTALIS-ENTALIS MOLLUSCA; APICAL SENSORY ORGAN; NEUROMUSCULAR SYSTEMS; NEURONAL DEVELOPMENT; PHYLOGENETIC IMPLICATIONS; HOPLOPLANA-INQUILINA; MUSCLE DEVELOPMENT; TROCHOPHORE LARVA; BONELLIA-VIRIDIS AB Background: Planktonic life history stages of spiralians share some muscular, nervous and ciliary system characters in common. The distribution of these characters is patchy and can be interpreted either as the result of convergent evolution, or as the retention of primitive spiralian larval features. To understand the evolution of these characters adequate taxon sampling across the Spiralia is necessary. Polyclad flatworms are the only free-living Platyhelminthes that exhibit a continuum of developmental modes, with direct development at one extreme, and indirect development via a trochophore-like larval stage at the other. Here I present embryological and larval anatomical data from the indirect developing polyclad Maritrigrella crozieri, and consider these data within a comparative spiralian context. Results: After 196 h hours of embryonic development, M. crozieri hatches as a swimming, planktotrophic larva. Larval myoanatomy consists of an orthogonal grid of circular and longitudinal body wall muscles plus parenchymal muscles. Diagonal body wall muscles develop over the planktonic period. Larval neuroanatomy consists of an apical plate, neuropile, paired nerve cords, a peri-oral nerve ring, a medial nerve, a ciliary band nerve net and putative ciliary photoreceptors. Apical neural elements develop first followed by posterior perikarya and later pharyngeal neural elements. The ciliated larva is encircled by a continuous, pre-oral band of longer cilia, which follows the distal margins of the lobes; it also possesses distinct apical and caudal cilia. Conclusions: Within polyclads heterochronic shifts in the development of diagonal bodywall and pharyngeal muscles are correlated with life history strategies and feeding requirements. In contrast to many spiralians, M. crozieri hatch with well developed nervous and muscular systems. Comparisons of the ciliary bands and apical organs amongst spiralian planktonic life-stages reveal differences; M. crozieri lack a distinct ciliary band muscle and flask-shaped epidermal serotonergic cells of the apical organ. Based on current phylogenies, the distribution of ciliary bands and apical organs between polyclads and other spiralians is not congruent with a hypothesis of homology. However, some similarities exist, and this study sets an anatomical framework from which to investigate cellular and molecular mechanisms that will help to distinguish between parallelism, convergence and homology of these features. C1 [Rawlinson, Kate A.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Rawlinson, KA (reprint author), UCL, Dept Genet Evolut & Environm, Gower St, London WC1E 6BT, England. EM k.rawlinson@ucl.ac.uk FU Smithsonian Marine Science Network FX This work was supported by a Smithsonian Marine Science Network Postdoctoral Fellowship and was carried out at the Smithsonian Marine Station in Fort Pierce, Florida. NR 97 TC 21 Z9 22 U1 0 U2 5 PU BIOMED CENTRAL LTD PI LONDON PA 236 GRAYS INN RD, FLOOR 6, LONDON WC1X 8HL, ENGLAND SN 1742-9994 J9 FRONT ZOOL JI Front. Zool. PD APR 28 PY 2010 VL 7 AR 12 DI 10.1186/1742-9994-7-12 PG 25 WC Zoology SC Zoology GA 604HH UT WOS:000278269600001 PM 20426837 ER PT J AU Machida, RJ Tsuda, A AF Machida, Ryuji J. Tsuda, Atsushi TI Dissimilarity of Species and Forms of Planktonic Neocalanus Copepods Using Mitochondrial COI, 12S, Nuclear ITS, and 28S Gene Sequences SO PLOS ONE LA English DT Article ID SEX-BIASED DISPERSAL; SUBARCTIC PACIFIC-OCEAN; SUB-ARCTIC PACIFIC; REGIONAL-VARIATIONS; OYASHIO REGION; LIFE-CYCLE; CRISTATUS CRUSTACEA; CALANIDAE COPEPODA; EUCALANUS-BUNGII; GRAZING COPEPODS AB Background: A total of six Neocalanus species inhabit the oceans of the world. Of these, three species plus form variants (N. cristatus, N. plumchrus, N. flemingeri large form, and N. flemingeri small form), which constitute a monophyletic group among Neocalanus copepods, occur in the Northwestern Pacific off Japan. In the present study, we have tried to discriminate the three species plus form variants of Neocalanus copepods based on sequences of four DNA marker regions. Methodology/Principal Findings: Discrimination was performed based on the DNA sequence information from four genetic markers, including the mitochondrial COI, 12S, nuclear ITS, and 28S gene regions. Sequence dissimilarity was compared using both distance- and character-based approaches. As a result, all three species were confirmed to be distinct based on the four genetic marker regions. On the contrary, distinction of the form variants was only confirmed based on DNA sequence of the mitochondrial COI gene region. Conclusions/Significance: Although discrimination was not successful for the form variants based on the mitochondrial 12S, nuclear ITS, and 28S genes, diagnostic nucleotide sequence characters were observed in their mitochondrial COI gene sequences. Therefore, these form variants are considered to be an important unit of evolution below the species level, and constitute a part of the Neocalanus biodiversity. C1 [Machida, Ryuji J.; Tsuda, Atsushi] Univ Tokyo, Ocean Res Inst, Tokyo 164, Japan. RP Machida, RJ (reprint author), Smithsonian Natl Museum Nat Hist, Washington, DC USA. EM MachidaR@si.edu FU Ministry of Education, Culture, Sports, Science and Technology of Japan [20241003]; Ministry of Education, Culture, Sports, Science and Technology of Japan FX The authors gratefully acknowledge the support of the Alfred P. Sloan Foundation. Additional support for this project was provided to R.J.M. and A. T. by a Grant-in-Aid for Scientific Research No. 20241003 from the Ministry of Education, Culture, Sports, Science and Technology of Japan. Data Integration & Analysis System from the Ministry of Education, Culture, Sports, Science and Technology of Japan provided funding to R.J.M. This study is a contribution from the Census of Marine Zooplankton (CMarZ), an ocean realm field project of the Census of Marine Life. NR 32 TC 18 Z9 18 U1 1 U2 10 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 185 BERRY ST, STE 1300, SAN FRANCISCO, CA 94107 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 28 PY 2010 VL 5 IS 4 AR e10278 DI 10.1371/journal.pone.0010278 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 589MV UT WOS:000277154200002 PM 20442767 ER PT J AU Mckey, D Rostain, S Iriarte, J Glaser, B Birk, JJ Holst, I Renard, D AF McKey, Doyle Rostain, Stephen Iriarte, Jose Glaser, Bruno Birk, Jago Jonathan Holst, Irene Renard, Delphine TI Pre-Columbian agricultural landscapes, ecosystem engineers, and self-organized patchiness in Amazonia SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE French Guiana; historical ecology; land-use legacy; raised-field agriculture; coupled human and natural systems ID RAISED-FIELD AGRICULTURE; IDENTIFYING MAIZE; BOLIVIAN AMAZON; COB PHYTOLITHS; STARCH GRAINS; FOREST; AMERICA; MODEL; CONSERVATION; MESOAMERICA AB The scale and nature of pre-Columbian human impacts in Amazonia are currently hotly debated. Whereas pre-Columbian people dramatically changed the distribution and abundance of species and habitats in some parts of Amazonia, their impact in other parts is less clear. Pioneer research asked whether their effects reached even further, changing how ecosystems function, but few in-depth studies have examined mechanisms underpinning the resilience of these modifications. Combining archeology, archeobotany, paleoecology, soil science, ecology, and aerial imagery, we show that pre-Columbian farmers of the Guianas coast constructed large raised-field complexes, growing on them crops including maize, manioc, and squash. Farmers created physical and biogeochemical heterogeneity in flat, marshy environments by constructing raised fields. When these fields were later abandoned, the mosaic of well-drained islands in the flooded matrix set in motion self-organizing processes driven by ecosystem engineers (ants, termites, earthworms, and woody plants) that occur preferentially on abandoned raised fields. Today, feedbacks generated by these ecosystem engineers maintain the human-initiated concentration of resources in these structures. Engineer organisms transport materials to abandoned raised fields and modify the structure and composition of their soils, reducing erodibility. The profound alteration of ecosystem functioning in these landscapes coconstructed by humans and nature has important implications for understanding Amazonian history and biodiversity. Furthermore, these landscapes show how sustainability of food-production systems can be enhanced by engineering into them fallows that maintain ecosystem services and biodiversity. Like anthropogenic dark earths in forested Amazonia, these self-organizing ecosystems illustrate the ecological complexity of the legacy of pre-Columbian land use. C1 [McKey, Doyle; Renard, Delphine] Univ Montpellier 2, F-34293 Montpellier 5, France. [McKey, Doyle; Renard, Delphine] CNRS, Ctr Ecol Fonct & Evolut, UMR 5175, F-34293 Montpellier 5, France. [Rostain, Stephen] CNRS, UMR 8096, F-92323 Nanterre, France. [Iriarte, Jose] Univ Exeter, Sch Geog Archaeol & Earth Resources, Dept Archaeol, Exeter EX4 4QE, Devon, England. [Glaser, Bruno; Birk, Jago Jonathan] Univ Bayreuth, Dept Soil Phys, D-95447 Bayreuth, Germany. [Holst, Irene] Smithsonian Trop Res Inst, Balboa, Panama. RP Mckey, D (reprint author), Univ Montpellier 2, F-34293 Montpellier 5, France. EM doyle.mckey@cefe.cnrs.fr RI Iriarte, Jose /A-1141-2010; OI Iriarte, Jose/0000-0002-8155-5360 FU CNRS; Amazonie and Ingenierie Ecologique; French Ministry of Culture and Communication FX The Centre Spatial Guyanais, particularly Sandrine Richard, kindly provided access to some of the field sites. The EcoFoG laboratory in Kourou, French Guiana, CNRS Guyane, and Philippe Jet gave logistical help. Prof. Dr. Eckehardt Klemt (University of Applied Sciences, Weingarten, Germany) assisted with the 137Cs analyses. The following persons helped during fieldwork: Lydie Clerc, Claude Coutet, Guy Dauphin, Laure Deodat, Nathalie Fromin, Eric Gassies, Gilles Grisard, Nicolas Guillaume-Gentil, Alexander H nel, Martin Hit-ziger, Johannes Karl, Robert Lensi, Verena Pfahler, Bruno Roux, Matthias Schnier, Susanne Stark, Timothy Thrippleton, and Jennifer Watling. Elisabeth Thiem helped with laboratory work on soils. Michael Hochberg (CNRS), Rebecca Hardin (University of Michigan), Manuel Arroyo-Kalin (University of Durham, UK), and two anonymous reviewers provided useful comments on the manuscript. Funding was provided by two interdisciplinary programs of the CNRS, Amazonie and Ingenierie Ecologique, and by the French Ministry of Culture and Communication. NR 67 TC 55 Z9 58 U1 7 U2 99 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 27 PY 2010 VL 107 IS 17 BP 7823 EP 7828 DI 10.1073/pnas.0908925107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 588QQ UT WOS:000277088700041 PM 20385814 ER PT J AU Sato, M Hirota, T Reid, MJ Honma, M Kobayashi, H Iwadate, K Miyaji, T Shibata, KM AF Sato, Mayumi Hirota, Tomoya Reid, Mark J. Honma, Mareki Kobayashi, Hideyuki Iwadate, Kenzaburo Miyaji, Takeshi Shibata, Katsunori M. TI Distance to G14.33-0.64 in the Sagittarius Spiral Arm: H2O Maser Trigonometric Parallax with VERA SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE Galaxy: kinematics and dynamics; Galaxy: structure; ISM: H II regions; ISM: individual (G14.33-0.64); masers (H2O) ID STAR-FORMING REGIONS; H-II REGIONS; PULSAR ROTATION MEASURES; GALACTIC MAGNETIC-FIELD; IRAS POINT SOURCES; MILKY-WAY; METHANOL MASERS; MOLECULAR CLOUDS; CO SURVEY; ORION-KL AB We report on trigonometric parallax measurements for the Galactic star-forming region G14.33-0.64 toward the Sagittarius spiral arm. We conducted multi-epoch phase-referencing observations of an H2O maser source in G14.33-0.64 with the Japanese VLBI array VERA. We successfully detected a parallax of pi = 0.893 +/- 0.101 mas. corresponding to a source distance of d = 1.12 +/- 0.13 kpc, which is less than half of the kinematic distance for G14.33-0.64. Our new distance measurement demonstrates that the Sagittarius arm lies at a closer distance of similar to 1 kpc, instead of the previously assumed similar to 2-3 kpc from the kinematic distances. The previously suggested deviation of the Sagittarius arm toward the Galactic center from the symmetrically fitted model (Taylor & Cordes 1993, ApJ, 411, 674) is likely clue to large errors of the kinematic distances at low galactic longitudes. G14.33-0.64 most likely traces the near side of the Sagittarius arm. We attempted to fit the pitch angle of the arm with other parallax measurements along the arm, which yielded two possible pitch angles of i = 34.degrees 7 +/- 2.degrees 7 and i = 11.degrees 2 +/- 10.degrees 5. Our proper-motion measurements suggest that G14.33-0.64 has no significant peculiar motion relative to the differential rotation of the Galaxy (assumed to be in a circular orbit), indicating that the source motion is in good agreement with the Galactic rotation. C1 [Sato, Mayumi; Hirota, Tomoya; Honma, Mareki; Kobayashi, Hideyuki; Iwadate, Kenzaburo; Miyaji, Takeshi; Shibata, Katsunori M.] Natl Astron Observ, Mizusawa VLBI Observ, Mizusawa Ku, Oshu, Iwate 0230861, Japan. [Sato, Mayumi; Kobayashi, Hideyuki] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Sato, Mayumi; Reid, Mark J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hirota, Tomoya; Honma, Mareki; Kobayashi, Hideyuki; Shibata, Katsunori M.] Grad Univ Adv Studies, Dept Astron Sci, Mitaka, Tokyo 1818588, Japan. RP Sato, M (reprint author), Natl Astron Observ, Mizusawa VLBI Observ, Mizusawa Ku, 2-12 Hoshi Ga Oka, Oshu, Iwate 0230861, Japan. EM mayumi.sato@nao.ac.jp FU Japan Society for the Promotion of Science (JSPS) FX We are deeply grateful to an anonymous referee for his/her careful reading of the paper and for a number of invaluable suggestions. We would like to express our sincere gratitude to all staff members and students at VERA and Kagoshima University for their continuous support. MS gratefully acknowledges the financial support from the Research Fellowships of the Japan Society for the Promotion of Science (JSPS) for Young Scientists. This work was supported by Grant-in-Aid for JSPS Fellows. NR 72 TC 31 Z9 31 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD APR 25 PY 2010 VL 62 IS 2 BP 287 EP 299 DI 10.1093/pasj/62.2.287 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 624QP UT WOS:000279834900009 ER PT J AU Kaufman, AG Borrett, SR AF Kaufman, Anthony G. Borrett, Stuart R. TI Ecosystem network analysis indicators are generally robust to parameter uncertainty in a phosphorus model of Lake Sidney Lanier, USA SO ECOLOGICAL MODELLING LA English DT Article DE Ecosystem; Network analysis; Coefficient of variation; Uncertainty; Ascendency; Input output analysis; Ecosystem indicators ID SCIENTIFIC BASIS; STEADY-STATE; MANAGEMENT; FISHERIES; SENSITIVITY; ENVIRONMENT; DYNAMICS; SOCIETY; GROWTH AB Understanding how data uncertainty influences ecosystem analysis is critical as we move toward ecosystem-based management. Here, we investigate how 18 Ecological Network Analysis (ENA) indicators that characterize ecosystem growth, development, and condition are affected by uncertainty in an ecosystem model of Lake Sidney Lanier (USA). We applied ENA to 122 plausible parameterizations of the ecosystem developed by Borrett and Osidele (2007, Ecological Modelling 200, 371-387), and then used the coefficient of variation (CV) to compare system indicator variability. We considered Total System Throughput (TST) as a measure of the underlying model uncertainty and tested three hypotheses. First, we hypothesized that non-ratio indicators whose calculation includes the TST would be at least as variable as TST if not more variable. Second, we postulated that indicators calculated as ratios, with TST in the numerator and denominator would tend to be less variable than TST because its influence will cancel. Last, we expected the Average Mutual Information (AMI) to be less variable than TST because it is a bounded function. Our work shows that the 18 indicators grouped into four categories. The first group has significantly larger CVs than the CV for TST. In this group, model uncertainty is amplified rendering these three indicators less useful. The second group of four indicators shows no significant difference in variability with respect to TST. Finally, there are two groups whose CV values are significantly lower than that for TST. The least variable group includes the ratio-based indicators and Average Mutual Information. Due to their low variability, we conclude that these indicators are the most robust to the parameter uncertainty and most useful for ecosystem assessment and comparative ecosystem analysis. In summary, this work suggests that we can be as certain, or more certain, in most of the selected ENA indicators as we are in the parameters of the model analyzed. (C) 2010 Elsevier B.V. All rights reserved. C1 [Kaufman, Anthony G.; Borrett, Stuart R.] Univ N Carolina, Dept Biol & Marine Biol, Wilmington, NC 28401 USA. RP Kaufman, AG (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM Kaufmana@si.edu RI Borrett, Stuart/E-6586-2010 OI Borrett, Stuart/0000-0002-5759-3711 FU Systems Ecology and Ecoinformatics Laboratory at UNCW FX We would like to thank Susan Simmons, Fred Scharf, and Joe Pawlik for early reviews of this manuscript, and the members of the Systems Ecology and Ecoinformatics Laboratory at UNCW for encouragement and support. NR 50 TC 15 Z9 15 U1 2 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 J9 ECOL MODEL JI Ecol. Model. PD APR 24 PY 2010 VL 221 IS 8 BP 1230 EP 1238 DI 10.1016/j.ecolmodel.2009.12.018 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 582DD UT WOS:000276574900015 ER PT J AU Swaisgood, RR Wei, FW Wildt, DE Kouba, AJ Zhang, ZJ AF Swaisgood, Ronald R. Wei, Fuwen Wildt, David E. Kouba, Andrew J. Zhang, Zejun TI Giant panda conservation science: how far we have come SO BIOLOGY LETTERS LA English DT Editorial Material DE giant panda; conservation science; habitat analysis; spatial ecology; molecular census; sustainable populations ID LANDSCAPE; BIOLOGY AB The giant panda is a conservation icon, but science has been slow to take up its cause in earnest. In the past decade, researchers have been making up for lost time, as reflected in the flurry of activity reported at the symposium Conservation Science for Giant Pandas and Their Habitat at the 2009 International Congress for Conservation Biology (ICCB) in Beijing. In reports addressing topics ranging from spatial ecology to molecular censusing, from habitat recovery in newly established reserves to earthquake-induced habitat loss, from new insights into factors limiting carrying capacity to the uncertain effects of climate change, this symposium displayed the vibrant and blossoming application of science to giant panda conservation. Collectively, we find that we have come a long way, but we also reach an all-too-familiar conclusion: the more we know, the more challenges are revealed. While many earlier findings are supported, many of our assumptions are debatable. Here we discuss recent advancements in conservation science for giant pandas and suggest that the way forward is more direct application of emerging science to management and policy. C1 [Zhang, Zejun] San Diego Zoo, Inst Conserv Res, San Diego, CA USA. [Wei, Fuwen; Zhang, Zejun] Chinese Acad Sci, Inst Zool, Key Lab Anim Ecol & Conserv Biol, Beijing 100864, Peoples R China. [Wildt, David E.] Smithsonians Natl Zool Pk, Conserv & Res Ctr, Front Royal, VA USA. [Kouba, Andrew J.] Memphis Zoo, Memphis, TN 38112 USA. RP Swaisgood, RR (reprint author), San Diego Zoo, Inst Conserv Res, San Diego, CA USA. EM rswaisgood@sandiegozoo.org NR 20 TC 30 Z9 31 U1 12 U2 59 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1744-9561 J9 BIOL LETTERS JI Biol. Lett. PD APR 23 PY 2010 VL 6 IS 2 BP 143 EP 145 DI 10.1098/rsbl.2009.0786 PG 3 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 567GO UT WOS:000275432900039 PM 19864275 ER PT J AU Matzel, JEP Ishii, HA Joswiak, D Hutcheon, ID Bradley, JP Brownlee, D Weber, PK Teslich, N Matrajt, G McKeegan, KD MacPherson, GJ AF Matzel, J. E. P. Ishii, H. A. Joswiak, D. Hutcheon, I. D. Bradley, J. P. Brownlee, D. Weber, P. K. Teslich, N. Matrajt, G. McKeegan, K. D. MacPherson, G. J. TI Constraints on the Formation Age of Cometary Material from the NASA Stardust Mission SO SCIENCE LA English DT Article ID ALUMINUM-RICH INCLUSIONS; EARLY SOLAR-SYSTEM; REFRACTORY INCLUSIONS; CHONDRULES; ALLENDE; AL-26; CHONDRITES; 81P/WILD-2; NEBULA; METEORITES AB We measured the (26)Al-(26)Mg isotope systematics of a similar to 5-micrometer refractory particle, Coki, returned from comet 81P/Wild 2 in order to relate the time scales of formation of cometary inclusions to their meteoritic counterparts. The data show no evidence of radiogenic (26)Mg and define an upper limit to the abundance of (26)Al at the time of particle formation: (26)Al/(27)Al < 1 x 10(-5). The absence of (26)Al indicates that Coki formed >1.7 million years after the oldest solids in the solar system, calcium-and aluminum-rich inclusions (CAIs). The data suggest that high-temperature inner solar system material formed, was subsequently transferred to the Kuiper Belt, and was incorporated into comets several million years after CAI formation. C1 [Matzel, J. E. P.; Ishii, H. A.; Hutcheon, I. D.; Bradley, J. P.; Teslich, N.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Matzel, J. E. P.; Hutcheon, I. D.; Weber, P. K.] Lawrence Livermore Natl Lab, Glenn T Seaborg Inst, Livermore, CA 94550 USA. [Joswiak, D.; Brownlee, D.; Matrajt, G.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [McKeegan, K. D.] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. [MacPherson, G. J.] Natl Museum Nat Hist, Dept Mineral Sci, Smithsonian Inst, Washington, DC 20560 USA. RP Matzel, JEP (reprint author), Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. EM matzel2@llnl.gov RI McKeegan, Kevin/A-4107-2008; UCLA, SIMS/A-1459-2011 OI McKeegan, Kevin/0000-0002-1827-729X; FU Lawrence Livermore National Laboratory (LLNL) [DE-AC52-07NA27344, 06-ERI-001]; NASA [NNH07AG46I, NNH04AB47I] FX This work was performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory (LLNL) under contract DE-AC52-07NA27344. Supported by NASA grants NNH07AG46I (H. A. I.) and NNH04AB47I (I. D. H.) and by LLNL grant 06-ERI-001 (J.P.B.). NR 32 TC 38 Z9 38 U1 0 U2 10 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD APR 23 PY 2010 VL 328 IS 5977 BP 483 EP 486 DI 10.1126/science.1184741 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586YR UT WOS:000276952400038 PM 20185683 ER PT J AU Lee, CF Hasegawa, TI Hirano, N Palau, A Shang, H Ho, PTP Zhang, QZ AF Lee, Chin-Fei Hasegawa, Tatsuhiko I. Hirano, Naomi Palau, Aina Shang, Hsien Ho, Paul T. P. Zhang, Qizhou TI THE REFLECTION-SYMMETRIC WIGGLE OF THE YOUNG PROTOSTELLAR JET HH 211 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (HH 211); ISM: jets and outflows; stars: formation ID SIO LINE EMISSION; SUBMILLIMETER ARRAY; BINARY POPULATION; INTERSTELLAR JETS; CLASS-0 SOURCES; STAR-FORMATION; SHOCK-WAVES; OUTFLOW; EVOLUTION; CLOUDS AB HH 211 is a highly collimated jet originating from a nearby young Class 0 protostar. Here is a follow-up study of the jet with our previous observations at unprecedented resolution up to similar to 0.'' 3 in SiO (J = 8-7), CO (J = 3-2), and SO (N(J) = 8(9)-7(8)). SiO, CO, and SO can all be a good tracer of the HH 211 jet, tracing the internal shocks in the jet. Although the emissions of these molecules show roughly the same morphology of the jet, there are detailed differences. In particular, the CO emission traces the jet closer to the source than the SiO and SO emissions. In addition, in the better resolved internal shocks, both the CO and SO emission are seen slightly ahead of the SiO emission. The jet is clearly seen on both sides of the source with more than one cycle of wiggle. The wiggle is reflection-symmetric about the source and can be reasonably fitted by an orbiting source jet model. The best-fit parameters suggest that the source itself could be a very low mass protobinary with a total mass of similar to 60 M(Jup) and a binary separation of similar to 4.6 AU. The abundances of SiO and SO in the gas phase are found to be highly enhanced in the jet as compared to the quiescent molecular clouds, even close to within 300 AU from the source where the dynamical timescale is < 10 yr. The abundance enhancements of these molecules are closely related to the internal shocks. The detected SiO is either the consequence of the release of Si-bearing material from dust grains or of its formation via gas chemistry in the shocks. The SO, on the other hand, seems to form via gas chemistry in the shocks. C1 [Lee, Chin-Fei; Hasegawa, Tatsuhiko I.; Hirano, Naomi; Shang, Hsien; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Palau, Aina] CSIC, Lab Astrofis Estelar & Exoplanetas, Ctr Astrobiol, INTA, E-28691 Madrid, Spain. [Ho, Paul T. P.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, CF (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM cflee@asiaa.sinica.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 NR 43 TC 27 Z9 27 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2010 VL 713 IS 2 BP 731 EP 737 DI 10.1088/0004-637X/713/2/731 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 578XF UT WOS:000276329400003 ER PT J AU Bush, SJ Cox, TJ Hayward, CC Thilker, D Hernquist, L Besla, G AF Bush, Stephanie J. Cox, T. J. Hayward, Christopher C. Thilker, David Hernquist, Lars Besla, Gurtina TI SPIRAL-INDUCED STAR FORMATION IN THE OUTER DISKS OF GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: spiral; galaxies: structure; ultraviolet: galaxies ID PARTICLE HYDRODYNAMICS SIMULATIONS; EXTENDED ULTRAVIOLET DISK; GALACTIC DISKS; FORMATION LAW; FORMATION THRESHOLDS; STELLAR DISKS; BLACK-HOLES; H-ALPHA; EVOLUTION; MODEL AB The outer regions of galactic disks have received increased attention since ultraviolet observations with Galaxy Evolution Explorer demonstrated that nearly 30% of galaxies have UV emission beyond their optical extents, indicating star formation activity. These galaxies have been termed extended UV (XUV) disks. Here, we address whether these observations contradict the gas surface density threshold for star formation inferred from Ha radial profiles of galaxies. We run smoothed particle hydrodynamic simulations of isolated disk galaxies with fiducial star formation prescriptions and show that over-densities owing to the presence of spiral structure can induce star formation in extended gas disks. For direct comparison with observations, we use the three-dimensional radiative transfer code Sunrise to create simulated FUV and K(s)-band images. We find that galaxies classified as Type I XUV disks are a natural consequence of spiral patterns, but we are unable to reproduce Type II XUV disks. We also compare our results to studies of the Kennicutt-Schmidt relation in outer disks. C1 [Bush, Stephanie J.; Cox, T. J.; Hayward, Christopher C.; Hernquist, Lars; Besla, Gurtina] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02143 USA. [Thilker, David] Johns Hopkins Univ, Ctr Astrophys Sci, Baltimore, MD 21218 USA. RP Bush, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02143 USA. EM sbush@cfa.harvard.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 NR 64 TC 25 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2010 VL 713 IS 2 BP 780 EP 799 DI 10.1088/0004-637X/713/2/780 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 578XF UT WOS:000276329400007 ER PT J AU Wright, NJ Drake, JJ Drew, JE Vink, JS AF Wright, N. J. Drake, J. J. Drew, J. E. Vink, J. S. TI THE MASSIVE STAR-FORMING REGION CYGNUS OB2. II. INTEGRATED STELLAR PROPERTIES AND THE STAR FORMATION HISTORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE open clusters and associations: individual (Cygnus OB2); stars: early-type; stars: formation; stars: pre-main sequence ID X-RAY-EMISSION; ORION ULTRADEEP PROJECT; ALL-SKY SURVEY; T-TAURI STARS; CIRCUMSTELLAR DISKS; NEBULA CLUSTER; YOUNG STARS; CYG-OB2 ASSOCIATION; MOLECULAR CLOUDS; ARCHES CLUSTER AB Cygnus OB2 is the nearest example of a massive star-forming region (SFR), containing over 50 O-type stars and hundreds of B-type stars. We have analyzed the properties of young stars in two fields in Cyg OB2 using the recently published deep catalog of Chandra X-ray point sources with complementary optical and near-IR photometry. Our sample is complete to similar to 1 M(circle dot) (excluding A- and B-type stars that do not emit X-rays), making this the deepest study of the stellar properties and star formation history in Cyg OB2 to date. From Siess et al. isochrone fits to the near-IR color-magnitude diagram, we derive ages of 3.5(-1.0)(+0.75) and 5.25(-1.0)(+1.5) Myr for sources in the two fields, both with considerable spreads around the pre-main-sequence isochrones. The presence of a stellar population somewhat older than the present-day O-type stars, also fits in with the low fraction of sources with inner circumstellar disks (as traced by the K-band excess) that we find to be very low, but appropriate for a population of age similar to 5 Myr. We also find that the region lacks a population of highly embedded sources that is often observed in young SFRs, suggesting star formation in the vicinity has declined. We measure the stellar mass functions (MFs) in this limit and find a power-law slope of Gamma = -1.09 +/- 0.13, in good agreement with the global mean value estimated by Kroupa. A steepening of the slope at higher masses is observed and suggested as due to the presence of the previous generation of stars that have lost their most massive members. Finally, combining our MF and an estimate of the radial density profile of the association suggests a total mass of Cyg OB2 of similar to 3 x 10(4) M(circle dot), similar to that of many of our Galaxy's most massive SFRs. C1 [Wright, N. J.; Drake, J. