FN Thomson Reuters Web of Science™ VR 1.0 PT J AU Hoyer, S Lopez-Morales, M Rojo, P Nascimbeni, V Hidalgo, S Astudillo-Defru, N Concha, F Contreras, Y Servajean, E Hinse, TC AF Hoyer, S. Lopez-Morales, M. Rojo, P. Nascimbeni, V. Hidalgo, S. Astudillo-Defru, N. Concha, F. Contreras, Y. Servajean, E. Hinse, T. C. TI TraMoS project - III. Improved physical parameters, timing analysis and starspot modelling of the WASP-4b exoplanet system from 38 transit observations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; techniques: photometric; planets and satellites: individual: WASP-4b; stars: individual: WASP-4; planetary systems; starspots ID PLANETARY SYSTEM; GLOBAL DYNAMICS; LIGHT CURVES; PHASE-SPACE; PHOTOMETRY; JUPITER AB We report 12 new transit observations of the exoplanet WASP-4b from the Transit Monitoring in the South (TraMoS) project. These transits are combined with all previously published transit data for this planet to provide an improved radius measurement of R-p = 1.395 +/- 0.022R(jup) and improved transit ephemerides. In a new homogeneous analysis in search for transit timing variations (TTVs) we find no evidence of those with rms amplitudes larger than 20 s over a 4-yr time span. This lack of TTVs rules out the presence of additional planets in the system with masses larger than about 2.5, 2.0 and 1.0 M-circle plus around the 1:2, 5:3 and 2:1 orbital resonances. Our search for the variation of other parameters, such as orbital inclination and transit depth, also yields negative results over the total time span of the transit observations. Finally, we perform a simple study of stellar spots configurations of the system and conclude that the star rotational period is about 34 d. C1 [Hoyer, S.; Rojo, P.; Astudillo-Defru, N.; Concha, F.; Contreras, Y.; Servajean, E.] Univ Chile, Dept Astron, Santiago, Chile. [Hoyer, S.; Hidalgo, S.] Inst Astrofis Canarias, E-38200 Tenerife, Canary Islands, Spain. [Hoyer, S.; Hidalgo, S.] Univ La Laguna, Dept Astrophys, E-38200 Tenerife, Canary Islands, Spain. [Lopez-Morales, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nascimbeni, V.] Univ Padua, Dipartimento Fis & Astron, I-35122 Padua, Italy. [Nascimbeni, V.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Astudillo-Defru, N.] UJF Grenoble 1 CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Hinse, T. C.] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hinse, T. C.] Armagh Observ, Armagh BT61 9DG, North Ireland. RP Hoyer, S (reprint author), Univ Chile, Dept Astron, Casilla 36-D, Santiago, Chile. EM shoyer@das.uchile.cl RI Rojo, Patricio/I-5765-2016; OI Astudillo-Defru, Nicola/0000-0002-8462-515X; Hidalgo, Sebastian/0000-0002-0002-9298; Contreras, Yanett/0000-0002-6388-3635 FU Basal [PFB06]; Fondap [15010003]; Fondecyt [11080271, 1120299]; ALMA-CONICYT FUND [31090030]; Spanish Ministry of Economy and Competitiveness (MINECO) under the Severo Ochoa Excellence Program MINECO at the IAC [SEV-2011-0187]; KRCF via the KRCF Young Scientist Fellowship program; KASI [2013-9-400-00]; SFI/HEA Irish Centre for High-End Computing (ICHEC); Universita a di Padova through the 'progetto di Ateneo' [CPDA103591]; SOAR Telescope at Cerro Pachon Observatory [CNTAC-08B-046, CNTAC-09A-089, CNTAC-09B-050, CNTAC-10A-089, CNTAC-10B-066] FX The authors would like thank D. Dragomir and S. Kane for providing TERMS light curves, M. Gillon for the VLT data and the anonymous referee for the useful and accurate comments which helped to improve this manuscript. SH and PR acknowledge support from Basal PFB06, Fondap #15010003 and Fondecyt #11080271 and #1120299. SH received support from ALMA-CONICYT FUND #31090030 and from the Spanish Ministry of Economy and Competitiveness (MINECO) under the 2011 Severo Ochoa Excellence Program MINECO SEV-2011-0187 at the IAC. TCH acknowledges support from KRCF via the KRCF Young Scientist Fellowship program and financial support from KASI grant number 2013-9-400-00. TCH wish to acknowledge the SFI/HEA Irish Centre for High-End Computing (ICHEC) for the provision of computational facilities and support. VN acknowledges partial support by the Universita a di Padova through the 'progetto di Ateneo' #CPDA103591. We thank the staff of CTIO and SOAR for the help and continuous support during the numerous observing nights, and R. Sanchis-Ojeda for helpful comments and discussions. Based on observations made with the SMARTS 1-m telescope at CTIO and the SOAR Telescope at Cerro Pachon Observatory under programmes ID CNTAC-08B-046, -09A-089, -09B-050, -10A-089 and -10B-066. NR 28 TC 5 Z9 5 U1 1 U2 9 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2013 VL 434 IS 1 BP 46 EP 58 DI 10.1093/mnras/stt962 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207XA UT WOS:000323636800004 ER PT J AU Ting, YS Rix, HW Bovy, J van de Ven, G AF Ting, Yuan-Sen Rix, Hans-Walter Bovy, Jo van de Ven, Glenn TI Constraining the Galactic potential via action-based distribution functions for mono-abundance stellar populations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE Galaxy: disc; Galaxy: fundamental parameters; Galaxy: halo; Galaxy: kinematics and dynamics; Galaxy: structure ID MILKY-WAY DISK; BLACK-HOLE; RADIAL MIGRATION; MASS MODELS; GALAXY; SUBPOPULATIONS; KINEMATICS; DENSITY; ORBITS; STARS AB We present a rigorous and practical way of constraining the Galactic potential based on the phase-space information for many individual stars. Such an approach is needed to dynamically model the data from ongoing spectroscopic surveys of the Galaxy and in the future Gaia. This approach describes the orbit distribution of stars by a family of parametrized distribution function (DF) proposed by McMillan and Binney, which are based on actions. We find that these parametrized DFs are flexible enough to capture well the observed phase-space distributions of individual abundance-selected Galactic subpopulations of stars ('mono-abundance populations') for a disc-like gravitational potential, which enables independent dynamical constraints from each of the Galactic mono-abundance populations. We lay out a statistically rigorous way to constrain the Galactic potential parameters by constructing the joint likelihood of potential and DF parameters, and subsequently marginalizing over the DF parameters. This approach explicitly incorporates the spatial selection function inherent to all Galactic surveys, and can account for the uncertainties of the individual position-velocity observations. On that basis, we study the precision of the parameters of the Galactic potential that can be reached with various sample sizes and realistic spatial selection functions. By creating mock samples from the DF, we show that, even under a restrictive and realistic spatial selection function, given a two-parameter gravitational potential, one can recover the true potential parameters to a few per cent with sample sizes of a few thousands. The assumptions of axisymmetry, of DFs that are smooth in the actions and of no time variation remain important limitations in our current study. C1 [Ting, Yuan-Sen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02139 USA. [Ting, Yuan-Sen; Rix, Hans-Walter; van de Ven, Glenn] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. RP Ting, YS (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02139 USA. EM yuan-sen.ting@cfa.harvard.edu OI Ting, Yuan-Sen/0000-0001-5082-9536; Bovy, Jo/0000-0001-6855-442X FU Max-Planck-Institut fur Astronomie; NASA through Space Telescope Science Institute [HST-HF-51285.01]; NASA [NAS5-26555]; German Research Foundation DFG; [SFB 881] FX We thank the anonymous referee for helpful comments. We also thank Elena D'Onghia for providing data from the simulation in D'Onghia et al. (2013). YST and JB are grateful to the Max-Planck-Institut fur Astronomie for its hospitality and financial support during the period in which this research was performed. JB was supported by NASA through the Hubble Fellowship grant HST-HF-51285.01 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under the NASA contract NAS5-26555. JB was also partially supported by SFB 881 funded by the German Research Foundation DFG. NR 33 TC 7 Z9 7 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 SEP PY 2013 VL 434 IS 1 BP 652 EP 660 DI 10.1093/mnras/stt1053 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207XA UT WOS:000323636800046 ER PT J AU Postigo, AD Campana, S Thone, CC D'Avanzo, P Sanchez-Ramirez, R Melandri, A Gorosabel, J Ghirlanda, G Veres, P Martin, S Petitpas, G Covino, S Fynbo, JPU Levan, AJ AF de Ugarte Postigo, A. Campana, S. Thoene, C. C. D'Avanzo, P. Sanchez-Ramirez, R. Melandri, A. Gorosabel, J. Ghirlanda, G. Veres, P. Martin, S. Petitpas, G. Covino, S. Fynbo, J. P. U. Levan, A. J. TI The obscured hyper-energetic GRB 120624B hosted by a luminous compact galaxy at z=2.20 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: individual: GRB 120624B ID GAMMA-RAY BURST; STAR-FORMATION; IMAGE SUBTRACTION; SPECTROSCOPY; METALLICITY; AFTERGLOWS; RESOLUTION; REDSHIFTS; SPECTRA; MASS AB Context. Gamma-ray bursts (GRBs) are the most luminous explosions that we can witness in the Universe. Studying the most extreme cases of these phenomena allows us to constrain the limits for the progenitor models. Aims. In this Letter, we study the prompt emission, afterglow, and host galaxy of GRB 120624B, one of the brightest GRBs detected by Fermi, to derive the energetics of the event and characterise the host galaxy in which it was produced. Methods. Following the high-energy detection we conducted a multi-wavelength follow-up campaign, including near-infrared imaging from HAWKI/VLT, optical from OSIRIS/GTC, X-ray observations from the Chandra X-ray Observatory and at submillimetre/millimetre wavelengths from SMA. Optical/NIR spectroscopy was performed with X-shooter/VLT. Results. We detect the X-ray and NIR afterglow of the burst and determine a redshift of z = 2.1974 +/- 0.0002 through identification of emission lines of [O II], [O III] and H-alpha from the host galaxy of the GRB. This implies an energy release of E-iso,E-gamma = (3.0 +/- 0.2)x10(54) erg, amongst the most luminous ever detected. The observations of the afterglow indicate high obscuration with A(V) > 1.5. The host galaxy is compact, with R-1/2 < 1.6 kpc, but luminous, at L similar to 1.5 L* and has a star formation rate of 91 +/- 6 M-circle dot/yr as derived from Ha. Conclusions. As for other highly obscured GRBs, GRB 120624B is hosted by a luminous galaxy, which we also prove to be compact, with very intense star formation. It is one of the most luminous host galaxies associated with a GRB, showing that the host galaxies of long GRBs are not always blue dwarf galaxies, as previously thought. C1 [de Ugarte Postigo, A.; Thoene, C. C.; Sanchez-Ramirez, R.; Gorosabel, J.] Inst Astrofis Andalucia IAA CSIC, Granada 18008, Spain. [de Ugarte Postigo, A.; Fynbo, J. P. U.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Campana, S.; D'Avanzo, P.; Melandri, A.; Ghirlanda, G.; Covino, S.] INAF Osservatorio Astron Brera, I-23807 Merate, LC, Italy. [Gorosabel, J.] Univ Pais Vasco UPV EHU, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, ETS Ingn, Bilbao 48013, Spain. [Gorosabel, J.] Basque Fdn Sci, Bilbao 48008, Spain. [Veres, P.] Penn State Univ, Dept Astron & Astrophys, Dept Phys, University Pk, PA 16802 USA. [Veres, P.] Penn State Univ, Ctr Particle & Gravitat Astrophys, University Pk, PA 16802 USA. [Martin, S.] European So Observ, Santiago De Compostela, Spain. [Petitpas, G.] Harvard Smithsonian Ctr Astrophys, Hilo, HI 96720 USA. [Levan, A. J.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. RP Postigo, AD (reprint author), Inst Astrofis Andalucia IAA CSIC, Glorieta Astron S-N, Granada 18008, Spain. EM adeugartepostigo@gmail.com RI Fynbo, Johan/L-8496-2014; OI Ghirlanda, Giancarlo/0000-0001-5876-9259; Fynbo, Johan/0000-0002-8149-8298; Campana, Sergio/0000-0001-6278-1576; Thone, Christina/0000-0002-7978-7648; de Ugarte Postigo, Antonio/0000-0001-7717-5085; Covino, Stefano/0000-0001-9078-5507; Sanchez-Ramirez, Ruben/0000-0002-7158-5099 FU Spanish research project [AYA2012-39362-C02-02]; European Commission under the Marie Curie Career Integration Grant programme [FP7-PEOPLE-2012-CIG 322307]; Unidad Asociada IAA-CSIC_ETSI-UPV/EHU; Ikerbasque Foundation for Science; DNRF; ASI [I/011/07/0]; PRIN-MIUR [2009ERC3HT] FX We thank the anonymous referee for the careful and constructive revision of our manuscript. We thank Thomas Kruhler for his help with the SED fitting and Lise Christensen for fruitful discussions. Based on observations made with the Gran Telescopio Canarias (GTC) at the Roque de los Muchachos Observatory (La Palma). The research activity of A.d. U. P., C. T., and J.G. is supported by Spanish research project AYA2012-39362-C02-02. AdUP acknowledges support by the European Commission under the Marie Curie Career Integration Grant programme (FP7-PEOPLE-2012-CIG 322307). J.G. is supported by the Unidad Asociada IAA-CSIC_ETSI-UPV/EHU and the Ikerbasque Foundation for Science. P. V. acknowledges NASA NNX13AH50G and OTKA K077795. The Dark Cosmology Centre is funded by the DNRF. S. C. acknowledges support by ASI grant I/011/07/0 and PRIN-MIUR grant 2009ERC3HT. We thank H. Tananbaum for granting the Chandra DDT. NR 45 TC 3 Z9 3 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2013 VL 557 AR L18 DI 10.1051/0004-6361/201322065 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900146 ER PT J AU Kristensen, LE van Dishoeck, EF Benz, AO Bruderer, S Visser, R Wampfler, SF AF Kristensen, L. E. van Dishoeck, E. F. Benz, A. O. Bruderer, S. Visser, R. Wampfler, S. F. TI Observational evidence for dissociative shocks in the inner 100 AU of low-mass protostars using Herschel-HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; ISM: molecules; ISM: jets and outflows ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; J CO OBSERVATIONS; NGC 1333; SUBMILLIMETER ARRAY; EMBEDDED PROTOSTARS; PACS SPECTROSCOPY; LINE SPECTRA; KEY PROGRAM; HH 46 AB Aims. Herschel-HIFI spectra of H2O towards low-mass protostars show a distinct velocity component not seen in observations from the ground of CO or other species. The aim is to characterise this component in terms of excitation conditions and physical origin. Methods. A velocity component with an offset of similar to 10 km s(-1) detected in spectra of the H2O 1(10)-1(01) 557 GHz transition towards six low-mass protostars in the "Water in star-forming regions with Herschel" (WISH) programme is also seen in higher-excited H2O lines. The emission from this component is quantified and local excitation conditions are inferred using 1D slab models. Data are compared to observations of hydrides (high-J CO, OH+, CH+, C+, OH) where the same component is uniquely detected. Results. The velocity component is detected in all six targeted H2O transitions (E-up similar to 50-250 K), as well as in CO 16-15 towards one source, Ser SMM1. Inferred excitation conditions imply that the emission arises in dense (n similar to 5 x 10(6)-10(8) cm(-3)) and hot (T similar to 750 K) gas. The H2O and CO column densities are greater than or similar to 10(16) and 10(18) cm(-2), respectively, implying a low H2O abundance of similar to 10(-2) with respect to CO. The high column densities of ions such as OH+ and CH+ (both greater than or similar to 10(13) cm(-2)) indicate an origin close to the protostar where the UV field is strong enough that these species are abundant. The estimated radius of the emitting region is 100 AU. This component likely arises in dissociative shocks close to the protostar, an interpretation corroborated by a comparison with models of such shocks. Furthermore, one of the sources, IRAS 4A, shows temporal variability in the offset component over a period of two years which is expected from shocks in dense media. High-J CO gas detected with Herschel-PACS with T-rot similar to 700 K is identified as arising in the same component and traces the part of the shock where H-2 reforms. Thus, H2O reveals new dynamical components, even on small spatial scales in low-mass protostars. C1 [Kristensen, L. E.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.; Bruderer, S.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Benz, A. O.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Visser, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Wampfler, S. F.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. [Wampfler, S. F.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. RP Kristensen, LE (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM lkristensen@cfa.harvard.edu RI Wampfler, Susanne/D-2270-2015; Kristensen, Lars/F-4774-2011 OI Wampfler, Susanne/0000-0002-3151-7657; Kristensen, Lars/0000-0003-1159-3721 FU Netherlands Research School for Astronomy (NOVA); Spinoza grant; Netherlands Organisation for Scientific Research (NWO) [614.001.008]; European Community [238258] FX The authors would like to thank the entire WISH team for many, many stimulating discussions. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the US under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology - MC2, RSS & GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm University - Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO), and by the European Community's Seventh Framework Programme FP7/2007-2013 under grant agreement 238258 (LASSIE). NR 50 TC 19 Z9 19 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2013 VL 557 AR A23 DI 10.1051/0004-6361/201321619 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900084 ER PT J AU Santerne, A Fressin, F Diaz, RF Figueira, P Almenara, JM Santos, NC AF Santerne, A. Fressin, F. Diaz, R. F. Figueira, P. Almenara, J. -M. Santos, N. C. TI The contribution of secondary eclipses as astrophysical false positives to exoplanet transit surveys SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE planetary systems; techniques: photometric; binaries: eclipsing ID SOLAR-TYPE STARS; CLOSE BINARY STARS; SOPHIE VELOCIMETRY; EXTRASOLAR PLANETS; MODEL ATMOSPHERES; LIGHT CURVES; KEPLER; CANDIDATES; STELLAR; CATALOG AB investigate the astrophysical false-positive configuration in exoplanet-transit surveys. It involves eclipsing binaries and giant planets that present only a secondary eclipse, as seen from the Earth. To test how an eclipsing binary configuration can mimic a planetary transit, we generated synthetic light curves of three examples of secondary-only eclipsing binary systems that we fit with a circular planetary model. Then, to evaluate its occurrence we modeled a population of binaries in double and triple systems based on binary statistics and occurrence. We find that 0.061% +/- 0.017% of main-sequence binary stars are secondary-only eclipsing binaries that mimics a planetary transit candidate with a size down to the size of the Earth. We then evaluate the occurrence that an occulting only giant planet can mimic an Earth-like planet or even a smaller one. We find that 0.009% +/- 0.002% of stars harbor a giant planet that only presents the secondary transit. Occulting-only giant planets mimic planets that are smaller than the Earth, and they are in the scope of space missions like Kepler and PLATO. We estimate that up to 43.1 +/- 5.6 Kepler objects of interest can be mimicked by this configuration of false positives, thereby re-evaluating the global false-positive rate of the Kepler mission from 9.4 +/- 0.9% to 11.3 +/- 1.1%. We note, however, that this new false positive scenario occurs at relatively long orbital periods compared with the median period of Kepler candidates. C1 [Santerne, A.; Figueira, P.; Santos, N. C.] Univ Porto, Ctr Astrofis, P-4150762 Oporto, Portugal. [Fressin, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Diaz, R. F.; Almenara, J. -M.] Aix Marseille Univ, CNRS, LAM, UMR 7326, F-13388 Marseille, France. [Santos, N. C.] Univ Porto, Fac Ciencias, Dept Fis & Astron, P-4100 Oporto, Portugal. RP Santerne, A (reprint author), Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Oporto, Portugal. EM alexandre.santerne@astro.up.pt RI Santos, Nuno/E-9957-2011; Figueira, Pedro/J-4916-2013; Santerne, Alexandre/M-9265-2013 OI Diaz, Rodrigo/0000-0001-9289-5160; Santos, Nuno/0000-0003-4422-2919; Figueira, Pedro/0000-0001-8504-283X; Santerne, Alexandre/0000-0002-3586-1316 FU European Research Council/European Community [239953]; Fundacao para a Ciencia e a Tecnologia (FCT) [PTDC/CTE-AST/098528/2008]; CNES FX We thank the anonymous referee for fruitful comments that helped us to substantially improve the quality of this paper. We also thank J. Johnson and T. Morton for their constructive comments about this paper. A. S., P. F., and N.C.S. acknowledge the support by the European Research Council/European Community under the FP7 through Starting Grant agreement number 239953. NCS also acknowledges the support from Fundacao para a Ciencia e a Tecnologia (FCT) in the form of grant reference PTDC/CTE-AST/098528/2008. RFD is supported by the CNES. NR 64 TC 17 Z9 17 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2013 VL 557 AR A139 DI 10.1051/0004-631/201321475 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900066 ER PT J AU Saulder, C Mieske, S Zeilinger, WW Chilingarian, I AF Saulder, Christoph Mieske, Steffen Zeilinger, Werner W. Chilingarian, Igor TI Calibrating the fundamental plane with SDSS DR8 data SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: distances and redshifts; galaxies: elliptical and lenticular, cD; galaxies: fundamental parameters; galaxies: statistics; galaxies: structure ID EARLY-TYPE GALAXIES; DIGITAL-SKY-SURVEY; SURFACE BRIGHTNESS TEST; TO-LIGHT RATIO; ELLIPTIC GALAXIES; DATA RELEASE; VELOCITY DISPERSIONS; PECULIAR VELOCITIES; STELLAR POPULATION; DISTANT CLUSTERS AB We present a calibration of the fundamental plane using SDSS Data Release 8. We analysed about 93 000 elliptical galaxies up to z < 0.2, the largest sample used for the calibration of the fundamental plane so far. We incorporated up-to-date K-corrections and used GalaxyZoo data to classify the galaxies in our sample. We derived independent fundamental plane fits in all five Sloan filters u, g, r, i, and z. A direct fit using a volume-weighted least-squares method was applied to obtain the coefficients of the fundamental plane, which implicitly corrects for the Malmquist bias. We achieved an accuracy of 15% for the fundamental plane as a distance indicator. We provide a detailed discussion on the calibrations and their influence on the resulting fits. These re-calibrated fundamental plane relations form a well-suited anchor for large-scale peculiar-velocity studies in the nearby universe. In addition to the fundamental plane, we discuss the redshift distribution of the elliptical galaxies and their global parameters. C1 [Saulder, Christoph; Mieske, Steffen] European So Observ, Santiago, Chile. [Saulder, Christoph; Zeilinger, Werner W.