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Drew, J. E.] Univ Hertfordshire, Ctr Astron Res Sci & Technol, Res Inst, Hatfield AL10 9AB, Herts, England. [Vink, J. S.] Armagh Observ, Armagh BT61 9DG, North Ireland. RP Wright, NJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM nwright@head.cfa.harvard.edu OI Drew, Janet/0000-0003-1192-7082 FU NASA [NAS8-39073]; NSF; UKIDSS; UKATC; CASU; SAO FX We thank Phil Lucas and Yvonne Unruh for careful reading of this paper and helpful discussions. We also thank the anonymous referee for helpful suggestions that have improved this work. This research has made use of data from the Chandra X-ray Observatory (operated by the Smithsonian Astrophysical Observatory on behalf of NASA) obtained from the Chandra Data Archive. 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), 2MASS (a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF), and UKIDSS (supported by the UKATC and CASU). J. J. D. was funded by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC) during the course of this research and thanks the CXC director, Harvey Tananbaum, and the science team for advice and support. N. J. W. acknowledges an SAO Pre-doctoral Fellowship. NR 90 TC 51 Z9 51 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2010 VL 713 IS 2 BP 871 EP 882 DI 10.1088/0004-637X/713/2/871 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 578XF UT WOS:000276329400013 ER PT J AU Assef, RJ Kochanek, CS Brodwin, M Cool, R Forman, W Gonzalez, AH Hickox, RC Jones, C Le Floc'h, E Moustakas, J Murray, SS Stern, D AF Assef, R. J. Kochanek, C. S. Brodwin, M. Cool, R. Forman, W. Gonzalez, A. H. Hickox, R. C. Jones, C. Le Floc'h, E. Moustakas, J. Murray, S. S. Stern, D. TI LOW-RESOLUTION SPECTRAL TEMPLATES FOR ACTIVE GALACTIC NUCLEI AND GALAXIES FROM 0.03 TO 30 mu m SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: distances and redshifts; galaxies: photometry; quasars: general ID WIDE-FIELD SURVEY; STELLAR POPULATION SYNTHESIS; IRAC SHALLOW SURVEY; X-RAY SOURCES; ENERGY-DISTRIBUTIONS; SKY-SURVEY; BOOTES-FIELD; PHOTOMETRIC REDSHIFTS; SURVEY TELESCOPE; DEEP AB We present a set of low-resolution empirical spectral energy distribution (SED) templates for active galactic nuclei (AGNs) and galaxies in the wavelength range from 0.03 mu m to 30 mu m based on the multi-wavelength photometric observations of the NOAO Deep-Wide Field Survey Bootes field and the spectroscopic observations of the AGN and Galaxy Evolution Survey. Our training sample is comprised of 14,448 galaxies in the redshift range 0 less than or similar to z less than or similar to 1 and 5347 likely AGNs in the range 0 less than or similar to z less than or similar to 5.58. The galaxy templates correspond to the SED templates presented in 2008 by Assef et al. extended into the UV and mid-IR by the addition of FUV and NUV GALEX and MIPS 24 mu m data for the field. We use our templates to determine photometric redshifts for galaxies and AGNs. While they are relatively accurate for galaxies (sigma(z)/(1 + z) = 0.04, with 5% outlier rejection), their accuracies for AGNs are a strong function of the luminosity ratio between the AGN and galaxy components. Somewhat surprisingly, the relative luminosities of the AGN and its host are well determined even when the photometric redshift is significantly in error. We also use our templates to study the mid-IR AGN selection criteria developed by Stern et al. in 2005 and Lacy et al. in 2004. We find that the Stern et al. criterion suffers from significant incompleteness when there is a strong host galaxy component and at z similar or equal to 4.5, when the broad H alpha emission line is redshifted into the [3.6] band, but that it is little contaminated by low-and intermediate-redshift galaxies. The Lacy et al. criterion is not affected by incompleteness at z similar or equal to 4.5 and is somewhat less affected by strong galaxy host components, but is heavily contaminated by low-redshift star-forming galaxies. Finally, we use our templates to predict the color-color distribution of sources in the upcoming Wide-Field Infrared Survey Explorer (WISE) mission and define a color criterion to select AGNs analogous to those developed for IRAC photometry. We estimate that in between 640,000 and 1,700,000 AGNs will be identified by these criteria, but without additional information, WISE-selected quasars will have serious completeness problems for z similar or equal to 3.4. C1 [Assef, R. J.; Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Cool, R.] Princeton Univ, Princeton, NJ 08540 USA. [Gonzalez, A. H.] Univ Florida, Bryant Space Sci Ctr, Dept Astron, Gainesville, FL 32611 USA. [Brodwin, M.; Forman, W.; Hickox, R. C.; Jones, C.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Le Floc'h, E.] CEA Saclay, Serv Astrophys, F-91191 Gif Sur Yvette, France. [Moustakas, J.] Univ Calif San Diego, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Assef, RJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. EM rjassef@astronomy.ohio-state.edu FU W. M. Keck Foundation; NASA; National Optical Astronomy Observatory (NOAO) FX We thank all the people in the NDWFS, FLAMEX, and SDWFS collaborations who did not directly participate in this work. We also thank Edward L. Wright for providing us with the filer functions of the WISE mission passbands. We thank the anonymous referee for providing useful comments and suggestions that improved this paper. Support for M. B. was provided by the W. M. Keck Foundation. The work of D. S. was carried out at Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. The AGES observations were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. This work made use of images and/or data products provided by the NOAO Deep Wide-Field Survey (Jannuzi & Dey 1999; B. T. Jannuzi et al. 2010, in preparation; A. Dey et al. 2010, in preparation), which is supported by the National Optical Astronomy Observatory (NOAO). This research draws upon data provided by Dr. Buell Jannuzi and Dr. Arjun Dey as distributed by the NOAO Science Archive. NOAO is operated by AURA, Inc., under a cooperative agreement with the National Science Foundation. NR 64 TC 131 Z9 131 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2010 VL 713 IS 2 BP 970 EP 985 DI 10.1088/0004-637X/713/2/970 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 578XF UT WOS:000276329400022 ER PT J AU Blum, JL Miller, JM Cackett, E Yamaoka, K Takahashi, H Raymond, J Reynolds, CS Fabian, AC AF Blum, J. L. Miller, J. M. Cackett, E. Yamaoka, K. Takahashi, H. Raymond, J. Reynolds, C. S. Fabian, A. C. TI SUZAKU OBSERVATIONS OF THE BLACK HOLE H1743-322 IN OUTBURST SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; stars: individual (H1743-322); X-rays: binaries ID QUASI-PERIODIC OSCILLATIONS; ACTIVE GALACTIC NUCLEI; ACCRETION DISK WIND; X-RAY REFLECTION; HIGH-FREQUENCY; GRS 1915+105; MICROQUASAR H1743-322; LOW/HARD STATE; XTE J1650-500; JET AB We observed the Galactic black hole candidate H1743-322 with Suzaku for approximately 32 ks, while the source was in a low/hard state during its 2008 outburst. We collected and analyzed the data with the HXD/PIN, HXD/GSO, and XIS cameras spanning the energy range 0.7-200 keV. Fits to the spectra with simple models fail to detect narrow Fe XXV and Fe XXVI absorption lines, with 90% confidence upper limits of 3.5 and 2.5 eV on the equivalent width, respectively. These limits are commensurate with those in the very high state, but are well below the equivalent widths of lines detected in the high/soft state, suggesting that disk winds are partially state-dependent. We discuss these results in the context of previous detections of ionized Fe absorption lines in H1743-322 and connections to winds and jets in accreting Additionally, we report the possible detection of disk reflection features, including an Fe K emission line. C1 [Blum, J. L.; Miller, J. M.; Cackett, E.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Yamaoka, K.] Aoyama Gakuin Univ, Dept Math & Phys, Tokyo, Japan. [Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Raymond, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reynolds, C. S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Blum, JL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. RI XRAY, SUZAKU/A-1808-2009 NR 42 TC 17 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2010 VL 713 IS 2 BP 1244 EP 1248 DI 10.1088/0004-637X/713/2/1244 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 578XF UT WOS:000276329400044 ER PT J AU Chornock, R Filippenko, AV Li, WD Silverman, JM AF Chornock, Ryan Filippenko, Alexei V. Li, Weidong Silverman, Jeffrey M. TI LARGE LATE-TIME ASPHERICITIES IN THREE TYPE IIP SUPERNOVAE SO ASTROPHYSICAL JOURNAL LA English DT Article DE polarization; supernovae: individual (SN 2006my, SN 2006ov, SN 2007aa) ID CORE-COLLAPSE SUPERNOVAE; EXPANDING PHOTOSPHERE METHOD; AUTOMATIC IMAGING TELESCOPE; BROAD-LINE REGIONS; IA SUPERNOVA; P SUPERNOVAE; INTERSTELLAR POLARIZATION; NI-56 EJECTA; CIRCUMSTELLAR ENVIRONMENT; ASYMMETRIC EXPLOSION AB Type II-plateau supernovae (SNe IIP) are the results of the explosions of red supergiants and are the most common subclass of core-collapse supernovae. Past observations have shown that the outer layers of the ejecta of SNe IIP are largely spherical, but the degree of asphericity increases toward the core. We present evidence for high degrees of asphericity in the inner cores of three recent SNe IIP (SNe 2006my, 2006ov, and 2007aa), as revealed by late-time optical spectropolarimetry. The three objects were all selected to have very low interstellar polarization (ISP), which minimizes the uncertainties in ISP removal and allows us to use the continuum polarization as a tracer of asphericity. The three objects have intrinsic continuum polarizations in the range of 0.83%-1.56% in observations taken after the end of the photometric plateau, with the polarization dropping to almost zero at the wavelengths of strong emission lines. Our observations of SN 2007aa at earlier times, taken on the photometric plateau, show contrastingly smaller continuum polarizations (similar to 0.1%). The late-time H alpha and [O I] line profiles of SN 2006ov provide further evidence for asphericities in the inner ejecta. Such high core polarizations in very ordinary core-collapse supernovae provide further evidence that essentially all core-collapse supernova explosions are highly aspherical, even if the outer parts of the ejecta show only small deviations from spherical symmetry. C1 [Chornock, Ryan; Filippenko, Alexei V.; Li, Weidong; Silverman, Jeffrey M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Chornock, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rchornock@cfa.harvard.edu FU W.M. Keck Foundation; NSF [AST-0607485, AST-0908886]; TABASGO Foundation; Sun Microsystems, Inc.; Hewlett-Packard Company, AutoScope Corporation, Lick Observatory; University of California; Sylvia & Jim Katzman Foundation FX We thank Douglas C. Leonard for supplying us with his SNe 1999em and 2004dj data and Ryan J. Foley, Mohan Ganeshalingam, Matthew Moore, and Thea N. Steele for their assistance with some of the observations. 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; it was made possible by the generous financial support of the W.M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. We also thank the expert assistance of the Keck and Lick staffs in making these observations possible. A.V.F.'s supernova group at U.C. Berkeley has been supported by NSF grants AST-0607485 and AST-0908886, as well as by the TABASGO Foundation. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. NR 101 TC 20 Z9 20 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 20 PY 2010 VL 713 IS 2 BP 1363 EP 1375 DI 10.1088/0004-637X/713/2/1363 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 578XF UT WOS:000276329400056 ER PT J AU Basri, G Walkowicz, LM Batalha, N Gilliland, RL Jenkins, J Borucki, WJ Koch, D Caldwell, D Dupree, AK Latham, DW Meibom, S Howell, S Brown, T AF Basri, Gibor Walkowicz, Lucianne M. Batalha, Natalie Gilliland, Ronald L. Jenkins, Jon Borucki, William J. Koch, David Caldwell, Doug Dupree, Andrea K. Latham, David W. Meibom, Soren Howell, Steve Brown, Tim TI PHOTOMETRIC VARIABILITY IN KEPLER TARGET STARS: THE SUN AMONG STARS-A FIRST LOOK SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: activity; starspots; stars: statistics ID ROTATION AB The Kepler mission provides an exciting opportunity to study the light curves of stars with unprecedented precision and continuity of coverage. This is the first look at a large sample of stars with photometric data of a quality that has heretofore been only available for our Sun. It provides the first opportunity to compare the irradiance variations of our Sun to a large cohort of stars ranging from very similar to rather different stellar properties, at a wide variety of ages. Although Kepler data are in an early phase of maturity, and we only analyze the first month of coverage, it is sufficient to garner the first meaningful measurements of our Sun's variability in the context of a large cohort of main-sequence stars in the solar neighborhood. We find that nearly half of the full sample is more active than the active Sun, although most of them are not more than twice as active. The active fraction is closer to a third for the stars most similar to the Sun, and rises to well more than half for stars cooler than mid-K spectral types. C1 [Basri, Gibor; Walkowicz, Lucianne M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Batalha, Natalie; Jenkins, Jon; Borucki, William J.; Koch, David; Caldwell, Doug] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Dupree, Andrea K.; Latham, David W.; Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Howell, Steve] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Brown, Tim] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. RP Basri, G (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU Kepler Fellowship; NASA's Science Mission Directorate FX The authors thank the entire Kepler Mission team, including the engineers and managers who were so pivotal in the ultimate success of the mission. L. W. is grateful for the support of the Kepler Fellowship for the Study of Planet- Bearing Stars. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. NR 11 TC 73 Z9 73 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L155 EP L159 DI 10.1088/2041-8205/713/2/L155 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900015 ER PT J AU Borucki, WJ Koch, DG Brown, TM Basri, G Batalha, NM Caldwell, DA Cochran, WD Dunham, EW Gautier, TN Geary, JC Gilliland, RL Howell, SB Jenkins, JM Latham, DW Lissauer, JJ Marcy, GW Monet, D Rowe, JF Sasselov, D AF Borucki, William J. Koch, David G. Brown, Timothy M. Basri, Gibor Batalha, Natalie M. Caldwell, Douglas A. Cochran, William D. Dunham, Edward W. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Howell, Steve B. Jenkins, Jon M. Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Monet, David Rowe, Jason F. Sasselov, Dimitar TI KEPLER-4b: A HOT NEPTUNE-LIKE PLANET OF A G0 STAR NEAR MAIN-SEQUENCE TURNOFF SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: fundamental parameters; stars: individual (Kepler-4, KIC 11853905, 2MASS 19022767+5008087) ID TRANSIT LIGHT-CURVE; SUPER-EARTH; STELLAR; PARAMETERS; RADII; EXOPLANETS; EVOLUTION; PROJECT; TRES-1; MODELS AB Early time-series photometry from NASA's Kepler spacecraft has revealed a planet transiting the star we term Kepler-4, at R.A. = 19(h)02(m)27.(s)68, delta = +50 degrees 08'08 '' 7. The planet has an orbital period of 3.213 days and shows transits with a relative depth of 0.87 x 10(-3) and a duration of about 3.95 hr. Radial velocity (RV) measurements from the Keck High Resolution Echelle Spectrometer show a reflex Doppler signal of 9.3(-1.9)(+1.1) m s(-1), consistent with a low-eccentricity orbit with the phase expected from the transits. Various tests show no evidence for any companion star near enough to affect the light curve or the RVs for this system. From a transit-based estimate of the host star's mean density, combined with analysis of high-resolution spectra, we infer that the host star is near turnoff from the main sequence, with estimated mass and radius of 1.223(-0.091)(+0.053) M(circle dot) and 1.487(-0.084)(+0.071) R(circle dot).We estimate the planet mass and radius to be {M(P), R(P)} = {24.5 +/- 3.8 M(circle plus), 3.99 +/- 0.21 R(circle plus)}. The planet's density is near 1.9 g cm(-3); it is thus slightly denser and more massive than Neptune, but about the same size. C1 [Borucki, William J.; Koch, David G.; Caldwell, Douglas A.; Jenkins, Jon M.; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, Timothy M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Basri, Gibor; Marcy, Geoffrey W.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Cochran, William D.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Geary, John C.; Latham, David W.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA. [Monet, David] USN Observ, Flagstaff, AZ 86002 USA. RP Borucki, WJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU W. M. Keck Foundation; NASA's Science Mission Directorate 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.; Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We are grateful first to the entire Kepler team, past and present. Their tireless efforts were all essential to the success of the mission. For special advice and assistance, we thank Lars Buchhave, David Ciardi, Megan Crane, Willie Torres, Mike Haas, and Riley Duran. NR 32 TC 66 Z9 66 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L126 EP L130 DI 10.1088/2041-8205/713/2/L126 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900009 ER PT J AU Caldwell, DA Kolodziejczak, JJ Van Cleve, JE Jenkins, JM Gazis, PR Argabright, VS Bachtell, EE Dunham, EW Geary, JC Gilliland, RL Chandrasekaran, H Li, J Tenenbaum, P Wu, H Borucki, WJ Bryson, ST Dotson, JL Haas, MR Koch, DG AF Caldwell, Douglas A. Kolodziejczak, Jeffery J. Van Cleve, Jeffrey E. Jenkins, Jon M. Gazis, Paul R. Argabright, Vic S. Bachtell, Eric E. Dunham, Edward W. Geary, John C. Gilliland, Ronald L. Chandrasekaran, Hema Li, Jie Tenenbaum, Peter Wu, Hayley Borucki, William J. Bryson, Stephen T. Dotson, Jessie L. Haas, Michael R. Koch, David G. TI INSTRUMENT PERFORMANCE IN KEPLER's FIRST MONTHS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: photometers; planetary systems; space vehicles: instruments; techniques: photometric AB The Kepler Mission relies on precise differential photometry to detect the 80 parts per million (ppm) signal from an Earth-Sun equivalent transit. Such precision requires superb instrument stability on timescales up to similar to 2 days and systematic error removal to better than 20 ppm. To this end, the spacecraft and photometer underwent 67 days of commissioning, which included several data sets taken to characterize the photometer performance. Because Kepler has no shutter, we took a series of dark images prior to the dust cover ejection, from which we measured the bias levels, dark current, and read noise. These basic detector properties are essentially unchanged from ground-based tests, indicating that the photometer is working as expected. Several image artifacts have proven more complex than when observed during ground testing, as a result of their interactions with starlight and the greater thermal stability in flight, which causes the temperature-dependent artifact variations to be on the timescales of transits. Because of Kepler's unprecedented sensitivity and stability, we have also seen several unexpected systematics that affect photometric precision. We are using the first 43 days of science data to characterize these effects and to develop detection and mitigation methods that will be implemented in the calibration pipeline. Based on early testing, we expect to attain Kepler's planned photometric precision over 80%-90% of the field of view. C1 [Caldwell, Douglas A.; Van Cleve, Jeffrey E.; Jenkins, Jon M.; Gazis, Paul R.; Chandrasekaran, Hema; Li, Jie; Tenenbaum, Peter; Wu, Hayley] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Kolodziejczak, Jeffery J.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Argabright, Vic S.; Bachtell, Eric E.] Ball Aerosp & Technol Corp, Boulder, CO 80301 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Geary, John C.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Caldwell, DA (reprint author), NASA, Ames Res Ctr, SETI Inst, MS 244-30, Moffett Field, CA 94035 USA. EM douglas.caldwell@nasa.gov RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU NASA's Science Mission Directorate FX We gratefully acknowledge the years of work by the many hundred members of the Kepler Team who conceived, designed, built, and now operate this wonderful mission. Funding for this Discovery mission is provided by NASA's Science Mission Directorate. NR 8 TC 88 Z9 88 U1 3 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L92 EP L96 DI 10.1088/2041-8205/713/2/L92 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900003 ER PT J AU Chaplin, WJ Appourchaux, T Elsworth, Y Garcia, RA Houdek, G Karoff, C Metcalfe, TS Molenda-Zakowicz, J Monteiro, MJPFG Thompson, MJ Brown, TM Christensen-Dalsgaard, J Gilliland, RL Kjeldsen, H Borucki, WJ Koch, D Jenkins, JM Ballot, J Basu, S Bazot, M Bedding, TR Benomar, O Bonanno, A Brandao, IM Bruntt, H Campante, TL Creevey, OL Di Mauro, MP Dogan, G Dreizler, S Eggenberger, P Esch, L Fletcher, ST Frandsen, S Gai, N Gaulme, P Handberg, R Hekker, S Howe, R Huber, D Korzennik, SG Lebrun, JC Leccia, S Martic, M Mathur, S Mosser, B New, R Quirion, PO Regulo, C Roxburgh, IW Salabert, D Schou, J Sousa, SG Stello, D Verner, GA Arentoft, T Barban, C Belkacem, K Benatti, S Biazzo, K Boumier, P Bradley, PA Broomhall, AM Buzasi, DL Claudi, RU Cunha, MS D'Antona, F Deheuvels, S Derekas, A Hernandez, AG Giampapa, MS Goupil, MJ Gruberbauer, M Guzik, JA Hale, SJ Ireland, MJ Kiss, LL Kitiashvili, IN Kolenberg, K Korhonen, H Kosovichev, AG Kupka, F Lebreton, Y Leroy, B Ludwig, HG Mathis, S Michel, E Miglio, A Montalban, J Moya, A Noels, A Noyes, RW Palle, PL Piau, L Preston, HL Cortes, TR Roth, M Sato, KH Schmitt, J Serenelli, AM Aguirre, VS Stevens, IR Suarez, JC Suran, MD Trampedach, R Turck-Chieze, S Uytterhoeven, K Ventura, R Wilson, PA AF Chaplin, W. J. Appourchaux, T. Elsworth, Y. Garcia, R. A. Houdek, G. Karoff, C. Metcalfe, T. S. Molenda-Zakowicz, J. Monteiro, M. J. P. F. G. Thompson, M. J. Brown, T. M. Christensen-Dalsgaard, J. Gilliland, R. L. Kjeldsen, H. Borucki, W. J. Koch, D. Jenkins, J. M. Ballot, J. Basu, S. Bazot, M. Bedding, T. R. Benomar, O. Bonanno, A. Brandao, I. M. Bruntt, H. Campante, T. L. Creevey, O. L. Di Mauro, M. P. Dogan, G. Dreizler, S. Eggenberger, P. Esch, L. Fletcher, S. T. Frandsen, S. Gai, N. Gaulme, P. Handberg, R. Hekker, S. Howe, R. Huber, D. Korzennik, S. G. Lebrun, J. C. Leccia, S. Martic, M. Mathur, S. Mosser, B. New, R. Quirion, P. -O. Regulo, C. Roxburgh, I. W. Salabert, D. Schou, J. Sousa, S. G. Stello, D. Verner, G. A. Arentoft, T. Barban, C. Belkacem, K. Benatti, S. Biazzo, K. Boumier, P. Bradley, P. A. Broomhall, A. -M. Buzasi, D. L. Claudi, R. U. Cunha, M. S. D'Antona, F. Deheuvels, S. Derekas, A. Garcia Hernandez, A. Giampapa, M. S. Goupil, M. J. Gruberbauer, M. Guzik, J. A. Hale, S. J. Ireland, M. J. Kiss, L. L. Kitiashvili, I. N. Kolenberg, K. Korhonen, H. Kosovichev, A. G. Kupka, F. Lebreton, Y. Leroy, B. Ludwig, H. -G. Mathis, S. Michel, E. Miglio, A. Montalban, J. Moya, A. Noels, A. Noyes, R. W. Palle, P. L. Piau, L. Preston, H. L. Roca Cortes, T. Roth, M. Sato, K. H. Schmitt, J. Serenelli, A. M. Aguirre, V. Silva Stevens, I. R. Suarez, J. C. Suran, M. D. Trampedach, R. Turck-Chieze, S. Uytterhoeven, K. Ventura, R. Wilson, P. A. TI THE ASTEROSEISMIC POTENTIAL OF KEPLER: FIRST RESULTS FOR SOLAR-TYPE STARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: interiors; stars: late-type; stars: oscillations ID TURBULENT CONVECTION; STELLAR OSCILLATIONS; PULSATIONAL STABILITY; ABUNDANCE ANALYSIS; HR DIAGRAM; EXCITATION; MODES; INTERFEROMETRY; AMPLITUDES; PARAMETERS AB We present preliminary asteroseismic results from Kepler on three G-type stars. The observations, made at one-minute cadence during the first 33.5 days of science operations, reveal high signal-to-noise solar-like oscillation spectra in all three stars: about 20 modes of oscillation may be clearly distinguished in each star. We discuss the appearance of the oscillation spectra, use the frequencies and frequency separations to provide first results on the radii, masses, and ages of the stars, and comment in the light of these results on prospects for inference on other solar-type stars that Kepler will observe. C1 [Chaplin, W. J.; Elsworth, Y.; Karoff, C.; Hekker, S.; Broomhall, A. -M.; Hale, S. J.; Stevens, I. R.] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Appourchaux, T.; Benomar, O.; Gaulme, P.; Boumier, P.] Univ Paris 11, CNRS, Inst Astrophys Spatiale, UMR8617, F-91405 Orsay, France. [Garcia, R. A.; Mathis, S.; Piau, L.; Sato, K. H.; Turck-Chieze, S.; Uytterhoeven, K.] Univ Paris Diderot, IRFU, CNRS, CEA,DSM,Lab AIM,SAp, F-91191 Gif Sur Yvette, France. [Houdek, G.; Kolenberg, K.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Metcalfe, T. S.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Metcalfe, T. S.] Natl Ctr Atmospher Res, Div Comp Sci, Boulder, CO 80307 USA. [Molenda-Zakowicz, J.] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Monteiro, M. J. P. F. G.; Bazot, M.; Brandao, I. M.; Campante, T. L.; Sousa, S. G.; Cunha, M. S.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Thompson, M. J.] Univ Sheffield, Sch Math & Stat, Sheffield S3 7RH, S Yorkshire, England. [Brown, T. M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Christensen-Dalsgaard, J.; Kjeldsen, H.; Campante, T. L.; Dogan, G.; Frandsen, S.; Handberg, R.; Quirion, P. -O.; Arentoft, T.] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Gilliland, R. L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Jenkins, J. M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Ballot, J.] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Basu, S.; Esch, L.; Gai, N.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bedding, T. R.; Huber, D.; Stello, D.; Derekas, A.; Ireland, M. J.; Kiss, L. L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Bonanno, A.; Ventura, R.] INAF Osservatorio Astrofis Catania, I-95123 Catania, Italy. [Bruntt, H.; Goupil, M. J.] Observ Paris, F-92190 Meudon, France. [Creevey, O. L.; Regulo, C.; Salabert, D.; Roca Cortes, T.] Univ La Laguna, Dept Astrofis, E-28207 Tenerife, Spain. [Creevey, O. L.; Regulo, C.; Salabert, D.; Palle, P. L.; Roca Cortes, T.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Di Mauro, M. P.] Ist Astrofis Spaziale & Fis Cosm, INAF IASF Roma, I-00133 Rome, Italy. [Dreizler, S.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Eggenberger, P.] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland. [Fletcher, S. T.; New, R.] Sheffield Hallam Univ, Fac Arts Comp Engn & Sci, Mat Engn Res Inst, Sheffield S1 1WB, S Yorkshire, England. [Gai, N.] Beijing Normal Univ, Beijing 100875, Peoples R China. [Howe, R.; Giampapa, M. S.] Natl Opt Astron Observ, Natl Solar Observ, Tucson, AZ 85726 USA. [Korzennik, S. G.; Noyes, R. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lebrun, J. C.; Martic, M.] Univ Versailles St Quentin, CNRS, LATMOS, F-91371 Verrieres Le Buisson, France. [Leccia, S.] INAF OAC, I-80131 Naples, Italy. [Mathur, S.] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Mosser, B.; Barban, C.; Deheuvels, S.; Leroy, B.; Michel, E.] Univ Paris 06, CNRS, LESIA, Observ Paris, F-92195 Meudon, France. [Quirion, P. -O.] Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. [Roxburgh, I. W.; Verner, G. A.] Univ London, Astron Unit, London E1 4NS, England. [Schou, J.; Kosovichev, A. G.] Stanford Univ, HEPL, Stanford, CA 94305 USA. [Belkacem, K.; Miglio, A.; Montalban, J.; Noels, A.] Univ Liege, Dept Astrophys Geophys & Oceanog, B-4000 Liege 1, Belgium. [Benatti, S.] Univ Padua, CISAS, I-35131 Padua, Italy. [Biazzo, K.] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Bradley, P. A.; Guzik, J. A.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Buzasi, D. L.; Preston, H. L.] Eureka Sci, Oakland, CA 94602 USA. [Claudi, R. U.] INAF Astron Observ Padova, I-35122 Padua, Italy. [D'Antona, F.] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Derekas, A.; Kiss, L. L.] Hungarian Acad Sci, Konkoly Observ Budapest, Budapest, Hungary. [Garcia Hernandez, A.; Suarez, J. C.] CSIC, Inst Astrofis Andalucia, Granada, Spain. [Gruberbauer, M.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kitiashvili, I. N.] Stanford Univ, Ctr Turbulence Res, Stanford, CA 94305 USA. [Korhonen, H.] European So Observ, D-85748 Garching, Germany. [Kupka, F.] Univ Vienna, Fac Math, A-1090 Vienna, Austria. [Lebreton, Y.; Ludwig, H. -G.] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92195 Meudon, France. [Moya, A.] CSIC, INTA, LAEX, CAB, Madrid 28691, Spain. [Preston, H. L.] Univ S Africa, Dept Math Sci, ZA-0003 Pretoria, South Africa. [Roth, M.] Kiepenheuer Inst Sonnenphys, D-79104 Freiburg, Germany. [Schmitt, J.] Observ Haute Provence, F-04870 St Michel lObservatoire, France. [Serenelli, A. M.; Aguirre, V. Silva] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Suran, M. D.] Romanian Acad, Astron Inst, RO-40557 Bucharest, Romania. [Trampedach, R.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Wilson, P. A.] Nord Opt Telescope, E-38700 Santa Cruz De La Palma, Santa Cruz Tene, Spain. [Wilson, P. A.] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. RP Chaplin, WJ (reprint author), Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. RI Ballot, Jerome/G-1019-2010; Sousa, Sergio/I-7466-2013; Brandao, Isa/M-5172-2013; Monteiro, Mario J.P.F.G./B-4715-2008; Karoff, Christoffer/L-1007-2013; Lebreton, Yveline/N-2268-2014; Hale, Steven/E-3472-2015; Palle, Pere/H-4720-2015; Suarez, Juan Carlos/C-1015-2009; Ventura, Rita/B-7524-2016; Korhonen, Heidi/E-3065-2016; Derekas, Aliz/G-2091-2016 OI Biazzo, Katia/0000-0002-1892-2180; Bazot, Michael/0000-0003-0166-1540; Bonanno, Alfio/0000-0003-3175-9776; Bradley, Paul/0000-0001-6229-6677; Bedding, Timothy/0000-0001-5943-1460; Cunha, Margarida/0000-0001-8237-7343; Garcia Hernandez, Antonio/0000-0002-6906-4526; Metcalfe, Travis/0000-0003-4034-0416; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776; Serenelli, Aldo/0000-0001-6359-2769; Di Mauro, Maria Pia/0000-0001-7801-7484; Handberg, Rasmus/0000-0001-8725-4502; Leccia, Silvio/0000-0001-5685-6930; Sousa, Sergio/0000-0001-9047-2965; Brandao, Isa/0000-0002-1153-0942; Monteiro, Mario J.P.F.G./0000-0003-0513-8116; Karoff, Christoffer/0000-0003-2009-7965; Hale, Steven/0000-0002-6402-8382; Suarez, Juan Carlos/0000-0003-3649-8384; Ventura, Rita/0000-0002-5152-0482; Korhonen, Heidi/0000-0003-0529-1161; Derekas, Aliz/0000-0002-6526-9444 FU NASA's Science Mission Directorate FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. The authors wish to thank the entire Kepler team, without whom these results would not be possible. We also thank all funding councils and agencies that have supported the activities of KASC Working Group 1, and the International Space Science Institute (ISSI). The analyses reported in this Letter also used observations made with FIES at the Nordic Optical Telescope, and with SOPHIE at Observatoire de Haute-Provence. NR 50 TC 93 Z9 93 U1 0 U2 16 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L169 EP L175 DI 10.1088/2041-8205/713/2/L169 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900018 ER PT J AU Dunham, EW Borucki, WJ Koch, DG Batalha, NM Buchhave, LA Brown, TM Caldwell, DA Cochran, WD Endl, M Fischer, D Furesz, G Gautier, TN Geary, JC Gilliland, RL Gould, A Howell, SB Jenkins, JM Kjeldsen, H Latham, DW Lissauer, JJ Marcy, GW Meibom, S Monet, DG Rowe, JF Sasselov, DD AF Dunham, Edward W. Borucki, William J. Koch, David G. Batalha, Natalie M. Buchhave, Lars A. Brown, Timothy M. Caldwell, Douglas A. Cochran, William D. Endl, Michael Fischer, Debra Furesz, Gabor Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Gould, Alan Howell, Steve B. Jenkins, Jon M. Kjeldsen, Hans Latham, David W. Lissauer, Jack J. Marcy, Geoffrey W. Meibom, Soren Monet, David G. Rowe, Jason F. Sasselov, Dimitar D. TI KEPLER-6b: A TRANSITING HOT JUPITER ORBITING A METAL-RICH STAR SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: individual (Kepler-6, KIC 10874614, 2MASS 19472094+4814238); techniques: spectroscopic ID PLANET AB We announce the discovery of Kepler-6b, a transiting hot Jupiter orbiting a star with unusually high metallicity, [Fe/H] = +0.34 +/- 0.04. The planet's mass is about 2/3 that of Jupiter, M(P) = 0.67 M(J), and the radius is 30% larger than that of Jupiter, R(P) = 1.32 R(J), resulting in a density of rho(P) = 0.35 g cm(-3), a fairly typical value for such a planet. The orbital period is P = 3.235 days. The host star is both more massive than the Sun, M(star) = 1.21 M(circle dot), and larger than the Sun, R(star) = 1.39 R(circle dot). C1 [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Borucki, William J.; Koch, David G.; Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Buchhave, Lars A.; Furesz, Gabor; Geary, John C.; Latham, David W.; Meibom, Soren; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Brown, Timothy M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas A.; Jenkins, Jon M.; Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.; Endl, Michael] Univ Texas Austin, Austin, TX 78712 USA. [Fischer, Debra] Yale Univ, New Haven, CT 06510 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Gould, Alan] Lawrence Hall Sci, Berkeley, CA 94720 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Kjeldsen, Hans] Univ Aarhus, Aarhus, Denmark. [Marcy, Geoffrey W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Monet, David G.] USN Observ, Flagstaff, AZ 86001 USA. RP Dunham, EW (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666 FU NASA's Science Mission Directorate FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. NR 21 TC 46 Z9 46 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L136 EP L139 DI 10.1088/2041-8205/713/2/L136 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900011 ER PT J AU Koch, DG Borucki, WJ Rowe, JF Batalha, NM Brown, TM Caldwell, DA Caldwell, J Cochran, WD DeVore, E Dunham, EW Dupree, AK Gautier, TN Geary, JC Gilliland, RL Howell, SB Jenkins, JM Latham, DW Lissauer, JJ Marcy, GW Morrison, D Tarter, J AF Koch, David G. Borucki, William J. Rowe, Jason F. Batalha, Natalie M. Brown, Timothy M. Caldwell, Douglas A. Caldwell, John Cochran, William D. DeVore, Edna Dunham, Edward W. Dupree, Andrea K. Gautier, Thomas N., III Geary, John C. Gilliland, Ron L. Howell, Steve B. Jenkins, Jon M. Latham, David W. Lissauer, Jack J. Marcy, Geoff W. Morrison, David Tarter, Jill TI DISCOVERY OF THE TRANSITING PLANET KEPLER-5b SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: individual (Kepler-5, KIC 8191672, 2MASS 19573768+4402061); techniques: spectroscopic ID PARAMETERS; STELLAR; FIELD; STAR AB We present 44 days of high duty cycle, ultra precise photometry of the 13th magnitude star Kepler-5 (KIC 8191672, T(eff) = 6300 K, log g = 4.1), which exhibits periodic transits with a depth of 0.7%. Detailed modeling of the transit is consistent with a planetary companion with an orbital period of 3.548460 +/- 0.000032 days and a radius of 1.431(-0.052)(+0.041) R(J). Follow-up radial velocity measurements with the Keck HIRES spectrograph on nine separate nights demonstrate that the planet is more than twice as massive as Jupiter with a mass of 2.114(-0.059)(+0.056) M(J) and a mean density of 0.894 +/- 0.079 g cm(-3). C1 [Koch, David G.; Borucki, William J.; Rowe, Jason F.; Lissauer, Jack J.; Morrison, David] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas A.; DeVore, Edna; Jenkins, Jon M.; Tarter, Jill] SETI Inst, Mountain View, CA 94043 USA. [Caldwell, John] York Univ, Toronto, ON M3J 2R7, Canada. [Cochran, William D.] Univ Texas Austin, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Dupree, Andrea K.; Geary, John C.; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ron L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Marcy, Geoff W.] Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Koch, DG (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 FU NASA's Science Mission Directorate FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We thank D. Fischer, A. Prsa, and everyone that has contributed to the Kepler Mission. NR 19 TC 61 Z9 61 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L131 EP L135 DI 10.1088/2041-8205/713/2/L131 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900010 ER PT J AU Koch, DG Borucki, WJ Basri, G Batalha, NM Brown, TM Caldwell, D Christensen-Dalsgaard, J Cochran, WD DeVore, E Dunham, EW Gautier, TN Geary, JC Gilliland, RL Gould, A Jenkins, J Kondo, Y Latham, DW Lissauer, JJ Marcy, G Monet, D Sasselov, D Boss, A Brownlee, D Caldwell, J Dupree, AK Howell, SB Kjeldsen, H Meibom, S Morrison, D Owen, T Reitsema, H Tarter, J Bryson, ST Dotson, JL Gazis, P Haas, MR Kolodziejczak, J Rowe, JF Van Cleve, JE Allen, C Chandrasekaran, H Clarke, BD Li, J Quintana, EV Tenenbaum, P Twicken, JD Wu, H AF Koch, David G. Borucki, William J. Basri, Gibor Batalha, Natalie M. Brown, Timothy M. Caldwell, Douglas Christensen-Dalsgaard, Jorgen Cochran, William D. DeVore, Edna Dunham, Edward W. Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Gould, Alan Jenkins, Jon Kondo, Yoji Latham, David W. Lissauer, Jack J. Marcy, Geoffrey Monet, David Sasselov, Dimitar Boss, Alan Brownlee, Donald Caldwell, John Dupree, Andrea K. Howell, Steve B. Kjeldsen, Hans Meibom, Soren Morrison, David Owen, Tobias Reitsema, Harold Tarter, Jill Bryson, Stephen T. Dotson, Jessie L. Gazis, Paul Haas, Michael R. Kolodziejczak, Jeffrey Rowe, Jason F. Van Cleve, Jeffrey E. Allen, Christopher Chandrasekaran, Hema Clarke, Bruce D. Li, Jie Quintana, Elisa V. Tenenbaum, Peter Twicken, Joseph D. Wu, Hayley TI KEPLER MISSION DESIGN, REALIZED PHOTOMETRIC PERFORMANCE, AND EARLY SCIENCE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE instrumentation: photometers; planetary systems; space vehicles: instruments; stars: statistics; stars: variables: general; techniques: photometric ID SOLAR-LIKE OSCILLATIONS; INITIAL CHARACTERISTICS; TRANSITING PLANET; TARGET STARS; CADENCE DATA; RED GIANT; 1ST; DISCOVERY; ASTEROSEISMOLOGY; VARIABILITY AB The Kepler Mission, launched on 2009 March 6, was designed with the explicit capability to detect Earth-size planets in the habitable zone of solar-like stars using the transit photometry method. Results from just 43 days of data along with ground-based follow-up observations have identified five new transiting planets with measurements of their masses, radii, and orbital periods. Many aspects of stellar astrophysics also benefit from the unique, precise, extended, and nearly continuous data set for a large number and variety of stars. Early results for classical variables and eclipsing stars show great promise. To fully understand the methodology, processes, and eventually the results from the mission, we present the underlying rationale that ultimately led to the flight and ground system designs used to achieve the exquisite photometric performance. As an example of the initial photometric results, we present variability measurements that can be used to distinguish dwarf stars from red giants. C1 [Koch, David G.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Basri, Gibor; Marcy, Geoffrey] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Batalha, Natalie M.] San Jose State Univ, Dept Phys & Astron, San Jose, CA 95192 USA. [Brown, Timothy M.] Las Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas; DeVore, Edna; Jenkins, Jon; Tarter, Jill; Gazis, Paul; Van Cleve, Jeffrey E.; Chandrasekaran, Hema; Clarke, Bruce D.; Li, Jie; Quintana, Elisa V.; Tenenbaum, Peter; Twicken, Joseph D.; Wu, Hayley] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans] Aarhus Univ, DK-8000 Aarhus C, Denmark. [Cochran, William D.] Univ Texas Austin, McDonald Observ, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Geary, John C.; Latham, David W.; Sasselov, Dimitar; Dupree, Andrea K.; Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Kondo, Yoji] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Monet, David] USN Observ, Flagstaff, AZ 86002 USA. [Boss, Alan] Carnegie Inst Washington, Washington, DC 20015 USA. [Brownlee, Donald] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Caldwell, John] York Univ, Dept Phys & Astron, Toronto, ON M3J 1P3, Canada. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Owen, Tobias] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Reitsema, Harold] Ball Aerosp & Technol Corp, Boulder, CO 80306 USA. [Kolodziejczak, Jeffrey] NASA, George C Marshall Space Flight Ctr, Space Sci Off, Huntsville, AL 35812 USA. [Allen, Christopher] NASA, Ames Res Ctr, Orbital Sci Corp, Moffett Field, CA 94035 USA. RP Koch, DG (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM D.Koch@NASA.gov RI Caldwell, Douglas/L-7911-2014 OI Caldwell, Douglas/0000-0003-1963-9616 NR 47 TC 497 Z9 499 U1 13 U2 65 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L79 EP L86 DI 10.1088/2041-8205/713/2/L79 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900001 ER PT J AU Latham, DW Borucki, WJ Koch, DG Brown, TM Buchhave, LA Basri, G Batalha, NM Caldwell, DA Cochran, WD Dunham, EW Furesz, G Gautier, TN Geary, JC Gilliland, RL Howell, SB Jenkins, JM Lissauer, JJ Marcy, GW Monet, DG Rowe, JF Sasselov, DD AF Latham, David W. Borucki, William J. Koch, David G. Brown, Timothy M. Buchhave, Lars A. Basri, Gibor Batalha, Natalie M. Caldwell, Douglas A. Cochran, William D. Dunham, Edward W. Furesz, Gabor Gautier, Thomas N., III Geary, John C. Gilliland, Ronald L. Howell, Steve B. Jenkins, Jon M. Lissauer, Jack J. Marcy, Geoffrey W. Monet, David G. Rowe, Jason F. Sasselov, Dimitar D. TI KEPLER-7b: A TRANSITING PLANET WITH UNUSUALLY LOW DENSITY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; stars: individual (Kepler-7, KIC 5780885, 2MASS 19141956+4105233); techniques: spectroscopic ID STELLAR AB We report on the discovery and confirmation of Kepler-7b, a transiting planet with unusually low density. The mass is less than half that of Jupiter, M(P) = 0.43 M(J), but the radius is 50% larger, R(P) = 1.48 R(J). The resulting density, rho(P) = 0.17 g cm(-3), is the second lowest reported so far for an extrasolar planet. The orbital period is fairly long, P = 4.886 days, and the host star is not much hotter than the Sun, T(eff) = 6000 K. However, it is more massive and considerably larger than the Sun, M(star) = 1.35 M(circle dot) and R(star) = 1.84R(circle dot), and must be near the end of its life on the main sequence. C1 [Latham, David W.; Buchhave, Lars A.; Furesz, Gabor; Geary, John C.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Borucki, William J.; Koch, David G.; Lissauer, Jack J.; Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Brown, Timothy M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Buchhave, Lars A.; Marcy, Geoffrey W.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Basri, Gibor] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Batalha, Natalie M.] San Jose State Univ, San Jose, CA 95192 USA. [Caldwell, Douglas A.; Jenkins, Jon M.] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.] Univ Texas Austin, Austin, TX 78712 USA. [Dunham, Edward W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Monet, David G.] USN Observ, Flagstaff, AZ 86001 USA. RP Latham, DW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Buchhave, Lars A./0000-0003-1605-5666 NR 10 TC 77 Z9 77 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L140 EP L144 DI 10.1088/2041-8205/713/2/L140 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900012 ER PT J AU Rowe, JF Borucki, WJ Koch, D Howell, SB Basri, G Batalha, N Brown, TM Caldwell, D Cochran, WD Dunham, E Dupree, AK Fortney, JJ Gautier, TN Gilliland, RL Jenkins, J Latham, DW Lissauer, JJ Marcy, G Monet, DG Sasselov, D Welsh, WF AF Rowe, Jason F. Borucki, William J. Koch, David Howell, Steve B. Basri, Gibor Batalha, Natalie Brown, Timothy M. Caldwell, Douglas Cochran, William D. Dunham, Edward Dupree, Andrea K. Fortney, Jonathan J. Gautier, Thomas N., III Gilliland, Ronald L. Jenkins, Jon Latham, David W. Lissauer, Jack J. Marcy, Geoff Monet, David G. Sasselov, Dimitar Welsh, William F. TI KEPLER OBSERVATIONS OF TRANSITING HOT COMPACT OBJECTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: individual (KOI-74, KIC 6889235, KOI-81, KIC 8823868) ID WHITE-DWARF COMPANION; MASS-RADIUS RELATION; OSCILLATIONS; HELIUM; STARS AB Kepler photometry has revealed two unusual transiting companions: one orbiting an early A-star and the other orbiting a late B-star. In both cases, the occultation of the companion is deeper than the transit. The occultation and transit with follow-up optical spectroscopy reveal a 9400 K early A-star, KOI-74 (KIC 6889235), with a companion in a 5.2 day orbit with a radius of 0.08R(circle dot) and a 10,000 K late B-star KOI-81 (KIC 8823868) that has a companion in a 24 day orbit with a radius of 0.2R(circle dot). We infer a temperature of 12,250 K for KOI-74b and 13,500 K for KOI-81b. We present 43 days of high duty cycle, 30 minute cadence photometry, with models demonstrating the intriguing properties of these objects, and speculate on their nature. C1 [Rowe, Jason F.; Borucki, William J.; Koch, David; Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Howell, Steve B.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Basri, Gibor; Marcy, Geoff] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Batalha, Natalie] San Jose State Univ, San Jose, CA 95192 USA. [Brown, Timothy M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Caldwell, Douglas; Jenkins, Jon] SETI Inst, Mountain View, CA 94043 USA. [Cochran, William D.] Univ Texas Austin, Austin, TX 78712 USA. [Dunham, Edward] Lowell Observ, Flagstaff, AZ 86001 USA. [Dupree, Andrea K.; Latham, David W.; Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fortney, Jonathan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95064 USA. [Gautier, Thomas N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Monet, David G.] USN Observ, Flagstaff, AZ 86001 USA. [Welsh, William F.] San Diego State Univ, San Diego, CA 92182 USA. RP Rowe, JF (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RI Caldwell, Douglas/L-7911-2014; OI Caldwell, Douglas/0000-0003-1963-9616; Fortney, Jonathan/0000-0002-9843-4354 FU NASA's Science Mission Directorate FX Funding for this Discovery mission is provided by NASA's Science Mission Directorate. We are indebted to the entire Kepler team for all the hard work and dedication that made such discoveries possible. NR 21 TC 39 Z9 39 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L150 EP L154 DI 10.1088/2041-8205/713/2/L150 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900014 ER PT J AU Stello, D Basu, S Bruntt, H Mosser, B Stevens, IR Brown, TM Christensen-Dalsgaard, J Gilliland, RL Kjeldsen, H Arentoft, T Ballot, J Barban, C Bedding, TR Chaplin, WJ Elsworth, YP Garcia, RA Goupil, MJ Hekker, S Huber, D Mathur, S Meibom, S Sangaralingam, V Baldner, CS Belkacem, K Biazzo, K Brogaard, K Suarez, JC D'Antona, F Demarque, P Esch, L Gai, N Grundahl, F Lebreton, Y Jiang, BW Jevtic, N Karoff, C Miglio, A Molenda-Zakowicz, J Montalban, J Noels, A Cortes, TR Roxburgh, IW Serenelli, AM Aguirre, VS Sterken, C Stine, P Szabo, R Weiss, A Borucki, WJ Koch, D Jenkins, JM AF Stello, Dennis Basu, Sarbani Bruntt, Hans Mosser, Benoitt Stevens, Ian R. Brown, Timothy M. Christensen-Dalsgaard, Jorgen Gilliland, Ronald L. Kjeldsen, Hans Arentoft, Torben Ballot, Jerome Barban, Caroline Bedding, Timothy R. Chaplin, William J. Elsworth, Yvonne P. Garcia, Rafael A. Goupil, Marie-Jo Hekker, Saskia Huber, Daniel Mathur, Savita Meibom, Soren Sangaralingam, Vinothini Baldner, Charles S. Belkacem, Kevin Biazzo, Katia Brogaard, Karsten Carlos Suarez, Juan D'Antona, Francesca Demarque, Pierre Esch, Lisa Gai, Ning Grundahl, Frank Lebreton, Yveline Jiang, Biwei Jevtic, Nada Karoff, Christoffer Miglio, Andrea Molenda-Zakowicz, Joanna Montalban, Josefina Noels, Arlette Roca Cortes, Teodoro Roxburgh, Ian W. Serenelli, Aldo M. Aguirre, Victor Silva Sterken, Christiaan Stine, Peter Szabo, Robert Weiss, Achim Borucki, William J. Koch, David Jenkins, Jon M. TI DETECTION OF SOLAR-LIKE OSCILLATIONS FROM KEPLER PHOTOMETRY OF THE OPEN CLUSTER NGC 6819 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE open clusters and associations: individual (NGC 6819); stars: fundamental parameters; stars: interiors; stars: oscillations; techniques: photometric ID VARIABLE-STARS; GLOBULAR-CLUSTER; STELLAR CLUSTERS; GIANT STARS; K-GIANTS; SEARCH; ASTEROSEISMOLOGY; ISOCHRONES; NGC-6791; PLANETS AB Asteroseismology of stars in clusters has been a long-sought goal because the assumption of a common age, distance, and initial chemical composition allows strong tests of the theory of stellar evolution. We report results from the first 34 days of science data from the Kepler Mission for the open cluster NGC 6819-one of the four clusters in the field of view. We obtain the first clear detections of solar-like oscillations in the cluster red giants and are able to measure the large frequency separation, Delta nu, and the frequency of maximum oscillation power, nu(max). We find that the asteroseismic parameters allow us to test cluster membership of the stars, and even with the limited seismic data in hand, we can already identify four possible non-members despite their having a better than 80% membership probability from radial velocity measurements. We are also able to determine the oscillation amplitudes for stars that span about 2 orders of magnitude in luminosity and find good agreement with the prediction that oscillation amplitudes scale as the luminosity to the power of 0.7. These early results demonstrate the unique potential of asteroseismology of the stellar clusters observed by Kepler. C1 [Stello, Dennis; Bedding, Timothy R.; Huber, Daniel] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Basu, Sarbani; Baldner, Charles S.; Demarque, Pierre; Esch, Lisa; Gai, Ning] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Bruntt, Hans; Mosser, Benoitt; Barban, Caroline; Goupil, Marie-Jo] Univ Paris 07, Univ Paris 06, CNRS, Observ Paris,LESIA, F-92195 Meudon, France. [Stevens, Ian R.; Chaplin, William J.; Elsworth, Yvonne P.; Hekker, Saskia; Sangaralingam, Vinothini; Karoff, Christoffer] Univ Birmingham, Sch Phys & Astron, Birmingham B15 2TT, W Midlands, England. [Brown, Timothy M.] Cumbres Observ Global Telescope, Goleta, CA 93117 USA. [Christensen-Dalsgaard, Jorgen; Kjeldsen, Hans; Arentoft, Torben; Brogaard, Karsten; Grundahl, Frank] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. [Gilliland, Ronald L.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ballot, Jerome] Univ Toulouse, CNRS, Lab Astrophys Toulouse Tarbes, F-31400 Toulouse, France. [Garcia, Rafael A.] Univ Paris 07, IRFU SAp, CEA DSM, CNRS,Lab AIM,Ctr Saclay, F-91191 Gif Sur Yvette, France. [Mathur, Savita] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Belkacem, Kevin; Miglio, Andrea; Montalban, Josefina; Noels, Arlette] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Biazzo, Katia] Osserv Astrofis Arcetri, I-50125 Florence, Italy. [Carlos Suarez, Juan] CSIC, Inst Astrofis Andalucia, Granada, Spain. [D'Antona, Francesca] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Gai, Ning; Jiang, Biwei] Beijing Normal Univ, Dept Astron, Beijing 100875, Peoples R China. [Lebreton, Yveline] Univ Paris Diderot, CNRS, Observ Paris, GEPI, F-92195 Meudon, France. [Jevtic, Nada; Stine, Peter] Bloomsburg Univ Penn, Dept Phys & Engn Technol, Bloomsburg, PA 17815 USA. [Molenda-Zakowicz, Joanna] Univ Wroclaw, Astron Inst, PL-51622 Wroclaw, Poland. [Roca Cortes, Teodoro] Univ La Laguna, Dept Astrofis, Tenerife 38207, Spain. [Roca Cortes, Teodoro] Inst Astrofis Canarias, Tenerife 38205, Spain. [Roxburgh, Ian W.] Queen Mary Univ London, London E1 4NS, England. [Serenelli, Aldo M.; Aguirre, Victor Silva; Weiss, Achim] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Sterken, Christiaan] Vrije Univ Brussels, B-1050 Brussels, Belgium. [Szabo, Robert] Konkoly Observ Budapest, H-1525 Budapest, Hungary. [Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Stello, D (reprint author), Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. RI Weiss, Achim/C-4870-2013; Karoff, Christoffer/L-1007-2013; Lebreton, Yveline/N-2268-2014; Suarez, Juan Carlos/C-1015-2009; Ballot, Jerome/G-1019-2010; OI Serenelli, Aldo/0000-0001-6359-2769; Weiss, Achim/0000-0002-3843-1653; Karoff, Christoffer/0000-0003-2009-7965; Suarez, Juan Carlos/0000-0003-3649-8384; Biazzo, Katia/0000-0002-1892-2180; Szabo, Robert/0000-0002-3258-1909; Brogaard, Karsten/0000-0003-2001-0276; Bedding, Timothy/0000-0001-5943-1460; Bedding, Tim/0000-0001-5222-4661; Garcia, Rafael/0000-0002-8854-3776 FU NASA's Science Mission Directorate 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 authors also thank all funding councils and agencies that have supported the activities of Working Group 2 of the Kepler Asteroseismic Science Consortium (KASC). NR 36 TC 60 Z9 60 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 20 PY 2010 VL 713 IS 2 BP L182 EP L186 DI 10.1088/2041-8205/713/2/L182 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 587DZ UT WOS:000276970900020 ER PT J AU Asher, RJ Helgen, KM AF Asher, Robert J. Helgen, Kristofer M. TI Nomenclature and placental mammal phylogeny SO BMC EVOLUTIONARY BIOLOGY LA English DT Article ID HORMONE RECEPTOR GENE; MITOGENOMIC RELATIONSHIPS; MITOCHONDRIAL GENOME; MOLECULAR EVIDENCE; MORPHOLOGY; AFROTHERIA; CETACEANS; ORDER; RNA; ARTIODACTYLS AB An issue arising from recent progress in establishing the placental mammal Tree of Life concerns the nomenclature of high-level clades. Fortunately, there are now several well-supported clades among extant mammals that require unambiguous, stable names. Although the International Code of Zoological Nomenclature does not apply above the Linnean rank of family, and while consensus on the adoption of competing systems of nomenclature does not yet exist, there is a clear, historical basis upon which to arbitrate among competing names for high-level mammalian clades. Here, we recommend application of the principles of priority and stability, as laid down by G. G. Simpson in 1945, to discriminate among proposed names for high-level taxa. We apply these principles to specific cases among placental mammals with broad relevance for taxonomy, and close with particular emphasis on the Afrotherian family Tenrecidae. We conclude that no matter how reconstructions of the Tree of Life change in years to come, systematists should apply new names reluctantly, deferring to those already published and maximizing consistency with existing nomenclature. C1 [Asher, Robert J.] Univ Cambridge, Museum Zool, Cambridge CB2 3EJ, England. [Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Asher, RJ (reprint author), Univ Cambridge, Museum Zool, Downing St, Cambridge CB2 3EJ, England. EM r.asher@zoo.cam.ac.uk NR 75 TC 46 Z9 48 U1 0 U2 27 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 APR 20 PY 2010 VL 10 AR 102 DI 10.1186/1471-2148-10-102 PG 9 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 594BW UT WOS:000277509000001 PM 20406454 ER PT J AU Swartz, DA Wolk, SJ Fruscione, A AF Swartz, Douglas A. Wolk, Scott J. Fruscione, Antonella TI Chandra's first decade of discovery SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Editorial Material DE review; X-rays ID X-RAY; SUPERNOVA REMNANT; EMISSION; JET; SPECTROSCOPY; CASSIOPEIA; ACCRETION; OBJECT; STATES C1 [Swartz, Douglas A.] NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. [Wolk, Scott J.; Fruscione, Antonella] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Swartz, DA (reprint author), NASA, Univ Space Res Assoc, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. EM doug.swartz@nasa.gov OI Wolk, Scott/0000-0002-0826-9261 NR 87 TC 2 Z9 2 U1 0 U2 1 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 20 PY 2010 VL 107 IS 16 BP 7127 EP 7134 DI 10.1073/pnas.0914464107 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586FU UT WOS:000276892300007 PM 20406906 ER PT J AU Testa, P AF Testa, Paola TI X-ray emission processes in stars and their immediate environment SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE activity; spectroscopy; magnetic fields; stellar winds; accretion ID T-TAURI-STARS; YOUNG STELLAR OBJECTS; K-ALPHA; PHOTOSPHERIC IRON; CORONAL STRUCTURE; ACCRETION SHOCKS; LINE PROFILES; SOLAR-FLARES; HERBIG STAR; AB-DORADUS AB A decade of X-ray stellar observations with Chandra and XMM-Newton has led to significant advances in our understanding of the physical processes at work in hot (magnetized) plasmas in stars and their immediate environment, providing new perspectives and challenges, and in turn the need for improved models. The wealth of high-quality stellar spectra has allowed us to investigate, in detail, the characteristics of the X-ray emission across the Hertzsprung-Russell (HR) diagram. Progress has been made in addressing issues ranging from classical stellar activity in stars with solar-like dynamos (such as flares, activity cycles, spatial and thermal structuring of the X-ray emitting plasma, and evolution of X-ray activity with age), to X-ray generating processes (e. g., accretion, jets, magnetically confined winds) that were poorly understood in the preChandra/XMM-Newton era. I will discuss the progress made in the study of high energy stellar physics and its impact in a wider astrophysical context, focusing on the role of spectral diagnostics now accessible. C1 Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Testa, P (reprint author), Smithsonian Astrophys Observ, MS-58,60 Garden St, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu FU National Aeronautics and Space Administration (NASA) [GO7-8016C] FX This work has benefited greatly from discussions with several people, and, in particular, I would like to warmly thank Jeremy Drake and Manuel Gudel. I also would like to thank Hans Moritz Gunther for permission to use original figure material. This work has been supported by National Aeronautics and Space Administration (NASA) Grant GO7-8016C. NR 78 TC 7 Z9 7 U1 0 U2 0 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 20 PY 2010 VL 107 IS 16 BP 7158 EP 7163 DI 10.1073/pnas.0913822107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586FU UT WOS:000276892300012 PM 20360562 ER PT J AU Blanton, EL Clarke, TE Sarazin, CL Randall, SW McNamara, BR AF Blanton, Elizabeth L. Clarke, T. E. Sarazin, Craig L. Randall, Scott W. McNamara, Brian R. TI Active galactic nucleus feedback in clusters of galaxies SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE clusters of galaxies; active galactic nuclei; X-ray observations; Chandra X-ray Observatory ID DEEP CHANDRA OBSERVATION; X-RAY CAVITIES; HYDRA-A CLUSTER; COOLING-FLOW; PERSEUS CLUSTER; INTRACLUSTER MEDIUM; GASEOUS ATMOSPHERE; CENTAURUS CLUSTER; HIGH-RESOLUTION; RADIO BUBBLES AB Observations made during the last ten years with the Chandra X-ray Observatory have shed much light on the cooling gas in the centers of clusters of galaxies and the role of active galactic nucleus (AGN) heating. Cooling of the hot intracluster medium in cluster centers can feed the supermassive black holes found in the nuclei of the dominant cluster galaxies leading to AGN outbursts which can reheat the gas, suppressing cooling and large amounts of star formation. AGN heating can come in the form of shocks, buoyantly rising bubbles that have been inflated by radio lobes, and the dissipation of sound waves. C1 [Blanton, Elizabeth L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Blanton, Elizabeth L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA. [Sarazin, Craig L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Randall, Scott W.; McNamara, Brian R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McNamara, Brian R.] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 2G1, Canada. Perimeter Inst Theoret Phys, N Waterloo, ON N2L 2Y5, Canada. RP Blanton, EL (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM eblanton@bu.edu RI Blanton, Elizabeth/H-4501-2014; OI Randall, Scott/0000-0002-3984-4337 FU National Aeronautics and Space Administration through Chandra [GO9-0147X, GO9-0035X] FX We are very grateful to our many collaborators. We thank the organizers for arranging a wonderful meeting highlighting the results from Chandra over the last 10 years. E. L. B. was supported by the National Aeronautics and Space Administration through Chandra award GO9-0147X. C. L. S. was supported in part by Chandra award GO9-0035X. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 base funding. NR 53 TC 8 Z9 8 U1 0 U2 2 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 20 PY 2010 VL 107 IS 16 BP 7174 EP 7178 DI 10.1073/pnas.0913904107 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586FU UT WOS:000276892300015 PM 20351250 ER PT J AU Vikhlinin, A AF Vikhlinin, Alexey TI Studies of dark energy with x-ray observatories SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE cosmology; galaxy clusters; x-ray astronomy ID RELAXED GALAXY CLUSTERS; ACCELERATING UNIVERSE; CHANDRA; CONSTRAINTS; SAMPLE; SIMULATIONS; COSMOLOGY; MASS; NORMALIZATION; SUPERNOVAE AB I review the contribution of Chandra X-ray Observatory to studies of dark energy. There are two broad classes of observable effects of dark energy: evolution of the expansion rate of the Universe, and slow down in the rate of growth of cosmic structures. Chandra has detected and measured both of these effects through observations of galaxy clusters. A combination of the Chandra results with other cosmological datasets leads to 5% constraints on the dark energy equation-of-state parameter, and limits possible deviations of gravity on large scales from general relativity. C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Vikhlinin, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM alexey@head.cfa.harvard.edu NR 46 TC 3 Z9 3 U1 0 U2 0 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 20 PY 2010 VL 107 IS 16 BP 7179 EP 7183 DI 10.1073/pnas.0914905107 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586FU UT WOS:000276892300016 PM 20404207 ER PT J AU Schwartz, D AF Schwartz, Daniel TI Chandra enables study of x-ray jets SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE black holes; quasars; radio sources ID ACTIVE GALACTIC NUCLEI; HUBBLE-SPACE-TELESCOPE; EXTENDED RADIO JETS; LARGE-SCALE; QUASAR JETS; CENTAURUS-A; R-AQUARII; DG-TAURI; M87 JET; DISCOVERY AB The exquisite angular resolution of the Chandra x-ray telescope has enabled the detection and study of resolved x-ray jets in a wide variety of astronomical systems. Chandra has detected extended jets in our galaxy from protostars, symbiotic binaries, neutron star pulsars, black hole binaries, extragalactic jets in radio sources, and quasars. The x-ray data play an essential role in deducing the emission mechanism of the jets, in revealing the interaction of jets with the intergalactic or intracluster media, and in studying the energy generation budget of black holes. C1 Smithsonian Astrophys Observ, Cambridge, MA USA. RP Schwartz, D (reprint author), Smithsonian Astrophys Observ, Cambridge, MA USA. EM das@head.cfa.harvard.edu FU National Aeronautics and Space Administration [NAS8-03060]; Astro-physical Observatory [GO9-0121B, GO7-8107X] FX This work was supported by the National Aeronautics and Space Administration contract NAS8-03060 and Smithsonian Astro-physical Observatory Grants GO9-0121B and GO7-8107X. NR 35 TC 2 Z9 2 U1 0 U2 1 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 20 PY 2010 VL 107 IS 16 BP 7190 EP 7195 DI 10.1073/pnas.0913890107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586FU UT WOS:000276892300018 PM 20378839 ER PT J AU Mooney, KA Gruner, DS Barber, NA Van Bael, SA Philpott, SM Greenberg, R AF Mooney, Kailen A. Gruner, Daniel S. Barber, Nicholas A. Van Bael, Sunshine A. Philpott, Stacy M. Greenberg, Russell TI Interactions among predators and the cascading effects of vertebrate insectivores on arthropod communities and plants SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE bottom-up and top-down control; intraguild predation; meta-analysis; trophic cascade; vertebrate predator exclusion ID TERRESTRIAL FOOD WEBS; INTRAGUILD PREDATION; TROPHIC CASCADES; TOP-DOWN; BIRDS; ECOSYSTEMS; STRENGTH; PREY; METAANALYSIS; DYNAMICS AB Theory on trophic interactions predicts that predators increase plant biomass by feeding on herbivores, an indirect interaction called a trophic cascade. Theory also predicts that predators feeding on predators, or intraguild predation, will weaken trophic cascades. Although past syntheses have confirmed cascading effects of terrestrial arthropod predators, we lack a comprehensive analysis for vertebrate insectivores-which by virtue of their body size and feeding habits are often top predators in these systems-and of how intraguild predation mediates trophic cascade strength. We report here on a meta-analysis of 113 experiments documenting the effects of insectivorous birds, bats, or lizards on predaceous arthropods, herbivorous arthropods, and plants. Although vertebrate insectivores fed as intraguild predators, strongly reducing predaceous arthropods (38%), they nevertheless suppressed herbivores (39%), indirectly reduced plant damage (40%), and increased plant biomass (14%). Furthermore, effects of vertebrate insectivores on predatory and herbivorous arthropods were positively correlated. Effects were strongest on arthropods and plants in communities with abundant predaceous arthropods and strong intraguild predation, but weak in communities depauperate in arthropod predators and intraguild predation. The naturally occurring ratio of arthropod predators relative to herbivores varied tremendously among the studied communities, and the skew to predators increased with site primary productivity and in trees relative to shrubs. Although intraguild predation among arthropod predators has been shown to weaken herbivore suppression, we find this paradigm does not extend to vertebrate insectivores in these communities. Instead, vertebrate intraguild predation is associated with strengthened trophic cascades, and insectivores function as dominant predators in terrestrial plant-arthropod communities. C1 [Mooney, Kailen A.] Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. [Gruner, Daniel S.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Barber, Nicholas A.] Univ Missouri, Dept Biol, St Louis, MO 63121 USA. [Van Bael, Sunshine A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Philpott, Stacy M.] Univ Toledo, Dept Environm Sci, Toledo, OH 43606 USA. [Greenberg, Russell] Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Mooney, KA (reprint author), Univ Calif Irvine, Dept Ecol & Evolutionary Biol, Irvine, CA 92697 USA. EM mooneyk@uci.edu RI Gruner, Daniel/A-5166-2010; Barber, Nicholas/N-1437-2014; Philpott, Stacy/F-2330-2011 OI Gruner, Daniel/0000-0002-3153-4297; NR 46 TC 59 Z9 65 U1 7 U2 93 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD APR 20 PY 2010 VL 107 IS 16 BP 7335 EP 7340 DI 10.1073/pnas.1001934107 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 586FU UT WOS:000276892300043 PM 20368418 ER PT J AU Ballentine, B Greenberg, R AF Ballentine, Barbara Greenberg, Russell TI Common Garden Experiment Reveals Genetic Control of Phenotypic Divergence between Swamp Sparrow Subspecies That Lack Divergence in Neutral Genotypes SO PLOS ONE LA English DT Article ID EVOLUTIONARY PROCESSES; BIOLOGICAL DIVERSITY; MITOCHONDRIAL-DNA; TIDAL MARSHES; CONSERVATION; POPULATIONS; DIFFERENTIATION; DIMORPHISM; ADAPTATION; MARKERS AB Background: Adaptive divergence between populations in the face of strong selection on key traits can lead to morphological divergence between populations without concomitant divergence in neutral DNA. Thus, the practice of identifying genetically distinct populations based on divergence in neutral DNA may lead to a taxonomy that ignores evolutionarily important, rapidly evolving, locally-adapted populations. Providing evidence for a genetic basis of morphological divergence between rapidly evolving populations that lack divergence in selectively neutral DNA will not only inform conservation efforts but also provide insight into the mechanisms of the early processes of speciation. The coastal plain swamp sparrow, a recent colonist of tidal marsh habitat, differs from conspecific populations in a variety of phenotypic traits yet remains undifferentiated in neutral DNA. Methods and Principal Findings: Here we use an experimental approach to demonstrate that phenotypic divergence between ecologically separated populations of swamp sparrows is the result of local adaptation despite the lack of divergence in neutral DNA. We find that morphological ( bill size and plumage coloration) and life history ( reproductive effort) differences observed between wild populations were maintained in laboratory raised individuals suggesting genetic divergence of fitness related traits. Conclusions and Significance: Our results support the hypothesis that phenotypic divergence in swamps sparrows is the result of genetic differentiation, and demonstrate that adaptive traits have evolved more rapidly than neutral DNA in these ecologically divergent populations that may be in the early stages of speciation. Thus, identifying evolutionarily important populations based on divergence in selectively neutral DNA could miss an important level of biodiversity and mislead conservation efforts. C1 [Ballentine, Barbara] Univ W Georgia, Smithsonian Migratory Bird Ctr, Natl Zool Pk, Carrollton, GA USA. [Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Ballentine, B (reprint author), Univ W Georgia, Smithsonian Migratory Bird Ctr, Natl Zool Pk, Carrollton, GA USA. EM bballent@westga.edu FU Smithsonian Institution Endowment; Smithsonian Institution; National Zoo; Maryland Ornithological Society FX Funding for this project was provided to Russell Greenberg through a Smithsonian Institution Endowment Grant. Funding for this project to Barbara Ballentine was provided by the Smithsonian Institution, Friends of the National Zoo and The Maryland Ornithological Society. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 35 TC 24 Z9 27 U1 0 U2 18 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 19 PY 2010 VL 5 IS 4 AR e10229 DI 10.1371/journal.pone.0010229 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 585UC UT WOS:000276853800019 PM 20419104 ER PT J AU Zavala, J Vogelsberger, M White, SDM AF Zavala, Jesus Vogelsberger, Mark White, Simon D. M. TI Relic density and CMB constraints on dark matter annihilation with Sommerfeld enhancement SO PHYSICAL REVIEW D LA English DT Article ID COSMIC-RAYS; SPECTRUM; TELESCOPE; ENERGIES; EXCESS; FERMI; COBE AB We calculate how the relic density of dark matter particles is altered when their annihilation is enhanced by the Sommerfeld mechanism due to a Yukawa interaction between the annihilating particles. Maintaining a dark matter abundance consistent with current observational bounds requires the normalization of the s-wave annihilation cross section to be decreased compared to a model without enhancement. The level of suppression depends on the specific parameters of the particle model, with the kinetic decoupling temperature having the most effect. We find that the cross section can be reduced by as much as an order of magnitude for extreme cases. We also compute the mu-type distortion of the CMB energy spectrum caused by energy injection from such Sommerfeld-enhanced annihilation. Our results indicate that in the vicinity of resonances, associated with bound states, distortions can be large enough to be excluded by the upper limit vertical bar mu vertical bar <= 9.0 X 10(-5) found by the FIRAS (Far Infrared Absolute Spectrophotometer) instrument on the COBE (Cosmic Background Explorer) satellite. C1 [Zavala, Jesus; Vogelsberger, Mark; White, Simon D. M.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Vogelsberger, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zavala, J (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM jesus@mpa-garching.mpg.de RI Zavala Franco, Jesus/M-5152-2014 OI Zavala Franco, Jesus/0000-0003-4442-908X FU Max Planck Institute for Astrophysics and the Shanghai Astronomical Observatory FX J.Z. is supported by the Joint Postdoctoral Program in Astrophysical Cosmology of the Max Planck Institute for Astrophysics and the Shanghai Astronomical Observatory. We thank the anonymous referee for helpful comments and suggestions. NR 44 TC 49 Z9 49 U1 0 U2 1 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD APR 15 PY 2010 VL 81 IS 8 AR 083502 DI 10.1103/PhysRevD.81.083502 PG 10 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 590DU UT WOS:000277205000019 ER PT J AU Miranda, LS Collins, AG Marques, AC AF Miranda, Lucilia S. Collins, Allen G. Marques, Antonio C. TI Molecules Clarify a Cnidarian Life Cycle - The "Hydrozoan'' Microhydrula limopsicola Is an Early Life Stage of the Staurozoan Haliclystus antarcticus SO PLOS ONE LA English DT Article ID SOUTHERN CHILE; ASEXUAL REPRODUCTION; WESTERN ATLANTIC; RDNA DATA; SCYPHOZOA; STAUROMEDUSA; PHYLOGENY; EVOLUTION; AURICULA; AURELIA AB Background: Life cycles of medusozoan cnidarians vary widely, and have been difficult to document, especially in the most recently proposed class Staurozoa. However, molecular data can be a useful tool to elucidate medusozoan life cycles by tying together different life history stages. Methodology/Principal Findings: Genetic data from fast-evolving molecular markers (mitochondrial 16S, nuclear ITS1, and nuclear ITS2) show that animals that were presumed to be a hydrozoan, Microhydrula limopsicola (Limnomedusae, Microhydrulidae), are actually an early stage of the life cycle of the staurozoan Haliclystus antarcticus (Stauromedusae, Lucernariidae). Conclusions/Significance: Similarity between the haplotypes of three markers of Microhydrula limopsicola and Haliclystus antarcticus settles the identity of these taxa, expanding our understanding of the staurozoan life cycle, which was thought to be more straightforward and simple. A synthetic discussion of prior observations makes sense of the morphological, histological and behavioral similarities/congruence between Microhydrula and Haliclystus. The consequences are likely to be replicated in other medusozoan groups. For instance we hypothesize that other species of Microhydrulidae are likely to represent life stages of other species of Staurozoa.45 C1 [Miranda, Lucilia S.; Marques, Antonio C.] Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Marine Fisheries Serv, Natl Systemat Lab, Washington, DC 20560 USA. RP Miranda, LS (reprint author), Univ Sao Paulo, Inst Biociencias, Dept Zool, Sao Paulo, Brazil. EM mirandals@ib.usp.br RI Collins, Allen/A-7944-2008; Marques, Antonio/E-8049-2011; Miranda, Lucilia/L-4930-2015 OI Collins, Allen/0000-0002-3664-9691; Marques, Antonio/0000-0002-2884-0541; FU Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) [2004/09961-4]; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [55.7333/2005-9, 490348/2006-8, 305735/2006-3, 474672/2007-7]; National Science Foundation [0531779] FX This work was supported by Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP) ( research grant 2004/09961-4), Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) (55.7333/2005-9, 490348/2006-8, 305735/2006-3, 474672/2007-7), and the National Science Foundation through Assembling the Tree of Life Grant (0531779). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 51 TC 26 Z9 29 U1 2 U2 10 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD APR 14 PY 2010 VL 5 IS 4 AR e10182 DI 10.1371/journal.pone.0010182 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 583VA UT WOS:000276706800019 PM 20418959 ER PT J AU Robbins, RK AF Robbins, Robert K. TI FOUR COMMONLY CONFUSED HAIRSTREAKS (LYCAENIDAE, THECLINAE, EUMAEINI): THREE NEED NAMES, ONE DOES NOT SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE Androconia; Aratcacus; Iaspis; Ignata; Larval foodplants; Michaelus ID LEPIDOPTERA; BUTTERFLIES AB Tine taxonomy or four relatively common Ncotropical hairstreak species has keen confused. Newly described are laspis andersoni Robbins, new species, differentiated from I. talayra (Hewitson), I. cast it as (Druce), and I. exiguus (Drnec Michaclus joseph Robbins, new species, differentiated from M. tra (Hewitson); raid Ignata caldas; Robbins, new species, differentiated from I. gadira sun laspis andersoni is unnamed because of taxonomic misidentification made more than a century ago. The latter two are undescribed because the types of M, ira and I. gadira are not the species that they had been thought to be. Populations in the Arawacus togarna (Hewitson) species complex from Mexico and Costa Pica have Cell treated as two distinct species. hut new data 011 geographical variation of wing pattern and male genitalia suggests that this classification is incorrect. A lectotype for Vicar! exiguus Deuce, 1907 is designated heciatisci taxonomy of the laspis talayra gritty in the Amazon Region is unresolved. A lectotype for Thecla togarna Hewitson, 1867 is designated hecanse hit incorrect type locality has engendered confusion. C1 Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. RP Robbins, RK (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,NHB Stop 105, Washington, DC 20013 USA. EM robbinsr@si.edu NR 43 TC 4 Z9 4 U1 0 U2 1 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD APR 13 PY 2010 VL 64 IS 1 BP 1 EP 13 PG 13 WC Entomology SC Entomology GA 587OQ UT WOS:000277002500001 ER PT J AU Solis, MA Scholtens, BG Adams, JK Funk, DH AF Solis, M. Alma Scholtens, Brian G. Adams, James K. Funk, David H. TI FIRST REPORT OF ECPYRRHORRHOE PURALIS (SOUTH) (PYRALOIDEA: CRAMBIDAE: PYRAUSTINAE) IN NORTH AMERICA: A NATURALIZED EXOTIC PYRAUSTINE FROM ASIA FEEDING ON PAULOWNIA SIEBOLD & ZUCC. SO JOURNAL OF THE LEPIDOPTERISTS SOCIETY LA English DT Article DE Crambidae; Pyraloidea; Pauloicnia; invasive; China; Yezobotys ID LEPIDOPTERA; TOMENTOSA C1 [Solis, M. Alma] USDA, Smithsonian Inst, Natl Museum Nat Hist, SEL, Washington, DC 20013 USA. [Scholtens, Brian G.] Coll Charleston, Dept Biol, Charleston, SC 29424 USA. [Adams, James K.] Dalton State Coll, Dept Biol, Dalton, GA 30720 USA. [Funk, David H.] Stroud Water Res Ctr, Avondale, PA 19311 USA. RP Solis, MA (reprint author), USDA, Smithsonian Inst, Natl Museum Nat Hist, SEL, POB 37012,E-517,MRC 168, Washington, DC 20013 USA. EM alma.solis@ars.usda.gov; scholtensb@cofc.edu; jadams@daltonstate.edu; dhfunk@stroudcenter.org NR 15 TC 2 Z9 4 U1 1 U2 4 PU LEPIDOPTERISTS SOC PI LOS ANGELES PA 900 EXPOSITION BLVD, LOS ANGELES, CA 90007-4057 USA SN 0024-0966 J9 J LEPID SOC JI J. Lepid. Soc. PD APR 13 PY 2010 VL 64 IS 1 BP 33 EP 35 PG 3 WC Entomology SC Entomology GA 587OQ UT WOS:000277002500005 ER PT J AU de Leon, LF Bermingham, E Podos, J Hendry, AP AF Fernando de Leon, Luis Bermingham, Eldredge Podos, Jeffrey Hendry, Andrew P. TI Divergence with gene flow as facilitated by ecological differences: within-island variation in Darwin's finches SO PHILOSOPHICAL TRANSACTIONS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE sympatric speciation; ecological speciation; disruptive selection; reproductive isolation; gene flow; Darwin's finches ID SMALL SPATIAL SCALE; SYMPATRIC SPECIATION; ADAPTIVE RADIATION; CHARACTER DISPLACEMENT; POPULATION-STRUCTURE; ASSIGNMENT TESTS; GEOSPIZA-FORTIS; BEAK MORPHOLOGY; F-STATISTICS; EVOLUTION AB Divergence and speciation can sometimes proceed in the face of, and even be enhanced by, ongoing gene flow. We here study divergence with gene flow in Darwin's finches, focusing on the role of ecological/adaptive differences in maintaining/promoting divergence and reproductive isolation. To this end, we survey allelic variation at 10 microsatellite loci for 989 medium ground finches (Geospiza fortis) on Santa Cruz Island, Galapagos. We find only small genetic differences among G. fortis from different sites. We instead find noteworthy genetic differences associated with beak. Moreover, G. fortis at the site with the greatest divergence in beak size also showed the greatest divergence at neutral markers; i.e. the lowest gene flow. Finally, morphological and genetic differentiation between the G. fortis beak-size morphs was intermediate to that between G. fortis and its smaller (Geospiza fuliginosa) and larger (Geospiza magnirostris) congeners. We conclude that ecological differences associated with beak size (i.e. foraging) influence patterns of gene flow within G. fortis on a single island, providing additional support for ecological speciation in the face of gene flow. Patterns of genetic similarity within and between species also suggest that interspecific hybridization might contribute to the formation of beak-size morphs within G. fortis. C1 [Fernando de Leon, Luis; Hendry, Andrew P.] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada. [Fernando de Leon, Luis; Hendry, Andrew P.] McGill Univ, Dept Biol, Montreal, PQ H3A 2K6, Canada. [Fernando de Leon, Luis; Bermingham, Eldredge] Smithsonian Trop Res Inst, Balboa, Panama. [Podos, Jeffrey] Univ Massachusetts, Dept Biol, Amherst, MA 01003 USA. RP de Leon, LF (reprint author), McGill Univ, Redpath Museum, 859 Sherbrooke St W, Montreal, PQ H3A 2K6, Canada. EM luis.deleonreyna@mail.mcgill.ca RI Hendry, Andrew/C-5765-2008; De Leon, Luis Fernando/H-1112-2011 OI Hendry, Andrew/0000-0002-4807-6667; FU Secretaria Nacional de Ciencia; Tecnologia e Innovacion and El Instituto para la Formacion y Aprovechamiento de los Recursos Humanos, Panama (L.F.d.L.); US National Science Foundation (J.P.); Natural Sciences and Engineering Research Council of Canada (A.P.H.); Smithsonian Tropical Research Institute (E.B.) FX Logistical support and permits were provided by the Galapagos National Park Service and the Charles Darwin Research Station. Field assistance was provided by Ana Gabela, Sarah Huber and David Delaney. Laboratory assistance was provided by Maribel Gonzalez, Jesus Mavarez and Oris Sanjur. K. Petren provided primer aliquots for the DNA analyses. L. Keller, K. Petren and J. S. Moore also provided helpful comments on an earlier draft of this manuscript. J. Raeymaekers and X. Thibert-Plante provided useful suggestion for data analysis. Anonymous reviewers gave helpful comments on the last version of the manuscript. This research was funded by the Secretaria Nacional de Ciencia, Tecnologia e Innovacion and El Instituto para la Formacion y Aprovechamiento de los Recursos Humanos, Panama (L.F.d.L.); the US National Science Foundation (J.P.); the Natural Sciences and Engineering Research Council of Canada (A.P.H.); and the Smithsonian Tropical Research Institute (E.B.). NR 97 TC 47 Z9 48 U1 16 U2 78 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 0962-8436 J9 PHILOS T R SOC B JI Philos. Trans. R. Soc. B-Biol. Sci. PD APR 12 PY 2010 VL 365 IS 1543 BP 1041 EP 1052 DI 10.1098/rstb.2009.0314 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 561UQ UT WOS:000275005200005 PM 20194167 ER PT J AU Townsend, LJ Coe, MJ McBride, VA Bird, AJ Schurch, MPE Corbet, RHD Haberl, F Galache, JL Udalski, A AF Townsend, L. J. Coe, M. J. McBride, V. A. Bird, A. J. Schurch, M. P. E. Corbet, R. H. D. Haberl, F. Galache, J. L. Udalski, A. TI Be/X-ray binary SXP6.85 undergoes large Type II outburst in the Small Magellanic Cloud SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: emission-line; Be; Magellanic Clouds; X-rays: binaries ID GRAVITATIONAL LENSING EXPERIMENT; H-ALPHA; PULSARS; STARS; LONG AB The Small Magellanic Cloud (SMC) Be/X-ray binary pulsar SXP6.85 = XTE J0103-728 underwent a large Type II outburst beginning on 2008 August 10. The source was consistently seen for the following 20 weeks (MJD = 54688-54830). We present X-ray timing and spectroscopic analysis of the source as a part of our ongoing Rossi X-ray Timing Explorer (RXTE) monitoring campaign and INTEGRAL key programme monitoring the SMC and 47 Tuc. A comparison with the Optical Gravitational Lensing Experiment (OGLE) III light curve of the Be counterpart shows the X-ray outbursts from this source coincide with times of optical maximum. We attribute this to the circumstellar disc increasing in size, causing mass accretion on to the neutron star. Ground based infrared photometry and H alpha spectroscopy obtained during the outburst are used as a measure of the size of the circumstellar disc and lend support to this picture. In addition, folded RXTE light curves seem to indicate complex changes in the geometry of the accretion regions on the surface of the neutron star, which may be indicative of an inhomogeneous density distribution in the circumstellar material causing a variable accretion rate on to the neutron star. Finally, the assumed inclination of the system and H alpha equivalent width measurements are used to make a simplistic estimate of the size of the circumstellar disc. C1 [Townsend, L. J.; Coe, M. J.; McBride, V. A.; Bird, A. J.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Schurch, M. P. E.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Corbet, R. H. D.] Univ Maryland Baltimore Cty, Xray Astrophys Lab, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Haberl, F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Galache, J. L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Udalski, A.] Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Townsend, LJ (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM ljt203@soton.ac.uk OI Haberl, Frank/0000-0002-0107-5237 FU National Aeronautics and Space Administration; National Science Foundation; US Department of Energy; University of California; Lawrence Livermore National Laboratory [W-7405-Eng-48]; National Science Foundation through the Center for Particle Astrophysics of the University of California [AST-8809616]; Mount Stromlo and Siding Spring Observatory; Australian National University; Polish MNiSW [N20303032/4275] FX This publication makes use of data products from the 2MASS, 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 paper utilizes public domain data originally obtained by the MACHO Project, whose work was performed under the joint auspices of the US Department of Energy, National Nuclear Security Administration by the University of California, Lawrence Livermore National Laboratory under contract No. W-7405-Eng-48, the National Science Foundation through the Center for Particle Astrophysics of the University of California under cooperative agreement AST-8809616, and the Mount Stromlo and Siding Spring Observatory, part of the Australian National University. The OGLE project is partially supported by the Polish MNiSW grant N20303032/4275. LJT wishes to thank the IRSF/SIRIUS team for providing the reduction pipeline for the IR photometry and the University of Southampton, whose support has made this research possible. We would like to thank the anonymous referee for their helpful and constructive comments. NR 26 TC 7 Z9 9 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2010 VL 403 IS 3 BP 1239 EP 1245 DI 10.1111/j.1365-2966.2009.16211.x PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 577TS UT WOS:000276247500012 ER PT J AU Sani, E Lutz, D Risaliti, G Netzer, H Gallo, LC Trakhtenbrot, B Sturm, E Boller, T AF Sani, E. Lutz, D. Risaliti, G. Netzer, H. Gallo, L. C. Trakhtenbrot, B. Sturm, E. Boller, T. TI Enhanced star formation in narrow-line Seyfert 1 active galactic nuclei revealed by Spitzer SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: starburst; infrared: galaxies ID BLACK-HOLE MASS; ULTRALUMINOUS INFRARED GALAXIES; QUASI-STELLAR OBJECTS; RAY-SELECTED AGNS; BH-SIGMA RELATION; COMPLETE SAMPLE; HOST GALAXIES; SPECTROSCOPIC PROPERTIES; OPTICAL-PROPERTIES; SPACE-TELESCOPE AB We present new low-resolution Spitzer mid-infrared spectroscopy of a sample of 20 ROSAT-selected local narrow-line Seyfert 1 galaxies (NLS1s). We detect strong active galactic nucleus (AGN) continuum in all and clear polycyclic aromatic hydrocarbon (PAH) emission in 70 per cent of the sources. The 6.2 mu m PAH luminosity spans three orders of magnitude, from similar to 1039 to similar to 1042 erg s-1, providing strong evidence for intense ongoing star formation in the circumnuclear regions of these sources. Using the Infrared Spectrograph/Spitzer archive, we gathered a large number of additional NLS1s and their broad-line counterparts (BLS1s) and constructed NLS1 and BLS1 subsamples to compare them in various ways. The comparison shows a clear separation according to full width at half-maximum (H beta) [FWHM(H beta)] such that objects with narrower broad H beta lines are the strongest PAH emitters. We test this division in various ways trying to remove biases due to luminosity and aperture size. Specifically, we find that star formation activity around NLS1 AGN is larger than around BLS1 of the same AGN luminosity. The above result seems to hold over the entire range of distance and luminosity. Moreover, the star formation rate is higher in low black hole mass and high L/L(Edd) systems indicating that black hole growth and star formation are occurring simultaneously. C1 [Sani, E.] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy. [Sani, E.; Lutz, D.; Sturm, E.; Boller, T.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Risaliti, G.] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Netzer, H.; Trakhtenbrot, B.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Sch Phys & Astron, IL-69978 Tel Aviv, Israel. [Netzer, H.; Trakhtenbrot, B.] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel. [Gallo, L. C.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. RP Sani, E (reprint author), Univ Florence, Dipartimento Astron, Largo E Fermi 2, I-50125 Florence, Italy. EM sani@arcetri.astro.it OI Risaliti, Guido/0000-0002-3556-977X FU Italian Space Agency [ASI-INAF I/088/06/0]; Israel Science Foundation [364/07]; DIP [15981] FX We thank the referee for helpful comments. We also thank Nico Hamaus for help with part of the initial data reduction. This work was partially supported by the Italian Space Agency through contract ASI-INAF I/088/06/0.; Funding for this work at Tel Aviv University has been provided by the Israel Science Foundation grant 364/07 and the a DIP grant 15981. NR 62 TC 50 Z9 50 U1 0 U2 0 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD APR 11 PY 2010 VL 403 IS 3 BP 1246 EP 1260 DI 10.1111/j.1365-2966.2009.16217.x PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 577TS UT WOS:000276247500013 ER PT J AU Shen, Y Kelly, BC AF Shen, Yue Kelly, Brandon C. TI THE IMPACT OF THE UNCERTAINTY IN SINGLE-EPOCH VIRIAL BLACK HOLE MASS ESTIMATES ON THE OBSERVED EVOLUTION OF THE BLACK HOLE-BULGE SCALING RELATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; quasars: general; surveys ID ACTIVE GALACTIC NUCLEI; BH-SIGMA RELATION; RADIUS-LUMINOSITY RELATIONSHIP; HOST-GALAXY STARLIGHT; COSMIC EVOLUTION; DATA RELEASE-3; QUASAR SURVEY; SPHEROIDS; COEVOLUTION; SELECTION AB Recent observations of the black hole (BH)-bulge scaling relations usually report positive redshift evolution, with higher redshift galaxies harboring more massive BHs than expected from the local relations. All of these studies focus on broad line quasars with BH mass estimated from virial estimators based on single-epoch spectra. Since the sample selection is largely based on quasar luminosity, the cosmic scatter in the BH-bulge relation introduces a statistical bias leading to on average more massive BHs given galaxy properties at high redshift (i.e., the Lauer et al. bias). We here emphasize a previously underappreciated statistical bias resulting from the uncertainty of single-epoch virial BH mass estimators and the shape of the underlying (true) BH mass function, which leads to on average overestimation of the true BH masses at the high-mass end. We demonstrate that the latter virial mass bias can contribute a substantial amount to the observed excess in BH mass at fixed bulge properties, comparable to the Lauer et al. bias. The virial mass bias is independent of the Lauer et al. bias; hence if both biases are at work, they can largely (or even fully) account for the observed BH mass excess at high redshift. C1 [Shen, Yue; Kelly, Brandon C.] 