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Chilingarian, Igor] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. RP Saulder, C (reprint author), European So Observ, Alonso Cordova 3107,Casilla 19001, Santiago, Chile. EM csaulder@eso.org; smieske@eso.org; werner.zeilinger@univie.ac.at; igor.chilingarian@cfa.harvard.edu RI Chilingarian, Igor/N-5117-2016; OI Chilingarian, Igor/0000-0002-7924-3253; Saulder, Christoph/0000-0002-0408-5633 FU Alfred P. Sloan Foundation FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the US Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. C. S. acknowledges the support from an ESO studentship. I. C. acknowledges the support from the Russian Federation President's grant MD-3288.2012.2. This research made use of the "K-corrections calculator" service available at http://kcor.sai.msu.ru/. I. C. acknowledges kind support from the ESO Visitor Program. The publication is supported by the Austrian Science Fund (FWF). NR 67 TC 13 Z9 13 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2013 VL 557 AR A21 DI 10.1051/0004-6361/201321466 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900065 ER PT J AU Schneider, PC Eisloffel, J Gudel, M Gunther, HM Herczeg, G Robrade, J Schmitt, JHMM AF Schneider, P. C. Eisloeffel, J. Guedel, M. Guenther, H. M. Herczeg, G. Robrade, J. Schmitt, J. H. M. M. TI HST far-ultraviolet imaging of DG Tauri Fluorescent molecular hydrogen emission from the wide opening-angle outflow SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: individual: DG Tauri; Herbig-Haro objects; ISM: jets and outflows; stars: variables: T Tauri; Herbig Ae/Be; stars: formation ID HUBBLE-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; HERBIG-HARO OBJECTS; X-RAY JET; T-TAURI; H-2 EMISSION; CIRCUMSTELLAR ENVIRONMENTS; LAUNCHING REGION; OPTICAL OUTFLOW; BOW SHOCK AB One of the most thoroughly studied jets from all young stellar objects is the jet of DG Tau, which we imaged in the far-ultraviolet with the Hubble Space Telescope for the first time. These high spatial resolution images were obtained with long-pass filters and allow us to construct images tracing mainly H-2 and C IV emission. We find that the H-2 emission appears as a limb-brightened cone with additional emission close to the jet axis. The length of the rims is about 0 ''.3 or 42 AU before their brightness strongly drops, and the opening angle is about 90 degrees. Comparing our far-ultraviolet data with near-infrared data we find that the fluorescent H-2 emission probably traces the outer, cooler part of the disk wind while an origin of the H-2 emission in the surface layers (atmosphere) of the (flared) disk is unlikely. Furthermore, the spatial shape of the H-2 emission shows little variation over six years which suggests that the outer part of the disk wind is rather stable and probably not associated with the formation of individual knots. The C IV image shows that the emission is concentrated towards the jet axis. We find no indications for additional C IV emission at larger distances, which strengthens the association with the X-ray emission observed to originate within the DG Tau jet. C1 [Schneider, P. C.; Robrade, J.; Schmitt, J. H. M. M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [Eisloeffel, J.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Guedel, M.] Univ Vienna, Dept Astrophys, A-1180 Vienna, Austria. [Guenther, H. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Herczeg, G.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. RP Schneider, PC (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM cschneider@hs.uni-hamburg.de RI Guedel, Manuel/C-8486-2015; OI Guedel, Manuel/0000-0001-9818-0588; Gunther, Hans Moritz/0000-0003-4243-2840 FU DLR [50 OR 1112]; NASA [NAS5-26555]; NASA Office of Space Science [NAG5-7584]; Austrian Science Fund (FWF) FX We thank Francesca Bacciotti and Lorenzo Maurri for providing the [S II] image. P. C. S was supported by the DLR under grant 50 OR 1112. The paper is based on observations obtained by the Hubble Space Telescope. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NAG5-7584 and by other grants and contracts. The publication is supported by the Austrian Science Fund (FWF). NR 50 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 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2013 VL 557 AR A110 DI 10.1051/0004-6361/201321564 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900076 ER PT J AU Wang, X McIntosh, SW Curdt, W Tian, H Peter, H Xia, LD AF Wang, X. McIntosh, S. W. Curdt, W. Tian, H. Peter, H. Xia, L. -D. TI Temperature dependence of ultraviolet line parameters in network and internetwork regions of the quiet Sun and coronal holes SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: atmosphere; Sun: UV radiation; line: profiles ID FAST SOLAR-WIND; DOPPLER WAVELENGTH SHIFTS; EUV IMAGING SPECTROMETER; TRANSITION-REGION; EMISSION-LINES; ACTIVE-REGION; SPECTROSCOPIC OBSERVATIONS; SUMER TELESCOPE; SOHO; CHROMOSPHERE AB Aims. We study the temperature dependence of the average Doppler shift and the non-thermal line width in network and internetwork regions for both the quiet Sun (QS) and the coronal hole (CH), by using observations of the Solar Ultraviolet Measurements of Emitted Radiation instrument onboard the Solar and Heliospheric Observatory spacecraft. Methods. We obtain the average Doppler shift and non-thermal line width in the network regions of QS, internetwork regions of QS, network regions of CH, and internetwork regions of CH by applying a single-Gaussian fit to the line profiles averaged in each of the four regions. The formation temperatures of the lines we use cover the range from 10(4) to 1.2 x 10(6) K. Two simple scenarios are proposed to explain the temperature dependence of the line parameters in the network regions. In one of the scenarios, the spectral line consists of three components: a rapid, weak upflow generated in the lower atmosphere, a nearly static background, and a slow cooling downflow. In the other scenario, there are just two components, which include a bright core component and a faint wide tail one. Results. An enhancement of the Doppler shift magnitude and the non-thermal line width in network regions compared to the internetwork regions is reported. We also report that most transition region lines are less redshifted (by 0-8 km s(-1)) and broader (by 0-5 km s(-1)) in CH compared to the counterparts of QS. In internetwork regions, the difference in the Doppler shifts between the coronal hole and the QS is slightly smaller, especially for the lines with formation temperatures lower than 2 x 10(5) K. And the two simple scenarios can reproduce the variation in the line parameters with the temperature very well. Conclusions. Our results suggest that the physical processes in network and internetwork regions are different and that one needs to separate network and internetwork when discussing dynamics and physical properties of the solar atmosphere. The agreement between the results of the observation and our scenarios suggests that the temperature dependence of Doppler shifts and line widths might be caused by the different relative contributions of the three components at different temperatures. The results may shed new light on our understanding of the complex chromosphere-corona mass cycle. However, the existing observational results do not allow us to distinguish between the two scenarios. At this stage, a high-resolution instrument Interface Region Imaging Spectrograph is highly desirable. C1 [Wang, X.] Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. [Wang, X.; McIntosh, S. W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. [Curdt, W.; Peter, H.] Max Planck Inst Sonnensyst Forsch, D-37191 Katlenburg Lindau, Germany. [Tian, H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Xia, L. -D.] Shandong Univ Weihai, Sch Space Sci & Phys, Weihai 264209, Peoples R China. RP Wang, X (reprint author), Peking Univ, Sch Earth & Space Sci, Beijing 100871, Peoples R China. EM wangxinpku0209@gmail.com RI Xia, Lidong/B-8836-2011 OI Xia, Lidong/0000-0001-8938-1038 FU China Scholarship Council; NSFC [41174148, 40931055, 41231069, 41222032]; NSF [ATM-0925177]; NASA [NNG06GC89G]; IRIS mission grant [NNG08FD61C]; ASP Postdoctoral Fellow-ship Program of NCAR; National Natural Science Foundation of China (NSFC) [40974105]; DLR; CNES; NASA; ESA PRODEX program (Swiss contribution) FX X. W. is supported by China Scholarship Council for her stay at HAO. X. W. is also supported by NSFC under contract Nos. 41174148, 40931055, 41231069, and 41222032. S. W. M. and H. T. are supported by NSF ATM-0925177 and NASA NNG06GC89G. SWM is partially supported by IRIS mission grant NNG08FD61C. H. T. is also supported by the ASP Postdoctoral Fellow-ship Program of NCAR. L. D. X. is supported by the National Natural Science Foundation of China (NSFC) under contract No. 40974105. The SUMER project is financially supported by DLR, CNES, NASA, and the ESA PRODEX program (Swiss contribution). SUMER is part of SOHO, the Solar and Heliospheric Observatory, of ESA and NASA. NR 60 TC 5 Z9 5 U1 0 U2 5 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 EI 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD SEP PY 2013 VL 557 AR A126 DI 10.1051/0004-6361/201220197 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900013 ER PT J AU Zaninoni, E Bernardini, MG Margutti, R Oates, S Chincarini, G AF Zaninoni, E. Bernardini, M. G. Margutti, R. Oates, S. Chincarini, G. TI Gamma-ray burst optical light-curve zoo: comparison with X-ray observations SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; radiation mechanisms: non-thermal ID SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; CONTINUOUS ENERGY INJECTION; FOLLOW-UP OBSERVATIONS; SMALL-MAGELLANIC-CLOUD; CENTRAL ENGINE; HOST GALAXIES; PROMPT EMISSION; MULTIWAVELENGTH OBSERVATIONS; AFTERGLOW OBSERVATIONS; SHALLOW-DECAY AB Aims. We present a comprehensive analysis of the optical and X-ray light curves (LCs) and spectral energy distributions (SEDs) of a large sample of gamma-ray burst (GRB) afterglows to investigate the relationship between the optical and X-ray emission after the prompt phase. We consider all data available in the literature, which where obtained with different instruments. Methods. We collected the optical data from the literature and determined the shapes of the optical LCs. Then, using previously presented X-ray data, we modeled the optical/X-ray SEDs. We studied the SED parameter distributions and compared the optical and X-ray LC slopes and shapes. Results. The optical and X-ray spectra become softer as a function of time while the gas-to-dust ratios of GRBs are higher than the values calculated for the Milky Way and the Large and Small Magellanic Clouds. For 20% of the GRBs the difference between the optical and X-ray slopes is consistent with 0 or 1/4 within the uncertainties (we did it not consider the steep decay phase), while in the remaining 80% the optical and X-ray afterglows show significantly different temporal behaviors. Interestingly, we find an indication that the onset of the forward shock in the optical LCs (initial peaks or shallow phases) could be linked to the presence of the X-ray flares. Indeed, when X-ray flares are present during the steep decay, the optical LC initial peak or end plateau occurs during the steep decay; if instead the X-ray flares are absent or occur during the plateau, the optical initial peak or end plateau takes place during the X-ray plateau. Conclusions. The forward-shock model cannot explain all features of the optical (e. g. bumps, late re-brightenings) and X-ray (e. g. flares) LCs. However, the synchrotron model is a viable mechanism for GRBs at late times. In particular, we found a relationship between the presence of the X-ray flares and the shape of the optical LC that indicates a link between the prompt emission and the optical afterglow. C1 [Zaninoni, E.; Bernardini, M. G.; Chincarini, G.] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Zaninoni, E.] Univ Padua, Phys & Astron Dept Galileo Galilei, I-35131 Padua, Italy. [Margutti, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oates, S.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Chincarini, G.] Univ Milano Bicocca, Dip Fis G Occhialini, I-20126 Milan, Italy. RP Zaninoni, E (reprint author), INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy. EM elena.zaninoni@brera.inaf.it FU ASI [Swift I/011/07/0]; Ministero degli Affari Esteri [I/004/11/0]; University of Milano - Bicocca FX We thank the anonymous referee for the helpful comments that have improved this paper. E.Z. thanks Daniele Malesani for the useful discussions, suggestions and support during the preparation of the paper; Paolo D'Avanzo and Andrea Melandri for the useful advices; Thomas Kruler for sharing the data of GRB 070802 and Fang Yuang for the data of GRB 081008; Craig B. Markwardt for the help with the MPFIT routine. This research has made use of the XRT Data Analysis Software (XRTDAS) developed under the responsibility of the ASI Science Data Center (ASDC), Italy. This work was supported by ASI grant Swift I/011/07/0 and in part by I/004/11/0, by Ministero degli Affari Esteri and the University of Milano - Bicocca. NR 336 TC 12 Z9 13 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 SEP PY 2013 VL 557 AR A12 DI 10.1051/0004-6361/201321221 PG 55 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 228TC UT WOS:000325211900044 ER PT J AU Sadler, PM Coyle, H Smith, NC Miller, J Mintzes, J Tanner, K Murray, J AF Sadler, Philip M. Coyle, Harold Smith, Nancy Cook Miller, Jaimie Mintzes, Joel Tanner, Kimberly Murray, John TI Assessing the Life Science Knowledge of Students and Teachers Represented by the K-8 National Science Standards SO CBE-LIFE SCIENCES EDUCATION LA English DT Article ID CONCEPT INVENTORY; PROFESSIONAL-DEVELOPMENT; MODEL; MISCONCEPTIONS; BIOLOGY AB We report on the development of an item test bank and associated instruments based on the National Research Council (NRC) K-8 life sciences content standards. Utilizing hundreds of studies in the science education research literature on student misconceptions, we constructed 476 unique multiple-choice items that measure the degree to which test takers hold either a misconception or an accepted scientific view. Tested nationally with 30,594 students, following their study of life science, and their 353 teachers, these items reveal a range of interesting results, particularly student difficulties in mastering the NRC standards. Teachers also answered test items and demonstrated a high level of subject matter knowledge reflecting the standards of the grade level at which they teach, but exhibiting few misconceptions of their own. In addition, teachers predicted the difficulty of each item for their students and which of the wrong answers would be the most popular. Teachers were found to generally overestimate their own students' performance and to have a high level of awareness of the particular misconceptions that their students hold on the K-4 standards, but a low level of awareness of misconceptions related to the 5-8 standards. C1 [Sadler, Philip M.; Coyle, Harold; Smith, Nancy Cook; Miller, Jaimie; Murray, John] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. [Mintzes, Joel] Calif State Univ Chico, Dept Biol Sci, Chico, CA 95929 USA. [Tanner, Kimberly] San Francisco State Univ, San Francisco, CA 94132 USA. RP Sadler, PM (reprint author), Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St, Cambridge, MA 02138 USA. EM psadler@cfa.harvard.edu FU NSF [NSF EHR-0830922]; NIH [NIH 1RC1HD63686-01]; University's Committee on the Use of Human Subjects [F15916-101]; Charles Alcock of the Harvard Smithsonian Center for Astrophysics FX This work was carried out with support from the NSF's grant for MOSART-LS (NSF EHR-0830922) and from the NIH's grant for ALSISE (NIH 1RC1HD63686-01). We thank those scientists who reviewed and commented on the items in the development process. Annette Trenga handled data input and tracking of test forms. We appreciate the advice and support of Charles Alcock of the Harvard Smithsonian Center for Astrophysics. We greatly appreciate the involvement of teachers and their students in this project, without whom this research would have been impossible. This project was conducted with the approval of Harvard University's Committee on the Use of Human Subjects (protocol #F15916-101). NR 78 TC 0 Z9 0 U1 0 U2 14 PU AMER SOC CELL BIOLOGY PI BETHESDA PA 8120 WOODMONT AVE, STE 750, BETHESDA, MD 20814-2755 USA SN 1931-7913 J9 CBE-LIFE SCI EDUC JI CBE-Life Sci. Educ. PD SEP PY 2013 VL 12 IS 3 BP 553 EP 575 DI 10.1187/cbe.12-06-0078 PG 23 WC Education, Scientific Disciplines SC Education & Educational Research GA 236JU UT WOS:000325792800028 PM 24006402 ER PT J AU Santos-Silva, A Komiya, Z Nearns, EH AF Santos-Silva, Antonio Komiya, Ziro Nearns, Eugenio H. TI REVISION OF THE GENUS PRIONACALUS WHITE, 1845 (COLEOPTERA: CERAMBYCIDAE: PRIONINAE: PRIONINI) SO COLEOPTERISTS BULLETIN LA English DT Article DE lectotype; longhorn beetles; South America; synonymy; taxonomy AB Prionacalus White, 1845, a genus restricted to western South America from Colombia to northern Argentina, is revised. Of the 15 species currently described, seven are considered as distinct and redescribed herein. The following five new synonymies are proposed: Prionacalus gunteri Gahan, 1894 is removed from synonymy with Prionacalus buckleyi Waterhouse, 1872 and proposed as a new synonym of Prionacalus cacicus (White, 1845); Prionacalus simonsi Waterhouse, 1900 is a new synonym of Prionacalus atys White, 1850; Prionacalus giovannii Hudepohl, 1985 is a new synonym of Prionacalus whymperi Bates, 1892; Prionacalus trigonodes Bates, 1892, currently a synonym of P. buckleyi, is proposed as a new synonym of P. whymperi; and P. buckleyi is a new synonym of Prionacalus iphis White, 1850. The following earlier synonymies are accepted: Prionacalus emmae Kolbe, 1902 and Prionacalus whitei Waterhouse, 1900 are synonyms of P. buckleyi (and consequently, synonyms of P. iphis); syntype female of Psalidognathus wallisi Taschenberg, 1870 is a synonym of P. cacicus. Waterhouse (1872) is considered the author of the designation of the lectotype for Prionacalus iphis. The designation of a lectotype for P. whymperi by Quentin and Villiers is considered invalid. Lectotypes are designated for P. whymperi, P. buckleyi, and Prionacalus uniformis Waterhouse, 1900. A key to species is provided and all species are figured. C1 [Santos-Silva, Antonio] Univ Sao Paulo, Museu Zool, BR-04218970 Sao Paulo, Brazil. [Nearns, Eugenio H.] USDA, Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Santos-Silva, A (reprint author), Univ Sao Paulo, Museu Zool, Caixa Postal 42-494, BR-04218970 Sao Paulo, Brazil. EM toncriss@uol.com.br; z-com321@eurus.dti.ne.jp; gino@nearns.com RI Museu de Zoologia da USP, MZ-USP/Q-2192-2016 NR 66 TC 0 Z9 0 U1 0 U2 0 PU COLEOPTERISTS SOC PI ATHENS PA UNIV GEORGIA, 413 BIOLOGICAL SCIENCES BUILDING, ATHENS, GA 30602-2603 USA SN 0010-065X EI 1938-4394 J9 COLEOPTS BULL JI Coleopt. Bull. PD SEP PY 2013 VL 67 IS 3 BP 201 EP 240 PG 40 WC Entomology SC Entomology GA 235HJ UT WOS:000325707600001 ER PT J AU Russell, PS Grant, JA Williams, KK Carter, LM Garry, WB Daubar, IJ AF Russell, Patrick S. Grant, John A. Williams, Kevin K. Carter, Lynn M. Garry, W. Brent Daubar, Ingrid J. TI Ground penetrating radar geologic field studies of the ejecta of Barringer Meteorite Crater, Arizona, as a planetary analog SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Impact ejecta; GPR; Meteor Crater; Size-frequency distribution; Mars; Moon ID SIZE-FREQUENCY DISTRIBUTIONS; MARS EXPLORATION; ELECTROMAGNETIC PROPAGATION; MARTIAN SUBSURFACE; BRITTLE SOLIDS; FRAGMENT SIZE; LAVA FLOWS; GPR; SCATTERING; FRACTURE AB Ground penetrating radar (GPR) has been a useful geophysical tool in investigating a variety of shallow subsurface geological environments on Earth. Here we investigate the capabilities of GPR to provide useful geologic information in one of the most common geologic settings of planetary surfaces, impact crater ejecta. Three types of ejecta are surveyed with GPR at two wavelengths (400MHz, 200MHz) at Meteor Crater, Arizona, with the goal of capturing the GPR signature of the subsurface rock population. In order to ground truth the GPR characterization, subsurface rocks are visually counted and measured in preexisting subsurface exposures immediately adjacent to and below the GPR transect. The rock size-frequency distribution from 10 to 50cm based on visual counts is well described by both power law and exponential functions, the former slightly better, reflecting the control of fragmentation processes during the impact-ejection event. GPR counts are found to overestimate the number of subsurface rocks in the upper meter (by a factor of 2-3x) and underestimate in the second meter of depth (0.6-1.0x), results attributable to the highly scattering nature of blocky ejecta. Overturned ejecta that is fractured yet in which fragments are minimally displaced from their complement fragments produces fewer GPR returns than well-mixed ejecta. The use of two wavelengths and division of results into multiple depth zones provides multiple aspects by which to characterize the ejecta block population. Remote GPR measurement of subsurface ejecta in future planetary situations with no subsurface exposure can be used to characterize those rock populations relative to that of Meteor Crater. C1 [Russell, Patrick S.; Grant, John A.] Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Williams, Kevin K.] SUNY Buffalo State, Dept Earth Sci & Sci Educ, Buffalo, NY USA. [Carter, Lynn M.; Garry, W. Brent] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Daubar, Ingrid J.] Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Russell, PS (reprint author), Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, MRC 315,POB 37012, Washington, DC 20013 USA. EM russellp@si.edu RI Carter, Lynn/D-2937-2012; Garry, Brent/I-5920-2013 FU NASA Lunar Science Institute [NNA09DB31A] FX Many thanks to D. Kring, B. Andes, and the Barringer family for access and guidance in performing research in the unique environment of Meteor Crater. Appreciation is given for the time taken by Gwen Bart and an anonymous reviewer for their helpful comments on the manuscript. This research was carried out as part of the NASA Lunar Science Institute team led by D. B. J. Bussey, Award #NNA09DB31A. NR 79 TC 1 Z9 1 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD SEP PY 2013 VL 118 IS 9 BP 1915 EP 1933 DI 10.1002/jgre.20145 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 234FT UT WOS:000325628300013 ER PT J AU Grocholski, B Shim, SH Prakapenka, VB AF Grocholski, B. Shim, S. -H. Prakapenka, V. B. TI Stability, metastability, and elastic properties of a dense silica polymorph, seifertite SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article DE seifertite; silica; Shergotty meteorite; lowermost mantle ID X-RAY-DIFFRACTION; POST-PEROVSKITE PHASE; EQUATION-OF-STATE; LOWER-MANTLE PRESSURES; DIAMOND-ANVIL CELL; SUBDUCTED BASALTIC CRUST; EARTHS LOWERMOST MANTLE; CRYSTAL-STRUCTURE; INDUCED TRANSFORMATIONS; SHERGOTTY METEORITE AB Dense silica polymorphs with sixfold coordinated Si have been found in SNC and lunar meteorites and may be important minerals for silica-rich components in the lower mantle. However, the stable crystal structure in the lower mantle and properties of dense silica remain controversial. Under stable heating and quasi-hydrostatic stress conditions, we found that the CaCl2 type undergoes a phase transition to the -PbO(2)type (seifertite) at 130-140GPa and 2500K. Our data suggest that this phase transition occurs at a greater depth than the perovskite postperovskite transition in the lowermost mantle. The molar volume measured at 1bar is the smallest among the reported silica polymorphs, therefore having the highest calculated density and in excellent agreement with recent first-principles calculations. The greater molar volume of seifertite found in the shergottite meteorite and previous experiments supports a metastable synthesis of the phase outside its stability field. Our data combined with the Hugoniots of silica polymorphs also rule out the possibility of the formation of seifertite in the meteorite within its stability field. We found very little change in bulk sound speed across the CaCl2-type seifertite transition. If shear wave velocity decreases at the transition to seifertite as suggested by some computational studies, this silica transition may provide an alternative explanation for the discontinuities with a shear wave velocity decrease found at depths greater than the Ddiscontinuity. C1 [Grocholski, B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Shim, S. -H.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Prakapenka, V. B.] Univ Chicago, GeoSoilEnviroCARS, Argonne, IL USA. RP Grocholski, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, 10th & Constitut Ave, Washington, DC 20560 USA. EM b.grocholski@gmail.com OI Shim, Sang-Heon/0000-0001-5203-6038 FU National Science Foundation-Earth Sciences [EAR-1128799]; Department of Energy-Geosciences [DE-FG02-94ER14466]; U. S. Department of Energy, Office of Science, Office of Basic Energy Sciences [DE-AC02-06CH11357]; NSF [EAR1301813]; Peter Buck Fellowship at the National Museum of Natural History, Smithsonian Institution FX We would like to thank three anonymous reviewers for helpful suggestions that greatly improved the manuscript. This work was performed at GeoSoilEnviroCARS (Sector 13), Advanced Photon Source (APS), Argonne National Laboratory. GeoSoilEnviroCARS is supported by the National Science Foundation-Earth Sciences (EAR-1128799) and Department of Energy-Geosciences (DE-FG02-94ER14466). Use of the Advanced Photon Source was supported by the U. . Department of Energy, Office of Science, Office of Basic Energy Sciences, under contract DE-AC02-06CH11357. This work is supported by NSF to S.H.S. (EAR1301813) with additional support to B.G. from the Peter Buck Fellowship at the National Museum of Natural History, Smithsonian Institution. NR 92 TC 6 Z9 6 U1 2 U2 30 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD SEP PY 2013 VL 118 IS 9 BP 4745 EP 4757 DI 10.1002/jgrb.50360 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 233FP UT WOS:000325553000005 ER PT J AU Cho, YS Hu, L Hou, HL Lee, H Xu, JH Kwon, S Oh, S Kim, HM Jho, S Kim, S Shin, YA Kim, BC Kim, H Kim, CU Luo, SJ Johnson, WE Koepfli, KP Schmidt-Kuntzel, A Turner, JA Marker, L Harper, C Miller, SM Jacobs, W Bertola, LD Kim, TH Lee, S Zhou, Q Jung, HJ Xu, X Gadhvi, P Xu, PW Xiong, YQ Luo, YD Pan, SK Gou, CY Chu, XH Zhang, JL Liu, SY He, J Chen, Y Yang, LF Yang, YL He, JJ Liu, S Wang, JY Kim, CH Kwak, H Kim, JS Hwang, S Ko, J Kim, CB Kim, S Bayarlkhagva, D Paek, WK Kim, SJ O'Brien, SJ Wang, J Bhak, J AF Cho, Yun Sung Hu, Li Hou, Haolong Lee, Hang Xu, Jiaohui Kwon, Soowhan Oh, Sukhun Kim, Hak-Min Jho, Sungwoong Kim, Sangsoo Shin, Young-Ah Kim, Byung Chul Kim, Hyunmin Kim, Chang-uk Luo, Shu-Jin Johnson, Warren E. Koepfli, Klaus-Peter Schmidt-Kuentzel, Anne Turner, Jason A. Marker, Laurie Harper, Cindy Miller, Susan M. Jacobs, Wilhelm Bertola, Laura D. Kim, Tae Hyung Lee, Sunghoon Zhou, Qian Jung, Hyun-Ju Xu, Xiao Gadhvi, Priyvrat Xu, Pengwei Xiong, Yingqi Luo, Yadan Pan, Shengkai Gou, Caiyun Chu, Xiuhui Zhang, Jilin Liu, Sanyang He, Jing Chen, Ying Yang, Linfeng Yang, Yulan He, Jiaju Liu, Sha Wang, Junyi Kim, Chul Hong Kwak, Hwanjong Kim, Jong-Soo Hwang, Seungwoo Ko, Junsu Kim, Chang-Bae Kim, Sangtae Bayarlkhagva, Damdin Paek, Woon Kee Kim, Seong-Jin O'Brien, Stephen J. Wang, Jun Bhak, Jong TI The tiger genome and comparative analysis with lion and snow leopard genomes SO NATURE COMMUNICATIONS LA English DT Article ID INITIAL SEQUENCE; TASMANIAN DEVIL; HIGH-ALTITUDE; ALIGNMENT; ADAPTATION; INSIGHTS; DATABASE; TOOL; CONSERVATION; TRANSCRIPTS AB Tigers and their close relatives (Panthera) are some of the world's most endangered species. Here we report the de novo assembly of an Amur tiger whole-genome sequence as well as the genomic sequences of a white Bengal tiger, African lion, white African lion and snow leopard. Through comparative genetic analyses of these genomes, we find genetic signatures that may reflect molecular adaptations consistent with the big cats' hypercarnivorous diet and muscle strength. We report a snow leopard-specific genetic determinant in EGLN1 (Met39 > Lys39), which is likely to be associated with adaptation to high altitude. We also detect a TYR260G > A mutation likely responsible for the white lion coat colour. Tiger and cat genomes show similar repeat composition and an appreciably conserved synteny. Genomic data from the five big cats provide an invaluable resource for resolving easily identifiable phenotypes evident in very close, but distinct, species. C1 [Cho, Yun Sung; Kim, Hak-Min; Jho, Sungwoong; Shin, Young-Ah; Kim, Byung Chul; Kim, Chang-uk; Lee, Sunghoon; Gadhvi, Priyvrat; Kim, Jong-Soo; Bhak, Jong] Genome Res Fdn, Personal Genom Inst, Suwon 443270, South Korea. [Hu, Li; Hou, Haolong; Xu, Jiaohui; Zhou, Qian; Xu, Pengwei; Xiong, Yingqi; Luo, Yadan; Pan, Shengkai; Gou, Caiyun; Chu, Xiuhui; Zhang, Jilin; Liu, Sanyang; He, Jing; Chen, Ying; Yang, Linfeng; Yang, Yulan; He, Jiaju; Liu, Sha; Wang, Junyi; Wang, Jun] BGI Shenzhen, Shenzhen 518083, Peoples R China. [Lee, Hang] Seoul Natl Univ, Tiger & Leopard Conservat Fund Korea, Seoul 151742, South Korea. [Lee, Hang] Seoul Natl Univ, Coll Vet Med, Seoul 151742, South Korea. [Kwon, Soowhan; Oh, Sukhun] Samsung Everland Zoo, Yongin 449715, South Korea. [Kim, Sangsoo] Soongsil Univ, Sch Syst Biomed Sci, Seoul 156743, South Korea. [Kim, Byung Chul; Kim, Hyunmin; Kim, Tae Hyung; Lee, Sunghoon; Jung, Hyun-Ju; Kim, Chul Hong; Kwak, Hwanjong; Ko, Junsu; Kim, Seong-Jin; Bhak, Jong] TheragenEtex, Theragen BiO Inst, Suwon 443270, South Korea. [Luo, Shu-Jin; Xu, Xiao] Peking Univ, Sch Life Sci, Peking Tsinghua Ctr Life Sci, Beijing 100871, Peoples R China. [Johnson, Warren E.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Koepfli, Klaus-Peter; O'Brien, Stephen J.] St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. [Schmidt-Kuentzel, Anne] Cheetah Conservat Fund, Life Technol Conservat Genet Lab, Otjiwarongo 9000, Namibia. [Turner, Jason A.] Tsau Conservancy, Global White Lion Protect Trust, ZA-1380 Limpopo, South Africa. [Marker, Laurie] Cheetah Conservat Fund, Otjiwarongo 9000, Namibia. [Harper, Cindy; Miller, Susan M.] Univ Pretoria, Fac Vet Sci, Vet Genet Lab, ZA-0110 Onderstepoort, South Africa. [Miller, Susan M.] Tshwane Univ Technol, Nat Conservat Dept, ZA-0001 Pretoria, South Africa. [Jacobs, Wilhelm] Ukutula Lodge & Lion Ctr, ZA-0250 Brits, Northwest Provi, South Africa. [Bertola, Laura D.] Leiden Univ, Inst Environm Sci CML, NL-2300 RA Leiden, Netherlands. [Hwang, Seungwoo] Korea Res Inst Biosci & Biotechnol, Korean Bioinformat Ctr, Taejon 305806, South Korea. [Kim, Chang-Bae] Sangmyung Univ, Dept Life Sci, Seoul 110743, South Korea. [Kim, Sangtae] Sungshin Womens Univ, Dept Biol, Seoul 142732, South Korea. [Bayarlkhagva, Damdin] Natl Univ Mongolia, Sch Biol & Biotechnol, Dept Mol Biol & Genet, Ulaanbaatar 210646A, Mongol Peo Rep. [Paek, Woon Kee] Natl Sci Museum, Taejon 305705, South Korea. [Kim, Seong-Jin] CHA Univ, CHA Canc Inst, Seoul 135081, South Korea. [O'Brien, Stephen J.] Nova SE Univ, Oceanog Ctr, Ft Lauderdale, FL 33004 USA. [Wang, Jun] Univ Copenhagen, Dept Biol, DK-2200 Copenhagen, Denmark. [Wang, Jun] King Abdulaziz Univ, Jeddah 21589, Saudi Arabia. [Bhak, Jong] Adv Inst Convergence Technol Nano Sci & Technol, Suwon 443270, South Korea. [Bhak, Jong] Seoul Natl Univ, Dept Transdisciplinary Studies, Program Nano Sci & Technol, Suwon 443270, South Korea. RP O'Brien, SJ (reprint author), St Petersburg State Univ, Theodosius Dobzhansky Ctr Genome Bioinformat, St Petersburg 199034, Russia. EM lgdchief@gmail.com; wangj@genomics.cn; jongbhak@genomics.org RI Wang, Jun/C-8434-2016; Johnson, Warren/D-4149-2016; Kim, Hak-Min/G-6012-2016; Wang, Jun/B-9503-2016; OI Cho, Yun Sung/0000-0003-4490-8769; Wang, Jun/0000-0002-8540-8931; Bertola, Laura/0000-0002-3445-0355; Johnson, Warren/0000-0002-5954-186X; Kim, Hak-Min/0000-0001-6066-2469; Zhang, Jilin/0000-0002-9976-1605; O'Brien, Stephen J./0000-0001-7353-8301; Wang, Jun/0000-0002-2113-5874; Hou, Haolong/0000-0002-3870-7226 FU Industrial Strategic Technology Development Program [10040231]; Ministry of Knowledge Economy (MKE, Korea); National Research Foundation of Korea [NRF-2011-0019745]; Ministry of Science, ICT & Future Planning (MSIP), Republic of Korea [2012R1A1A2043851, NRF-2008-2004707]; Russian Ministry of Science Mega-grant [11.G34.31.0068] FX This work was supported by the Industrial Strategic Technology Development Program, 10040231, 'Bioinformatics platform development for next generation bioinformation analysis' funded by the Ministry of Knowledge Economy (MKE, Korea). This work was partly supported by the National Research Foundation of Korea (NRF-2011-0019745) and grants from the Ministry of Science, ICT & Future Planning (MSIP), Republic of Korea (2012R1A1A2043851 and NRF-2008-2004707). This research was also supported in part by Russian Ministry of Science Mega-grant no.11.G34.31.0068; SJ O'Brien Principal Investigator. Scaffolds (sequence data) and gene sets are available at http://tigergenome.org. We thank Dr Rui-Qiang Li for contributing to the manuscript. We thank Maryana Bhak for editing. Authors thank many people not listed as authors who gave us feedback, samples and encouragement, especially Won-shik Min. This project was initiated with the generous support of TheragenEtex, Seong-Jin Kim and Jin-Up Goh. We thank the following people and organization for providing valuable samples, data and time for this project: Johannesburg Zoo, in particular Director Dominic Moss for pedigree information and permission to use samples, Janine Fearon and Lucia Muuhlu for laboratory work done at the Life Technologies Conservation Genetics Laboratory of the Cheetah Conservation Fund, Ukutula Lodge & Lion Centre, Global White Lion Protection Trust and Tsau Conservancy, Bhagavan "Doc" Antle from Tiger's Preserve, Myrtle Beach, and Ouwehands Dierenpark for contributing to this project with their lion population, Dr Carlos Driscoll for making one control sample (PLE171) available to this project, and Life Technologies and Biomatters for generous support with software (Life Technologies and Geneious) and equipment (Life Technologies) of the Genetics Laboratory at the Cheetah Conservation Fund. Finally, we thank the many conservationists who have helped protect endangered big cats throughout the world. NR 50 TC 51 Z9 57 U1 22 U2 162 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD SEP PY 2013 VL 4 AR 2433 DI 10.1038/ncomms3433 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 232ZM UT WOS:000325533700030 PM 24045858 ER PT J AU Ross, CN Power, ML Artavia, JM Tardif, SD AF Ross, Corinna N. Power, Michael L. Artavia, Joselyn M. Tardif, Suzette D. TI Relation of Food Intake Behaviors and Obesity Development in Young Common Marmoset Monkeys SO OBESITY LA English DT Article ID LOW-INCOME MOTHERS; CALLITHRIX-JACCHUS; GROWTH; CHILDREN; CHILDHOOD; NUTRITION; PRIMATE; RISK; PREVENTION; ORIGINS AB Objective: Increasing prevalence of childhood obesity and associated risks of adult type disease have led to worldwide concern. It remains unclear how genetic predisposition, environmental exposure to obesogenic food, and developmental programming interact to lead to overweight and obese children. The development of a nonhuman primate model of obesity, and particularly juvenile obesity, is an important step to elucidating the factors associated with obesity and evaluating intervention strategies. Design and Methods: Infant marmosets were followed from birth to 12 months of age. Feeding phenotypes were determined through the use of behavioral observation, solid food intake trials, and liquid feeding trials monitored via lickometer. Results: Marmosets found to be obese at 12 months of age (more than 14%body fat) start consuming solid food sooner and initiate more time off of care givers. These individuals developed stable feeding phenotypes that included being more efficient consumers during liquid intake trials, drinking more grams of diet per contact with the licksit. Conclusions: The weaning process appears to be particularly important in the development of feeding phenotypes and the development of juvenile obesity for the marmosets, and thus this is the time that should be focused upon for intervention testing in both nonhuman primates and children. C1 [Ross, Corinna N.; Artavia, Joselyn M.; Tardif, Suzette D.] Univ Texas Hlth Sci Ctr San Antonio, Dept Cellular & Struct Biol, Barshop Inst Longev & Aging, San Antonio, TX USA. [Power, Michael L.] Smithsonian Conservat Biol Inst, Nutr Lab, Conservat Ecol Ctr, Natl Zool Pk, Washington, DC USA. [Power, Michael L.] Amer Coll Obstetricians & Gynecologists, Res Dept, Washington, DC 20024 USA. RP Ross, CN (reprint author), Univ Texas Hlth Sci Ctr San Antonio, Dept Cellular & Struct Biol, Barshop Inst Longev & Aging, San Antonio, TX USA. EM rossc4@uthscsa.edu OI Power, Michael/0000-0002-6120-3528 FU NIH [R01 DK077639] FX This study was supported by a grant from NIH: R01 DK077639. NR 39 TC 6 Z9 6 U1 2 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1930-7381 EI 1930-739X J9 OBESITY JI Obesity PD SEP PY 2013 VL 21 IS 9 BP 1891 EP 1899 DI 10.1002/oby.20432 PG 9 WC Endocrinology & Metabolism; Nutrition & Dietetics SC Endocrinology & Metabolism; Nutrition & Dietetics GA 231ON UT WOS:000325426600050 PM 23512878 ER PT J AU Carvalho, MR Wilf, P Hermsen, EJ Gandolfo, MA Cuneo, NR Johnson, KR AF Carvalho, Monica R. Wilf, Peter Hermsen, Elizabeth J. Gandolfo, Maria A. Ruben Cuneo, N. Johnson, Kirk R. TI FIRST RECORD OF TODEA (OSMUNDACEAE) IN SOUTH AMERICA, FROM THE EARLY EOCENE PALEORAINFORESTS OF LAGUNA DEL HUNCO (PATAGONIA, ARGENTINA) SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE biogeography; fossil; Gondwana; Laguna del Hunco; Osmundaceae; phylogeny; Todea; Todites ID WESTERN NORTH-AMERICA; MIDDLE TRIASSIC FLORA; ADDITIONAL EVIDENCE; MACROFOSSIL RECORD; FERNS CLADOPHLEBIS; LIVINGSTON ISLAND; PLANT DIVERSITY; EXTANT FERNS; NEW-ZEALAND; BOTANY BAY AB Premise of the Study: The early Eocene Laguna del Hunco caldera-lake paleoflora (ca. 52 Ma) from Chubut Province, Argentina, is notably diverse and includes many conifer and angiosperm lineages that are extinct in South America but extant in Australasian rainforests. No ferns have been previously described from Laguna del Hunco. We describe and interpret a new species of fossil Osmundaceae based on fertile and sterile pinnae. Methods: The fossil specimens were compared with other extant and fossil Osmundaceae based on living and herbarium material and published descriptions. A morphological matrix based on 29 characters was constructed for 17 living species in Osmundaceae, four species assigned to the fossil genus Todites, and the new fossil species. Phylogenetic analyses were conducted under parsimony using morphology and total evidence matrices. Key Results: Both the new fossil and the Todites species were consistently resolved within the leptopteroid clade of Osmundaceae, and the new species resolved in a clade with the two living Todea species, which are now restricted to Australia, New Guinea, New Zealand, and southern Africa. Conclusions: Todea amissa sp. nov. is the first record of Todea, living or fossil, in South America and only the second fossil record worldwide. The distribution of extant Todea on Gondwanan continents other than South America is broadly shared with other taxa from Laguna del Hunco, further indicating that a large component of this flora represents a Gondwanic biome that is no longer found on the South American continent. C1 [Carvalho, Monica R.; Gandolfo, Maria A.] Cornell Univ, Dept Plant Biol, LH Bailey Hortorium, Ithaca, NY 14850 USA. [Carvalho, Monica R.; Wilf, Peter] Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. [Hermsen, Elizabeth J.] Ohio Univ, Dept Environm & Plant Biol, Athens, OH 45701 USA. [Ruben Cuneo, N.] Consejo Nacl Invest Cient & Tecn, Museo Paleontol Egidio Feruglio, RA-9100 Trelew, Chubut, Argentina. [Johnson, Kirk R.