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. FU Clay Postdoctoral Fellowship through the Smithsonian Astrophysical Observatory (SAO); NASA [HF-51243.01, NAS 5-26555]; Space Telescope Science Institute FX We thank the anonymous referee, as well as Tod Lauer, Scott Tremaine, Jenny Greene, and Avi Loeb for useful comments. Y.S. acknowledges support from a Clay Postdoctoral Fellowship through the Smithsonian Astrophysical Observatory (SAO). B. K. acknowledges support by NASA through Hubble Fellowship grant No. HF-51243.01 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 34 TC 12 Z9 12 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2010 VL 713 IS 1 BP 41 EP 45 DI 10.1088/0004-637X/713/1/41 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573MR UT WOS:000275918500004 ER PT J AU Xu, CK Domingue, D Cheng, YW Lu, NY Huang, JS Gao, Y Mazzarella, JM Cutri, R Sun, WH Surace, J AF Xu, C. Kevin Domingue, Donovan Cheng, Yi-Wen Lu, Nanyao Huang, Jiasheng Gao, Yu Mazzarella, Joseph M. Cutri, Roc Sun, Wei-Hsin Surace, Jason TI LOCAL BENCHMARKS FOR THE EVOLUTION OF MAJOR-MERGER GALAXIES-SPITZER OBSERVATIONS OF A K-BAND SELECTED SAMPLE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: general; galaxies: interactions; galaxies: starburst ID DIGITAL SKY SURVEY; STAR-FORMING GALAXIES; MULTIBAND IMAGING PHOTOMETER; LUMINOUS INFRARED GALAXIES; FRANCE REDSHIFT SURVEY; 24 MU-M; SPACE-TELESCOPE; FIELD GALAXIES; CLOSE PAIRS; INTERACTING GALAXIES AB We present Spitzer observations for a sample of close major-merger galaxy pairs (KPAIR sample) selected from cross-matches between the Two Micron All Sky Survey and Sloan Digital Sky Survey Data Release 3. The goals are to study the star formation activity in these galaxies and to set a local bench mark for the cosmic evolution of close major mergers. The Spitzer KPAIR sample (27 pairs, 54 galaxies) includes all spectroscopically confirmed spiral-spiral (S+S) and spiral-elliptical (S+E) pairs in a parent sample that is complete for primaries brighter than K = 12.5 mag, projected separations of 5 h(-1) kpc <= s <= 20 h(-1) kpc, and mass ratios <= 2.5. The Spitzer data, consisting of images in seven bands (3.6, 4.5, 5.8, 8, 24, 70, 160 mu m), show very diversified IR emission properties. Compared to single spiral galaxies in a control sample, only spiral galaxies in S+S pairs show significantly enhanced specific star formation rate (sSFR = SFR/M), whereas spiral galaxies in S+E pairs do not. Furthermore, the SFR enhancement of spiral galaxies in S+S pairs is highly mass-dependent. Only those with M greater than or similar to 10(10.5) M-circle dot show significant enhancement. Relatively low-mass (M similar to 10(10) M circle dot) spirals in S+S pairs have about the same SFR/M compared to their counterparts in the control sample, while those with 10(11) M-circle dot have on average a similar to 3 times higher SFR/M than single spirals. There is evidence for a correlation between the global star formation activities (but not the nuclear activities) of the component galaxies in massive S+S major-merger pairs (the "Holmberg effect"). There is no significant difference in the SFR/M between the primaries and the secondaries, nor between spirals of SEP < 1 and those of SEP >= 1, SEP being the normalized separation parameter. The contribution of KPAIR galaxies to the cosmic SFR density in the local universe is only 1.7%, and amounts (rho) over dot(KPAIR) = 2.54 x 10(-4) (M-circle dot yr(-1) Mpc(-3)). C1 [Xu, C. Kevin; Cheng, Yi-Wen; Lu, Nanyao; Mazzarella, Joseph M.; Cutri, Roc] CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. [Domingue, Donovan] Georgia Coll & State Univ, Milledgeville, GA 31061 USA. [Cheng, Yi-Wen] Natl Cent Univ, Inst Astron, Chungli 32054, Taiwan. [Cheng, Yi-Wen; Sun, Wei-Hsin] Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan. [Cheng, Yi-Wen; Sun, Wei-Hsin] Natl Taiwan Univ, Leung Ctr Cosmol & Particle Astrophys, Taipei 10617, Taiwan. [Huang, Jiasheng] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gao, Yu] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Surace, Jason] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. RP Xu, CK (reprint author), CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. OI SUN, WEI-HSIN/0000-0002-7474-8658; Domingue, Donovan/0000-0001-5662-7169; Mazzarella, Joseph/0000-0002-8204-8619 FU NSF of China [10833006, 10621303]; National Science Council in Taiwan [NSC 97-2112-M-002-014]; NASA FX C. K. X. thanks David Shupe for useful discussions on the SWIRE data handling. Y.G.'s research is partly supported by grants 10833006 and 10621303 of NSF of China. W.-H. S. and Y.-W. C. acknowledge the support of the National Science Council in Taiwan under the grant NSC 97-2112-M-002-014. Constructive comments by an anonymous referee are acknowledged. 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. 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 119 TC 16 Z9 17 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2010 VL 713 IS 1 BP 330 EP 355 DI 10.1088/0004-637X/713/1/330 PG 26 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573MR UT WOS:000275918500029 ER PT J AU Galvan-Madrid, R Montes, G Ramirez, EA Kurtz, S Araya, E Hofner, P AF Galvan-Madrid, Roberto Montes, Gabriela Ramirez, Edgar A. Kurtz, Stan Araya, Esteban Hofner, Peter TI THE RARE 23.1 GHz METHANOL MASERS IN NGC 7538 IRS 1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE H II regions; ISM: individual objects (NGC 7538); ISM: molecules; masers; radio lines: ISM; stars: formation ID STAR-FORMING REGIONS; ULTRACOMPACT HII-REGIONS; LARGE ARRAY OBSERVATIONS; H II REGIONS; VLA OBSERVATIONS; NGC-7538 IRS-1; RECOMBINATION LINE; (NH3)-N-15 MASER; FORMALDEHYDE MASERS; CIRCUMSTELLAR DISK AB We present high angular resolution (theta(syn) less than or similar to 0 ''.2) observations of the 23.1 GHz methanol (CH(3)OH) transition toward the massive star-forming region NGC 7538 IRS 1. The two velocity components previously reported by Wilson et al. are resolved into distinct spatial features with brightness temperatures (T(B)) greater than 10(4) K, proving their maser nature. Thus, NGC 7538 IRS 1 is the third region confirmed to show methanol maser emission at this frequency. The brighter 23.1 GHz spot coincides in position with a rare formaldehyde (H(2)CO) maser, and marginally with a 22.2 GHz water (H(2)O) maser, for which we report archival observations. The weaker CH(3)OH spot coincides with an H(2)O maser. The ratio of T(B) for the 23.1 GHz masers to that of the well-known 12.2 GHz CH(3)OH masers in this region roughly agrees with model predictions. However, the 23.1 GHz spots are offset in position from the CH(3)OH masers at other frequencies. This is difficult to interpret in terms of models that assume that all the masers arise from the same clumps, but it may result from turbulent conditions within the gas or rapid variations in the background radiation field. C1 [Galvan-Madrid, Roberto] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Galvan-Madrid, Roberto; Montes, Gabriela; Ramirez, Edgar A.; Kurtz, Stan] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Morelia 58090, Michoacan, Mexico. [Galvan-Madrid, Roberto] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Montes, Gabriela] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. [Ramirez, Edgar A.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Araya, Esteban] Western Illinois Univ, Dept Phys, Macomb, IL 61455 USA. [Hofner, Peter] New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. [Hofner, Peter] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Hofner, Peter] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Galvan-Madrid, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rgalvan@cfa.harvard.edu FU SMA predoctoral fellowship; NRAO Jansky Fellowship; NSF [AST-0908901] FX We thank the anonymous referee for comments that significantly improved this paper. We are grateful to the VLA staff for supporting the initial phase of this project via the NRAO program of observing time for university classes. We thank R. Franco-Hernandez for providing the 2 cm image; A. Sobolev, J. Ballesteros-Paredes, and M. Reid for helpful discussions; and V. Minier for providing us with maser positions. R. G.-M. acknowledges support from an SMA predoctoral fellowship. E. A. was partially supported by a NRAO Jansky Fellowship. P. H. acknowledges partial support from NSF grant AST-0908901. NR 44 TC 5 Z9 5 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2010 VL 713 IS 1 BP 423 EP 428 DI 10.1088/0004-637X/713/1/423 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573MR UT WOS:000275918500036 ER PT J AU Liao, YW Wu, JHP Ho, PTP Huang, CWL Koch, PM Lin, KY Liu, GC Molnar, SM Nishioka, H Umetsu, K Wang, FC Altamirano, P Birkinshaw, M Chang, CH Chang, SH Chang, SW Chen, MT Chiueh, T Han, CC Huang, YD Hwang, YJ Jiang, HM Kesteven, M Kubo, DY Li, CT Martin-Cocher, P Oshiro, P Raffin, P Wei, TS Wilson, W AF Liao, Yu-Wei Wu, Jiun-Huei Proty Ho, Paul T. P. Huang, Chih-Wei Locutus Koch, Patrick M. Lin, Kai-Yang Liu, Guo-Chin Molnar, Sandor M. Nishioka, Hiroaki Umetsu, Keiichi Wang, Fu-Cheng Altamirano, Pablo Birkinshaw, Mark Chang, Chia-Hao Chang, Shu-Hao Chang, Su-Wei Chen, Ming-Tang Chiueh, Tzihong Han, Chih-Chiang Huang, Yau-De Hwang, Yuh-Jing Jiang, Homin Kesteven, Michael Kubo, Derek Y. Li, Chao-Te Martin-Cocher, Pierre Oshiro, Peter Raffin, Philippe Wei, Tashun Wilson, Warwick TI AMiBA: SUNYAEV-ZEL'DOVICH EFFECT-DERIVED PROPERTIES AND SCALING RELATIONS OF MASSIVE GALAXY CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic background radiation; cosmology: observations; galaxies: clusters: general ID X-RAY MEASUREMENTS; MICROWAVE BACKGROUND ANISOTROPY; COSMIC DISTANCE SCALE; TELESCOPE; ARRAY; GAS; PROJECT AB The Sunyaev-Zel'dovich Effect ( SZE) has been observed toward six massive galaxy clusters, at redshifts 0.091 <= z <= 0.322 in the 86-102 GHz band with the Y. T. Lee Array for Microwave Background Anisotropy (AMiBA). We modify an iterative method, based on the isothermal beta models, to derive the electron temperature T(e), total mass M(t), gas mass M(g), and integrated Compton Y within r(2500), from the AMiBA SZE data. Non-isothermal universal temperature profile (UTP) beta models are also considered in this paper. These results are in good agreement with those deduced from other observations. We also investigate the embedded scaling relations, due to the assumptions that have been made in the method we adopted, between these purely SZE-deduced T(e), M(t), M(g), and Y. Our results suggest that cluster properties may be measurable with SZE observations alone. However, the assumptions built into the pure-SZE method bias the results of scaling relation estimations and need further study. C1 [Liao, Yu-Wei; Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Lin, Kai-Yang; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. [Liao, Yu-Wei; Wu, Jiun-Huei Proty; Huang, Chih-Wei Locutus; Lin, Kai-Yang; Wang, Fu-Cheng; Chiueh, Tzihong] Natl Taiwan Univ, Ctr Theoret Sci, Taipei 10617, Taiwan. [Liao, Yu-Wei; Ho, Paul T. P.; Koch, Patrick M.; Lin, Kai-Yang; Liu, Guo-Chin; Molnar, Sandor M.; Nishioka, Hiroaki; Umetsu, Keiichi; Altamirano, Pablo; Chang, Chia-Hao; Chang, Shu-Hao; Chang, Su-Wei; Chen, Ming-Tang; Han, Chih-Chiang; Huang, Yau-De; Hwang, Yuh-Jing; Jiang, Homin; Kubo, Derek Y.; Li, Chao-Te; Martin-Cocher, Pierre; Oshiro, Peter; Raffin, Philippe; Wei, Tashun] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Liu, Guo-Chin] Tamkang Univ, Dept Phys, Tamsui 25137, Taipei County, Taiwan. [Birkinshaw, Mark] Univ Bristol, Bristol BS8 1TL, Avon, England. [Kesteven, Michael; Wilson, Warwick] Australia Telescope Natl Facil, Epping, NSW 1710, Australia. RP Liao, YW (reprint author), Natl Taiwan Univ, Dept Phys, Inst Astrophys, Taipei 10617, Taiwan. OI WU, JIUN-HUEI/0000-0001-9608-7662; CHIUEH, TZI-HONG/0000-0003-2654-8763; Umetsu, Keiichi/0000-0002-7196-4822 FU Ministry of Education; National Science Council (NSC); Academia Sinica, Taiwan; National Center for Theoretical Science, and Center for Theoretical Sciences, National Taiwan University; STFC FX We thank the Ministry of Education, the National Science Council (NSC), and the Academia Sinica, Taiwan, for their funding and supporting of AMiBA project. Y. W. L. thanks the AMiBA team for their guiding, supporting, hard working, and helpful discussions. We are grateful for computing support from the National Center for High-Performance Computing, Taiwan. This work is also supported by National Center for Theoretical Science, and Center for Theoretical Sciences, National Taiwan University for J.-H.P.W. Support from the STFC for M. Birkinshaw is also acknowledged. NR 40 TC 7 Z9 7 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 10 PY 2010 VL 713 IS 1 BP 584 EP 591 DI 10.1088/0004-637X/713/1/584 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 573MR UT WOS:000275918500052 ER PT J AU Chen, HR Liu, SY Su, YN Zhang, QZ AF Chen, Huei-Ru Liu, Sheng-Yuan Su, Yu-Nung Zhang, Qizhou TI DEUTERIUM FRACTIONATION AS AN EVOLUTIONARY PROBE IN THE INFRARED DARK CLOUD G28.34+0.06 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: abundances; ISM: clouds; ISM: individual objects (G28.34+0.06); stars: formation ID STAR-FORMATION; PHYSICAL CONDITIONS; INITIAL CONDITIONS; CORES; N2H+; NH3; DEPLETION; N2D+ AB We have observed the J = 3 - 2 transition of N(2)H(+) and N(2)D(+) to investigate the trend of deuterium fractionation with evolutionary stage in three selected regions in the infrared dark cloud (IRDC) G28.34+0.06 with the Submillimeter Telescope and the Submillimeter Array. A comprehensible enhancement of roughly 3 orders of magnitude in deuterium fractionation over the local interstellar D/H ratio is observed in all sources. In particular, our sample of massive star-forming cores in G28.34+0.06 shows a moderate decreasing trend over a factor of 3 in the N(N(2)D(+))/N(N(2)H(+)) ratio with evolutionary stage, a behavior resembling that previously found in low-mass protostellar cores. This suggests a possible extension for the use of the N(N(2)D(+))/N(N(2)H(+)) ratio as an evolutionary tracer to high-mass protostellar candidates. In the most evolved core, MM1, the N(2)H(+) (3 - 2) emission appears to avoid the warm region traced by dust continuum emission and emission of (13)CO sublimated from grain mantles, indicating an instant release of gas-phase CO. The majority of the N(2)H(+) and N(2)D(+) emission is associated with extended structures larger than 8 '' (similar to 0.2 pc). C1 [Chen, Huei-Ru] Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. [Chen, Huei-Ru] Natl Tsing Hua Univ, Dept Phys, Hsinchu, Taiwan. [Chen, Huei-Ru; Liu, Sheng-Yuan; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Chen, HR (reprint author), Natl Tsing Hua Univ, Inst Astron, Hsinchu, Taiwan. EM hchen@phys.nthu.edu.tw OI Zhang, Qizhou/0000-0003-2384-6589 FU National Science Council of Taiwan [NSC 97-2112-M-001-006-MY2, NSC 97-2112-M-007-006-MY3] FX This research is supported by the National Science Council of Taiwan through grants NSC 97-2112-M-001-006-MY2 and NSC 97-2112-M-007-006-MY3. NR 28 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2010 VL 713 IS 1 BP L50 EP L54 DI 10.1088/2041-8205/713/1/L50 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 582KA UT WOS:000276594900011 ER PT J AU Ciaravella, A Raymond, JC Giordano, S AF Ciaravella, A. Raymond, J. C. Giordano, S. TI ULTRAVIOLET SPECTRA OF THE C-2003K7 COMET: EVIDENCE FOR DUST SUBLIMATION IN Si AND C LINES SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE comets: general; comets: individual (C/2001 C2); ultraviolet: general ID CORONAGRAPH SPECTROMETER; INTERSTELLAR DUST; UVCS OBSERVATION; C/1995 O1; HALE-BOPP; SOHO; PARTICLES; P/HALLEY; SUN AB UV spectra of the bright sungrazing comet C-2003K7 detected at 2.37 R(circle dot) above the Sun surface by the Ultraviolet Coronagraph Spectrometer (UVCS) during the daily synoptic scan show bright lines of Hi Ly alpha, Si III lambda 1206, and C III lambda 977. The derived outgassing rate is an order of magnitude larger than those of the other sungrazers observed by UVCS. Analysis of the spectra suggests that the comet broke apart into smaller pieces before it reached the UVCS slit. The observations provide lower and upper limits to the values of the Si III/C III ratio, in the range 8-22. The ratio indicates a larger abundance of silicates in the cometary dust as compared to organic refractory materials. C1 [Ciaravella, A.] Osserv Astron Palermo, INAF, I-90134 Palermo, Italy. [Ciaravella, A.; Raymond, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Giordano, S.] Osserv Astron Torino, INAF, I-10025 Pino Torinese, Italy. RP Ciaravella, A (reprint author), Osserv Astron Palermo, INAF, Pza Parlamento 1, I-90134 Palermo, Italy. EM aciaravella@astropa.unipa.it OI Ciaravella, Angela/0000-0002-3127-8078; Giordano, Silvio/0000-0002-3468-8566 FU NASA [NNG06GG78G] FX We are grateful to the referee, Dr. M. A'Hearn, for very helpful comments. This comet was discovered during a search for UV spectra of Coronal Mass Ejections supported by the NASA Grant NNG06GG78G to the Smithsonian Astrophysical Observatory. NR 30 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD APR 10 PY 2010 VL 713 IS 1 BP L69 EP L73 DI 10.1088/2041-8205/713/1/L69 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 582KA UT WOS:000276594900015 ER PT J AU Kessler, EM Yelin, S Lukin, MD Cirac, JI Giedke, G AF Kessler, E. M. Yelin, S. Lukin, M. D. Cirac, J. I. Giedke, G. TI Optical Superradiance from Nuclear Spin Environment of Single-Photon Emitters SO PHYSICAL REVIEW LETTERS LA English DT Article ID SPONTANEOUS EMISSION; SUPER-RADIANCE; DIAMOND AB We show that superradiant optical emission can be observed from the polarized nuclear spin ensemble surrounding a single-photon emitter such as a single quantum dot or nitrogen-vacancy center. The superradiant light is emitted under optical pumping conditions and would be observable with realistic experimental parameters. C1 [Kessler, E. M.; Cirac, J. I.; Giedke, G.] Max Planck Inst Quantum Opt, D-85748 Garching, Germany. [Yelin, S.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. [Yelin, S.; Lukin, M. D.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Kessler, EM (reprint author), Max Planck Inst Quantum Opt, Hans Kopfermann Str 1, D-85748 Garching, Germany. RI Kessler, Eric Matthias/E-6981-2012; OI Kessler, Eric Matthias/0000-0001-9959-538X; Giedke, Geza/0000-0002-9676-5686 FU GIF; DFG [SFB 631]; Cluster of Excellence NIM; NSF; DARPA; Packard Foundation FX We acknowledge support by GIF, the DFG within SFB 631 and the Cluster of Excellence NIM, the NSF, DARPA, and the Packard Foundation. NR 29 TC 16 Z9 16 U1 0 U2 15 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD APR 9 PY 2010 VL 104 IS 14 AR 143601 DI 10.1103/PhysRevLett.104.143601 PG 4 WC Physics, Multidisciplinary SC Physics GA 581RL UT WOS:000276541900019 PM 20481939 ER PT J AU Fishbaugh, KE Hvidberg, CS Byrne, S Russell, PS Herkenhoff, KE Winstrup, M Kirk, R AF Fishbaugh, Kathryn E. Hvidberg, Christine S. Byrne, Shane Russell, Patrick S. Herkenhoff, Kenneth E. Winstrup, Mai Kirk, Randolph TI First high-resolution stratigraphic column of the Martian north polar layered deposits SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID MARS; REGION; TOPOGRAPHY; HISTORY AB This study achieves the first high-spatial-resolution, layer-scale, measured stratigraphic column of the Martian north polar layered deposits using a 1m-posting DEM. The marker beds found throughout the upper North Polar Layered Deposits range in thickness from 1.6 m-16.0 m +/-1.4 m, and 6 of 13 marker beds are separated by similar to 25-35 m. Thin-layer sets have average layer separations of 1.6 m. These layer separations may account for the spectral-power-peaks found in previous brightness-profile analyses. Marker-bed layer thicknesses show a weak trend of decreasing thickness with depth that we interpret to potentially be the result of a decreased accumulation rate in the past, for those layers. However, the stratigraphic column reveals that a simple rhythmic or bundled layer sequence is not immediately apparent throughout the column, implying that the relationship between polar layer formation and cyclic climate forcing is quite complex. Citation: Fishbaugh, K. E., C. S. Hvidberg, S. Byrne, P. S. Russell, K. E. Herkenhoff, M. Winstrup, and R. Kirk (2010), First high-resolution stratigraphic column of the Martian north polar layered deposits, Geophys. Res. Lett., 37, L07201, doi: 10.1029/2009GL041642. C1 [Fishbaugh, Kathryn E.; Russell, Patrick S.] Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Hvidberg, Christine S.; Winstrup, Mai] Univ Copenhagen, Niels Bohr Inst, Ctr Ice & Climate, DK-2100 Copenhagen, Denmark. [Byrne, Shane] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Herkenhoff, Kenneth E.; Kirk, Randolph] US Geol Survey, Flagstaff, AZ 86001 USA. RP Fishbaugh, KE (reprint author), Smithsonian Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315,POB 30712, Washington, DC 20013 USA. EM fishbaughke@si.edu RI Byrne, Shane/B-8104-2012; Winstrup, Mai/M-5844-2014; Hvidberg, Christine/E-8934-2015 OI Winstrup, Mai/0000-0002-4794-4004; Hvidberg, Christine/0000-0002-9665-1339 FU NASA; Danish Council for Independent Research FX This work was funded by a NASA Mars Reconnaissance Orbiter Participating Scientist grant to KEF. The DEM was created at the USGS Astrogeology Science Center in Flagstaff, AZ. Thanks are gratefully extended to the International Space Science Institute (ISSI) in Bern, Switzerland for hosting the KEF-led team, "Are the Martian polar deposits a Rosetta Stone for the climate?"; the fruitful discussions during those meetings greatly improved our understanding of the NPLD stratigraphy. CSH thanks the Danish Council for Independent Research for support. NR 30 TC 9 Z9 9 U1 0 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD APR 2 PY 2010 VL 37 AR L07201 DI 10.1029/2009GL041642 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 578SD UT WOS:000276314600001 ER PT J AU Colwell-Chanthaphonh, C Ferguson, TJ Lippert, D McGuire, RH Nicholas, GP Watkins, JE Zimmerman, LJ AF Colwell-Chanthaphonh, Chip Ferguson, T. J. Lippert, Dorothy McGuire, Randall H. Nicholas, George P. Watkins, Joe E. Zimmerman, Larry J. TI THE PREMISE AND PROMISE OF INDIGENOUS ARCHAEOLOGY SO AMERICAN ANTIQUITY LA English DT Editorial Material ID ORAL TRADITION; AMERICANS AB Researchers have increasingly promoted an emerging paradigm of Indigenous archaeology, which includes an array of practices conducted by, for and with Indigenous communities to challenge the discipline's intellectual breadth and political economy. McGhee (2008) argues that Indigenous archaeology is not viable because it depends upon the essentialist concept of "Aboriginalism." In this reply, we correct McGhee's description of Indigenous Archaeology and demonstrate why Indigenous rights are not founded on essentialist imaginings. Rather, the legacies of colonialism, sociopolitical context of scientific inquiry, and insights of traditional knowledge provide a strong foundation for collaborative and community-based archaeology projects that include Indigenous peoples. C1 [Colwell-Chanthaphonh, Chip] Denver Museum Nat & Sci, Denver, CO 80205 USA. [Ferguson, T. J.] Univ Arizona, Tucson, AZ 85745 USA. [Lippert, Dorothy] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [McGuire, Randall H.] Binghamton Univ, Binghamton, NY 13902 USA. [Nicholas, George P.] Simon Fraser Univ, Burnaby, BC V5A 1S6, Canada. [Watkins, Joe E.] Univ Oklahoma, Norman, OK 73019 USA. [Zimmerman, Larry J.] Indiana Univ Purdue Univ, Indianapolis, IN 46202 USA. RP Colwell-Chanthaphonh, C (reprint author), Denver Museum Nat & Sci, Denver, CO 80205 USA. NR 99 TC 20 Z9 20 U1 2 U2 15 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 APR PY 2010 VL 75 IS 2 BP 228 EP 238 PG 11 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 592RH UT WOS:000277396700004 ER PT J AU Needell, AA AF Needell, Allan A. TI In Sputnik's Shadow: The President's Science Advisory Committee and Cold War America. SO AMERICAN HISTORICAL REVIEW LA English DT Book Review C1 [Needell, Allan A.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Needell, AA (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 0002-8762 J9 AM HIST REV JI Am. Hist. Rev. PD APR PY 2010 VL 115 IS 2 BP 573 EP 574 PG 2 WC History SC History GA 584TV UT WOS:000276776900099 ER PT J AU Echegaray, J Vila, C AF Echegaray, J. Vila, C. TI Noninvasive monitoring of wolves at the edge of their distribution and the cost of their conservation SO ANIMAL CONSERVATION LA English DT Article DE mitochondrial DNA; microsatellites; noninvasive monitoring; Spain; Canis lupus; dog; predator control ID WOLF CANIS-LUPUS; DOMESTIC DOGS; NORTHWESTERN MINNESOTA; GENOTYPING FECES; RURAL ZIMBABWE; FOOD-HABITS; POPULATION; IDENTIFICATION; CARNIVORES; FAMILIARIS AB Large predators are recolonizing areas in industrialized countries, where they have been absent for decades or centuries. As they reach these areas, the predators often encounter unwary livestock and unprepared keepers, which translates into large economic costs. The cost per individual may have important repercussions on the conservation and management of large predators. During the years 2003-2004, we collected 136 feces preliminarily identified as belonging to gray wolves Canis lupus along the north-eastern limit of the wolf range in the Iberia peninsula (Basque Country, Spain). Genetic analyses allowed us to identify the species of origin in 86 cases: 31 corresponded to wolves, two to red foxes Vulpes vulpes and 53 to dogs Canis familiaris. Among the wolves, we identified 16 different individuals. We estimated the cost of conserving wolves to be > euro3000 per wolf per year, based on the cost of damage compensation and prevention during the 2003-2004 period. However, most of the wolf feces contained wild prey whereas dog feces contained mostly remains of domestic animals. This finding suggests that uncontrolled dogs could be responsible for some of the attacks on livestock, contributing to negative public attitudes toward wolf conservation and increasing its cost. C1 [Echegaray, J.; Vila, C.] Estac Biol Donana CSIC, Seville 41092, Spain. [Echegaray, J.] Basque Wolf Grp, Vitoria, Spain. [Echegaray, J.] Smithsonian Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20560 USA. RP Echegaray, J (reprint author), Estac Biol Donana CSIC, Avd Amer Vespucio S-N, Seville 41092, Spain. EM echegaray@ebd.csic.es RI Vila, Carles/H-4893-2013; CSIC, EBD Donana/C-4157-2011 OI Vila, Carles/0000-0002-4206-5246; CSIC, EBD Donana/0000-0003-4318-6602 FU Biodiversity Area of the Environment Department of the Basque Government; US National Science Foundation [OPP 0352634]; Direccio General de Recerca [2005SGR00090]; 'Generalitat de Catalunya,' Spain; Smithsonian Institution FX This study was supported by the Biodiversity Area of the Environment Department of the Basque Government, the US National Science Foundation (OPP 0352634) and the 'Direccio General de Recerca' (2005SGR00090) of the 'Generalitat de Catalunya,' Spain. The 'Programa de Captacion del Conocimiento para Andalucia' and Gas Natural SDG S.A. supported C.V. The Genetics Program, Smithsonian Institution, provided logistical support. We thank people of the Evolutionary Biology Department in Sweden for their help and assistance during the laboratory work, and also Andres Illana, Alberto Hernando, Felix Martinez de Lecea, Juane Bayona, Juan Angel de la Torre, Iratxe Covela and Diana Paniagua for their participation in the field and office work, and Jennifer A. Leonard for critical review of the paper. NR 41 TC 14 Z9 14 U1 2 U2 46 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD APR PY 2010 VL 13 IS 2 BP 157 EP 161 DI 10.1111/j.1469-1795.2009.00315.x PG 5 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 573MA UT WOS:000275916800010 ER PT J AU Bobrowiec, PED Gribel, R AF Bobrowiec, P. E. D. Gribel, R. TI Effects of different secondary vegetation types on bat community composition in Central Amazonia, Brazil SO ANIMAL CONSERVATION LA English DT Article DE bat community structure; Chiroptera; landscape characteristic; habitat use; secondary forest ID PHYLLOSTOMID BATS; RAIN-FOREST; FRAGMENTED LANDSCAPE; SPECIES RICHNESS; STURNIRA-LILIUM; SPATIAL AUTOCORRELATION; NEOTROPICAL FOREST; MOVEMENT PATTERNS; EASTERN AMAZONIA; FRUGIVOROUS BATS AB The process of secondary succession on degraded lands in the Amazon depends on their land-use histories. In this scenario, little is known about how animal communities respond to different types of secondary vegetation in the region. We examined the effects of abandoned cattle pasture, Vismia- and Cecropia-dominated regrowth on the abundance of bat species and community composition in the Central Amazon, Brazil, based on 11 netting sites and on landscape characteristics. We captured 1444 bats, representing 26 species and two families (Phyllostomidae and Mormoopidae). Among the six most-captured Phyllostomidae bats, Sturnira lilium and Sturnira tildae had significantly higher capture rates in abandoned pasture, while Rhinophylla pumilio predominated in both Vismia- and Cecropia-dominated regrowth. An hybrid multidimensional scaling ordination revealed significant differences in the bat community among the three types of secondary vegetation. Phyllostominae bats were more common and richer in the less-disturbed areas of Cecropia-dominated regrowth, while Stenodermatinae species were more captured in abandoned pastures. Our results suggest that the type of secondary vegetation, together with its land-use history, affects bat community composition in the Central Amazon. The Phyllostominae subfamily (gleaning animalivores) was habitat selective and disappeared from areas experiencing constant disturbances. On the other hand, Stenodermatinae frugivorous bats often used and foraged in altered areas. We suggest that secondary vegetations in more-advanced successional stages can be used to augment the total area protected by forest conservation units. C1 [Bobrowiec, P. E. D.] Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, BR-69011970 Manaus, Amazonas, Brazil. [Bobrowiec, P. E. D.] Smithsonian Trop Res Inst, Manaus, Amazonas, Brazil. RP Bobrowiec, PED (reprint author), Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, CP 478, BR-69011970 Manaus, Amazonas, Brazil. EM pauloedb@inpa.gov.br RI Bobrowiec, Paulo Estefano/A-2630-2013; Adapta, Inct/J-8371-2013; Gribel, Rogerio/C-5392-2013 OI Gribel, Rogerio/0000-0002-0850-5578 FU BDFFP; Smithsonian Institution, WWF - Brazil [CSR 250-2001]; National Council of Scientific and Technological Development (CNPq) [133388/2001-8] FX This study was financed by the BDFFP, administered in cooperation with the National Institute for Research in the Amazon (INPA) and the Smithsonian Institution, WWF - Brazil (Programa Sociedade e Natureza, grant no. CSR 250-2001 to PEDB), and the National Council of Scientific and Technological Development (CNPq grant no 133388/2001-8 to PEDB), whom we gratefully acknowledge. We are grateful to Marcelo Paustein Moreira and Marcelo A. dos Santos Jr for landscape measurements. We thank Jose Francisco Tenacol Jr, Ocirio 'Juruna' de Souza Pereira, Osmaildo Ferreira da Silva and Alaercio 'Leo' Marajo dos Reis for their help in collecting field data. We are also grateful to S.V. Wilson for improving the English paper for publication. We thank three anonymous reviewers for commenting on drafts of the paper. This is publication 546 in the Technical Series of the BDFPP. NR 59 TC 18 Z9 19 U1 2 U2 23 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1367-9430 J9 ANIM CONSERV JI Anim. Conserv. PD APR PY 2010 VL 13 IS 2 BP 204 EP 216 DI 10.1111/j.1469-1795.2009.00322.x PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 573MA UT WOS:000275916800015 ER PT J AU Caro, F Douglas, JG Im, S AF Caro, F. Douglas, J. G. Im, S. TI TOWARDS A QUANTITATIVE PETROGRAPHIC DATABASE OF KHMER STONE MATERIALS-KOH KER STYLE SCULPTURE SO ARCHAEOMETRY LA English DT Article DE SANDSTONE; PETROGRAPHY; PROVENANCE; CAMBODIA; SCULPTURE; POINT COUNTING ID DETRITAL MODES AB A comprehensive quantitative petrographic database of sandstones used by the Khmers for sculptural purposes would be a helpful tool for archaeologists, museum curators and others interested in pursuing research on early stone usage, geological source and provenance. Towards that end, this paper presents quantitative petrographic analysis of stone materials used in the production of some free-standing sculptures and architectural elements in the Koh Ker style of the 10th century from the collections of the National Museum of Cambodia and The Metropolitan Museum of Art. These materials are compared to samples from the quarry of Thma Anlong near the foothills of the Phnom Kulen, Sieam Reap province. Primary and secondary detrital modes and key grain-size parameters are used to identify three sandstone types. The free-standing sculptures are carved from feldspathic arenite and feldspato-lithic to litho-feldspathic arenite. Finely carved lintels are worked from a quartz arenite, which is significantly richer in quartz grains and of a finer grain size. The geological source of the two other lithotypes will have to await detailed geological survey of the Koh Ker area accompanied by petrographic study of selected samples from documented quarries. The significance and potentiality of quantitative petrographic study of Khmer stone materials are shown in supporting and integrating archaeological investigations in South-East Asia. C1 [Caro, F.] Metropolitan Museum Art, Dept Sci Res, New York, NY 10028 USA. [Douglas, J. G.] Smithsonian Inst, Dept Conservat & Sci Res, Washington, DC 20013 USA. [Im, S.] APSARA Author, Siem Reap, Cambodia. RP Caro, F (reprint author), Metropolitan Museum Art, Dept Sci Res, New York, NY 10028 USA. FU Metropolitan Museum of Art FX This research was supported by an Andrew W. Mellon Fellowship at The Metropolitan Museum of Art. The authors are also grateful to several key staff members at the Metropolitan of Art for their comments and suggestions during the research, including John Guy, Curator of South and Southeast Asian Art; Kurt Behrendt, Assistant Curator; Donna Strahan, Conservator; and Paul Lavy, J. Clawson Mills Fellow. Paul Jett, Head of the Department of Conservation and Scientific Research at the Smithsonian's Freer Gallery of Art and Arthur M. Sackler Gallery, is thanked for his support for the project and help in obtaining quarry samples. Bertrand Porte, stone conservator with the Ecole Francaise d'Extreme-Orient (EFEO), working at the National Museum of Cambodia, kindly provided sandstone fragments from Koh Ker sculptures that had been generated during stone conservation treatments in 2001 and 2002. Special thanks go to Sieng Sotham, Director of the Department of Geology, Ministry of Industry, Mines and Energy in Phnom Penh, for his valuable comments on the Mesozoic geology of Cambodia, and to Masahiko Tsukada, Associate Research Scientist at the Department of Scientific Research of The Metropolitan Museum of Art, for his accurate translation of the Japanese papers cited in this work. NR 27 TC 1 Z9 1 U1 1 U2 6 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0003-813X J9 ARCHAEOMETRY JI Archaeometry PD APR PY 2010 VL 52 BP 191 EP 208 DI 10.1111/j.1475-4754.2009.00475.x PN 2 PG 18 WC Archaeology; Chemistry, Analytical; Chemistry, Inorganic & Nuclear; Geosciences, Multidisciplinary SC Archaeology; Chemistry; Geology GA 567JH UT WOS:000275442400002 ER PT J AU Woodman, N AF Woodman, Neal TI History and dating of the publication of the Philadelphia (1822) and London (1823) editions of Edwin James's Account of an expedition from Pittsburgh to the Rocky Mountains SO ARCHIVES OF NATURAL HISTORY LA English DT Article DE Stephen Harriman Long; Thomas Say; North America; exploration; nomenclature; publication history; taxonomy AB The public record of Major Stephen H. Long's 1819-1820 exploration of the American north-west, Account of an expedition from Pittsburgh to the Rocky Mountains, compiled by Edwin James, contains valuable contributions regarding the natural landscapes, native peoples and wildlife of a mostly unexplored region of the American west compiled from the notes of some of America's foremost naturalists, and it includes the first descriptions of 67 new species. The original plan was to publish the Account in Philadelphia and London simultaneously, yet these two editions differ substantially in ways that are relevant to the taxonomic contributions in the work. It is generally assumed that the Philadelphia edition was published in early January 1823 and was available first, but little substantive evidence has been presented to support its priority over the London edition. Review of contemporary correspondence and periodicals indicates the Philadelphia edition was available and for sale on 31 December 1822, whereas the London edition was available in late February 1823. As previously assumed by most sources, the Philadelphia edition has priority of publication and is the authority for most species names. Its correct year of publication, however, is 1822 rather than 1823. 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, MRC 111,POB 37012, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 70 TC 3 Z9 5 U1 0 U2 3 PU EDINBURGH UNIV PRESS PI EDINBURGH PA 22 GEORGE SQUARE, EDINBURGH EH8 9LF, MIDLOTHIAN, SCOTLAND SN 0260-9541 J9 ARCH NAT HIST JI Arch. Nat. Hist. PD APR PY 2010 VL 37 IS 1 BP 28 EP 38 DI 10.3366/E0260954109001636 PG 11 WC History & Philosophy Of Science; Multidisciplinary Sciences SC History & Philosophy of Science; Science & Technology - Other Topics GA 838UZ UT WOS:000296319300003 ER PT J AU Nantais, JB Huchra, JP McLeod, B Strader, J Brodie, JP AF Nantais, Julie B. Huchra, John P. McLeod, Brian Strader, Jay Brodie, Jean P. TI STAR CLUSTER CANDIDATES IN M81 SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (M81); galaxies: spiral; galaxies: star clusters: general; galaxies: stellar content ID GLOBULAR-CLUSTERS; SYSTEMS; CALIBRATION; GALAXIES; CATALOG; CAMERA; MODELS AB We present a catalog of extended objects in the vicinity of M81 based on a set of 24 Hubble Space Telescope Advanced Camera for Surveys Wide Field Camera F814W (I-band) images. We have found 233 good globular cluster (GC) candidates; 92 candidate H II regions, OB associations, or diffuse open clusters; 489 probable background galaxies; and 1719 unclassified objects. We have color data from ground-based g- and r-band MMT Megacam images for 79 galaxies, 125 GC candidates, 7 H II regions, and 184 unclassified objects. The color-color diagram of GC candidates shows that most fall into the range 0.25 < g - r < 1.25 and 0.5 < r - I < 1.25, similar to the color range of Milky Way GCs. Unclassified objects are often blue, suggesting that many of them are likely to be H II regions and open clusters, although a few galaxies and GCs may be among them. C1 [Nantais, Julie B.; Huchra, John P.; McLeod, Brian; Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodie, Jean P.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. RP Nantais, JB (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU Space Telescope Science Institute [GO 10250]; National Science Foundation [AST 0507729] FX This research was supported by the NASA grant GO 10250 from the Space Telescope Science Institute and the National Science Foundation grant AST 0507729. We thank Andreas Zezas and Kosmas Gazeas for providing us with F435-W and F606-W data and a matching mosaic of our I-band data in order to check for proper motion in the pointlike cluster candidates. Wealso thank the extremely helpful staff of the Space Telescope Science Institute, especially Ray Lucas and Mauro Gavalisco (now at UMASS). NR 22 TC 5 Z9 5 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2010 VL 139 IS 4 BP 1413 EP 1425 DI 10.1088/0004-6256/139/4/1413 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568BO UT WOS:000275496900010 ER PT J AU Bianco, FB Zhang, ZW Lehner, MJ Mondal, S King, SK Giammarco, J Holman, MJ Coehlo, NK Wang, JH Alcock, C Axelrod, T Byun, YI Chen, WP Cook, KH Dave, R de Pater, I Kim, DW Lee, T Lin, HC Lissauer, JJ Marshall, SL Protopapas, P Rice, JA Schwamb, ME Wang, SY Wen, CY AF Bianco, F. B. Zhang, Z. -W. Lehner, M. J. Mondal, S. King, S. -K. Giammarco, J. Holman, M. J. Coehlo, N. K. Wang, J. -H. Alcock, C. Axelrod, T. Byun, Y. -I. Chen, W. P. Cook, K. H. Dave, R. de Pater, I. Kim, D. -W. Lee, T. Lin, H. -C. Lissauer, J. J. Marshall, S. L. Protopapas, P. Rice, J. A. Schwamb, M. E. Wang, S. -Y. Wen, C. -Y. TI THE TAOS PROJECT: UPPER BOUNDS ON THE POPULATION OF SMALL KUIPER BELT OBJECTS AND TESTS OF MODELS OF FORMATION AND EVOLUTION OF THE OUTER SOLAR SYSTEM SO ASTRONOMICAL JOURNAL LA English DT Article DE Kuiper belt: general; occultations ID AMERICAN OCCULTATION SURVEY; JUPITER-FAMILY COMETS; TRANS-NEPTUNIAN BODIES; SIZE DISTRIBUTION; STELLAR OCCULTATIONS; COLLISIONAL EVOLUTION; SCATTERED DISK; OORT CLOUD; SEARCH; ACCRETION AB We have analyzed the first 3.75 years of data from the Taiwanese American Occultation Survey (TAOS). TAOS monitors bright stars to search for occultations by Kuiper Belt objects (KBOs). This data set comprises 5 x 10(5) star hours of multi-telescope photometric data taken at 4 or 5 Hz. No events consistent with KBO occultations were found in this data set. We compute the number of events expected for the Kuiper Belt formation and evolution models of Pan & Sari, Kenyon & Bromley, Benavidez & Campo Bagatin, and Fraser. A comparison with the upper limits we derive from our data constrains the parameter space of these models. This is the first detailed comparison of models of the KBO size distribution with data from an occultation survey. Our results suggest that the KBO population is composed of objects with low internal strength and that planetary migration played a role in the shaping of the size distribution. C1 [Bianco, F. B.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Bianco, F. B.] Global Telescope Network Inc, Cumbres Observ, Santa Barbara, CA 93117 USA. [Bianco, F. B.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bianco, F. B.; Lehner, M. J.; Holman, M. J.; Alcock, C.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zhang, Z. -W.; Lehner, M. J.; King, S. -K.; Wang, J. -H.; Lee, T.; Lin, H. -C.; Wang, S. -Y.; Wen, C. -Y.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Zhang, Z. -W.; Wang, J. -H.; Chen, W. P.] Natl Cent Univ, Inst Astron, Jhongli 32054, Taiwan. [Mondal, S.] ARIES, Naini Tal 263129, India. [Giammarco, J.] Eastern Univ, Dept Phys & Astron, St Davids, PA 19087 USA. [Giammarco, J.] Villanova Univ, Dept Phys, Villanova, PA 19085 USA. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Byun, Y. -I.; Kim, D. -W.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Cook, K. H.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94550 USA. [Dave, R.; Kim, D. -W.; Protopapas, P.] Initiat Innovat Comp Harvard, Cambridge, MA 02138 USA. [de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Lissauer, J. J.] NASA, Ames Res Ctr, Space Sci & Astrobiol Div 245 3, Moffett Field, CA 94035 USA. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Schwamb, M. E.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. RP Bianco, FB (reprint author), Univ Calif Santa Barbara, Dept Phys, Mail Code 9530, Santa Barbara, CA 93106 USA. EM fbianco@lcogt.net RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985 FU NSF [AST-0501681, DMS-0636667]; NASA [NNG04G113G]; NSC [96-2112-M008- 024-MY3]; National Research Foundation of Korea [2009-0075376]; NASA's Planetary Geology & Geophysics Program; [AS-88-TP-A02] FX The authors thank Scott Kenyon, for insightful conversations. Work at the CfA was supported in part by the NSF under grant AST-0501681 and by NASA under grant NNG04G113G. Work at NCU was supported by the grant NSC 96-2112-M008- 024-MY3. Work at ASIAA was supported in part by the thematic research program AS-88-TP-A02. Work at Yonsei was supported by National Research Foundation of Korea through grant 2009-0075376 (Space Science Institute). The work of N. Coehlo was supported in part by NSF grant DMS-0636667. Work at LLNL was performed in part under USDOE Contract W-7405-Eng-48 and Contract DE-AC52-07NA27344. Work at SLAC was performed under USDOE contract DE-AC0276SF00515. Work at NASA Ames was supported by NASA's Planetary Geology & Geophysics Program. NR 51 TC 25 Z9 25 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2010 VL 139 IS 4 BP 1499 EP 1514 DI 10.1088/0004-6256/139/4/1499 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568BO UT WOS:000275496900018 ER PT J AU Foster, C Forbes, DA Proctor, RN Strader, J Brodie, JP Spitler, LR AF Foster, Caroline Forbes, Duncan A. Proctor, Robert N. Strader, Jay Brodie, Jean P. Spitler, Lee R. TI DERIVING METALLICITIES FROM THE INTEGRATED SPECTRA OF EXTRAGALACTIC GLOBULAR CLUSTERS USING THE NEAR-INFRARED CALCIUM TRIPLET SO ASTRONOMICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1407); galaxies: star clusters: general; techniques: spectroscopic ID EARLY-TYPE GALAXIES; STELLAR POPULATION SYNTHESIS; INITIAL MASS FUNCTION; CAII TRIPLET; EMPIRICAL CALIBRATION; COLOR DISTRIBUTIONS; CHEMICAL ABUNDANCES; ELLIPTIC GALAXIES; FITTING FUNCTIONS; EFFECTIVE RADII AB The Ca II triplet (CaT) feature in the near-infrared has been employed as a metallicity indicator for individual stars as well as integrated light of Galactic globular clusters (GCs) and galaxies with varying degrees of success, and sometimes puzzling results. Using the DEIMOS multi-object spectrograph on Keck we obtain a sample of 144 integrated light spectra of GCs around the brightest group galaxy NGC 1407 to test whether the CaT index can be used as ametallicity indicator for extragalactic GCs. Different sets of single stellar population models make different predictions for the behavior of the CaT as a function of metallicity. In this work, the metallicities of the GCs around NGC 1407 are obtained from CaT index values using an empirical conversion. The measured CaT/metallicity distributions show unexpected features, the most remarkable being that the brightest red and blue GCs have similar CaT values despite their large difference in mean color. Suggested explanations for this behavior in the NGC 1407 GC system are (1) the CaT may be affected by a population of hot blue stars, (2) the CaT may saturate earlier than predicted by the models, and/or (3) color may not trace metallicity linearly. Until these possibilities are understood, the use of the CaT as a metallicity indicator for the integrated spectra of extragalactic GCs will remain problematic. C1 [Foster, Caroline; Forbes, Duncan A.; Proctor, Robert N.; Spitler, Lee R.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Proctor, Robert N.] Univ Sao Paulo, IAG, BR-05508900 Sao Paulo, Brazil. [Strader, Jay] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brodie, Jean P.] Univ Calif Santa Cruz, Lick Observ, UCO, Santa Cruz, CA 95064 USA. RP Foster, C (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. EM cfoster@astro.swin.edu.au RI Spitler, Lee/A-9867-2013; OI Spitler, Lee/0000-0001-5185-9876; Foster, Caroline/0000-0003-0247-1204 NR 75 TC 26 Z9 26 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD APR PY 2010 VL 139 IS 4 BP 1566 EP 1578 DI 10.1088/0004-6256/139/4/1566 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 568BO UT WOS:000275496900025 ER PT J AU Pribulla, T Rucinski, SM Latham, DW Quinn, SN Siwak, M Matthews, JM Kuschnig, R Rowe, JF Guenther, DB Moffat, AFJ Sasselov, D Walker, GAH Weiss, WW AF Pribulla, T. Rucinski, S. M. Latham, D. W. Quinn, S. N. Siwak, M. Matthews, J. M. Kuschnig, R. Rowe, J. F. Guenther, D. B. Moffat, A. F. J. Sasselov, D. Walker, G. A. H. Weiss, W. W. TI Eclipsing binaries in the MOST satellite fields SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE binaries close; binaries eclipsing; binaries: spectroscopic ID RADIAL-VELOCITY; EE AQUARII; UBV PHOTOMETRY; NGC 2244; STARS; CLUSTERS; ALGORITHM; EVOLUTION; CONTACT; SYSTEMS AB Sixteen new eclipsing binaries have been discovered by the MOST satellite among guide stars used to point its telescope in various fields Several previously known eclipsing binaries were also observed by MOST with unprecedented quality. Among the objects we discuss in more detail are short-period eclipsing binaries with eccentric orbits in young open clusters V578 Mon in NGC 2244 and HD 47934 in NGC 2264 Long nearly-continuous photometric runs made it possible to discover three long-period eclipsing binaries with orbits seen almost edge-on HD 45972 with P = 28 1 clays and two systems (GSC 154 1247 and GSC 2141 526) with P > 25 days. The high precision of the satellite data led to discoveries of binaries with very shallow eclipses (e.g, HD 46180 with A = 0 016 mag, and HD 47934 with A = 0 025 mag). Ground-based spectroscopy to support the space-based photometry was used to refine the models of several of the systems (C) 2010 WILEY-VCH Verlag GmbH & Co KGaA, Weinheim C1 [Pribulla, T.] Astrophys Inst, D-07740 Jena, Germany. [Pribulla, T.] Univ Sternwarte, D-07740 Jena, Germany. [Pribulla, T.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica 05960, Slovakia. [Rucinski, S. M.; Siwak, M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Latham, D. W.; Quinn, S. N.; Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matthews, J. M.; Rowe, J. F.; Walker, G. A. H.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Kuschnig, R.; Weiss, W. W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Guenther, D. B.] St Marys Univ, Dept Phys & Astron, Inst Computat Astrophys, Halifax, NS B3H 3C3, Canada. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Observ Astron Mt Megant, Montreal, PQ H3C 3J7, Canada. RP Pribulla, T (reprint author), Astrophys Inst, Schillergasschen 2-3, D-07740 Jena, Germany. FU Canadian Space Agency Space Enhancement Program (SSEP); Natural Sciences and Engineering Research Council of Canada (NSERC); Canadian Space Agency; Austrian Space Agency; Austrian Science Fund [P17580]; EU; [MTKD-CT-2006-042514] FX The authors are grateful to an anonymous referee for the comments which improved the manuscript This study has been funded by a grant to SMR within the Canadian Space Agency Space Enhancement Program (SSEP) while TP held a Post-Doctoral Fellowship position at the University of Toronto The Natural Sciences and Engineering Research Council of Canada (NSERC) supports the research of DBG, JMM, AFJM, and SMR Additional support for AFJM comes from FQRNT (Quebec) RK is supported by the Canadian Space Agency and WWW is supported by the Austrian Space Agency and the Austrian Science Fund (P17580). TP acknowledges support from the EU in the FP6 MC ToK project MTKD-CT-2006-042514. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France and NASA's Astrophysics Data System Bibliographic Services NR 47 TC 11 Z9 11 U1 0 U2 1 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 0004-6337 J9 ASTRON NACHR JI Astro. Nachr. PD APR PY 2010 VL 331 IS 4 BP 397 EP 411 DI 10.1002/asna.201011351 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 599ME UT WOS:000277916200006 ER PT J AU Huang, RHH Becker, W Edmonds, PD Elsner, RF Heinke, CO Hsieh, BC AF Huang, R. H. H. Becker, W. Edmonds, P. D. Elsner, R. F. Heinke, C. O. Hsieh, B. C. TI Study of Hubble Space Telescope counterparts to Chandra X-ray sources in the globular cluster M71 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE globular clusters: individual: M71 globular clusters: individual: NGC 6838 ID CATACLYSMIC VARIABLES; MILLISECOND PULSAR; GLOBULAR-CLUSTER-47 TUCANAE; OBSERVATORY OBSERVATIONS; PHOTOMETRIC PERFORMANCE; EXTENSIVE CENSUS; CATALOG; ROSAT; CALIBRATION; BINARIES AB Aims. We report on archival Hubble Space Telescope (HST) observations of the globular cluster M71 (NGC 6838). Methods. These observations, covering the core of the globular cluster, were performed by the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2). Inside the half-mass radius (r(h) = 1.'65) of M71, we find 33 candidate optical counterparts to 25 out of 29 Chandra X-ray sources, while 6 possible optical counterparts to 4 X-ray sources are found outside the half-mass radius. Results. Based on the X-ray and optical properties of the identifications, we find 1 certain and 7 candidate cataclysmic variables (CVs). We also classify 2 X-ray sources as certain and 12 as potential chromospherically active binaries (ABs), respectively. The only star in the error circle of the known millisecond pulsar (MSP) is inconsistent with being the optical counterpart. Conclusions. The number of X-ray faint sources with L-X > 4 x 10(30) erg s(-1) (0.5-6.0 keV) found in M71 is higher than extrapolations from other clusters on the basis of either collision frequency or mass. Since the core density of M71 is relatively low, we suggest that those CVs and ABs are primordial in origin. C1 [Huang, R. H. H.; Becker, W.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Edmonds, P. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Elsner, R. F.] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Heinke, C. O.] Univ Alberta, Dept Phys, Edmonton, AB, Canada. [Hsieh, B. C.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. RP Huang, RHH (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM rhuang@mpe.mpg.de OI Heinke, Craig/0000-0003-3944-6109 FU Max-Planck Society; NASA; NSERC; University of Alberta FX This work made use of the Chandra and HST data archives. We acknowledge that Stairs et al. kindly provided the information of M71A in advance of publication. We also thank Anderson et al. for the photometry. The first author thanks Albert K.H. Kong for some helpful suggestions and acknowledges the receipt of funding provided by the Max-Planck Society in the frame of the International Max-Planck Research School (IMPRS). COH acknowledges support from NASA Chandra grants, and funding from NSERC and the University of Alberta. NR 54 TC 11 Z9 11 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD APR PY 2010 VL 513 AR A16 DI 10.1051/0004-6361/200811245 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 584TX UT WOS:000276777200021 ER PT J AU Hudson, DS Mittal, R Reiprich, TH Nulsen, PEJ Andernach, H Sarazin, CL AF Hudson, D. S. Mittal, R. Reiprich, T. H. Nulsen, P. E. J. Andernach, H. Sarazin, C. L. TI What is a cool-core cluster? a detailed analysis of the cores of the X-ray flux-limited HIFLUGCS cluster sample SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE intergalactic medium; galaxies: clusters: general ID XMM-NEWTON OBSERVATIONS; VLA SKY SURVEY; GALAXY CLUSTERS; RADIO HALO; CHANDRA OBSERVATIONS; TEMPERATURE PROFILES; INTRACLUSTER MEDIUM; NEARBY CLUSTERS; EMITTING GAS; CENTAURUS CLUSTER AB We use the largest complete sample of 64 galaxy clusters (HIghest X-ray FLUx Galaxy Cluster Sample) with available high-quality X-ray data from Chandra, and apply 16 cool-core diagnostics to them, some of them new. In order to identify the best parameter for characterizing cool-core clusters and quantify its relation to other parameters, we mainly use very high spatial resolution profiles of central gas density and temperature, and quantities derived from them. We also correlate optical properties of brightest cluster galaxies (BCGs) with X-ray properties. To segregate cool core and non-cool-core clusters, we find that central cooling time, t(cool), is the best parameter for low redshift clusters with high quality data, and that cuspiness is the best parameter for high redshift clusters. 72% of clusters in our sample have a cool core (t(cool) < 7.7 h(71)(-1/2) Gyr) and 44% have strong cool cores (t(cool) < 1.0 h(71)(-1/2) Gyr). We find strong cool-core clusters are characterized as having low central entropy and a systematic central temperature drop. Weak cool-core clusters have enhanced central entropies and temperature profiles that are flat or decrease slightly towards the center. Non-cool-core clusters have high central entropies. For the first time we show quantitatively that the discrepancy in classical and spectroscopic mass deposition rates can not be explained with a recent formation of the cool cores, demonstrating the need for a heating mechanism to explain the cooling flow problem. We find that strong cool-core clusters have a distribution of central temperature drops, centered on 0.4T(vir). However, the radius at which the temperature begins to drop varies. This lack of a universal inner temperature profile probably reflects the complex physics in cluster cores not directly related to the cluster as a whole. Our results suggest that the central temperature does not correlate with the mass of the BCGs and weakly correlates with the expected radiative cooling only for strong cool-core clusters. Since 88% of the clusters in our sample have a BCG within a projected distance of 50 h(71)(-1) kpc from the X-ray peak, we argue that it is easier to heat the gas (e. g. with mergers or non-gravitational processes) than to separate the dense core from the brightest cluster galaxy. Diffuse, Mpc-scale radio emission, believed to be associated with major mergers, has not been unambiguously detected in any of the strong cool-core clusters in our sample. Of the weak cool-core clusters and non-cool-core clusters, most of the clusters (seven out of eight) that have diffuse, Mpc-scale radio emission have a large (> 50 h(71)(-1) kpc) projected separation between their BCG and X-ray peak. In contrast, only two of the 56 clusters with a small separation between the BCG and X-ray peak (<50 h(71)(-1) kpc) show large-scale radio emission. Based on this result, we argue that a large projected separation between the BCG and the X-ray peak is a good indicator of a major merger. The properties of weak cool-core clusters as an intermediate class of objects are discussed. Finally we describe individual properties of all 64 clusters in the sample. C1 [Hudson, D. S.; Mittal, R.; Reiprich, T. H.; Andernach, H.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Mittal, R.] Rochester Inst Technol, Rochester, NY 14623 USA. [Nulsen, P. E. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. RP Hudson, DS (reprint author), Univ Bonn, Argelander Inst Astron, Hugel 71, D-53121 Bonn, Germany. EM rmittal@astro.rit.edu OI Nulsen, Paul/0000-0003-0297-4493 FU Deutsche Forschungsgemeinschaft [RE 1462/2, RE 1462/4]; CONACyT [50921-F, 81356]; Transregional Collaborative Research Center [TRR33]; NASA [NAS8-03060, GO7-8129X, AR7-8012X, NNX06AE76G] FX The authors wish to thank D. A. Buote, T. E. Clarke, M. Markevitch and A. Vikhlinin for providing proprietary data before it was publicly available. We would like to thank E. Murphy for providing pointed radio measurements of NH for several clusters. We thank E. Blanton, H. Bohringer, Y. Ikebe, E. Pierpaoli, S. Randall, P. Schuecker, and G. Sivakoff for help in the early stages of this work. We would like to thank R. Smith for providing the data for the APEC model. We thank the referee for a beneficial feedback and James Wicker for useful correspondence. T. H. R. and D. S. H. acknowledge support from the Deutsche Forschungsgemeinschaft through Emmy Noether research grant RE 1462/2. R. M. acknowledges support from the Deutsche Forschungsgemeinschaft through the Schwerpunkt Program 1177 (RE 1462/4). H. A. acknowledges financial support from CONACyT under grants 50921-F and 81356, and partial support from the Transregional Collaborative Research Center TRR33 "The Dark Universe". P. E. J. N. acknowledges support from NASA grant NAS8-03060. C. L. S. was supported in part by NASA Chandra grants GO7-8129X and AR7-8012X and NASA XMM-Newton grant NNX06AE76G. 