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Carvalho, MR (reprint author), Cornell Univ, Dept Plant Biol, LH Bailey Hortorium, Ithaca, NY 14850 USA. EM mjr383@cornell.edu FU Schlumberger Faculty for the Future Foundation; National Science Foundation [DEB-0919071, DEB-0918932, DEB-0345750]; David and Lucile Packard Foundation; National Geographic Society [7337-02]; University of Pennsylvania Research Foundation; Andrew W. Mellon Foundation FX The authors thank staff from the Museo Paleontologico Egidio Feruglio, especially M. Caffa, L. Canessa, P. Puerta, L. Reiner, and E. Ruigomez, for field-collection and sample-processing efforts; S. Wing, A. Iglesias, C. Gonzalez, B. Cariglino, R. Horwitt, and the IOPC 2004 field trip for additional collection assistance; E. Ruigomez and A. Iglesias for arduous efforts to obtain international loans; and R. Kooyman for taking M. R. C. and P. W. to the Border Ranges, New South Wales, Australia. M. R. C. thanks the staffs of CANB (B. Lepschi and C. Cargill), NSW (D. Dixon), A (E. Wood), and BH (A. Stalter), two anonymous reviewers, and G. Jordan, R. Carpenter, G. Lim, S. Gunner, and S. Kiuhan for providing comments; F. Herrera for help with the figures; and the Schlumberger Faculty for the Future Foundation for financial support. This project received funding from National Science Foundation (grants DEB-0919071, DEB-0918932, and DEB-0345750 to P. W., M. A. G., and N.R.C.) and the David and Lucile Packard Foundation (to P. W.), as well as early support from National Geographic Society grant 7337-02, the University of Pennsylvania Research Foundation, and the Andrew W. Mellon Foundation (to P.W.). NR 129 TC 15 Z9 16 U1 3 U2 13 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 SEP PY 2013 VL 100 IS 9 BP 1831 EP 1848 DI 10.3732/ajb.1200637 PG 18 WC Plant Sciences SC Plant Sciences GA 228HK UT WOS:000325176400014 PM 24018858 ER PT J AU Manchester, SR Kapgate, DK Wen, J AF Manchester, Steven R. Kapgate, Dashrath K. Wen, Jun TI OLDEST FRUITS OF THE GRAPE FAMILY (VITACEAE) FROM THE LATE CRETACEOUS DECCAN CHERTS OF INDIA SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Deccan; fruits; grapes; Indovitis; Maastrichtian; seeds; Leeoxylon; Vitaceae ID INTERTRAPPEAN BEDS; PHYLOGENETIC ANALYSIS; INTERCONTINENTAL DISJUNCTIONS; SEED MORPHOLOGY; GENE-SEQUENCES; LATE EOCENE; DIPTEROCARPACEAE; CRYPTERONIACEAE; BIOGEOGRAPHY; AMPELOCISSUS AB Premise of the study: Despite the inferred Cretaceous origin of the Vitaceae, fossils of the grape family are relatively young, with the oldest previously known examples limited to the Paleocene of Europe and North America. New fossil evidence indicates that the family was already present in India in the Late Cretaceous (Maastrichtian), about 10-15 million years before the tectonic collision of India with Eurasia. Methods: Fruits and seeds were investigated by serial sections and peels of chert from the Deccan Intertrappean beds of central India, and compared anatomically with those of extant genera. Key results: Indovitis chitaleyae gen. et sp. n. is described based on immature fruits bearing four to six seeds, and isolated mature seeds. The seeds possess paired ventral infolds and a dorsal chalaza, features diagnostic of the order Vitales. Characters of chalaza shape, infold morphology, and seed coat anatomy place I. chitaleyae within Vitaceae and favor a phylogenetic position either sister to the Vitis-Ampelocissus clade or sister to the Ampelopsis-Clematicissus-Rhoicissus clade. Conclusions: Presence of the oldest known vitaceous fossils in the latest Cretaceous of India indicates a previously undocumented Gondwanan history and a possible southern hemisphere origin for the Vitales. An "out-of-India" scenario might explain the relatively sudden appearance of diverse Vitaceae in the Late Paleocene and Early Eocene of the Northern Hemisphere. C1 [Manchester, Steven R.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Kapgate, Dashrath K.] JM Patel Coll, Dept Bot, Bhandara 441904, MS, India. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, MRC166, Washington, DC 20013 USA. RP Manchester, SR (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM steven@ufl.edu FU National Science Foundation [DEB 0743474] FX The authors thank N. R. Sangrame, M. H. Wanjari, and R. W. Ukey for helpful field and laboratory assistance. Images of extant Vitaceae were made available by Iju Chen. Jonathon Bloch provided access to a computer workstation running Avizo software, Selena Smith and Terry Lott provided assistance and advice for the 3-D visualization and virtual sectioning methodology. Specimens from the Cleveland Museum of Natural History were loaned through the courtesy of Carole Camillo and the late Shyamala Chitaley, and Hongshan Wang assisted with curation of specimens deposited at the Florida Museum of Natural History. Helpful review comments were provided by Susana Magallon, Steffi Ickert-Bond, and Bruce Tiffney. This research was funded by National Science Foundation grant DEB 0743474 to S. R. Manchester and J. Wen. NR 50 TC 7 Z9 8 U1 1 U2 15 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 SEP PY 2013 VL 100 IS 9 BP 1849 EP 1859 DI 10.3732/ajb.1300008 PG 11 WC Plant Sciences SC Plant Sciences GA 228HK UT WOS:000325176400015 PM 24036414 ER PT J AU Collin, R Starr, MJ AF Collin, Rachel Starr, Matthew J. TI Comparative Ontogenetic Changes in Enzyme Activity During Embryonic Development of Calyptraeid Gastropods SO BIOLOGICAL BULLETIN LA English DT Article ID TEMPERATURE-MEDIATED PLASTICITY; DIGESTIVE ENZYMES; MARINE-INVERTEBRATES; CREPIDULA-FORNICATA; CRASSOSTREA-GIGAS; SUSPENSION-FEEDERS; LARVAL DEVELOPMENT; HATCHING SIZE; EGG SIZE; EVOLUTION AB A modification of a semi-quantitative color-based enzyme assay was used to quantify the activity of 19 enzymes (5 peptidases, 3 lipases, 3 phosphotases, and 8 carbohydrases) during five stages of development in eight species of calyptraeid gastropods. Sixteen of the 19 enzymes showed a significant effect of mode of development on the concentration of the reaction product after incubation of homogenates standardized for protein content. The overall pattern was that planktotrophs showed the highest activities, followed by adelphophages, and nonfeeding embryos, which had the lowest enzyme activities. Thirteen enzymes showed significant differences across developmental stages. Of these, eight showed a clear increase during development. Only one of the enzymes showed a sudden jump in activity between the unfed, pre-hatching stage and post-hatching stages that were fed Isochrysis galbana. In three cases, ANOVA identified two exclusive, significantly different groups of species. In naphthol-AS-BI-phosphohydrolase, the measured absorbance of Crucibulum spinosum samples was significantly higher than in all of the other species. The activity of alpha-fucosidase in Crepipatella occulta was significantly greater than in the other seven species. Finally, the activity of beta-galactosidase was significantly higher in C. occulta, Crucibulum spinosum, and Bostrycapulus calyptraeformis than in the four Crepidula species. This is the only enzyme for which there is an indication of a phylogenetic effect. Relative enzyme activities were similar to those reported for other herbivorous gastropods, with the three phosphohydrolases, four carbohydrases (beta-galactosidase, beta-glucuronidase, N-acetyl-beta-glucosaminidase, and alpha-fucosidase), and leucine arylamidase showing high activities. C1 [Collin, Rachel; Starr, Matthew J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Starr, Matthew J.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. RP Collin, R (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM collinr@si.edu OI Collin, Rachel/0000-0001-5103-4460 FU United States National Science Foundation [IOS-1019727] FX We thank members of the Collin Lab for help in the laboratory and field; the staff of the Smithsonian Marine Station who provided logistic support in Florida; and the government of Panama, which issued collecting and import permits. This is Smithsonian Marine Station at Fort Pierce, Florida, Contribution No. 922. This work was supported by a United States National Science Foundation grant IOS-1019727 to RC. NR 45 TC 2 Z9 2 U1 1 U2 9 PU MARINE BIOLOGICAL LABORATORY PI WOODS HOLE PA 7 MBL ST, WOODS HOLE, MA 02543 USA SN 0006-3185 J9 BIOL BULL-US JI Biol. Bull. PD SEP PY 2013 VL 225 IS 1 BP 8 EP 17 PG 10 WC Biology; Marine & Freshwater Biology SC Life Sciences & Biomedicine - Other Topics; Marine & Freshwater Biology GA 227CK UT WOS:000325085600002 PM 24088792 ER PT J AU He, FL Hubbell, S AF He, Fangliang Hubbell, Stephen TI Estimating extinction from species-area relationships: why the numbers do not add up SO ECOLOGY LA English DT Article DE conservation biology; endemics-area relationship; extinction; Pasoh Nature Reserve; Malaysia; power-law model; species-area relationships (SAR) ID CONSERVATION OPPORTUNITY; BRAZILIAN AMAZON; SCALE DEPENDENCE; DIVERSITY; BIODIVERSITY; PATTERNS; IMPACTS; WINDOWS; FOREST; DEBT AB Researchers commonly use species-area relationships (SAR) to estimate extinction rates caused by habitat loss by reversing the SAR, extrapolating backward from area to calculate expected species loss. We have previously shown that the backward SAR method considerably overestimates extinction rates due to a previously unrecognized sampling artifact. Jacob Bock Axelsen, Uri Roll, Lewi Stone, and Andrew Solow recently argued that the backward SAR method is correct and the method does not overestimate extinction rates. In this paper, we further elaborate and clarify our previous results. We show that the backward SAR method gives the correct extinction rate only under a strict complementary-area sampling design, which is not used in practice because it requires knowing which species are endemic to the area of destroyed habitat, or the number of species in the complementary area. Because of this problem, researchers substitute a power-law model for the SAR in the backward SAR equation. However, this substitution violates the backward SAR method's requirement for complementary sampling. With this model substitution, the backward SAR equation is no longer correct, except in the special case of randomly distributed species. For the complementary sampling or random distribution of species, the first individual of a species to be encountered and the last individual to be encountered to lose the species are exchangeable (or the same individual). But this is not the case for other sampling designs or if species are not randomly distributed and explains why the backward SAR method fails to correctly estimate extinction rates. Our proofs and results are general and explain the widely recognized overestimation of extinction by the backward SAR method. We suggest future directions for developing general theory for estimating species extinction from species-area relationships. Until then, however, the backward SAR method should not be used to estimate species extinction in practice. C1 [He, Fangliang] Sun Yat Sen Univ, State Key Lab Biocontrol, SYSU Alberta Joint Lab Biodivers Conservat, Guangzhou 510275, Guangdong, Peoples R China. [He, Fangliang] Sun Yat Sen Univ, Sch Life Sci, Guangzhou 510275, Guangdong, Peoples R China. [He, Fangliang] Univ Alberta, Dept Renewable Resources, Edmonton, AB T6G 2H1, Canada. [Hubbell, Stephen] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Unit 0948, Apo Aa 340020948, Panama. RP He, FL (reprint author), Sun Yat Sen Univ, State Key Lab Biocontrol, SYSU Alberta Joint Lab Biodivers Conservat, Guangzhou 510275, Guangdong, Peoples R China. EM fhe@ualberta.ca FU Sun Yat-sen University; Natural Sciences and Engineering Research Council (Canada); NASA (National Aeronautics and Space Administration); U.S. National Science Foundation FX We thank the authors of Axelsen et al. (2013) for their contribution to the discussion of this topic, which has given us the opportunity to clarify the exact meaning of our theoretical findings on species-area relationships and extinction. This work was supported by Sun Yat-sen University, the Natural Sciences and Engineering Research Council (Canada), NASA (National Aeronautics and Space Administration), and the U.S. National Science Foundation. NR 26 TC 8 Z9 8 U1 5 U2 78 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD SEP PY 2013 VL 94 IS 9 BP 1905 EP 1912 DI 10.1890/12-1795.1 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 219TL UT WOS:000324532900003 PM 24279261 ER PT J AU Hubbell, SP AF Hubbell, Stephen P. TI Tropical rain forest conservation and the twin challenges of diversity and rarity SO ECOLOGY AND EVOLUTION LA English DT Article DE tropical forest conservation; tropical tree rarity ID NEUTRAL THEORY; DISTRIBUTIONS; PATTERNS; SYSTEMS; FUTURE; AMAZON; MODEL AB Data from a global network of large, permanent plots in lowland tropical forests demonstrate (1) that the phenomenon of tropical tree rarity is real and (2) that almost all the species diversity in such forests is due to rare species. Theoretical and empirically based reasoning suggests that many of these rare species are not as geographically widespread as previously thought. These findings suggest that successful strategies for conserving global tree diversity in lowland tropical forests must pay much more attention to the biogeography of rarity, as well as to the impact of climate change on the distribution and abundance of rare species. Because the biogeography of many tropical tree species is poorly known, a high priority should be given to documenting the distribution and abundance of rare tropical tree species, particularly in Amazonia, the largest remaining tropical forested region in the world. C1 [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Hubbell, Stephen P.] Smithsonian Trop Res Inst, Ctr Trop Forest Sci, Washington, DC 20521 USA. RP Hubbell, SP (reprint author), Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. EM shubbell@eeb.ucla.edu FU National Science Foundation [DEB-0640386, DEB-0425651, DEB-0346488, DEB-0129874, DEB-00753102, DEB-9909347, DEB-9615226, DEB-9405933, DEB-9221033, DEB-9100058, DEB-8906869, DEB-8605042, DEB-8206992, DEB-7922197] FX The BCI portion of this research 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, and DEB-7922197. NR 25 TC 9 Z9 10 U1 3 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD SEP PY 2013 VL 3 IS 10 BP 3263 EP 3274 DI 10.1002/ece3.705 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 224ZR UT WOS:000324932600006 PM 24223266 ER PT J AU Lyson, TR Bhullar, BAS Bever, GS Joyce, WG de Queiroz, K Abzhanov, A Gauthier, JA AF Lyson, Tyler R. Bhullar, Bhart-Anjan S. Bever, Gabe S. Joyce, Walter G. de Queiroz, Kevin Abzhanov, Arhat Gauthier, Jacques A. TI Homology of the enigmatic nuchal bone reveals novel reorganization of the shoulder girdle in the evolution of the turtle shell SO EVOLUTION & DEVELOPMENT LA English DT Article ID PHYLOGENETIC-RELATIONSHIPS; AMNIOTE PHYLOGENY; SISTER GROUP; FOSSILS; POSITION; ORIGIN; INTERRELATIONSHIPS; KAYENTACHELYS; TRIONYCHIDAE; MUSCULATURE AB The turtle shell represents a unique modification of the ancestral tetrapod body plan. The homologies of its approximately 50 bones have been the subject of debate for more than 200 years. Although most of those homologies are now firmly established, the evolutionary origin of the dorsal median nuchal bone of the carapace remains unresolved. We propose a novel hypothesis in which the nuchal is derived from the paired, laterally positioned cleithradorsal elements of the ancestral tetrapod pectoral girdle that are otherwise retained among extant tetrapods only in frogs. This hypothesis is supported by origin of the nuchal as paired, mesenchymal condensations likely derived from the neural crest followed by a unique two-stage pattern of ossification. Further support is drawn from the establishment of the nuchal as part of a highly conserved muscle scaffold wherein the cleithrum (and its evolutionary derivatives) serves as the origin of the Musculus trapezius. Identification of the nuchal as fused cleithra is congruent with its general spatial relationships to other elements of the shoulder girdle in the adult morphology of extant turtles, and it is further supported by patterns of connectivity and transformations documented by critical fossils from the turtle stem group. The cleithral derivation of the nuchal implies an anatomical reorganization of the pectoral girdle in which the dermal portion of the girdle was transformed from a continuous lateral-ventral arc into separate dorsal and ventral components. This transformation involved the reduction and eventual loss of the scapular rami of the clavicles along with the dorsal and superficial migration of the cleithra, which then fused with one another and became incorporated into the carapace. C1 [Lyson, Tyler R.; Bhullar, Bhart-Anjan S.; Bever, Gabe S.; Gauthier, Jacques A.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06511 USA. [Bhullar, Bhart-Anjan S.; Abzhanov, Arhat] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Bever, Gabe S.] Coll Osteopath Med, New York Inst Technol, Dept Anat, New York, NY USA. [Bever, Gabe S.] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Joyce, Walter G.] Univ Tubingen, Dept Geosci, D-72074 Tubingen, Germany. [Lyson, Tyler R.; Joyce, Walter G.; Gauthier, Jacques A.] Yale Peabody Museum Nat Hist, Div Vertebrate Paleontol, New Haven, CT 06511 USA. [Lyson, Tyler R.; de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Lyson, TR (reprint author), Yale Univ, Dept Geol & Geophys, POB 6666, New Haven, CT 06511 USA. EM tyler.lyson@gmail.com FU YPM's Divisions of Vertebrate Zoology and Vertebrate Paleontology; NSF Graduate Research Fellowship; NSF grant [EF 0334966]; Yale Institute for Biospheric Studies FX We thank the following people for access to material under their care: B. de Klerk (AM), L. Chun (IVPP), J. Neveling (M), F. Jenkins (MCZ), J. Gillette (MNA), J. Botha-Brink (NMQR), R. Smith (SAM), R. Schoch (SMNS), T. Rowe (TMM), K. Padian (UCMP), R. McDiarmid (USNM), and G. Zug (USNM). G. Watkins-Colwell (YPM) is thanked for assistance with the dissections. T. Scheyer (UZ) provided photos used in Figure 2. Funding for this project was provided by YPM's Divisions of Vertebrate Zoology and Vertebrate Paleontology, NSF Graduate Research Fellowship, NSF grant EF 0334966 "Deep Scaly: Assembling a Tree of Life for Squamata" and the Yale Institute for Biospheric Studies. NR 75 TC 24 Z9 24 U1 2 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1520-541X J9 EVOL DEV JI Evol. Dev. PD SEP PY 2013 VL 15 IS 5 BP 317 EP 325 DI 10.1111/ede.12041 PG 9 WC Evolutionary Biology; Developmental Biology; Genetics & Heredity SC Evolutionary Biology; Developmental Biology; Genetics & Heredity GA 226DF UT WOS:000325013900001 PM 24074278 ER PT J AU Sofaer, HR Chapman, PL Sillett, TS Ghalambor, CK AF Sofaer, Helen R. Chapman, Phillip L. Sillett, T. Scott Ghalambor, Cameron K. TI Advantages of nonlinear mixed models for fitting avian growth curves SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID SIBLING COMPETITION; NESTLING GROWTH; HATCHING ASYNCHRONY; ALTRICIAL BIRDS; FLEDGING SUCCESS; TREE SWALLOWS; CHICK GROWTH; HOUSE FINCH; CLUTCH SIZE; RATES AB Our understanding of avian growth rates can benefit from the use of two statistical approaches that explicitly model the sources of intraspecific variation. First, random effects can evaluate whether there are consistent differences between individuals and groups of siblings within a population, and also account for any lack of statistical independence among data points. Second, nonlinear fixed-effect functions can be extended to test specific biological hypotheses of interest, such as for differences between groups or populations. We illustrate the advantages of these methods by using nonlinear mixed models to study variation in the growth trajectories of nestling orange-crowned warblers Oreothylpis celata. Specifically, we quantify the sources of variation within populations, analyze the effects of asynchronous hatching, and test for a difference in the growth rates of populations in Alaska and California, which are at the northern and southern limits of the species' breeding distribution. We found that growth rates did not consistently vary between nests and individuals within populations and were not affected by asynchronous hatching, but were higher in Alaska than in California. Our extensions of traditional methods allowed us to accurately quantify this difference between populations, which is consistent with life history theory but has rarely been demonstrated in previous comparisons of intraspecific passerine populations. The methods we present can be applied to any taxonomic group and adjusted to fit any nonlinear function, and we provide code and implementation advice to facilitate the use of this analytical framework in future studies. C1 [Sofaer, Helen R.; Ghalambor, Cameron K.] Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. [Sofaer, Helen R.; Ghalambor, Cameron K.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Chapman, Phillip L.] Colorado State Univ, Dept Stat, Ft Collins, CO 80523 USA. [Sillett, T. Scott] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP Sofaer, HR (reprint author), Colorado State Univ, Grad Degree Program Ecol, Ft Collins, CO 80523 USA. EM helen@lamar.colostate.edu FU Nature Conservancy; Smithsonian Instit.; American Ornithologists' Union Graduate Research Award; Frank M. Chapman Memorial Grant from the American Museum of Natural History; NSF-IGERT Grant DGE [0221595]; NSF Grant DEB [0846175] FX Our research was supported by the The Nature Conservancy, the Smithsonian Instit., an American Ornithologists' Union Graduate Research Award, and a Frank M. Chapman Memorial Grant from the American Museum of Natural History. HRS was supported by NSF-IGERT Grant DGE-#0221595 (administered by the PRIMES program at Colorado State Univ.) and NSF Grant DEB-#0846175 to CKG. The Catalina Island Conservancy provided logistical support. We thank users of the R mixed effect models message board for advice. Comments from B. R. Noon, K. M. Pepin, and C. T. Webb improved the manuscript. NR 70 TC 11 Z9 12 U1 3 U2 44 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD SEP PY 2013 VL 44 IS 5 BP 469 EP 478 DI 10.1111/j.1600-048X.2013.05719.x PG 10 WC Ornithology SC Zoology GA 226AG UT WOS:000325005900007 ER PT J AU McKellar, AE Marra, PP Ratcliffe, LM AF McKellar, Ann E. Marra, Peter P. Ratcliffe, Laurene M. TI Starting over: experimental effects of breeding delay on reproductive success in early-arriving male American redstarts SO JOURNAL OF AVIAN BIOLOGY LA English DT Article ID FLYCATCHER FICEDULA-HYPOLEUCA; PENGUIN PYGOSCELIS ANTARCTICA; MIGRATORY BIRD; MATE CHOICE; PARENTAL QUALITY; PIED FLYCATCHER; CLUTCH SIZE; GREAT TITS; SETOPHAGA-RUTICILLA; SEASONAL DECLINE AB Birds that arrive and breed early often have higher reproductive success than late individuals, either as a consequence of timing-specific advantages (the timing hypothesis) or because these individuals and/or their resources are of higher quality (the quality hypothesis). In this study, we examined the potential influence of several factors affecting reproductive success by experimentally delaying breeding of early-arriving male American redstarts Setophaga ruticilla, a species for which early male arrival is strongly related to increased reproductive success. Our manipulation involved the capture, holding, and release of males following pairing and territory establishment, resulting in the majority of subjects (67%) losing their initial mate (47%) or mate and territory (20%) and forcing them to start over approximately 12 d after their initial arrival. Males forced to start over (i.e. those losing their first territory and/or mate) did not experience any decrease in body condition, nor did their reproductive behaviour differ from that of early-arriving control males. We found that naturally early-arriving but experimentally manipulated males suffered reduced fledging success in comparison to early-arriving males that bred early or late, but equivalent success in comparison to males that arrived and bred late. Based on our results, we propose that the relationship between early arrival and higher reproductive success in this species is mediated not simply by individual male quality or absolute arrival timing alone, but rather some other aspect of resource quality is likely important. We discuss and present evidence for two alternative explanations under the quality hypothesis: female quality and territory quality. To our knowledge, our study is the first to investigate the effects of experimentally delaying male breeding time, strengthening previous correlational evidence for resource quality as a potentially important selective agent driving early arrival in migratory birds. C1 [McKellar, Ann E.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Marra, Peter P.] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20013 USA. RP McKellar, AE (reprint author), Univ Missouri, Dept Fisheries & Wildlife Sci, Columbia, MO 65211 USA. EM mckellara@missouri.edu FU J. Fotheringham; Natural Sciences and Engineering Research Council of Canada; National Science Foundation; Animal Behavior Society; American Ornithologists' Union FX We thank C. Crossman, M. Daniel, N. Koomen, R. Kresnick, A. Porter, P. Pulgarin-Restrepo, C. Toth and C. Willis for help in the field and the staff of the Queen's Univ. Biological Station for logistical support. J. Churchill and P. Martin helped with the experimental design, and P. Martin M. Reudink provided insightful comments on the manuscript. Financial support was provided by J. Fotheringham, the Natural Sciences and Engineering Research Council of Canada, the National Science Foundation, the Animal Behavior Society, and the American Ornithologists' Union. All work was performed in accordance with permits from the Queen's Univ. Animal Care Committee (Ratcliffe-2010-006) and CWS (banding permit 10771E and collection permit CA0261). NR 62 TC 6 Z9 6 U1 1 U2 28 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0908-8857 J9 J AVIAN BIOL JI J. Avian Biol. PD SEP PY 2013 VL 44 IS 5 BP 495 EP 503 DI 10.1111/j.1600-048X.2013.00180.x PG 9 WC Ornithology SC Zoology GA 226AG UT WOS:000325005900010 ER PT J AU Pestle, WJ Curet, LA Ramos, RR Lopez, MR AF Pestle, William J. Curet, L. Antonio Ramos, Reniel Rodriguez Lopez, Miguel Rodriguez TI NEW QUESTIONS AND OLD PARADIGMS: REEXAMINING CARIBBEAN CULTURE HISTORY SO LATIN AMERICAN ANTIQUITY LA English DT Article ID PUERTO-RICO; ARCHAEOLOGY; PREHISTORY; SERIATION; AGE AB One of the central goals of archaeology is the definition of regional cultural succession. Since at least the 1960s, archaeology has purported to have moved beyond the strictures of Culture History, and yet the constructs of that paradigm (styles, periods, cultures) continue to be used routinely. This work aims to show that by doing so, one is still implicitly subscribing to that theoretical perspective's assumptions and biases. In the end, this article is intended to be a self-critical assessment of the shortcomings of Caribbean archaeology vis-a-vis issues inherent in that region's dominant culture-history framework. Moreover, it aims to provide an example for Caribbeanists, and archaeologists working in other regions, of the value of moving beyond the products of, and not just beyond the term, Culture History. C1 [Pestle, William J.] Univ Miami, Dept Anthropol, Coral Gables, FL 33124 USA. [Curet, L. Antonio] Smithsonian Inst Cultural Resources Ctr, Natl Museum Amer Indian, Suitland, MD 20746 USA. [Ramos, Reniel Rodriguez] Univ Puerto Rico Utuado, Social Sci Program, Utuado, PR 00641 USA. [Lopez, Miguel Rodriguez] Ctr Estudios Avanzados Puerto Rico & El Caribe, San Juan, PR USA. RP Pestle, WJ (reprint author), Univ Miami, Dept Anthropol, 102E Merrick Hall, Coral Gables, FL 33124 USA. EM w.pestle@miami.edu NR 117 TC 3 Z9 3 U1 0 U2 6 PU SOC AMER ARCHAEOLOGY PI WASHINGTON PA 900 SECOND ST., NE STE 12, WASHINGTON, DC 20002-3557 USA SN 1045-6635 J9 LAT AM ANTIQ JI Lat. Am. Antiq. PD SEP PY 2013 VL 24 IS 3 BP 243 EP 261 PG 19 WC Archaeology SC Archaeology GA 218ON UT WOS:000324442100001 ER PT J AU Falzoni, F Petrizzo, MR MacLeod, KG Huber, BT AF Falzoni, Francesca Petrizzo, Maria Rose MacLeod, Kenneth G. Huber, Brian T. TI Santonian-Campanian planktonic foraminifera from Tanzania, Shatsky Rise and Exmouth Plateau: Species depth ecology and paleoceanographic inferences SO MARINE MICROPALEONTOLOGY LA English DT Article DE Planktonic foraminifera; Late Cretaceous; Stable isotopes; Paleo-habitats; Ecological intervals; Paleoceanography ID SEA-SURFACE TEMPERATURES; STABLE ISOTOPIC SIGNALS; SOUTHERN HIGH-LATITUDES; EASTERN INDIAN-OCEAN; EVOLUTIONARY HISTORY; COASTAL TANZANIA; TROPICAL ATLANTIC; DEMERARA RISE; NW AUSTRALIA; BIOSTRATIGRAPHY AB The Santonian-Campanian interval is of particular interest as it encompasses a cooling trend after the Late Cretaceous greenhouse maximum warmth of the Turonian as well as a possibly related major faunal turnover among planktonic foraminifera. The recovery of pristinely preserved planktonic foraminifera from Santonian-Campanian sequences in southeastern Tanzania allows examination of faunal changes and documentation of species-specific stable isotope (delta C-13 and delta O-18) signatures. These isotopic data are ideal for inferring species paleoecological preferences and for tracing major paleoceanographic changes. This study reports the first delta O-18 and delta C-13 data generated on "glassy" specimens of Marginotruncana coronata, M. undulata, M. marginata, and M. pseudolinneiana and Sigalia carpatica. Additional results from Shatsky Rise (Ocean Drilling Program Leg 198, Hole 1210B) and Exmouth Plateau (ODP Leg 122, Hole 762C) provide geographic control on species habitat preferences and paleoceanographic context. Isotopic analyses suggest that double-keeled species, including Globotruncana bulloides, Contusotruncana fornicata, C. plummerae and probably marginotruncanids, inhabited the surface mixed layer, whereas the biserial Gublerina rajagopalani was a permanent thermocline dweller. Thus, our study confirms recent suggestions that the depth-distribution models based on shell morphology and analogies with modern taxa are not applicable. At all the examined localities, changes in planktonic foraminiferal assemblages are used to define several ecological intervals, each one characterized by a distinctive taxonomic composition and/or increasing/decreasing species diversity. Combined geochemical and paleontological observations suggest that, by the middle-late Campanian, a stratified upper water column developed in Tanzania while less stratified and/or mesotrophic conditions prevailed at Shatsky Rise and Exmouth Plateau. (C) 2013 Elsevier B.V. All rights reserved. C1 [Falzoni, Francesca; Petrizzo, Maria Rose] Univ Milan, Dipartimento Sci Terra A Desio, I-20133 Milan, Italy. [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO USA. [Huber, Brian T.] Smithsonian Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Falzoni, F (reprint author), Univ Milan, Dipartimento Sci Terra A Desio, Via Mangiagalli 34, I-20133 Milan, Italy. EM francesca.falzoni1@gmail.com; mrose.petrizzo@unimi.it; MacLeodK@missouri.edu; HUBERB@si.edu RI MacLeod, Kenneth/C-4042-2017; Petrizzo, Maria Rose/M-8672-2013; OI MacLeod, Kenneth/0000-0002-6016-0837; Petrizzo, Maria Rose/0000-0002-9584-8471; Falzoni, Francesca/0000-0002-5694-9827 FU Cushman Foundation for Foraminiferal Research; Smithsonian Institution; Universita degli Studi di Milano; PUR (Universita degli Studi di Milano, Italy) FX The Tanzania Petroleum Development Corporation and the Tanzania Commission for Science and Technology are acknowledged for logistical support to the drilling expeditions. The Tanzania Drilling Project and the Ocean Drilling Program are thanked for making available the samples for this study. F.F. warmly thanks the Cushman Foundation for Foraminiferal Research (Johanna M. Resig Fellowship), the Smithsonian Institution (Smithsonian Institution Pre-doctoral Fellowship) and the PhD program of the Universita degli Studi di Milano for funding this study. Financial support of PUR 2008 (Universita degli Studi di Milano, Italy) to M.R.P. is acknowledged. NR 76 TC 11 Z9 11 U1 1 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-8398 J9 MAR MICROPALEONTOL JI Mar. Micropaleontol. PD SEP PY 2013 VL 103 BP 15 EP 29 DI 10.1016/j.marmicro.2013.07.003 PG 15 WC Paleontology SC Paleontology GA 228OC UT WOS:000325195100002 ER PT J AU Yasuhara, M Hunt, G Okahashi, H Brandao, SN AF Yasuhara, Moriaki Hunt, Gene Okahashi, Hisayo Brandao, Simone N. TI THE 'OXYCYTHEREIS' PROBLEM: TAXONOMY AND PALAEOBIOGEOGRAPHY OF DEEP-SEA OSTRACOD GENERA PENNYELLA AND RUGOCYTHEREIS SO PALAEONTOLOGY LA English DT Article DE Deep sea; Ostracoda; taxonomy; palaeobiogeography; Pennyella; Rugocythereis ID SUBPOLAR NORTH-ATLANTIC; SOUTHERN-OCEAN; SPECIES-DIVERSITY; INDIAN-OCEAN; PALAEOCEANOGRAPHICAL CHANGES; BATHYAL OSTRACODA; CLIMATE-CHANGE; NEW-ZEALAND; MAUD RISE; CRUSTACEA AB Systematic revision of the globally distributed deep-sea ostracod genera Pennyella Neale, 1974 and Rugocythereis Dingle, Lord and Boomer, 1990, which have been considered to correspond, at least partially, to nomen nudum but widely used genus name 'Oxycythereis,' was conducted to reduce taxonomic uncertainty of these important components of the Modern and fossil deep-sea ostracod community. Approximately 100 specimens from 18 species were examined, ranging in age from the Cretaceous to the present day. Nine new species are described: Pennyella rexi, Pennyella sanfordae, Pennyella liowae, Pennyella schellenbergi, Pennyella majorani, Pennyella iani, Pennyella ayressi, Rugocythereis melonis and Rugocythereis zarikiani. Emended generic concepts of Pennyella and Rugocythereis are proposed, and the palaeobiogeographical distributions of these two genera are discussed. C1 [Yasuhara, Moriaki; Okahashi, Hisayo] Univ Hong Kong, Swire Inst Marine Sci, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China. [Yasuhara, Moriaki; Okahashi, Hisayo] Univ Hong Kong, Dept Earth Sci, Hong Kong, Hong Kong, Peoples R China. [Hunt, Gene] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Brandao, Simone N.] Univ Hamburg, Biozentrum Grindel, D-20146 Hamburg, Germany. [Brandao, Simone N.] Univ Hamburg, Zool Museum, D-20146 Hamburg, Germany. [Brandao, Simone N.] DZMB, D-26382 Wilhelmshaven, Germany. RP Yasuhara, M (reprint author), Univ Hong Kong, Swire Inst Marine Sci, Sch Biol Sci, Hong Kong, Hong Kong, Peoples R China. EM moriakiyasuhara@gmail.com; hunte@si.edu; hisaseal@gmail.com; brandao.sn.100@gmail.com RI Hunt, Gene/B-3783-2010; Brandao, Simone/K-4672-2012 OI Hunt, Gene/0000-0001-6430-5020; FU Seed Funding Programme for Basic Research of the University of Hong Kong [201105159002]; Smithsonian Postdoctoral Fellowship; Smithsonian Marine Science Network Postdoctoral Fellowship; Alexander von Humboldt Stiftung and SYNTHESYS FX We thank T. M. Cronin for providing us specimens and valuable comments; D. Hodell for loaning us ODP 982 core samples; M. A. Ayress for providing us specimens and SEM negatives; C. Sanford for continuous support; S. Whittaker for help in SEM imaging; D. Levin and K. Hollis for help in depositing type and figured specimens; M. Lowe and G. Miller for carefully assisting S.N.B. during her visits to the Natural History Museum, London, and providing access to the ostracod collections housed in the Natural History Museum; K. Swanson, S. Thomas and two anonymous referees for valuable comments. Considerable part of specimens used for this research comes from late R. H. Benson's deep-sea ostracod collection housed in the National Museum of Natural History, Smithsonian Institution. Some samples used for this research were provided by the Integrated Ocean Drilling Program (IODP). This work was supported by the Seed Funding Programme for Basic Research of the University of Hong Kong (project code: 201105159002), Smithsonian Postdoctoral Fellowship and Smithsonian Marine Science Network Postdoctoral Fellowship (to M.Y.) and by the Alexander von Humboldt Stiftung and SYNTHESYS (to S.N.B.). NR 87 TC 2 Z9 2 U1 1 U2 3 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-0239 EI 1475-4983 J9 PALAEONTOLOGY JI Paleontology PD SEP PY 2013 VL 56 IS 5 BP 1045 EP 1080 DI 10.1111/pala.12035 PG 36 WC Paleontology SC Paleontology GA 227AW UT WOS:000325080600008 ER PT J AU Tornabene, L Ahmadia, GN Williams, JT AF Tornabene, Luke Ahmadia, Gabby N. Williams, Jeffrey T. TI Four new species of dwarfgobies (Teleostei: Gobiidae: Eviota) from the Austral, Gambier, Marquesas and Society Archipelagos, French Polynesia SO SYSTEMATICS AND BIODIVERSITY LA English DT Article DE coral reef fish; Gobioidei; Gobiiformes; goby; phylogeny; systematics ID CORAL-REEF FISHES; RYUKYU ISLANDS; PACIFIC-OCEAN; GENUS EVIOTA; GOBY AB Four new species of Eviota (Teleostei: Gobiidae) are described from French Polynesia. Eviota hinanoae occurs from the Gambier, Austral and Society Archipelagos and differs from its closest relatives primarily in sensory pore pattern, having cuplike male urogenital papilla, and in lacking prominent dark pigmentation on the base of the pectoral fin. Three other new species, E. dorsimaculata, E. lacrimosa and E. deminuta, are known only from the Marquesas Islands and are distinguished from congeners by differences in pigmentation, sensory pore pattern, urogenital papilla shape, the number of rays in the dorsal and anal fins, and the length of the fifth pelvic-fin ray. Eviota deminuta represents one of the smallest known species of Eviota and features reductions in several morphological characters, including the loss of all head pores. Three of the new species are included in a phylogenetic analysis based on mitochondrial cytochrome c oxidase-I, along with 21 additional species of Eviota. C1 [Tornabene, Luke] Texas A&M Univ, Coll Sci & Engn, Corpus Christi, TX 78412 USA. [Ahmadia, Gabby N.] World Wildlife Fund, Conservat Sci Program, Washington, DC 20037 USA. [Williams, Jeffrey T.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Div Fishes, Suitland, MD 20746 USA. RP Tornabene, L (reprint author), Texas A&M Univ, Coll Sci & Engn, 6300 Ocean Dr, Corpus Christi, TX 78412 USA. EM luke.tornabene@tamucc.edu FU Agence des Aires Marines Protegees in France; Texas AM University; Centre Plongee Marquises; Fondation TOTAL; Ministere de l'Environnement de Polynesie; Delegation a la Recherche de Polynesie; Mairie of Nuku-Hiva; 'Contrat de projet Etat-Polynesie'; ANR 'IMODEL'; French Ministry for Environment, Sustainable Development and Transport (MEDDTL); Biocode Moorea programme; Jeff Hunt of the Laboratories of Analytical Biology (Smithsonian Institution) FX We thank Frank Murphy, Hinano Murphy and the staff of the Berkeley Gump Station in Moorea for assistance with coordinating fieldwork. The Marquesas specimens were collected during part of the Pakaihi i te Moana expedition organized and funded by the Agence des Aires Marines Protegees in France. Serge Planes organized and led expeditions to French Polynesia that resulted in the collection of representatives of these and other new species. We thank Jocelyn Curtis-Quick for her help in the field. Diane Pitassy at USNM, Dave Catania at CAS and Romain Causse at MNHN helped with deposition of specimens. We gratefully acknowledge Dave Greenfield for helpful discussion, and he and Richard Winterbottom for providing preliminary unpublished dichotomous keys for Eviota species. Fieldwork by LT and GA in Moorea was graciously funded by Frank Pezold and by the Texas A&M University - Corpus Christi International Studies Study Abroad Scholarship. We thank the Centre Plongee Marquises, Xavier (Pipapo) and Marie Curvat, l'Agence des Aires Marines Marine Protegees, the Fondation TOTAL, the Ministere de l'Environnement de Polynesie, the Delegation a la Recherche de Polynesie, the Mairie of Nuku-Hiva, and the people of the Marquesas Islands for their kind and generous support of the project as JTW travelled throughout the islands. The Captain, crew and owner of the M/V "Braveheart' (Marquesas Expedition) and the crew of the M/V "Claymore II' (Gambier Expedition) provided invaluable assistance during those cruises. The Coralspot expedition to Gambier was funded by the 'Contrat de projet Etat-Polynesie', by the ANR 'IMODEL' and the French Ministry for Environment, Sustainable Development and Transport (MEDDTL). We thank Jerry Finan, Erika Wilbur, Shirleen Smith, Kris Murphy, David Smith and Sandra Raredon of the Division of Fishes (National Museum of Natural History) for assistance in expedition preparations and processing specimens. Sandra Raredon and Kris Murphy provided digital and film radiographs. Chris Meyer (USNM) and the Biocode Moorea programme provided funding for the sequencing of tissues from the Gambier collections. Lee Weight, Amy Driskell and Jeff Hunt of the Laboratories of Analytical Biology (Smithsonian Institution) provided support for and assistance with molecular analysis of samples. We are especially grateful to Serge Planes, Erwan Delrieu-Trottin, Tom Cribb, Rene Galzin, Pierre Sasal and Johan Mourier for their field assistance collecting fishes in the Marquesas. We thank Labex 'CORAIL' and the staff of the Centre de Recherche Insulaire et Observatoire de l'Environnement (CRIOBE), Moorea, for logistical support. The Leonard P. Schultz Fund (Division of Fishes, National Museum of Natural History) provided grants in support of fieldwork and museum visits. NR 30 TC 4 Z9 4 U1 0 U2 17 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 1477-2000 EI 1478-0933 J9 SYST BIODIVERS JI Syst. Biodivers. PD SEP 1 PY 2013 VL 11 IS 3 BP 363 EP 380 DI 10.1080/14772000.2013.819822 PG 18 WC Biodiversity Conservation; Biology SC Biodiversity & Conservation; Life Sciences & Biomedicine - Other Topics GA 227OY UT WOS:000325124400007 ER PT J AU Eberhard, WG AF Eberhard, William G. TI The Polysphinctine Wasps Acrotaphus tibialis, Eruga ca. gutfreundi, and Hymenoepimecis tedfordi (Hymenoptera, Ichneumonidae, Pimplinae) Induce Their Host Spiders to Build Modified Webs SO ANNALS OF THE ENTOMOLOGICAL SOCIETY OF AMERICA LA English DT Article DE host manipulation; spider web; polysphinctine wasp ID NEPHILA-CLAVIPES ARANEAE; MANIPULATION; BEHAVIOR; TETRAGNATHIDAE; PARASITOIDS; ARANEIDAE; PHYLOGENY; UCHIDA AB The wasps Acrotaphus tibialis (Cameron), Eruga ca. gutfreundi Gauld, and Hymenoepimecis tedfordi Gauld induce their host spiders to spin modified "cocoon" webs just before they kill them and pupate. The cocoon webs induced by all three wasp species appear better designed to support and protect the waspsO pupal cocoons than are the normal orbs of their hosts. The typical cocoon webs induced by A. tibialis were similar to the protected resting webs built by their host spiders Argiope trifasciata (Forskal) but had more elaborate protective barrier tangles. The other two species of wasp induced the same host spider, Leucauge mariana (Keyserling) to build quite different cocoon webs. The cocoon webs of H. tedfordi varied somewhat, but usually included radial lines and a tangle below. They resembled the resting webs of the host in having a planar radial organization and (often) a tangle below, but lacked a hub and had their lines that were apparently composed of high numbers of individual strands. The three dimensional, radially arranged cocoon web of E. ca. gutfreundi had no clear counterpart in the webs of unparasitized L. mariana. The substantial intraspecific variation in the cocoon webs, especially those of A. tibialis, emphasizes the apparent difficulty of precise host manipulation by these wasps. C1 [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Eberhard, WG (reprint author), Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. EM william.eberhard@gmail.com FU Smithsonian Tropical Research Institute; Universidad de Costa Rica FX I am indebted to Paul Hanson for kindly identifying the wasps and help with literature, to Gilbert Barrantes and Ruth Madrigal-Brenes for help finding parasitized spiders in the field, and to two anonymous reviewers for helpful comments. I am grateful for financial support from the Smithsonian Tropical Research Institute and the Universidad de Costa Rica. NR 25 TC 10 Z9 11 U1 2 U2 25 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0013-8746 EI 1938-2901 J9 ANN ENTOMOL SOC AM JI Ann. Entomol. Soc. Am. PD SEP PY 2013 VL 106 IS 5 BP 652 EP 660 DI 10.1603/AN12147 PG 9 WC Entomology SC Entomology GA 219QF UT WOS:000324522500013 ER PT J AU Pimiento, C Gonzalez-Barba, G Ehret, DJ Hendy, AJW MacFadden, BJ Jaramillo, C AF Pimiento, Catalina Gonzalez-Barba, Gerardo Ehret, Dana J. Hendy, Austin J. W. MacFadden, Bruce J. Jaramillo, Carlos TI SHARKS AND RAYS (CHONDRICHTHYES, ELASMOBRANCHII) FROM THE LATE MIOCENE GATUN FORMATION OF PANAMA SO JOURNAL OF PALEONTOLOGY LA English DT Article ID CENTRAL-AMERICAN SEAWAY; MIDDLE MIOCENE; SOUTH-AMERICA; WHITE SHARK; CARCHARODON LAMNIFORMES; FISH ASSEMBLAGE; WESTERN PANAMA; NEOGENE; ISTHMUS; CLOSURE AB The late Miocene Gatun Formation of northern Panama Contains a highly diverse and well sampled fossil marine assemblage that occupied a shallow-water embayment close to a purported connection between the Pacific and Atlantic (Caribbean) oceans. However, the diverse chondrichthyan fauna has been poorly documented. Based on recent field discoveries and further analysis of existing collections, the chondrichthyan fauna from this unit comprises at least 26 taxa, of which four species are extinct today. The remaining portion of the total chondrichthyan biodiversity has affmities with modern taxa and is therefore comprised of long-lived species. Based on known records of the modern geographic distribution range of the Gatun chondrichthyans, the fauna has mixed biogeographic affinities suggesting that around 10 million yr ago, a connection likely occurred between the Pacific Ocean and the Caribbean Sea. Given the known habitat preferences for modern chondrichthyans, the Gatun fauna was primarily adapted to shallow waters within the neritic zone. Finally, comparisons of Gatun dental measurements with other faunas suggest that many of the taxa have an abundance of small individuals, in agreement with previous studies that proposed this area as a paleonursery habitat for the species Carcharocles megalodon. C1 [Pimiento, Catalina; Hendy, Austin J. W.; MacFadden, Bruce J.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Pimiento, Catalina; Hendy, Austin J. W.; Jaramillo, Carlos] Ctr Trop Paleoecol & Archaeol, Smithsonian Trop Res Inst, Panama City, Panama. [Pimiento, Catalina] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Gonzalez-Barba, Gerardo] Univ Autonoma Baja California Sur, Area Ciencias Mar, Museo Hist Nat, Mexico City 23080, DF, Mexico. [Ehret, Dana J.] Univ Alabama, Alabama Museum Nat Hist, Tuscaloosa, AL 35487 USA. RP Pimiento, C (reprint author), Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. EM pimientoc@ufl.edu; gerardo@uabcs.mx; djehret@ua.edu; ahendy@flmnh.ufl.edu; bmacfadd@flmnh.ufl.edu; jaramilloc@si.edu FU NSF [EAR 0418042, PIRE 0966884]; Autoridad del Canal de Panama contrato [SAA-199520-KRP]; Ricardo Perez S.A., M. Tupper, National Geographic Channel; Smithsonian Institution; Jon A. and Beverly L. Thompson Endowment FX This project was funded by NSF EAR 0418042, PIRE 0966884, Autoridad del Canal de Panama contrato SAA-199520-KRP, Ricardo Perez S.A., M. Tupper, National Geographic Channel, and the Smithsonian Institution. We thank the Direccion de Recursos Minerales of Panama for collecting permits; R. Hulbert, J. Bloch, G. Morgan for beneficial suggestions; G. Hubbell and R. Leder for helping with the identification of the material; A. Rincon, F. Rodriguez, C. De Gracia, and the Panama Canal Project Field Team in the Center for Tropical Paleobiology and Archaeology at STRI for helping with the collection; D. Winkler of SMU and M. Florence of the USNM for access to collections; and M. Shippritt, R. G. Reina, and C. Symister for logistical support. Lastly, we thank J. Ceballos for editing an earlier version of this manuscript, and O. Aguilera and an anonymous reviewer who helped improving it. C. Jaramillo thanks the University of Yale Edward P. Bass Distinguished Visiting Environmental Scholarship and A. Hendy acknowledges support from the Jon A. and Beverly L. Thompson Endowment. C. Pimiento thanks J. McLaughlin for support. This is University of Florida Contribution to Paleontology number 628. NR 131 TC 13 Z9 16 U1 3 U2 25 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD SEP PY 2013 VL 87 IS 5 BP 755 EP 774 DI 10.1666/12-117 PG 20 WC Paleontology SC Paleontology GA 217IJ UT WOS:000324352900001 ER PT J AU Paez-Reyes, M Head, MJ AF Paez-Reyes, Manuel Head, Martin J. TI THE CENOZOIC GONYAULACACEAN DINOFLAGELLATE GENERA OPERCULODINIUM WALL, 1967 AND PROTOCERATIUM BERGH, 1881 AND THEIR PHYLOGENETIC RELATIONSHIPS SO JOURNAL OF PALEONTOLOGY LA English DT Article ID HARMFUL ALGAL BLOOMS; GREAT BAHAMA BANK; RETICULATUM DINOPHYCEAE; PLEISTOCENE SERIES/EPOCH; QUATERNARY SYSTEM/PERIOD; FORMAL RATIFICATION; RECENT SEDIMENTS; NORTH-SEA; CYSTS; MORPHOLOGY AB To clarify the systematic positions of the important gonyaulacacean genera Operculodinium Wall, 1967 emend. Matsuoka et al., 1997 and Protoceratium Bergh, 1881, we present in detail the tabulation of the Oligocene- Pleistocene, thermophilic, cyst-defined species Operculodinium bahamense Head in Head and Westphal, 1999 emend., and the extant, cosmopolitan, theca-defined species Protoceratium reticulatum (Claparede and Lachmann, 1859) Butschli, 1885. Both species have a sexiform hyposomal tabulation, and L-type (Protoceratium reticulatum) or modified L-type (Operculodinium bahamense) ventral organization. Protoceratium reticulatum has dextral torsion of the hypotheca, requiring assignation of the genus to the subfamily Cribroperidinioideae Fensome et al., 1993, whereas Operculodinium bahamense has neutral torsion requiring assignation to the subfamily Leptodinioideae Fensome et al., 1993. The stratigraphic range of this subfamily is now extended upwards to the lower Pleistocene. Paradoxically, Protoceratium reticulatum produces a cyst whose morphology is circumscribed by the cyst-defined genus Operculodinium, either implying polyphyletic origins for this genus or that combinations of ventral organization and torsion used to subdivide the family Gonyaulacaceae cannot always be applied rigidly. In detail, Operculodinium bahamense is shown to have an unusual ventral tabulation in which the first apical plate contacts the apical pore complex but not the sulcus. The new term "episert" is proposed to describe this plate relationship, which appears to have evolved independently in several lineages of the suborder Gonyaulacineae. C1 [Paez-Reyes, Manuel; Head, Martin J.] Brock Univ, Dept Earth Sci, St Catharines, ON L2S 3A1, Canada. [Paez-Reyes, Manuel] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Paez-Reyes, M (reprint author), Brock Univ, Dept Earth Sci, 500 Glenridge Ave, St Catharines, ON L2S 3A1, Canada. EM manuel.paez@gmail.com; mjhead@broku.ca FU Natural Sciences and Engineering Research Council of Canada; Brock University; Smithsonian Tropical Research Institute FX We thank M. Hoppenrath (DZMB, Forschungsinstitut Senckenberg) for making available published and unpublished microphotographs of Protoceratium reticulatum, and K. Mertens (Ghent University) for bringing our attention to some of the older literature. K. Matsuoka (Nagasaki University) and K. Mertens provided helpful comments on the episert condition in extant species. The Integrated Ocean Drilling Program provided the samples for this research. MJH acknowledges support from a Discovery Grant of the Natural Sciences and Engineering Research Council of Canada. MP-R is grateful to Brock University and the Smithsonian Tropical Research Institute for financial support at various stages of this research. Mr. Jorge Ceballos (Smithsonian Tropical Research institute) helped with SEM photography. Helpful reviews of the manuscript by L. E. Edwards and J. Lucas-Clark are greatly appreciated, especially insightful comments from L. E. Edwards regarding the episert condition. NR 94 TC 6 Z9 6 U1 1 U2 7 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD SEP PY 2013 VL 87 IS 5 BP 786 EP 803 DI 10.1666/12-103 PG 18 WC Paleontology SC Paleontology GA 217IJ UT WOS:000324352900003 ER PT J AU Prothero, DR Beatty, BL Stucky, RM AF Prothero, Donald R. Beatty, Brian L. Stucky, Richard M. TI SIMOJOVELHYLIS IS A PECCARY, NOT A HELOHYID (MAMMALIA, ARTIODACTYLA) SO JOURNAL OF PALEONTOLOGY LA English DT Article ID MIOCENE; AMERICA AB Simojovelhyus pocitosense is based on a lower jaw fragment with three molars from the late Oligocene amber mine deposits near the village of Simojovel, Chiapas Province, Mexico. It is the oldest fossil mammal known from Central America. It was described by Ferrusquia-Villafranca in 2006 as a helohyid, a group of primitive artiodactyls known from the Bridgerian and Uintan (older than 49-42 Ma), yet it comes from early Arikareean deposits about 25-27 Ma, suggesting that it was a very late helohyid living more than 10 m.y. after their apparent Uintan extinction. We re-examined the specimen, and compared it to the large collection of recently described peccaries from the Chadronian (Perchoerus minor) and Orellan (Perchoerus nanus) and Bridgerian helohyids (Helohyus sp.). Once the range of variation of characters in helohyids and peccaries is accounted for, Simojovelhyus shows derived similarities to early peccaries, especially in the bunodont molars with inflated cusps and the configuration of cristids and accessory cuspulids, and none of the incipient lophodonty and primitive morphology seen in helohyids. In fact, the only real similarity other than symplesiomorphies between Simojovelhyus and helohyids is its small size, but it is close to the size range of the tiny Chadronian peccary P. minor. Thus, based on both derived tooth characters and its age, it is much more parsimonious to regard Simojovelhyus as a tiny Mexican peccary from the Arikareean, not a very late helohyid. This removes the anomalously late occurrence of helohyids from the mammalian fossil record, and forces a re-examination of our view of mammalian evolution in Central America. C1 [Prothero, Donald R.] Los Angeles Cty Museum Nat Hist, Dept Vertebrate Paleontol, Los Angeles, CA 90007 USA. [Beatty, Brian L.] New York Inst Technol, Coll Osteopath Med, Old Westbury, NY 11568 USA. [Beatty, Brian L.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Beatty, Brian L.] Virginia Museum Nat Hist, Martinsville, VA USA. [Stucky, Richard M.] Denver Museum Nat & Sci, Denver, CO 80205 USA. RP Prothero, DR (reprint author), Los Angeles Cty Museum Nat Hist, Dept Vertebrate Paleontol, Los Angeles, CA 90007 USA. EM donaldprothero@att.net; bbeatty@nyit.edu; Richard.stucky@dmns.org NR 8 TC 1 Z9 1 U1 0 U2 3 PU PALEONTOLOGICAL SOC INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044 USA SN 0022-3360 J9 J PALEONTOL JI J. Paleontol. PD SEP PY 2013 VL 87 IS 5 BP 930 EP 933 DI 10.1666/12-084 PG 4 WC Paleontology SC Paleontology GA 217IJ UT WOS:000324352900013 ER PT J AU Bret, A Stockem, A Fiuza, F Alvaro, EP Ruyer, C Narayan, R Silva, LO AF Bret, Antoine Stockem, Anne Fiuza, Frederico Perez Alvaro, Erica Ruyer, Charles Narayan, Ramesh Silva, Luis O. TI The formation of a collisionless shock SO LASER AND PARTICLE BEAMS LA English DT Article DE Collisionless shocks; Weibel instability; Plasma fluctuations ID PARTICLE-ACCELERATION; MAGNETIC-FIELD; INSTABILITY; PLASMA; FILAMENTATION; GENERATION; WEIBEL AB Collisionless shocks are key processes in astrophysics where the energy dissipation at the shock front is provided by collective plasma effects rather than particle collisions. While numerous simulations and laser-plasma experiments have shown they can result from the encounter of two plasma shells, a first principle theory of the shock formation is still lacking. In this respect, a series of 2D Particle-In-Cells simulations have been performed of two identical cold colliding pair plasmas. The simplicity of this system allows for an accurate analytical tracking of the physics. To start with, the Weibel-filamentation instability is triggered in the overlapping region, which generates a turbulent region after a saturation time tau(s). The incoming flow then piles-up in this region, building-up the shock density region according to some nonlinear processes, which will be the subject of future works. By evaluating the seed field giving rise to the instability, we derive an analytical expression for tau(s) in good agreement with simulations. In view of the importance of the filamentation instability, we show a static magnetic field can cancel it if and only if it is perfectly aligned with the flow. C1 [Bret, Antoine; Perez Alvaro, Erica] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Bret, Antoine; Perez Alvaro, Erica] Inst Invest Energet & Aplicaciones Ind, Ciudad Real, Spain. [Stockem, Anne; Fiuza, Frederico; Silva, Luis O.] Inst Super Tecn, Lab Associado, GoLP Inst Plasmas & Fusao Nucl, Lisbon, Portugal. [Ruyer, Charles] CEA, DAM, DIF, F-91297 Arpajon, France. [Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bret, A (reprint author), Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. EM antoineclaude.bret@uclm.es RI Silva, Luis/C-3169-2009; Bret, Antoine/C-9112-2009; OI Silva, Luis/0000-0003-2906-924X; Bret, Antoine/0000-0003-2030-0046; Fiuza, Frederico/0000-0002-8502-5535; Stockem, Anne Gabriele/0000-0003-4614-8118; Narayan, Ramesh/0000-0002-1919-2730 FU Spanish Ministerio de Educacion y Ciencia [ENE2009-09276]; European Research Council [267841]; FCT (Portugal) [PTDC/FIS/111720/2009, SFRH/BD/38952/2007] FX This work was supported by projects ENE2009-09276 of the Spanish Ministerio de Educacion y Ciencia, the European Research Council (ERC-2010-AdG Grant 267841) and FCT (Portugal) grants PTDC/FIS/111720/2009 and SFRH/BD/38952/2007. Thanks are due to LorenzoSironi for useful discussions. NR 34 TC 1 Z9 1 U1 0 U2 18 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0263-0346 EI 1469-803X J9 LASER PART BEAMS JI Laser Part. Beams PD SEP PY 2013 VL 31 IS 3 BP 487 EP 491 DI 10.1017/S0263034613000372 PG 5 WC Physics, Applied SC Physics GA 220NY UT WOS:000324592500015 ER PT J AU Abeytia, R Guman, HM Breedy, O AF Abeytia, Rosalinda Guman, Hector M. Breedy, Odalisca TI Species composition and bathymetric distribution of gorgonians (Anthozoa: Octocorallia) on the Southern Mexican Pacific coast SO REVISTA DE BIOLOGIA TROPICAL LA English DT Article DE abundance; bathymetrical