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. We acknowledge the usage of the HyperLeda database (http://leda.univ-lyonl.fr). NR 143 TC 130 Z9 131 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 APR PY 2010 VL 513 AR A37 DI 10.1051/0004-6361/200912377 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 698GH UT WOS:000285581500014 ER PT J AU Tian, WW Li, Z Leahy, DA Yang, J Yang, XJ Yamazaki, R Lu, D AF Tian, W. W. Li, Z. Leahy, D. A. Yang, J. Yang, X. J. Yamazaki, R. Lu, D. TI X-RAY EMISSION FROM HESS J1731-347/SNR G353.6-0.7 AND CENTRAL COMPACT SOURCE XMMS J173203-344518 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: molecules; ISM: supernova remnants; pulsars: general; radio lines: stars; X-rays: stars ID OLD SUPERNOVA-REMNANTS; WIND NEBULAE; GAMMA-RAYS; ACCELERATION; DISCOVERY; PULSAR; TELESCOPE; CHANDRA; SHOCK AB We present new results of the HESS J1731-347/SNR G353.6-0.7 system from XMM-Newton and Suzaku X-ray observations and Delinha CO observations. We discover extended hard X-rays coincident with the bright, extended TeV source HESS J1731-347 and the shell of the radio supernova remnant (SNR). We find that spatially resolved X-ray spectra can generally be characterized by an absorbed power-law model, with a photon index of similar to 2, typical of non-thermal emission. A bright X-ray compact source, XMMS J173203-344518, is also detected near the center of the SNR. We find no evidence of a radio counterpart or an extended X-ray morphology for this source, making it unlikely to be a pulsar wind nebular (PWN). The spectrum of the source can be well fitted by an absorbed blackbody with a temperature of similar to 0.5 keV plus a power-law tail with a photon index of similar to 5, reminiscent of the X-ray emission of a magnetar. CO observations toward the inner part of the High Energy Stereoscopic System (HESS) source reveal a bright cloud component at -20 +/- 4 km s(-1), which is likely located at the same distance of similar to 3.2 kpc as the SNR. Based on the probable association between the X-ray and gamma-ray emissions and likely association between the CO cloud and the SNR, we argue that the extended TeV emission originates from the interaction between the SNR shock and the adjacent CO clouds rather than from a PWN. C1 [Tian, W. W.] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Tian, W. W.; Leahy, D. A.] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N 1N4, Canada. [Li, Z.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Yang, J.; Lu, D.] Chinese Acad Sci, Purple Mt Observ, Nanjing 210008, Peoples R China. [Yang, X. J.] Xiangtan Univ, Dept Phys, Xiangtan, Hunan, Peoples R China. [Yamazaki, R.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima 7398526, Japan. RP Tian, WW (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM tww@bao.ac.cn; zyli@head.cfa.harvard.edu RI XRAY, SUZAKU/A-1808-2009 FU Natural Science Foundation of China; Natural Sciences and Engineering Research Council of Canada; Ministry of Education, Culture, Sports, Science, and Technology of Japan [21740184] FX W.W.T. acknowledges support from the Natural Science Foundation of China and Bairen Program of the CAS. D. A. L. thanks the Natural Sciences and Engineering Research Council of Canada for support. We thank Drs. A. Bamba, C. Heinke, and S. Zhang for their help on analyzing Suzaku and INTEGRAL data. R.Y. was supported in part by a Grant-in-aid from the Ministry of Education, Culture, Sports, Science, and Technology of Japan (No. 21740184). NR 34 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 790 EP 796 DI 10.1088/0004-637X/712/2/790 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600003 ER PT J AU Gogarten, SM Dalcanton, JJ Williams, BF Roskar, R Holtzman, J Seth, AC Dolphin, A Weisz, D Cole, A Debattista, VP Gilbert, KM Olsen, K Skillman, E de Jong, RS Karachentsev, ID Quinn, TR AF Gogarten, Stephanie M. Dalcanton, Julianne J. Williams, Benjamin F. Roskar, Rok Holtzman, Jon Seth, Anil C. Dolphin, Andrew Weisz, Daniel Cole, Andrew Debattista, Victor P. Gilbert, Karoline M. Olsen, Knut Skillman, Evan de Jong, Roelof S. Karachentsev, Igor D. Quinn, Thomas R. TI THE ADVANCED CAMERA FOR SURVEYS NEARBY GALAXY SURVEY TREASURY. V. RADIAL STAR FORMATION HISTORY OF NGC 300 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: evolution; galaxies: individual (NGC 300); galaxies: spiral; galaxies: stellar content ID HUBBLE-SPACE-TELESCOPE; H-II REGIONS; SCULPTOR GROUP GALAXIES; SMALL-MAGELLANIC-CLOUD; SPIRAL GALAXIES; ABUNDANCE GRADIENTS; ARAUCARIA-PROJECT; DISK GALAXIES; OUTER DISK; MILKY-WAY AB We present new Hubble Space Telescope (HST) observations of NGC 300 taken as part of the Advanced Camera for Surveys Nearby Galaxy Survey Treasury (ANGST). Individual stars are resolved in these images down to an absolute magnitude of M(F814W) = 1.0 (below the red clump). We determine the star formation history of the galaxy in six radial bins by comparing our observed color-magnitude diagrams (CMDs) with synthetic CMDs based on theoretical isochrones. We find that the stellar disk out to 5.4 kpc is primarily old, in contrast with the outwardly similar galaxy M33. We determine the scale length as a function of age and find evidence for inside-out growth of the stellar disk: the scale length has increased from 1.1 +/- 0.1 kpc 10 Gyr ago to 1.3 +/- 0.1 kpc at present, indicating a buildup in the fraction of young stars at larger radii. As the scale length of M33 has recently been shown to have increased much more dramatically with time, our results demonstrate that two galaxies with similar sizes and morphologies can have very different histories. With an N-body simulation of a galaxy designed to be similar to NGC 300, we determine that the effects of radial migration should be minimal. We trace the metallicity gradient as a function of time and find a present-day metallicity gradient consistent with that seen in previous studies. Consistent results are obtained from archival images covering the same radial extent but differing in placement and filter combination. C1 [Gogarten, Stephanie M.; Dalcanton, Julianne J.; Williams, Benjamin F.; Roskar, Rok; Gilbert, Karoline M.; Quinn, Thomas R.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Holtzman, Jon] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 USA. [Seth, Anil C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dolphin, Andrew] Raytheon Co, Tucson, AZ 85756 USA. [Weisz, Daniel; Skillman, Evan] Univ Minnesota, Dept Astron, Minneapolis, MN 55455 USA. [Cole, Andrew] Univ Tasmania, Sch Math & Phys, Hobart, Tas, Australia. [Debattista, Victor P.] Univ Cent Lancashire, Jeremiah Horrocks Inst, Preston PR1 2HE, Lancs, England. [Olsen, Knut] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [de Jong, Roelof S.] AIP, D-14482 Potsdam, Germany. [Karachentsev, Igor D.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz, Kchr, Russia. RP Gogarten, SM (reprint author), Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA. EM stephanie@astro.washington.edu OI Cole, Andrew/0000-0003-0303-3855; Gogarten, Stephanie/0000-0002-7231-9745 FU NASA [GO-10915, NAS5-26555]; Space Telescopes Science Institute; Association of Universities for Research in Astronomy, Inc.; U.S. Government [NAG W-2166]; UK Science and Engineering Research Council FX Support for this work was provided by NASA through grant GO-10915 from the Space Telescopes Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. J.J.D. was partially supported as a Wycoff Fellow. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by JPL/Caltech, under contract with NASA. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The UK Schmidt Telescope was operated by the Royal Observatory Edinburgh, with funding from the UK Science and Engineering Research Council (later the UK Particle Physics and Astronomy Research Council), until 1988 June, and thereafter by the Anglo-Australian Observatory. NR 76 TC 54 Z9 54 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 858 EP 874 DI 10.1088/0004-637X/712/2/858 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600008 ER PT J AU Raymond, JC Winkler, PF Blair, WP Lee, JJ Park, S AF Raymond, John C. Winkler, P. Frank Blair, William P. Lee, Jae-Joon Park, Sangwook TI NON-MAXWELLIAN H alpha PROFILES IN TYCHO'S SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: lines and bands; ISM: supernova remnants; line: profiles; shock waves ID BALMER-DOMINATED SHOCKS; MAGNETIC-FIELD; CYGNUS LOOP; NONRADIATIVE SHOCKS; OPTICAL-EMISSION; NOVA; ACCELERATION; WAVE; AMPLIFICATION; PICKUP AB The broad components of the Ha lines in most non-radiative shocks can be fit with single-Gaussian components. We have obtained a high-quality spectrum of a position in Tycho's supernova remnant with the MMT and Blue Channel Spectrograph which shows, for the first time, that a single Gaussian does not provide an acceptable fit. This implies that a single temperature Maxwellian particle velocity distribution cannot produce the emission. Possible alternative explanations are explored, including multiple shocks along the line of sight, a pickup ion contribution, a non-thermal tail (Kappa distribution), emission from a precursor in a cosmic ray modified shock, or turbulence. An Hubble Space Telescope image shows a bright knot that might account for a low temperature contribution, and all the possibilities probably contribute at some level. We discuss the implications of each explanation for the shock parameters and physics of collisionless shocks, but cannot conclusively rule out any of them. C1 [Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Winkler, P. Frank] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Blair, William P.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Lee, Jae-Joon; Park, Sangwook] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. RP Raymond, JC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM jraymond@cfa.harvard.edu; winkler@middlebury.edu; wpb@pha.jhu.edu; lee.j.joon@gmail.com; park@astro.psu.edu FU Smithsonian Astrophysical Observatory from STScI [GO-11184.01-A-R]; National Science Foundation [PHY05-51164, AST-0908566] FX We thank Kevin Heng and Matt van Adelsberg for providing the theoretical line profiles used to assess the importance of the velocity dependence of the charge transfer cross section on the line profiles. This research was supported by grant GO-11184.01-A-R to the Smithsonian Astrophysical Observatory from STScI, and it was supported in part by the National Science Foundation under grant number PHY05-51164. PFW's research is supported by the National Science Foundation under grant number AST-0908566. We further acknowledge stimulating discussions at the KITP meeting in Santa Barbara in 2009. NR 29 TC 15 Z9 15 U1 1 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 901 EP 907 DI 10.1088/0004-637X/712/2/901 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600011 ER PT J AU Shetty, R Collins, DC Kauffmann, J Goodman, AA Rosolowsky, E Norman, ML AF Shetty, Rahul Collins, David C. Kauffmann, Jens Goodman, Alyssa A. Rosolowsky, Erikw. Norman, Michael L. TI THE EFFECT OF PROJECTION ON DERIVED MASS-SIZE AND LINEWIDTH-SIZE RELATIONSHIPS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: structure; methods: analytical; stars: formation ID MOLECULAR CLOUD MODELS; VIRIAL-THEOREM; STAR-FORMATION; VELOCITY; DENSITY; CLUMPS; TURBULENCE; SPECTRUM; WARM AB Power-law mass-size and linewidth-size correlations, two of "Larson's laws," are often studied to assess the dynamical state of clumps within molecular clouds. Using the result of a hydrodynamic simulation of a molecular cloud, we investigate how geometric projection may affect the derived Larson relationships. We find that large-scale structures in the column density map have similar masses and sizes to those in the three-dimensional simulation (position-position-position, PPP). Smaller scale clumps in the column density map are measured to be more massive than the PPP clumps, due to the projection of all emitting gas along lines of sight. Further, due to projection effects, structures in a synthetic spectral observation (position-position-velocity, PPV) may not necessarily correlate with physical structures in the simulation. In considering the turbulent velocities only, the linewidth-size relationship in the PPV cube is appreciably different from that measured from the simulation. Including thermal pressure in the simulated line widths imposes a minimum line width, which results in a better agreement in the slopes of the linewidth-size relationships, though there are still discrepancies in the offsets, as well as considerable scatter. Employing commonly used assumptions in a virial analysis, we find similarities in the computed virial parameters of the structures in the PPV and PPP cubes. However, due to the discrepancies in the linewidth-size and mass-size relationships in the PPP and PPV cubes, we caution that applying a virial analysis to observed clouds may be misleading due to geometric projection effects. We speculate that consideration of physical processes beyond kinetic and gravitational pressure would be required for accurately assessing whether complex clouds, such as those with highly filamentary structure, are bound. C1 [Shetty, Rahul; Kauffmann, Jens; Goodman, Alyssa A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shetty, Rahul; Kauffmann, Jens; Goodman, Alyssa A.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Collins, David C.; Norman, Michael L.] Univ Calif San Diego, Ctr Astrophys & Space Sci, Lab Computat Astrophys, La Jolla, CA 92093 USA. [Rosolowsky, Erikw.] Univ British Columbia Okanagan, Kelowna, BC V1V 1V7, Canada. RP Shetty, R (reprint author), Univ Heidelberg, Inst Theoret Astrophys, Zentrum Astron, Albert Ueberle Str 2, D-69120 Heidelberg, Germany. EM rshetty@ita.uni-heidelberg.de RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU NSF [AST0808184, AST0908740]; National Institute for Computational Sciences [MCA98N020]; National Science Foundation [AST-0908159]; Harvard Initiative in Innovative Computing FX We are grateful to F. Shu for suggesting, after A.G.'s 2008 Tucson "Stromfest" talk on the "self-gravity" results now found in Goodman et al. (2009), that we carry out "tests of the test," or, in other words for suggesting that we investigate the translation and meaning of the a virial parameter between PPP and PPV space. We also thank E. Ostriker, P. Myers, and S. Offner for very useful comments that improved this work. This presentation benefitted from many suggestions from an anonymous referee. We acknowledge use of NEMO software (Teuben 1995) to perform our analysis. D. C. acknowledges support from NSF grant AST0808184 and AST0908740, and performed the simulation at the National Institute for Computational Sciences with computing time provided by LRAC allocation MCA98N020. R. S., J.K., and A. G. acknowledge support by the National Science Foundation under grant No. AST-0908159, and from the Harvard Initiative in Innovative Computing, which hosts the Star-Formation Taste Tests Community at which further details on these results can be found and discussed (see http://www.cfa.harvard.edu/similar to agoodman/tastetests). NR 30 TC 40 Z9 40 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 1049 EP 1056 DI 10.1088/0004-637X/712/2/1049 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600023 ER PT J AU Sankrit, R Williams, BJ Borkowski, KJ Gaetz, TJ Raymond, JC Blair, WP Ghavamian, P Long, KS Reynolds, SP AF Sankrit, Ravi Williams, Brian J. Borkowski, Kazimierz J. Gaetz, Terrance J. Raymond, John C. Blair, William P. Ghavamian, Parviz Long, Knox S. Reynolds, Stephen P. TI DUST DESTRUCTION IN A NON-RADIATIVE SHOCK IN THE CYGNUS LOOP SUPERNOVA REMNANT SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; ISM: individual objects (Cygnus Loop); ISM: supernova remnants; shock waves ID LARGE-MAGELLANIC-CLOUD; INFRARED-EMISSION; NORTHEASTERN RIM; X-RAY; TELESCOPE; GRAINS; GAS; SPECTROSCOPY; SPECTRA AB We present 24 mu m and 70 mu m images of a non-radiative shock in the Cygnus Loop supernova remnant, obtained with the Multiband Imaging Photometer for Spitzer on board the Spitzer Space Telescope. The post-shock region is resolved in these images. The ratio of the 70 mu m to the 24 mu m flux rises from about 14 at a distance 0.'1 behind the shock front to about 22 in a zone 0.'75 further downstream, as grains are destroyed in the hot plasma. Models of dust emission and destruction using post-shock electron temperatures between 0.15 keV and 0.30 keV and post-shock densities, n(H) similar to 2.0 cm(-3), predict flux ratios that match the observations. Non-thermal sputtering (i.e., sputtering due to bulk motion of the grains relative to the gas) contributes significantly to the dust destruction under these shock conditions. From the model calculations, we infer that about 35% by mass of the grains are destroyed over a 0.14 pc region behind the shock front. C1 [Sankrit, Ravi] NASA, Ames Res Ctr, SOFIA USRA, Moffett Field, CA 94035 USA. [Williams, Brian J.; Borkowski, Kazimierz J.; Reynolds, Stephen P.] N Carolina State Univ, Raleigh, NC 27695 USA. [Gaetz, Terrance J.; Raymond, John C.] Smithsonian Astrophys Observ, Tucson, AZ USA. [Blair, William P.] Johns Hopkins Univ, Baltimore, MD USA. [Ghavamian, Parviz; Long, Knox S.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Sankrit, R (reprint author), NASA, Ames Res Ctr, SOFIA USRA, M-S N211-3, Moffett Field, CA 94035 USA. FU JPL [1278412]; USRA at the SOFIA Science Center; NASA [NAS8-03060] FX We thank the referee for a careful reading of the paper and useful comments. This work was supported in part by JPL Award 1278412 to the University of California, Berkeley and North Carolina State University, Raleigh. R. S. acknowledges support from USRA at the SOFIA Science Center. T.J.G. acknowledges support under NASA contract NAS8-03060 with the Chandra X-ray Center. NR 28 TC 21 Z9 21 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 1092 EP 1099 DI 10.1088/0004-637X/712/2/1092 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600026 ER PT J AU Morgan, CW Kochanek, CS Morgan, ND Falco, EE AF Morgan, Christopher W. Kochanek, C. S. Morgan, Nicholas D. Falco, Emilio E. TI THE QUASAR ACCRETION DISK SIZE-BLACK HOLE MASS RELATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; dark matter; gravitational lensing: micro; gravitational lensing: strong; quasars: general ID ACTIVE GALACTIC NUCLEI; GRAVITATIONALLY LENSED QUASAR; NON-LTE MODELS; TIME-DELAY; PG 1115+080; X-RAY; FE-II; MICROLENSING VARIABILITY; THEORETICAL SPECTRA; CONTINUUM EMISSION AB We use the microlensing variability observed for 11 gravitationally lensed quasars to show that the accretion disk size at a rest-frame wavelength of 2500 angstrom is related to the black hole mass by log(R-2500/cm) = (15.78 +/- 0.12) + (0.80 +/- 0.17) log(M-BH/10(9) M-circle dot). This scaling is consistent with the expectation from thin-disk theory (R proportional to M-BH(2/3) ), but when interpreted in terms of the standard thin-disk model (T proportional to R-3/4), it implies that black holes radiate with very low efficiency, log(eta) = -1.77 +/- 0.29 + log(L/L-E), where eta = L/((M) over dotc(2)). Only by making the maximum reasonable shifts in the average inclination, Eddington factors, and black hole masses can we raise the efficiency estimate to be marginally consistent with typical efficiency estimates (eta approximate to 10%). With one exception, these sizes are larger by a factor of similar to 4 than the size needed to produce the observed 0.8 mu m quasar flux by thermal radiation from a thin disk with the same T proportional to R-3/4 temperature profile. While scattering a significant fraction of the disk emission on large scales or including a large fraction of contaminating line emission can reduce the size discrepancy, resolving it also appears to require that accretion disks have flatter temperature/surface brightness profiles. C1 [Morgan, Christopher W.] USN Acad, Dept Phys, Annapolis, MD 21402 USA. [Kochanek, C. S.; Morgan, Nicholas D.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Morgan, CW (reprint author), USN Acad, Dept Phys, 572C Holloway Rd, Annapolis, MD 21402 USA. EM cmorgan@usna.edu; ckochanek@astronomy.ohio-state.edu; nmorgan@astronomy.ohio-state.edu; efalco@cfa.harvard.edu FU NASA [HST-GO-9744, NAS-5-26666]; National Science Foundation [AST 0907848]; Research Corporation for Science Advancement FX We thank O. Blaes, E. Agol, M. Dietrich, C. Onken, B. Peterson, M. Pinsonneault, R. Pogge, and P. Osmer for discussions on quasar structure and M. Mortonson, S. Poindexter, S. Rappaport, and P. Schechter for discussions on microlensing. We also thank the anonymous referee for valuable suggestions, particularly in the expansion of our discussion of radiative efficiencies. This research made extensive use of a Beowulf computer cluster obtained through the Cluster Ohio program of the Ohio Supercomputer Center. Support for program HST-GO-9744 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-5-26666. This material is based upon work supported by the National Science Foundation under grant No. AST 0907848. This research was also supported by an award from the Research Corporation for Science Advancement. NR 82 TC 116 Z9 116 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 1129 EP 1136 DI 10.1088/0004-637X/712/2/1129 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600030 ER PT J AU Kauffmann, J Pillai, T Shetty, R Myers, PC Goodman, AA AF Kauffmann, J. Pillai, T. Shetty, R. Myers, P. C. Goodman, A. A. TI THE MASS-SIZE RELATION FROM CLOUDS TO CORES. I. A NEW PROBE OF STRUCTURE IN MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; methods: data analysis; stars: formation ID C2D LEGACY CLOUDS; STAR-FORMATION; INITIAL CONDITIONS; PERSEUS; DUST; SCALES AB We use a new contour-based map analysis technique to measure the mass and size of molecular cloud fragments continuously over a wide range of spatial scales (0.05 <= r/pc <= 10), i.e., from the scale of dense cores to those of entire clouds. The present paper presents the method via a detailed exploration of the Perseus molecular cloud. Dust extinction and emission data are combined to yield reliable scale-dependent measurements of mass. This scale-independent analysis approach is useful for several reasons. First, it provides a more comprehensive characterization of a map (i.e., not biased toward a particular spatial scale). Such a lack of bias is extremely useful for the joint analysis of many data sets taken with different spatial resolution. This includes comparisons between different cloud complexes. Second, the multi-scale mass-size data constitute a unique resource to derive slopes of mass-size laws (via power-law fits). Such slopes provide singular constraints on large-scale density gradients in clouds. C1 [Kauffmann, J.; Shetty, R.; Goodman, A. A.] IIC, Cambridge, MA 02138 USA. [Kauffmann, J.; Pillai, T.; Shetty, R.; Myers, P. C.; Goodman, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kauffmann, J (reprint author), IIC, 60 Oxford St, Cambridge, MA 02138 USA. EM jens.kauffmann@jpl.nasa.gov RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU Harvard Interfaculty Initiative; National Science Foundation [AST-0908159] FX We are grateful to a considerate and knowledgeable referee, Nicolas Peretto, who helped to significantly improve the quality of the paper. This project would not have been possible without help from Erik Rosolowsky. His dendrogram analysis code (Rosolowsky et al. 2008b) was instrumental for our analysis. We thank Jaime Pineda for his help with the CLUMPFIND experiments presented in Figure 4. Enoch et al. (2006) contributed maps to the present study. We are grateful for their help. This work was in part made possible through Harvard Interfaculty Initiative funding to the Harvard Initiative in Innovative Computing (IIC). It is based upon work supported by the National Science Foundation under grant No. AST-0908159. NR 29 TC 34 Z9 34 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 1137 EP 1146 DI 10.1088/0004-637X/712/2/1137 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600031 ER PT J AU Pech, G Loinard, L Chandler, CJ Rodriguez, LF D'Alessio, P Brogan, CL Wilner, DJ Ho, PTP AF Pech, Gerardo Loinard, Laurent Chandler, Claire J. Rodriguez, Luis F. D'Alessio, Paola Brogan, Crystal L. Wilner, David J. Ho, Paul T. P. TI CONFIRMATION OF A RECENT BIPOLAR EJECTION IN THE VERY YOUNG HIERARCHICAL MULTIPLE SYSTEM IRAS 16293-2422 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; binaries: general; radio continuum: stars; stars: formation; stars: individual (IRAS 16293-2422) ID LARGE PROPER MOTIONS; IRAS-16293-2422; OUTFLOW; EMISSION; SUBMILLIMETER; OPHIUCHUS; ENVELOPE; COMPACT; OBJECTS; CORE AB We present and analyze two new high-resolution (similar to 0 ''.3), high-sensitivity (similar to 50 mu Jy beam(-1)) Very Large Array 3.6 cm observations of IRAS 16293-2422 obtained in 2007 August and 2008 December. The components A2 alpha and A2 beta recently detected in this system are still present, and have moved roughly symmetrically away from source A2 at a projected velocity of 30-80 km s(-1). This confirms that A2 alpha and A2 beta were formed as a consequence of a very recent bipolar ejection from A2. Powerful bipolar ejections have long been known to occur in low-mass young stars, but this is-to our knowledge-the first time that such a dramatic one is observed from its very beginning. Under the reasonable assumption that the flux detected at radio wavelengths is optically thin free-free emission, one can estimate the mass of each ejecta to be of the order of 10(-8) M(circle dot). If the ejecta were created as a consequence of an episode of enhanced mass loss accompanied by an increase in accretion onto the protostar, then the total luminosity of IRAS 16293-2422 ought to have increased by 10%-60% over the course of at least several months. Between A2 alpha and A2 beta, component A2 has reappeared, and the relative position angle between A2 and A1 is found to have increased significantly since 2003-2005. This strongly suggests that A1 is a protostar rather than a shock feature, and that the A1/A2 pair is a tight binary system. Including component B, IRAS 16293-2422 therefore appears to be a very young hierarchical multiple system. C1 [Pech, Gerardo; Loinard, Laurent; Rodriguez, Luis F.; D'Alessio, Paola] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Chandler, Claire J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Brogan, Crystal L.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Wilner, David J.; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pech, Gerardo] Univ Autonoma Yucatan, Fac Ingn, Merida, Yucatan, Mexico. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. RP Pech, G (reprint author), Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Apartado Postal 72-3 Xangari, Morelia 58089, Michoacan, Mexico. EM g.pech@crya.unam.mx; l.loinard@crya.unam.mx; cchandle@nrao.edu; l.rodriguez@crya.unam.mx; p.dalessio@crya.unam.mx; cbrogan@nrao.edu; dwilner@cfa.harvard.edu; pho@cfa.harvard.edu FU DGAPA, Mexico; UNAM, Mexico; CONACyT, Mexico; NASA [NAG5-11777] FX L. L., L. F. R., and P. A. acknowledge the financial support of DGAPA, UNAM and CONACyT, Mexico. D.J.W. acknowledges partial support from NASA Origins of Solar Systems Program Grant NAG5-11777. NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 26 TC 23 Z9 24 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD APR 1 PY 2010 VL 712 IS 2 BP 1403 EP 1409 DI 10.1088/0004-637X/712/2/1403 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 569KF UT WOS:000275594600053 ER PT J AU Tinetti, G Deroo, P Swain, MR Griffith, CA Vasisht, G Brown, LR Burke, C McCullough, P AF Tinetti, G. Deroo, P. Swain, M. R. Griffith, C. A. Vasisht, G. Brown, L. R. Burke, C. McCullough, P. TI PROBING THE TERMINATOR REGION ATMOSPHERE OF THE HOT-JUPITER XO-1b WITH TRANSMISSION SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planetary systems; techniques: spectroscopic ID EXTRASOLAR GIANT PLANETS; SUN-LIKE STAR; EXOPLANET XO-1B; HD 209458B; METHANE; WATER; TRANSITS; SPECTRA AB We report here the first infrared spectrum of the hot-Jupiter XO-1b. The observations were obtained with the NICMOS instrument on board the Hubble Space Telescope during a primary eclipse of the XO-1 system. Near photon-noise-limited spectroscopy between 1.2 and 1.8 mu m allows us to determine the main composition of this hot-Jupiter's planetary atmosphere with good precision. This is the third hot-Jupiter's atmosphere for which spectroscopic data are available in the near-IR. The spectrum shows the presence of water vapor (H(2)O), methane (CH(4)), and carbon dioxide (CO(2)), and suggests the possible presence of carbon monoxide (CO). We show that the published IRAC secondary transit emission photometric data are compatible with the atmospheric composition at the terminator determined from the NICMOS spectrum, with a range of possible mixing ratios and thermal profiles; additional emission spectroscopy data are needed to reduce the degeneracy of the possible solutions. Finally, we note the similarity between the 1.2-1.8 mu m transmission spectra of XO-1b and HD 209458b, suggesting that in addition to having similar stellar/orbital and planetary parameters the two systems may also have a similar exoplanetary atmospheric composition. C1 [Tinetti, G.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Deroo, P.; Swain, M. R.; Vasisht, G.; Brown, L. R.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Griffith, C. A.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. [Burke, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McCullough, P.