distribution; diversity; gorgonians assemblages; Mexican Pacific ID SHALLOW-WATER GORGONIANS; CORAL-REEFS; DISTRIBUTION PATTERNS; CARIBBEAN GORGONIANS; PARAMURICEA-CLAVATA; MARINE OCTOCORAL; PUERTO-RICO; COELENTERATA; REVISION; SEA AB Gorgonians are important components of coastal ecosystems, as they provide niches, natural compounds with medical applications and are used as bioindicators. Species composition and assemblage structure of gorgonians (Anthozoa: Octocorallia) were studied along a bathymetric profile in the Southern Mexican Pacific coast. Species composition was based on specimens collected within a depth range of 0-70m in 15 sites. The relative abundance of species was determined in six sites at four depths (5, 10, 20 and 25m) using three 10m(2) transects at each depth level. Twenty-seven species of gorgonians belonging to six genera and three families were registered. The species composition varied with depth: 11 species were distributed between 0-25m depth, while 17 species were found between 40-70m depth interval. The shallow zone is characterized by a relatively large abundance of gorgonians, dominated by colonies of Leptogorgia cuspidata and L. ena. In contrast, the deepest zone was characterized by relatively low abundance of gorgonians, dominated by L. alba, the only species observed in both depth intervals. The similarity analysis showed differences in the composition and abundance of species by depth and site, suggesting that the main factor in determining the assemblage structure is depth. Results of this study suggest that the highest richness of gorgonian species in the study area may be located at depths of 40-70m, whereas the highest abundances are found between 5 and 10m depth. This study represents a contribution to the poorly known eastern Pacific gorgonian biota. C1 [Abeytia, Rosalinda] Univ Nacl Autonoma Mexico, Unidad Acad Puerto Morelos, Inst Ciencias Mar & Limnol, Cancun 77500, QR, Mexico. [Guman, Hector M.] Smithsonian Trop Res Inst, Balboa, Panama. [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscap, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. RP Abeytia, R (reprint author), Univ Nacl Autonoma Mexico, Unidad Acad Puerto Morelos, Inst Ciencias Mar & Limnol, Ap Postal 1152, Cancun 77500, QR, Mexico. EM r.abeytia@gmail.com; GuzmanH@si.edu; odalisca.breedy@ucr.ac.cr FU Smithsonian Tropical Research Institute, Panama; Universidad del Mar, Puerto Angel, Mexico FX We thank Valeria Hernandez Urraca, Imelda Perez Maldonado, Fernando Diaz and Gonzales for assistance in the field. This manuscript was greatly improved by comments from Eric Jordan Dahlgren, Rosa Rodriguez Martinez, Lorenzo Alvarez Filip and Andres Ramon Lopez Perez. This work was supported by the Smithsonian Tropical Research Institute, Panama and Universidad del Mar, Puerto Angel, Mexico. NR 52 TC 3 Z9 3 U1 2 U2 11 PU REVISTA DE BIOLOGIA TROPICAL PI SAN JOSE PA UNIVERSIDAD DE COSTA RICA CIUDAD UNIVERSITARIA, SAN JOSE, 00000, COSTA RICA SN 0034-7744 EI 2215-2075 J9 REV BIOL TROP JI Rev. Biol. Trop. PD SEP PY 2013 VL 61 IS 3 BP 1157 EP 1166 PG 10 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 219LT UT WOS:000324509200013 PM 24027914 ER PT J AU Geatz, GW Needelman, BA Weil, RR Megonigal, JP AF Geatz, George W. Needelman, Brian A. Weil, Raymond R. Megonigal, J. Patrick TI Nutrient Availability and Soil Organic Matter Decomposition Response to Prescribed Burns in Mid-Atlantic Brackish Tidal Marshes SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID SALT-MARSH; PLANT ZONATION; CELLULOSE DECOMPOSITION; SPARTINA-ALTERNIFLORA; FLORIDA EVERGLADES; NORTH-CAROLINA; FIRE; NITROGEN; VEGETATION; PHOSPHORUS AB Prescribed fire in tidal marshes has been shown to generate short-term increases in plant-available nutrients, but the long-term implications of fire on nutrient availability and organic matter decomposition have not been well established. Two manipulative experiments were conducted over 1 yr within long-term annual burn and no-burn blocks at the Blackwater National Wildlife Refuge in Cambridge, MD to study the effects of canopy removal and ash deposition on nutrient availability and organic matter decomposition rates following burning. Ash deposition had no significant effects on study variables. At no-burn sites, porewater NH4+ and PO43+ were significantly lower in July in sites with canopy removal (0.15 mg NH4+ L-1 and 0.04 mg PO43+ L-1) compared to sites with a canopy (0.73 mg NH4+ L-1 and 0.08 mg PO43+ L-1). Similar results were found through a canopy replacement treatment at annual burn sites. Decreased porewater NH4+ and PO43+ corresponded to increased total biomass nutrient content. No-burn sites with canopy removal treatments showed significantly lower organic matter decomposition rates than did treatments with a canopy in July (66.5 vs. 74.1% cotton tensile strength loss), corresponding to decreases in porewater NH4+ and PO43+. Plant ash provided a fertilizer pulse of 0.22 g N m(-2) and 0.16 g P m(-2), which were amounts of N and P likely too small to increase plant productivity when deposited during late winter/early spring. Prescribed fire appears to affect nutrient availability and organic matter decomposition in these marsh soils primarily through the mechanism of increased biomass production due to canopy removal. C1 [Geatz, George W.] Univ Illinois, Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Needelman, Brian A.; Weil, Raymond R.] Univ Maryland, Dep Environm Sci & Technol, College Pk, MD 20742 USA. [Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Needelman, BA (reprint author), Univ Maryland, Dep Environm Sci & Technol, College Pk, MD 20742 USA. EM bneed@umd.edu FU Maryland Sea Grant [NA10OAR4170072] FX We thank the Maryland Sea Grant for funding this project (award no. NA10OAR4170072). We also thank the staff at the Blackwater National Wildlife Refuge, especially Suzanne Baird, Bill Giese, Matt Whitbeck, Leticia Melendez, and Nate Carle, for their continuous suggestions, support, assistance, and collaboration on the study. We are appreciative of the field and lab work help received from members of the Soil and Water Geospatial Analysis Lab (SAWGAL) at the University of Maryland especially George Geatz, Michele Miller, Asia Vinnikova, Amanda Garzio-Hadzick, Emily Hutchins, Becca Mead, Miriam Meyers, and Joey Schlosnagle. We would also like to thank Don Cahoon, Glenn Guntenspergen, and Jim Lynch of USGS Patuxent Wildlife Research Center for collaborating throughout the study. We thank Dennis Skultety of te Illinois Natural History survey for help with making the GIS maps in this article. NR 66 TC 1 Z9 2 U1 1 U2 36 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 SEP-OCT PY 2013 VL 77 IS 5 BP 1852 EP 1864 DI 10.2136/sssaj2012.0272 PG 13 WC Soil Science SC Agriculture GA 220ZO UT WOS:000324626600038 ER PT J AU Robertson, BA Rehage, JS Sih, A AF Robertson, Bruce A. Rehage, Jennifer S. Sih, Andrew TI Ecological novelty and the emergence of evolutionary traps SO TRENDS IN ECOLOGY & EVOLUTION LA English DT Review ID BEHAVIORAL SYNDROMES; ENVIRONMENTAL-CHANGE; HABITAT SELECTION; NATIVE FROGS; CONSERVATION; LANDSCAPES; PREDATION; DYNAMICS; FOREST; FISH AB Human-induced rapid environmental change (HIREC; e.g., climate change or exotic species) has caused global species declines. Although behavioral plasticity has buffered some species against HIREC, maladaptive behavioral scenarios called 'evolutionary traps' are increasingly common, threatening the persistence of affected species. Here, we review examples of evolutionary traps to identify their anthropogenic causes, behavioral mechanisms, and evolutionary bases, and to better forecast forms of HIREC liable to trigger traps. We summarize a conceptual framework for explaining the susceptibility of animals to traps that integrates the cost benefit approach of standard behavioral ecology with an evolutionary approach (reaction norms) to understanding cue response systems (signal detection). Finally, we suggest that a significant revision of conceptual thinking in wildlife conservation and management is needed to effectively eliminate and mitigate evolutionary traps. C1 [Robertson, Bruce A.] Bard Coll, Div Sci Math & Comp, Annandale On Hudson, NY 12504 USA. [Robertson, Bruce A.] Natl Zool Pk, Migratory Bird Ctr, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Rehage, Jennifer S.] Florida Int Univ, Earth & Environm Dept, Southeast Environm Res Ctr, Miami, FL 33199 USA. [Sih, Andrew] Univ Calif Davis, Dept Environm Sci & Policy, Davis, CA 95616 USA. RP Robertson, BA (reprint author), Bard Coll, Div Sci Math & Comp, Annandale On Hudson, NY 12504 USA. EM broberts@bard.edu FU Bard College; Smithsonian Conservation Biology Institute; National Science Foundation (NSF) [WSC-1204762]; Florida Coastal Everglades Long-term Ecological Research (FCE LTER) program [NSF DBI-0620409] FX B.A.R. was supported by funding from Bard College and the Smithsonian Conservation Biology Institute. J.S.R. was supported by National Science Foundation (NSF) WSC-1204762 and works in collaboration with the Florida Coastal Everglades Long-term Ecological Research (FCE LTER) program (NSF DBI-0620409). NR 75 TC 70 Z9 70 U1 30 U2 243 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 SEP PY 2013 VL 28 IS 9 BP 552 EP 560 DI 10.1016/j.tree.2013.04.004 PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 225PV UT WOS:000324975700012 PM 23756104 ER PT J AU Newman, JA Cooper, MC Davis, M Faber, SM Coil, AL Guhathakurta, P Koo, DC Phillips, AC Conroy, C Dutton, AA Finkbeiner, DP Gerke, BF Rosario, DJ Weiner, BJ Willmer, CNA Yan, RB Harker, JJ Kassin, SA Konidaris, NP Lai, K Madgwick, DS Noeske, KG Wirth, GD Connolly, AJ Kaiser, N Kirby, EN Lemaux, BC Lin, L Lotz, JM Luppino, GA Marinoni, C Matthews, DJ Metevier, A Schiavon, RP AF Newman, Jeffrey A. Cooper, Michael C. Davis, Marc Faber, S. M. Coil, Alison L. Guhathakurta, Puragra Koo, David C. Phillips, Andrew C. Conroy, Charlie Dutton, Aaron A. Finkbeiner, Douglas P. Gerke, Brian F. Rosario, David J. Weiner, Benjamin J. Willmer, C. N. A. Yan, Renbin Harker, Justin J. Kassin, Susan A. Konidaris, N. P. Lai, Kamson Madgwick, Darren S. Noeske, K. G. Wirth, Gregory D. Connolly, A. J. Kaiser, N. Kirby, Evan N. Lemaux, Brian C. Lin, Lihwai Lotz, Jennifer M. Luppino, G. A. Marinoni, C. Matthews, Daniel J. Metevier, Anne Schiavon, Ricardo P. TI THE DEEP2 GALAXY REDSHIFT SURVEY: DESIGN, OBSERVATIONS, DATA REDUCTION, AND REDSHIFTS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE cosmology: observations; galaxies: distances and redshifts; galaxies: evolution; galaxies: fundamental parameters; galaxies: high-redshift; galaxies: statistics; large-scale structure of universe; methods: data analysis; surveys ID SIMILAR-TO 1; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; ACTIVE GALACTIC NUCLEI; GROTH STRIP SURVEY; EXTRAGALACTIC LEGACY SURVEY; SPITZER-SPACE-TELESCOPE; OPTICAL-ROTATION CURVES; COLOR-DENSITY RELATION; TULLY-FISHER RELATION AB We describe the design and data analysis of the DEEP2 Galaxy Redshift Survey, the densest and largest high-precision redshift survey of galaxies at z similar to 1 completed to date. The survey was designed to conduct a comprehensive census of massive galaxies, their properties, environments, and large-scale structure down to absolute magnitude M-B = -20 at z similar to 1 via similar to 90 nights of observation on the Keck telescope. The survey covers an area of 2.8 deg(2) divided into four separate fields observed to a limiting apparent magnitude of R-AB = 24.1. Objects with z less than or similar to 0.7 are readily identifiable using BRI photometry and rejected in three of the four DEEP2 fields, allowing galaxies with z > 0.7 to be targeted similar to 2.5 times more efficiently than in a purely magnitude-limited sample. Approximately 60% of eligible targets are chosen for spectroscopy, yielding nearly 53,000 spectra and more than 38,000 reliable redshift measurements. Most of the targets that fail to yield secure redshifts are blue objects that lie beyond z similar to 1.45, where the [O II] 3727 angstrom doublet lies in the infrared. The DEIMOS 1200 line mm(-1) grating used for the survey delivers high spectral resolution (R similar to 6000), accurate and secure redshifts, and unique internal kinematic information. Extensive ancillary data are available in the DEEP2 fields, particularly in the Extended Groth Strip, which has evolved into one of the richest multiwavelength regions on the sky. This paper is intended as a handbook for users of the DEEP2 Data Release 4, which includes all DEEP2 spectra and redshifts, as well as for the DEEP2 DEIMOS data reduction pipelines. Extensive details are provided on object selection, mask design, biases in target selection and redshift measurements, the spec2d two-dimensional data-reduction pipeline, the spec1d automated redshift pipeline, and the zspec visual redshift verification process, along with examples of instrumental signatures or other artifacts that in some cases remain after data reduction. Redshift errors and catastrophic failure rates are assessed through more than 2000 objects with duplicate observations. Sky subtraction is essentially photon-limited even under bright OH sky lines; we describe the strategies that permitted this, based on high image stability, accurate wavelength solutions, and powerful B-spline modeling methods. We also investigate the impact of targets that appear to be single objects in ground-based targeting imaging but prove to be composite in Hubble Space Telescope data; they constitute several percent of targets at z similar to 1, approaching similar to 5%-10% at z > 1.5. Summary data are given that demonstrate the superiority of DEEP2 over other deep high-precision redshift surveys at z similar to 1 in terms of redshift accuracy, sample number density, and amount of spectral information. We also provide an overview of the scientific highlights of the DEEP2 survey thus far. C1 [Newman, Jeffrey A.; Matthews, Daniel J.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [Cooper, Michael C.] Univ Calif Irvine, Dept Phys & Astron, Ctr Galaxy Evolut, Irvine, CA 92697 USA. [Davis, Marc; Madgwick, Darren S.] Univ Calif Berkeley, Dept Phys & Astron, Berkeley, CA 94720 USA. [Faber, S. M.; Guhathakurta, Puragra; Koo, David C.; Phillips, Andrew C.; Conroy, Charlie; Harker, Justin J.; Lai, Kamson] Univ Calif Santa Cruz, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Coil, Alison L.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Conroy, Charlie; Finkbeiner, Douglas P.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Dutton, Aaron A.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Gerke, Brian F.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Rosario, David J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Weiner, Benjamin J.; Willmer, C. N. A.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Yan, Renbin] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Kassin, Susan A.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Kassin, Susan A.; Noeske, K. G.; Lotz, Jennifer M.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Konidaris, N. P.; Kirby, Evan N.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Wirth, Gregory D.] Keck Observ, Kamuela, HI 96743 USA. [Connolly, A. J.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Kaiser, N.; Luppino, G. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Lemaux, Brian C.] Lab Astrophys Marseille, Marseilles, France. [Lin, Lihwai] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Marinoni, C.] Ctr Phys Theor Marseilles, Marseilles, France. [Metevier, Anne] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Schiavon, Ricardo P.] Liverpool John Moores Univ, Astrophys Res Inst, Wirral H41 1LD, Merseyside, England. RP Newman, JA (reprint author), Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. EM janewman@pitt.edu; m.cooper@uci.edu; mdavis@berkeley.edu; faber@ucolick.org; acoil@ucsd.edu; raja@ucolick.org; koo@ucolick.org; phillips@ucolick.org; cconroy@cfa.harvard.edu; dutton@mpia.de; dfinkbeiner@cfa.harvard.edu; bfgerke@lbl.gov; rosario@mpe.mpg.de; bjw@as.arizona.edu; cnaw@as.arizona.edu; yanrenbin@gmail.com; jharker@ucolick.org; susan.kassin@nasa.gov; npk@astro.caltech.edu; klai@ucolick.org; noeske@stsci.edu; wirth@keck.hawaii.edu; ajc@astro.washington.edu; kaiser@ifa.hawaii.edu; enk@astro.caltech.edu; brian.lemaux@oamp.fr; lihwailin@asiaa.sinica.edu.tw; lotz@stsci.edu; ger@ifa.hawaii.edu; marinoni@cpt.univ-mrs.fr; djm70@pitt.edu; ajmetevier@gmail.com; R.P.Schiavon@ljmu.ac.uk OI Weiner, Benjamin/0000-0001-6065-7483; Kirby, Evan/0000-0001-6196-5162 FU NSF Center for Particle Astrophysics; National Science Foundation [AST 95-29098, 00-711098, 05-07483, 08-08133, AST 00-71048, 05-07428, 08-07630, 08-06732, ARI 92-14621]; NASA [HST-AR-01947]; NASA through Hubble Fellowship [51256.01, 51269.01, NAS 5-26555]; Space Telescope Science Institute; CARA; Hubble Fellowships; Hubble Fellowship; Spitzer Fellowship; W. M. Keck Foundation; University of California; NASA; California Association for Research in Astronomy (Keck Observatory); University of California/Lick Observatory FX The DEEP2 survey was initiated under the auspices of the NSF Center for Particle Astrophysics. Major grant support was provided by National Science Foundation grants AST 95-29098, 00-711098, 05-07483, and 08-08133 to UCSC, AST 00-71048, 05-07428, and 08-07630 to UCB, and 08-06732 to the University of Pittsburgh. Computing hardware used to analyze DEEP2 data was provided by Sun Microsystems. The HST ACS imaging mosaic in EGS was constructed by Anton Koekemoer and Jennifer Lotz and was funded by grant HST-AR-01947 from NASA. NASA imaging of the original Groth Strip was planned and executed by Ed Groth and Jason Rhodes with support from NAS5-1661 and NAG5-6279 to the WFPC1 IDT. Support for this work was provided by NASA through Hubble Fellowship grants 51256.01 and 51269.01 awarded to E.N.K. and M.C.C., respectively, 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. Sandra Faber thank CARA for a generous research grant and the Miller Institute at UC Berkeley for a Visiting Miller Professorship, during which much of this paper was written. Jeffrey Newman and Alison Coil acknowledge support from Hubble Fellowships during their DEEP2 work, and Michael Cooper acknowledges support from both Hubble and Spitzer Fellowships.; Thanks are due to the many institutions and individuals who have made the DEEP2 survey possible. First thanks go to the W. M. Keck Foundation, the University of California, and NASA for providing funds to construct and operate the Keck telescopes. Second, we wish to thank the technical teams in the UCO/Lick Shops and at Keck Observatory for their role in building and commissioning the DEIMOS spectrograph and for their superb support during many observing runs. Funds for the spectrograph were provided by instrumentation grant ARI 92-14621 from the National Science Foundation and instrument funds from the California Association for Research in Astronomy (Keck Observatory) and from the University of California/Lick Observatory. NR 156 TC 181 Z9 181 U1 2 U2 13 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 SEP PY 2013 VL 208 IS 1 AR UNSP 5 DI 10.1088/0067-0049/208/1/5 PG 57 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 214XS UT WOS:000324172700005 ER PT J AU Ratnayake, R Liu, YX Paul, VJ Luesch, H AF Ratnayake, Ranjala Liu, Yanxia Paul, Valerie J. Luesch, Hendrik TI Cultivated Sea Lettuce is a Multiorgan Protector from Oxidative and Inflammatory Stress by Enhancing the Endogenous Antioxidant Defense System SO CANCER PREVENTION RESEARCH LA English DT Article ID LOS-ANGELES-COUNTY; PROSTATE-CANCER; RESPONSE ELEMENT; UNITED-STATES; ULVA-LACTUCA; SAITAMA PREFECTURE; ENZYME INDUCERS; MARINE-ALGAE; IN-VITRO; CELLS AB The health-promoting effects of seaweeds have been linked to antioxidant activity that may counteract cancer-causing oxidative stress-induced damage and inflammation. Although antioxidant activity is commonly associated with direct radical scavenging activity, an alternative way to increase the antioxidant status of a cell is to enhance the endogenous (phase II) defense system consisting of cytoprotective antioxidant enzymes, including NAD(P)H:quinone oxidoreductase 1 (NQO1). These enzymes are transcriptionally regulated by the