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. RP Tinetti, G (reprint author), UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England. EM g.tinetti@ucl.ac.uk OI Tinetti, Giovanna/0000-0001-6058-6654 FU Royal Society University Research Fellowship. FX G. T. is supported by a Royal Society University Research Fellowship. NR 26 TC 63 Z9 64 U1 1 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 APR 1 PY 2010 VL 712 IS 2 BP L139 EP L142 DI 10.1088/2041-8205/712/2/L139 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 581WP UT WOS:000276556500004 ER PT J AU Christian, DJ Bodewits, D Lisse, CM Dennerl, K Wolk, SJ Hsieh, H Zurbuchen, TH Zhao, L AF Christian, D. J. Bodewits, D. Lisse, C. M. Dennerl, K. Wolk, S. J. Hsieh, H. Zurbuchen, T. H. Zhao, L. TI CHANDRA OBSERVATIONS OF COMETS 8P/TUTTLE AND 17P/HOLMES DURING SOLAR MINIMUM SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE comets: individual (Comet 8P/Tuttle, Comet 17P/Holmes); solar wind; techniques: spectroscopic; X-rays: general ID X-RAY-EMISSION; ALL-SKY SURVEY; WIND IONS; ULTRAVIOLET EMISSION; HYAKUTAKE; SPECTRA AB We present results for Chandra X-ray Observatory observations of two comets made during the minimum of solar cycle 24. The two comets, 17P/Holmes (17P) and 8P/Tuttle (8P), were very different in their activity and geometry. 17P was observed, for 30 ks right after its major outburst, on 2007 October 31 (10:07 UT), and comet 8P/Tuttle was observed in 2008 January for 47 ks. During the two Chandra observations, 17P was producing at least 100 times more water than 8P but was 2.2 times further away from the Sun. Also, 17P was at a relatively high solar latitude (+19 degrees.1) while 8P was observed at a lower solar latitude (3 degrees.4). The X-ray spectrum of 17P is unusually soft with little significant emission at energies above 500 eV. Depending on our choice of background, we derive a 300-1000 eV flux of 0.5-4.5 x 10(-13) erg cm(-2) s(-1), with over 90% of the emission in the 300-400 eV range. This corresponds to an X-ray luminosity between 0.4 and 3.3 x 10(15) erg s(-1). However, we cannot distinguish between this significant excess emission and possible instrumental effects, such as incomplete charge transfer across the CCD. 17P is the first comet observed at high latitude during solar minimum. Its lack of X-rays in the 400-1000 eV range, in a simple picture, may be attributed to the polar solar wind, which is depleted in highly charged ions. 8P/Tuttle was much brighter, with an average count rate of 0.20 counts s(-1) in the 300-1000 eV range. We derive an average X-ray flux in this range of 9.4 x 10(-13) erg cm(-2) s(-1) and an X-ray luminosity for the comet of 1.7 x 10(14) erg s(-1). The light curve showed a dramatic decrease in flux of over 60% between observations on January 1 and 4. When comparing outer regions of the coma to inner regions, its spectra showed a decrease in ratios of C VI/C V, O VIII/O VII, as predicted by recent solar wind charge exchange (SWCX) emission models. There are remarkable differences between the X-ray emission from these two comets, further demonstrating the qualities of cometary X-ray observations, and SWCX emission in general as a means of remote diagnostics of the interaction of astrophysical plasmas. C1 [Christian, D. J.] Eureka Sci, Oakland, CA 94602 USA. [Christian, D. J.] Calif State Univ Northridge, Dept Phys & Astron, Northridge, CA 91330 USA. [Bodewits, D.] NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. [Lisse, C. M.] Johns Hopkins Univ, Appl Phys Lab, Dept Space, Planetary Explorat Grp, Laurel, MD 20723 USA. [Dennerl, K.] Max Planck Inst Extraterr Phys, D-85740 Garching, Germany. [Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Chandra Xray Ctr, Cambridge, MA 02138 USA. [Hsieh, H.] Queens Univ Belfast, Dept Phys & Astron, Astron Res Ctr, Belfast, Antrim, North Ireland. [Zurbuchen, T. H.] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. RP Christian, DJ (reprint author), Eureka Sci, 2420 Delmer Ave,Suite 100, Oakland, CA 94602 USA. EM damian.christ@gmail.com; Dennis.Bodewits@nasa.gov; carey.lisse@jhuapl.edu; kod@mpe.mpg.de; swolk@cfa.harvard.edu; h.hseih@qub.c.uk; thomasz@umich.edu; lzh@umich.edu RI Zhao, Liang/B-8215-2012; Lisse, Carey/B-7772-2016; OI Lisse, Carey/0000-0002-9548-1526; Wolk, Scott/0000-0002-0826-9261; Bodewits, Dennis/0000-0002-2668-7248; Christian, Damian/0000-0003-1746-3020; Zhao, Liang/0000-0002-5975-7476 FU Chandra X-ray Observatory [CXO-09100452, CXO-9100455, CXO-07108248]; NASA [NAS8-03060]; California State University Northridge FX This work was supported by the Chandra X-ray Observatory's cycle 9 GO program, CXO-09100452, and archival program CXO-9100455. We thank Harvey Tannenbaum for Director's Discretionary Time to observe Comet 17P/Holmes (CXO-08108279), and we thank the Chandra X-ray Observatory's Scheduling and Mission Operations teams for executing these difficult and time-critical moving target observations. S.J.W. was supported by NASA contract NAS8-03060. D.J.C. thanks the California State University Northridge for support, and C. M. L. gratefully acknowledges support from Chandra GO program CXO-07108248. We also thank A. Fitzsimmons for useful discussions on 17P and Geronimo L. Villanueva for assistance in understanding the comet's orbital geometry. We are grateful for the cometary ephemerides of D.K. Yeomans published at the JPL/Horizons Web site. NR 37 TC 15 Z9 15 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2010 VL 187 IS 2 BP 447 EP 459 DI 10.1088/0067-0049/187/2/447 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 585QJ UT WOS:000276841500006 ER PT J AU Long, KS Blair, WP Winkler, PF Becker, RH Gaetz, TJ Ghavamian, P Helfand, DJ Hughes, JP Kirshner, RP Kuntz, KD McNeil, EK Pannuti, TG Plucinsky, PP Saul, D Tullmann, R Williams, B AF Long, Knox S. Blair, William P. Winkler, P. Frank Becker, Robert H. Gaetz, Terrance J. Ghavamian, Parviz Helfand, David J. Hughes, John P. Kirshner, Robert P. Kuntz, Kip D. McNeil, Emily K. Pannuti, Thomas G. Plucinsky, Paul P. Saul, Destry Tuellmann, Ralph Williams, Benjamin TI THE CHANDRA ACIS SURVEY OF M33: X-RAY, OPTICAL, AND RADIO PROPERTIES OF THE SUPERNOVA REMNANTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: individual (M33); galaxies: ISM; ISM: supernova remnants; radio continuum: galaxies ID LARGE-MAGELLANIC-CLOUD; XMM-NEWTON SURVEY; CURRENTLY FORMING STARS; NEARBY SPIRAL GALAXIES; H-II REGION; NOVA REMNANTS; CASSIOPEIA-A; EMISSION; CHASEM33; SPECTROSCOPY AB M33 contains a large number of emission nebulae identified as supernova remnants (SNRs) based on the high [S II]:H alpha ratios characteristic of shocked gas. Using Chandra data from the ChASeM33 survey with a 0.35-2 keV sensitivity of similar to 2 x 10(34) erg s(-1), we have detected 82 of 137 SNR candidates, yielding confirmation of (or at least strongly support for) their SNR identifications. This provides the largest sample of remnants detected at optical and X-ray wavelengths in any galaxy, including the Milky Way. A spectral analysis of the seven X-ray brightest SNRs reveals that two, G98-31 and G98-35, have spectra that appear to indicate enrichment by ejecta from core-collapse supernova explosions. In general, the X-ray-detected SNRs have soft X-ray spectra compared to the vast majority of sources detected along the line of sight to M33. It is unlikely that there are any other undiscovered thermally dominated X-ray SNRs with luminosities in excess of similar to 4 x 10(35) erg s(-1) in the portions of M33 covered by the ChASeM33 survey. We have used a combination of new and archival optical and radio observations to attempt to better understand why some objects are detected as X-ray sources and others are not. We have also developed a morphological classification scheme for the optically identified SNRs and discussed the efficacy of this scheme as a predictor of X-ray detectability. Finally, we have compared the SNRs found in M33 to those that have been observed in the Galaxy and the Magellanic Clouds. There are no close analogs of Cas A, Kepler's SNR, Tycho's SNR, or the Crab Nebula in the regions of M33 surveyed, but we have found an X-ray source with a power-law spectrum coincident with a small-diameter radio source that may be the first pulsar-wind nebula recognized in M33. C1 [Long, Knox S.; Ghavamian, Parviz] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Blair, William P.; Kuntz, Kip D.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Winkler, P. Frank; McNeil, Emily K.] Middlebury Coll, Dept Phys, Middlebury, VT 05753 USA. [Becker, Robert H.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Becker, Robert H.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Gaetz, Terrance J.; Kirshner, Robert P.; Plucinsky, Paul P.; Tuellmann, Ralph] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Helfand, David J.; Saul, Destry] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hughes, John P.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Pannuti, Thomas G.] Morehead State Univ, Dept Earth & Space Sci, Ctr Space Sci, Morehead, KY 40351 USA. [Williams, Benjamin] Univ Washington, Dept Astron, Seattle, WA 98195 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; winkler@middlebury.edu FU National Aeronautics and Space Administration [G06-7073A, NAS8-03060]; National Science Foundation [AST-0307613, AST-0908566]; US Department of Energy by Lawrence Livermore National Laboratory [DE-AC52-07NA27344] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G06-7073A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. P. P. P. and T. J. G. acknowledge support under NASA contract NAS8-03060. P. F. W. and E. K. M. acknowledge additional support from the National Science Foundation through grants AST-0307613 and AST-0908566. The work by R. H. B. was partly performed under the auspices of the US Department of Energy by Lawrence Livermore National Laboratory under contract DE-AC52-07NA27344. We acknowledge our extensive use of the optical data on M33 from the Local Group Galaxies Survey, and are grateful to P. Massey and his colleagues for obtaining these data and for making them freely available. This work has made extensive use of SAOImage DS9 (Joye & Mandel 2003), developed by the Smithsonian Astrophysical Observatory. We also acknowledge the heroic efforts of the referee, M. Filipovic, for an extremely careful reading of the original manuscript and numerous comments that have improved this paper. NR 82 TC 40 Z9 40 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD APR PY 2010 VL 187 IS 2 BP 495 EP 559 DI 10.1088/0067-0049/187/2/495 PG 65 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 585QJ UT WOS:000276841500008 ER PT J AU Kaltenegger, L Eiroa, C Fridlund, CVM AF Kaltenegger, L. Eiroa, C. Fridlund, C. V. M. TI Target star catalogue for Darwin Nearby Stellar sample for a search for terrestrial planets SO ASTROPHYSICS AND SPACE SCIENCE LA English DT Article DE Darwin/TPF; Nearby stars; Habitability; Extrasolar planet search ID EXTRA-SOLAR PLANETS; EARTH-LIKE PLANETS; M-DWARFS; HABITABLE ZONES; SYSTEMS; MULTIPLICITY; MISSION; COLOR; TRANSFORMATIONS; INTERFEROMETER AB In order to evaluate and develop mission concepts for a search for Terrestrial Exoplanets, we have prepared a list of potential target systems. In this paper we present and discuss the criteria for selecting potential target stars, suitable for the search for Earth-like planets, with a special emphasis on the aspects of the habitable zone for these stellar systems. Planets found within these zones would be potentially able to host complex life forms. We derive a final target star sample of potential target stars, the Darwin All Sky Star Catalogue (DASSC). The DASSC contains a sample of 2303 identified objects of which 284 are F-, 464 G-, 883 K- and 615 M-type stars and 57 stars without B-V index. Of these objects 949 objects are flagged in the DASSC as multiple systems, resulting in 1229 single main sequence stars of which 107 are F, 235 are G, 536 are K, and 351 are M type. We derive configuration dependent sub-catalogues from the DASSC for two technical designs, the initial baseline design and the advanced Emma design as well as a catalogue using an inner working angle cutoff. We discuss the selection criteria, derived parameters and completeness of sample for different classes of stars. C1 [Fridlund, C. V. M.] European Space Agcy, ESTEC, NL-2200 AG Noordwijk, Netherlands. [Kaltenegger, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Eiroa, C.] Univ Autonoma Madrid, Madrid, Spain. RP Fridlund, CVM (reprint author), European Space Agcy, ESTEC, POB 299, NL-2200 AG Noordwijk, Netherlands. EM malcolm.fridlund@esa.int FU NASA [NAG5-13045]; NSF FX Special thanks to G. Torres and E. Mamajek for many stimulating discussions and very constructive suggestions. Part of this work was supported by NASA grant NAG5-13045. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, NASA's Astrophysics Data System and data products from the Two Micron All Sky Survey, which is a joint project of the UMass and IPAC, funded by NASA and NSF. NR 48 TC 8 Z9 8 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0004-640X J9 ASTROPHYS SPACE SCI JI Astrophys. Space Sci. PD APR PY 2010 VL 326 IS 2 BP 233 EP 247 DI 10.1007/s10509-009-0223-3 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 562YE UT WOS:000275091100012 ER PT J AU Claramunt, S Derryberry, EP Chesser, RT Aleixo, A Brumfield, RT AF Claramunt, Santiago Derryberry, Elizabeth P. Chesser, R. Terry Aleixo, Alexandre Brumfield, Robb T. TI POLYPHYLY OF CAMPYLORHAMPHUS, AND DESCRIPTION OF A NEW GENUS FOR C. PUCHERANI (DENDROCOLAPTINAE) SO AUK LA English DT Article DE Campylorhamphus; Dendrocolaptinae; Drymotoxeres; morphometric heterogeneity; phylogeny; ranking criteria; taxonomy ID MOLECULAR SYSTEMATICS; PHYLOGENETIC ANALYSIS; WOODCREEPERS AVES; PASSERIFORMES; BIOGEOGRAPHY; CHARACTERS; INCONGRUENCE; ALLOMETRY; EVOLUTION; SELECTION AB We investigated the phylogenetic relationships of Campylorhamphus pucherani using DNA sequences from three mitochondrial genes and a nuclear intron, as well as 84 morphological characters from the skeleton, the integument, and the musculature. The molecular phylogeny indicated that C. pucherani is not part of Campylorhamphus; instead, it is the sister species to Drymornis bridgesii, in a clade that also contains Lepidocolaptes. The morphological phylogeny also placed C. pucherani in a clade that contains Drymornis and Lepidocolaptes. Using a morphometric analysis of size and shape diversity, we demonstrated that the inclusion of C. pucherani in Drymornis would create an excessively heterogeneous genus compared with other dendrocolaptine genera. Because no generic name is available for C. pucherani, we describe the new genus Drymotoxeres for this species. Received 18 June 2009, accepted 12 October 2009. C1 [Claramunt, Santiago; Derryberry, Elizabeth P.; Brumfield, Robb T.] Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. [Claramunt, Santiago; Derryberry, Elizabeth P.; Brumfield, Robb T.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. [Chesser, R. Terry] US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Aleixo, Alexandre] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. RP Claramunt, S (reprint author), Louisiana State Univ, Museum Nat Sci, Baton Rouge, LA 70803 USA. EM sclara1@tigers.lsu.edu RI Derryberry, Elizabeth/C-2396-2011; Aleixo, Alexandre/L-3135-2013; Brumfield, Robb/K-6108-2015 OI Brumfield, Robb/0000-0003-2307-0688 FU National Science Foundation [DBI-0400797, DEB-0543562] FX We are grateful to the following people and institutions for providing tissue samples: G. Barrowclough and P. Sweet, Department of Ornithology, American Museum of Natural History; J. Bates and D. Willard, Bird Division, Field Museum of Natural History; F. Sheldon and D. Dittmann, Genetic Resources Collection, Louisiana State University Museum of Natural Science; and Laboratorio de Genetica e Evolucao Molecular de Ayes, Universidade de Sao Paulo. For access to anatomical specimens, we thank J. Cracraft and P. Sweet, Department of Ornithology, American Museum of Natural History; J. V. Remsen and S. Cardiff, Louisiana State University Museum of Natural Science; and J. Cuello, Museo Nacional de Historia Natural (MNHN), Uruguay. We are grateful to G. Bravo, P. Chakrabarty, A. Cuervo, L. Naka, J. V. Remsen, and three anonymous reviewers for comments and discussion concerning the manuscript. This research was supported in part by National Science Foundation grants DBI-0400797 and DEB-0543562 to R.T.B. Use of trade, product, or firm names does not imply endorsement by the U.S. Government. NR 52 TC 7 Z9 7 U1 0 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 APR PY 2010 VL 127 IS 2 BP 430 EP 439 DI 10.1525/auk.2009.09022 PG 10 WC Ornithology SC Zoology GA 592RT UT WOS:000277398000021 ER PT J AU Kolowski, JM Alonso, A AF Kolowski, J. M. Alonso, A. TI Density and activity patterns of ocelots (Leopardus pardalis) in northern Peru and the impact of oil exploration activities SO BIOLOGICAL CONSERVATION LA English DT Article DE Seismic; Disturbance; Amazon; Camera traps; Carnivore; Population size ID WOODLAND CARIBOU; NORTHEASTERN ALBERTA; RESOURCE-EXTRACTION; MILITARY ACTIVITY; FELIS-PARDALIS; BIGHORN SHEEP; CAMERA-TRAPS; POPULATIONS; MOVEMENTS; BEHAVIOR AB The western Amazon is experiencing unprecedented levels of oil and gas exploration, a trend of particular concern given the high levels of biodiversity found in this relatively pristine and unstudied region Despite the widespread use of seismic reflection technology for exploration, no studies have investigated the response of wildlife populations to this disturbance in the tropics. We conducted a trail camera survey inside a large oil concession (Block 39) in the Peruvian Amazon near the Ecuador border with ongoing 2D seismic explorations to investigate its effects on ocelot (Leopardus pardalis) activity and abundance The estimated size of the ocelot population within our 22 km(2) study area was the same before (control period. 34 +/- 69 ocelots) and during exploration operations (disturbance period, 34 +/- 46 ocelots) and we detected no change in activity patterns between the two periods Ocelot capture rate was unaffected by the presence of seismic crews, and distance to the nearest seismic line was not col related with capture rate at individual stations Our density estimates (ocelots/100 km(2)) from the control (75 2) and disturbance period (94 7) include the highest reported for the species, and represent the first ocelot density estimates from the northwest Amazon forest These high values conform to recent research showing a positive association between ocelot density, annual rainfall, and proximity to the equator (this study >2500 mm annual rainfall; <200 km from equator) We discuss the potential short- and long-term environmental impacts of seismic operations, particularly as they relate to large mammal populations. (C) 2009 Elsevier Ltd All rights reserved. C1 [Kolowski, J. M.; Alonso, A.] Smithsonian Inst, Ctr Conservat Educ & Sustainabil, Washington, DC 20013 USA. RP Kolowski, JM (reprint author), Smithsonian Inst, Ctr Conservat Educ & Sustainabil, Natl Zool Pk,1100 Jefferson Dr SW,Suite 3123, Washington, DC 20013 USA. FU Repsol FX We thank Gegner Pastor, Enrique Pinedo, Luis Fernando, Guillermo Jipa, Antonio Pastrana and Anibal Lichi Perez for their invaluable field support and local knowledge of the forest and its fauna. Special thanks to Repsol personnel in Lima, Madrid, Houston, and in Block 39 during field operations. We are also thankful to the staff of Global Geophysical Services for their generous assistance with field support. Sulema Castro provided critical project coordination and organization Helpful comments were provided by Marcella Kelly, Mark Higgins, and Ricardo Moreno during study design and preparation for field activities, and Ann Henderson provided important suggestions to an earlier draft of this manuscript. Funding for this project and generous logistical support were provided by Repsol. This research was conducted under permit No. 016-2008-INRENA-IFFS-DCB. This publication is contribution #7 of the Peru Biodiversity Program. NR 60 TC 27 Z9 30 U1 11 U2 82 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 EI 1873-2917 J9 BIOL CONSERV JI Biol. Conserv. PD APR PY 2010 VL 143 IS 4 BP 917 EP 925 DI 10.1016/j.biocon.2009.12.039 PG 9 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 580CV UT WOS:000276425400013 ER PT J AU Mena-Correa, J Sivinski, J Anzures-Dadda, A Ramirez-Romero, R Gates, M Aluja, M AF Mena-Correa, J. Sivinski, J. Anzures-Dadda, A. Ramirez-Romero, R. Gates, M. Aluja, M. TI Consideration of Eurytoma sivinskii Gates and Grissell, a eurytomid (Hymenoptera) with unusual foraging behaviors, as a biological control agent of tephritid (Diptera) fruit flies SO BIOLOGICAL CONTROL LA English DT Article DE Demography; Eurytomidae; Fruit fly; Parasitoid; Tephritidae; Hyperparasitism ID LONGICAUDATA ASHMEAD HYMENOPTERA; HAYWARDI OGLOBLIN HYMENOPTERA; ANASTREPHA SPP. DIPTERA; FLY DIPTERA; PUPAL PARASITOIDS; IMMATURE STAGES; POULTRY MANURE; ATTACK RATE; BRACONIDAE; MEXICO AB A recently discovered Mexican parasitoid species of Eurytomidae (Hymenoptera), Eurytoma sivinskii Gates and Grissell, has the unique behavior, for its family, of attacking tephritid fruit fly pupae (Anastrepha spp.) on or in the soil. Adults burrowed but did so rarely, thus pupae on the soil surface were significantly more vulnerable than those underground. Females facultatively hyperparasitized other larval-prepupal and pupal parasitoids such as Opius hirtus (Braconidae), Coptera haywardi (Diapriidae) and Pachycrepoideus vindemiae (Pteromalidae). While E. sivinskii developed in the pupae of various other Anastrepha, including, A. serpentina and A. striata, it also attacked cyclorraphous Diptera such as Musca domestica and a tachinid species. The number of expected female offspring (R(o)) was 44.3 when measured as eclosed eggs (i.e., that became larvae) and 34.3 when measured as the number of emerged adults, and the intrinsic rate of natural increase (r(m)) was 0.34. This is high relative to other fruit fly parasitoids and suggests that E. sivinskii could rapidly exploit a clumped resource. We conclude that the marginal ability of E. sivinskii to attack buried pupae and the environmental risks it poses through its broad host range and capacity for hyperparasitism make it a poor candidate for tephritid biological control. (c) 2009 Elsevier Inc. All rights reserved. C1 [Mena-Correa, J.; Anzures-Dadda, A.; Ramirez-Romero, R.; Aluja, M.] Inst Ecol AC, Xalapa 91000, Veracruz, Mexico. [Sivinski, J.] USDA ARS, Ctr Med Agr & Vet Entomol, Gainesville, FL 32604 USA. [Gates, M.] ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20013 USA. RP Aluja, M (reprint author), Inst Ecol AC, Apartado Postal 63, Xalapa 91000, Veracruz, Mexico. EM martin.aluja@inecol.edu.mx FU Mexican Campana Nacional contra las Moscas de la Fruta; United States Department of Agriculture - Agricultural Research Service (USDA-ARS); INECOL; Comision Nacional para el Conocimiento y Uso de la Biodiversidad [FB325/H296/96]; Consejo Nacional de Ciencia y Tecnologia (CONACyT)/Fondo del Sistema de Investigacion del Golfo de Mexico [SIG96001/96-01003-V, 79449] FX We gratefully acknowledge the help of Alberto Mata, Armando Torres Anaya, Cecilia Martinez Arcos, Melissa Galicia, Jovita Martinez Tlapa and Sandy Mendez Trejo (all Instituto de Ecologia, A.C., Xalapa, Veracruz, Mexico [INECOL]), who helped rear all the parasitoids used during this study. Larissa Guillen, Andrea Birke, Martin Pale and Guadalupe Cordova (also INECOL) helped organize experiments, provided needed materials and provided critical advice along the way. We thank several anonymous expert taxonomists at the Systematic Entomology Laboratory, USDA-ARS for identifying the tachinid, Paleaosepsis sp. and M. domestica specimens. Financial support for this study was principally furnished by the Mexican Campana Nacional contra las Moscas de la Fruta (Secretaria de Agricultura, Ganaderia, Desarrollo Rural y Pesca Instituto Interamericano de Cooperacion para la Agricultura (SAGARPA-IICA). Additional funds were provided by the United States Department of Agriculture - Agricultural Research Service (USDA-ARS) and INECOL. Given that E. sivinskii was discovered while conducting studies financed by the Comision Nacional para el Conocimiento y Uso de la Biodiversidad (CONABIO; Proyect Number FB325/H296/96) and the Consejo Nacional de Ciencia y Tecnologia (CONACyT)/Fondo del Sistema de Investigacion del Golfo de Mexico (SIGOLFO, Project Number SIG96001/96-01003-V), we also gratefully acknowledge their financial support. Information reported here forms part of the undergraduate thesis of JMC (Universidad Nacional Autonoma de Mexico [UNAM]), directed by MA. M.A. also acknowledges support from CONACyT through a Sabbatical Year Fellowship (Ref. 79449) and thanks Benno Graf and Jorg Samietz (Forschungsanstalt Agroscope Changins-Wadenswil ACW), for providing ideal working conditions to finish writing/editing this paper. NR 41 TC 0 Z9 1 U1 5 U2 18 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-9644 J9 BIOL CONTROL JI Biol. Control PD APR PY 2010 VL 53 IS 1 BP 9 EP 17 DI 10.1016/j.biocontrol.2009.03.019 PG 9 WC Biotechnology & Applied Microbiology; Entomology SC Biotechnology & Applied Microbiology; Entomology GA 559XG UT WOS:000274862500002 ER PT J AU Olson, SL AF Olson, Storrs L. TI Stasis and turnover in small shearwaters on Bermuda over the last 400 000 years (Aves: Procellariidae: Puffinus lherminieri group) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Cape Verde Islands; competitive exclusion; fossil record; Pleistocene; P; boydi; P; parvus ID CAPE-VERDE ISLANDS; FOSSIL; OCEAN; BIRDS; LIST AB The extinct species Puffinus parvus Shufeldt of Bermuda is shown to be synonymous with the living taxon Puffinus boydi of the Cape Verde islands. This species occurred on Bermuda throughout the last 400 000 years, during both glacial and interglacial intervals, and into the Holocene up until the arrival of humans when introduced predators evidently caused its extirpation. Subsequently, the island was colonized briefly by the Caribbean species Puffinus lherminieri, which in turn was extirpated from the island in the 20th Century. The indications are that P. boydi successfully outcompeted P. lherminieri on Bermuda until it was removed through human agency, thus closely paralleling the situation documented for two species of Megadyptes penguins in New Zealand. Thus P. lherminieri and P. boydi have long functioned as biological species and should be considered as full species along with the cold-water species Puffinus baroli of the North Atlantic. Restoration efforts for small shearwaters on Bermuda should now focus on P. boydi rather than P. lherminieri. (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 99, 699-707. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20013 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, POB 37012, Washington, DC 20013 USA. EM olsons@si.edu NR 66 TC 6 Z9 7 U1 0 U2 7 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD APR PY 2010 VL 99 IS 4 BP 699 EP 707 PG 9 WC Evolutionary Biology SC Evolutionary Biology GA 576SH UT WOS:000276168100004 ER PT J AU Honnen, AC Hailer, F Kenntner, N Literak, I Dubska, L Zachos, FE AF Honnen, Ann-Christin Hailer, Frank Kenntner, Norbert Literak, Ivan Dubska, Lenka Zachos, Frank E. TI Mitochondrial DNA and nuclear microsatellites reveal high diversity and genetic structure in an avian top predator, the white-tailed sea eagle, in central Europe SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE birds of prey; phylogeography; population genetics; raptors ID RECENT POPULATION BOTTLENECKS; HALIAEETUS-ALBICILLA; CONTROL REGION; PHYLOGEOGRAPHY; ACCIPITRIDAE; POLYMORPHISM; SOFTWARE; AQUILA; TESTS; FALCONIFORMES AB We analysed 123 white-tailed sea eagles (Haliaeetus albicilla) from (primarily central) Europe with respect to variability and differentiation based on 499 bp of the mitochondrial control region and genotypes at seven unlinked nuclear microsatellites. Variability was high (overall expected heterozygosity, haplotype and nucleotide diversity being 0.70, 0.764 and 0.00698, respectively) and both marker systems showed a subdivision into two main genetic clusters (microsatellites) or haplogroups (mtDNA). In line with earlier analyses focusing on populations from northern and eastern Europe, as well as from Asia, we found a high level of admixture in Europe and no signs of a bottleneck - despite a severe decline of white-tailed sea eagle populations during the 20th century. Europe is thus a global stronghold for this species not only with respect to the number of breeding pairs but also regarding the proportion of species-wide genetic diversity. Our dense sampling revealed a possibly clinal variation within central Europe from north-west to south-east that was reflected by the distribution of mtDNA haplotypes as well as the two microsatellite-based clusters. This population differentiation in central Europe probably originated from a geographically structured postglacial colonization and was later enhanced by recent demographic fluctuations. (C) 2010 The Linnean Society of London, Biological Journal of the Linnean Society, 2010, 99, 727-737. C1 [Honnen, Ann-Christin; Zachos, Frank E.] Univ Kiel, Inst Zool, D-24118 Kiel, Germany. [Hailer, Frank] Smithsonian Inst, Natl Zool Pk, Ctr Conservat & Evolutionary Genet, Washington, DC 20013 USA. [Hailer, Frank] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Kenntner, Norbert] Leibniz Inst Zoo & Wildlife Res, D-10315 Berlin, Germany. [Literak, Ivan; Dubska, Lenka] Univ Vet & Pharmaceut Sci, Fac Vet Hyg & Ecol, Dept Biol & Wildlife Dis, Brno 61242, Czech Republic. RP Zachos, FE (reprint author), Univ Kiel, Inst Zool, Olshaussenstr 40, D-24118 Kiel, Germany. EM fzachos@zoologie.uni-kiel.de RI Hailer, Frank/C-9114-2012; Literak, Ivan/H-1652-2014; OI Hailer, Frank/0000-0002-2340-1726; Literak, Ivan/0000-0001-9885-6840; Honnen, Ann-Christin/0000-0003-4355-7231 FU Ministry of Education, Youth and Sports of the Czech Republic [MSM6215712402] FX The following people provided samples and expertise, which are both gratefully acknowledged: Hermann Ansorge, Gorlitz, Germany; Bernd-Struwe-Juhl, Kiel, Germany, and the Projektgruppe Seeadlerschutz Schleswig-Holstein, Germany; Anita Gamauf and Elisabeth Haring, Natural History Museum Vienna, Austria; Bjorn Helander and the Swedish Society for Nature Conservation/Project Sea Eagle. I. Literak and L. Dubska were funded by grant no. MSM6215712402 from the Ministry of Education, Youth and Sports of the Czech Republic. NR 46 TC 10 Z9 10 U1 0 U2 29 PU WILEY-BLACKWELL PUBLISHING, INC PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0024-4066 J9 BIOL J LINN SOC JI Biol. J. Linnean Soc. PD APR PY 2010 VL 99 IS 4 BP 727 EP 737 PG 11 WC Evolutionary Biology SC Evolutionary Biology GA 576SH UT WOS:000276168100007 ER EF