antioxidant response element (ARE) via the transcription factor Nrf2. Extracts derived from cultivated Ulva sp., a green alga regarded as a marine vegetable (sea lettuce), potently activated the Nrf2-ARE pathway in IMR-32 neuroblastoma and LNCaP prostate cancer cells. RNA interference studies showed that Nrf2 and phosphoinositide 3-kinase (PI3K) are essential for the phase II response in IMR-32 cells. Activity-enriched fractions induced Nrf2 nuclear translocation and target gene transcription, and boosted the cellular glutathione level and therefore antioxidant status. A single-dose gavage feeding of Ulva-derived fractions increased Nqo1 transcript levels in various organs. Nqo1 induction spiked in different tissues, depending on the specific chemical composition of each administered fraction. We purified and characterized four ARE inducers in this extract, including loliolide (1), isololiolide (2), a megastigmen (3), and a novel chlorinated unsaturated aldehyde (4). The ARE-active fractions attenuated lipopolysaccharide-induced iNOS and Cox2 gene expression in macrophagic RAW264.7 cells, decreasing nitric oxide (NO) and prostaglandin E2 (PGE(2)) production, respectively. Nqo1 activity and NO production were abrogated in nrf2(-/-) mouse embryonic fibroblasts, providing a direct link between the induction of phase II response and anti-inflammatory activity. Cancer Prev Res; 6(9); 989-99. (C)2013 AACR. C1 [Ratnayake, Ranjala; Liu, Yanxia; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Luesch, H (reprint author), Univ Florida, 1600 SW Archer Rd,POB 100485, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU NIH, NCI [R21CA133681] FX This study was supported by NIH, NCI Grant R21CA133681. NR 50 TC 3 Z9 3 U1 3 U2 29 PU AMER ASSOC CANCER RESEARCH PI PHILADELPHIA PA 615 CHESTNUT ST, 17TH FLOOR, PHILADELPHIA, PA 19106-4404 USA SN 1940-6207 EI 1940-6215 J9 CANCER PREV RES JI Cancer Prev. Res. PD SEP PY 2013 VL 6 IS 9 BP 989 EP 999 DI 10.1158/1940-6207.CAPR-13-0014 PG 11 WC Oncology SC Oncology GA 214XH UT WOS:000324171000012 PM 24005795 ER PT J AU Sharma, S Dutta, T Maldonado, JE Wood, TC Panwar, HS Seidensticker, J AF Sharma, Sandeep Dutta, Trishna Maldonado, Jesus E. Wood, Thomas C. Panwar, Hemendra Singh Seidensticker, John TI A highly informative microsatellite panel for individual identification and sex determination of jungle cats (Felis chaus) SO CONSERVATION GENETICS RESOURCES LA English DT Article DE Noninvasive DNA sampling; Felis chaus; Individual identification; Microsatellite; Sex assignment ID COMPUTER-PROGRAM; SAMPLES; SOFTWARE AB The jungle cat (Felis chaus), a small-sized felid, is distributed across Southeast and South Asia to Egypt in Africa. In India, it is one of the most common small cat species but no reliable methods are available to monitor its population status. We describe a non-invasive genetic monitoring technique using fecal samples for individual identification and sex determination of jungle cats. We evaluated 21 feline microsatellites and optimized a panel of 11 highly polymorphic microsatellite loci that yield a cumulative Probability of Identity between siblings value of 5.51x10(-6). We used this panel to identify 110 individuals from 118 jungle cat scats collected from tiger reserves in Central India. We identified 22 males and 35 females by amplifying a fragment of the Amelogenin protein gene. This panel will be helpful to study genetic structure, gene flow, relatedness, sex ratio, and population estimation in jungle cats. C1 [Sharma, Sandeep; Dutta, Trishna; Maldonado, Jesus E.; Seidensticker, John] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. [Sharma, Sandeep; Dutta, Trishna; Maldonado, Jesus E.; Wood, Thomas C.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. RP Sharma, S (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, 3001-7012 Connecticut Ave NW, Washington, DC 20013 USA. EM sandeeps17@gmail.com FU Smithsonian Conservation Biology Institute (SCBI); Kathryn Fuller science for nature fund of World Wildlife Fund (WWF); International Bear Association; George Mason University FX Funding was provided by the Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo, Kathryn Fuller science for nature fund of World Wildlife Fund (WWF), International Bear Association, and George Mason University. We thank the Principal Chief Conservator of Forests (PCCF) Wildlife, Madhya Pradesh and Maharashtra, and field directors and staff of all five tiger reserves (Kanha, Satpura, Melghat, Pench MP and Mh) for providing research permissions and logistical help. We thank Robert Fleischer, Center for Conservation and Evolutionary Genetics, SCBI, and Yogesh S. Shouche, National Center for Cell Sciences (NCCS), Pune, Maharashtra, India, for providing laboratory space and facilitating lab work; Nancy Rotzel, Libby Dougan, and Hitendra Munot for logistical support, and Susan Lumpkin for editorial comments. We also thank two anonymous reviewers for suggestions that greatly improved the quality of this manuscript. NR 17 TC 1 Z9 1 U1 9 U2 42 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1877-7252 EI 1877-7260 J9 CONSERV GENET RESOUR JI Conserv. Genet. Resour. PD SEP PY 2013 VL 5 IS 3 BP 863 EP 866 DI 10.1007/s12686-013-9873-0 PG 4 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 194GT UT WOS:000322619900062 ER PT J AU Pisano, DA AF Pisano, Dominick A. TI Blue Sky Metropolis: The Aerospace Century in Southern California SO JOURNAL OF AMERICAN HISTORY LA English DT Book Review C1 [Pisano, Dominick A.] Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. RP Pisano, DA (reprint author), Smithsonian Inst, Natl Air & Space Museum, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU ORGANIZATION AMER HISTORIANS PI BLOOMINGTON PA 112 N BRYAN ST, BLOOMINGTON, IN 47408 USA SN 0021-8723 J9 J AM HIST JI J. Am. Hist. PD SEP PY 2013 VL 100 IS 2 BP 600 EP 600 DI 10.1093/jahist/jat234 PG 1 WC History SC History GA 205EI UT WOS:000323424600147 ER PT J AU Huang, YM Rueda, LM AF Huang, Yiau-Min Rueda, Leopoldo M. TI A NEW SPECIES OF THE GENUS ORTHOPODOMYIA FROM OTOTOMO, CAMEROON, WITH NOTES ON OTHER ORTHOPODOMYIA GROUP-SPECIES SO JOURNAL OF THE AMERICAN MOSQUITO CONTROL ASSOCIATION LA English DT Article DE Orthopodomyia ototomoensis; Ototomoensis Group; Nkolbissonensis Group; morphology; Cameroon AB A new species belonging to the new Ototomoensis Group, Orthopodomyia ototomoensis Huang and Rueda, is described from Ototomo, Cameroon. Diagnostic features for separating members of Nkolbissonensis Group and Ototomoensis Group from other Orthopodomyia groups are provided. Two supplemental keys are presented: "A Pictorial Key to the Species of the Genus Orthopodomyia Ototomoensis Group in the Afrotropical Region (Diptera: Culicidae)" and "A Pictorial Key to the Species of the Genus Orthopodomyia Nkolbissonensis Group in the Afrotropical Region (Diptera: Culicidae).'' C1 [Huang, Yiau-Min] Smithsonian Inst, Dept Entomol, Washington, DC 20013 USA. [Rueda, Leopoldo M.] Walter Reed Army Inst Res, Entomol Branch, Walter Reed Biosystemat Unit, Silver Spring, MD 20910 USA. RP Huang, YM (reprint author), Smithsonian Inst, Dept Entomol, POB 37012,MSC C1109,MRC 534, Washington, DC 20013 USA. NR 12 TC 1 Z9 1 U1 0 U2 1 PU AMER MOSQUITO CONTROL ASSOC PI MOUNT LAUREL PA 15000 COMMERCE PARKWAY, SUITE C, MOUNT LAUREL, NJ 08054 USA SN 8756-971X EI 1943-6270 J9 J AM MOSQUITO CONTR JI J. Am. Mosq. Control Assoc. PD SEP PY 2013 VL 29 IS 3 BP 270 EP 274 PG 5 WC Entomology SC Entomology GA 217SJ UT WOS:000324380600007 PM 24199501 ER PT J AU Sues, HD Schoch, RR AF Sues, Hans-Dieter Schoch, Rainer R. TI ANATOMY AND PHYLOGENETIC RELATIONSHIPS OF CALAMOPS PALUDOSUS (TEMNOSPONDYLI, STEREOSPONDYLI) FROM THE TRIASSIC OF THE NEWARK BASIN, PENNSYLVANIA SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID MIDDLE; MICROPOSAURUS; AMPHIBIANS AB The holotype of the large temnospondyl Calamops paludosus is the oldest known tetrapod fossil from the Triassic of the Newark basin in Pennsylvania. Although it is usually placed in Metoposauridae, its affinities have remained unknown since its original description because the unique specimen had never been prepared. Preparation and casting of the specimen, which comprises three pieces of a left mandibular ramus, now permits detailed anatomical description of the jaw and assessment of its affinities. Calamops paludosus is a valid taxon of trematosauroid temnospondyls that can be diagnosed by several autapomorphies. It represents one of the geologically youngest known records of long-snouted trematosaurs and the first record of these temnospondyls from the Late Triassic of North America. C1 [Sues, Hans-Dieter] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20013 USA. [Schoch, Rainer R.] Staatliches Museum Nat Kunde Stuttgart, D-70191 Stuttgart, Germany. RP Sues, HD (reprint author), Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu; rainer.schoch@smns-bw.de FU Alexander von Humboldt Foundation FX We are indebted to the late D. Baird for the casts of Calamops paludosus and associated data, A. D. Lewis for his excellent preparation work, and P. E. Olsen for many informative discussions on the geology and paleontology of the Newark Supergroup. H.-D.S. gratefully acknowledges an Award for Excellence in Research and Teaching from the Alexander von Humboldt Foundation. We thank J.-S. Steyer and especially A. Warren for helpful comments on the manuscript. NR 38 TC 2 Z9 2 U1 0 U2 4 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD SEP 1 PY 2013 VL 33 IS 5 BP 1061 EP 1070 DI 10.1080/02724634.2013.759120 PG 10 WC Paleontology SC Paleontology GA 213GH UT WOS:000324042900005 ER PT J AU Mikheyev, AS McBride, CS Mueller, UG Parmesan, C Smee, MR Stefanescu, C Wee, B Singer, MC AF Mikheyev, Alexander S. McBride, Carolyn S. Mueller, Ulrich G. Parmesan, Camille Smee, Melanie R. Stefanescu, Constanti Wee, Brian Singer, Michael C. TI Host-associated genomic differentiation in congeneric butterflies: now you see it, now you do not SO MOLECULAR ECOLOGY LA English DT Article DE Castilleja; Collinsia; Lonicera; Nymphalidae; Pedicularis; Succisa ID PARTIAL MANTEL TESTS; ADAPTIVE GENETIC-DIVERGENCE; LONG-DISTANCE DISPERSAL; APPLE MAGGOT FLY; ECOLOGICAL SPECIATION; EUPHYDRYAS-EDITHA; LOCAL ADAPTATION; CHECKERSPOT BUTTERFLIES; REPRODUCTIVE ISOLATION; SYMPATRIC SPECIATION AB Ecotypic variation among populations may become associated with widespread genomic differentiation, but theory predicts that this should happen only under particular conditions of gene flow, selection and population size. In closely related species, we might expect the strength of host-associated genomic differentiation (HAD) to be correlated with the degree of phenotypic differentiation in host-adaptive traits. Using microsatellite and Amplified Fragment Length Polymorphism (AFLP) markers, and controlling for isolation by distance between populations, we sought HAD in two congeneric species of butterflies with different degrees of host plant specialization. Prior work on Euphydryas editha had shown strong interpopulation differentiation in host-adapted traits, resulting in incipient reproductive isolation among host-associated ecotypes. We show here that Euphydryas aurinia had much weaker host-associated phenotypic differentiation. Contrary to our expectations, we detected HAD in Euphydryas aurinia, but not in E.editha. Even within an E.aurinia population that fed on both hosts, we found weak but significant sympatric HAD that persisted in samples taken 9years apart. The finding of significantly stronger HAD in the system with less phenotypic differentiation may seem paradoxical. Our findings can be explained by multiple factors, ranging from differences in dispersal or effective population size, to spatial variation in genomic or phenotypic traits and to structure induced by past histories of host-adapted populations. Other infrequently measured factors, such as differences in recombination rates, may also play a role. Our result adds to recent work as a further caution against assumptions of simple relationships between genomic and adaptive phenotypic differentiation. C1 [Mikheyev, Alexander S.] Okinawa Inst Sci & Technol, Okinawa 9040495, Japan. [McBride, Carolyn S.] Rockefeller Univ, Lab Neurogenet & Behav, New York, NY 10021 USA. [Mueller, Ulrich G.; Parmesan, Camille; Singer, Michael C.] Univ Texas Austin, Austin, TX 78712 USA. [Parmesan, Camille] Univ Plymouth, Inst Marine, Plymouth PL4 8AA, Devon, England. [Smee, Melanie R.] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England. [Stefanescu, Constanti] Museo Ciencies Nat, Catalan Butterfly Monitoring Scheme, Granollers 08402, Spain. [Stefanescu, Constanti] CREAF, Global Ecol Unit, Cerdanyola Del Valles 08193, Spain. [Wee, Brian] Smithsonian Inst, NEON Inc, Washington, DC 20560 USA. [Singer, Michael C.] Univ Plymouth, Sch Biomed & Biol Sci, Plymouth PL4 8AA, Devon, England. RP Mikheyev, AS (reprint author), Okinawa Inst Sci & Technol, Okinawa 9040495, Japan. EM sasha@homologo.us RI Mikheyev, Alexander/O-7670-2014; Smee, Melanie/K-4201-2015 OI Mikheyev, Alexander/0000-0003-4369-1019; Smee, Melanie/0000-0002-6973-0365 FU San Diego Foundation; NSF [DEB-0215436, DEB-0815145]; Ulrich Mueller; Okinawa Institute of Science and Technology; Howard Hughes Medical Institute FX We are most grateful to Jordi Artola, Agnes Batlle, Rafel Carbonell, Henri Descimon, Juexin Jiang, Mark Kirkpatrick, Michael Lockwood, James Mallet, Toni Marine, Joan Strassman, Tanya Vo and Chris Wheat. Funding was provided by the authors, by the San Diego Foundation and by NSF DEB-0215436 to MCS and Ulrich Mueller and by the Okinawa Institute of Science and Technology. CSM was supported by NSF DEB-0815145 to Michael Turelli during the early stages of this work and by the Howard Hughes Medical Institute. NR 90 TC 6 Z9 6 U1 4 U2 48 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD SEP PY 2013 VL 22 IS 18 BP 4753 EP 4766 DI 10.1111/mec.12423 PG 14 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 212ZP UT WOS:000324022600013 PM 23927539 ER PT J AU Hayasaki, K Stone, N Loeb, A AF Hayasaki, Kimitake Stone, Nicholas Loeb, Abraham TI Finite, intense accretion bursts from tidal disruption of stars on bound orbits SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; gravitational waves; hydrodynamics ID MASSIVE BLACK-HOLE; CENTER CLOUD G2; X-RAY OUTBURSTS; GALACTIC-CENTER; STELLAR DISRUPTION; BINARIES; NUCLEI; DISKS; SIMULATIONS; SYSTEMS AB We study accretion processes for tidally disrupted stars approaching supermassive black holes on bound orbits, by performing three-dimensional smoothed particle hydrodynamics simulations with a pseudo-Newtonian potential. We find that there is a critical value of the orbital eccentricity below which all the stellar debris remains bound to the black hole. For high but subcritical eccentricities, all the stellar mass is accreted on to the black hole in a finite time, causing a significant deviation from the canonical t(-5/3) mass fallback rate. When a star is on a moderately eccentric orbit and its pericentre distance is deeply inside the tidal disruption radius, there can be several orbit crossings of the debris streams due to relativistic precession. This dissipates orbital energy in shocks, allowing for rapid circularization of the debris streams and formation of an accretion disc. The resultant accretion rate greatly exceeds the Eddington rate and differs strongly from the canonical rate of t(-5/3). By contrast, there is little dissipation due to orbital crossings for the equivalent simulation with a purely Newtonian potential. This shows that general relativistic precession is crucial for accretion disc formation via circularization of stellar debris from stars on moderately eccentric orbits. C1 [Hayasaki, Kimitake] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hayasaki, Kimitake; Stone, Nicholas; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hayasaki, Kimitake] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. RP Hayasaki, K (reprint author), Kyoto Univ, Dept Astron, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. EM kimi@kusastro.kyoto-u.ac.jp RI Hayasaki, Kimitake/B-3192-2015 OI Hayasaki, Kimitake/0000-0003-4799-1895 FU Ministry of Education, Science, Culture, and Sport and Technology [21540304, 22340045, 22540243, 23540271]; Education and Research Promotion Foundation in Kyoto University; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX The authors thank to the anonymous referee for fruitful comments and suggestions, and thank to Ramesh Narayan for helpful discussions about the recent G2 problem. KH is also grateful to Atsuo. T Okazaki, Takahiro Tanaka and Shin Mineshige for helpful discussions and their continuous encouragement. The numerical simulations reported here were performed using the computer facilities of Yukawa Institute of Theoretical Physics, Kyoto University and Harvard-Smithsonian Center for Astrophysics, Harvard University. This work was supported in part by the Grants-in-Aid of the Ministry of Education, Science, Culture, and Sport and Technology [21540304, 22340045, 22540243, 23540271 KH], Education and Research Promotion Foundation in Kyoto University [KH], and NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A [NS, AL]. NR 68 TC 39 Z9 39 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2013 VL 434 IS 2 BP 909 EP 924 DI 10.1093/mnras/stt871 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207XO UT WOS:000323638200001 ER PT J AU Fu, J Kauffmann, G Huang, ML Yates, RM Moran, S Heckman, TM Dave, R Guo, Q Henriques, BMB AF Fu, Jian Kauffmann, Guinevere Huang, Mei-ling Yates, Robert M. Moran, Sean Heckman, Timothy M. Dave, Romeel Guo, Qi Henriques, Bruno M. B. TI Star formation and metallicity gradients in semi-analytic models of disc galaxy formation SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: formation; ISM: atoms; ISM: molecules; galaxies: evolution; galaxies: formation; galaxies: ISM ID GALACTIC ABUNDANCE GRADIENT; TO-MOLECULAR TRANSITION; IRAM LEGACY SURVEY; RADIAL GAS-FLOWS; PROBE WMAP OBSERVATIONS; I MASS FUNCTION; MILKY-WAY DISK; CHEMICAL EVOLUTION; H-I; NEARBY GALAXIES AB We have updated our radially resolved semi-analytic models (SAMs) of galaxy formation, which track both the atomic and molecular gas phases of the interstellar medium. The models are adapted from those of Guo et al. using similar methodology as by Fu et al. and are run on halo merger trees from the Millennium and Millennium-II simulations with the following main changes. (1) We adopt a simple star formation law Sigma(SFR) Sigma(H2). (2) We inject the heavy elements produced by supernovae directly into the halo hot gas, instead of first mixing them with the cold gas in the disc. (3) We include radial gas inflows in discs using a model of the form v(inflow) = alpha r. The models are used to study the radial profiles of star formation rate and gas-phase metallicity in present-day galaxies. The surface density profiles of molecular gas in L-* galaxies place strong constraints on inflow velocities, favouring models where v(inflow) similar to 7 km s(-1) at a galactocentric radius of 10 kpc. Radial gas inflow has little influence on gas-phase and stellar metallicity gradients, which are affected much more strongly by the fraction of metals that are directly injected into the halo gas, rather than mixed with the cold gas. Metals ejected out of the galaxy in early epochs result in late infall of pre-enriched gas and flatter present-day gas-phase metallicity gradients. A prescription in which 80 per cent of the metals are injected into the halo gas results in good fits to the flat observed metallicity gradients in galaxies with stellar masses greater than 10(10) M-circle dot, as well as the relations between gas-phase metallicity and specific star formation rate in the outer parts of galactic discs. We examine the correlation between the gas-phase metallicity gradient and global galaxy properties, finding that it is most strongly correlated with the bulge-to-total ratio of the galaxy. This is because gas is consumed when the bulge forms during galaxy mergers, and the gas-phase metallicity gradient is then set by newly accreted gas. C1 [Fu, Jian; Kauffmann, Guinevere; Huang, Mei-ling; Yates, Robert M.; Henriques, Bruno M. B.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Fu, Jian] Chinese Acad Sci, Shanghai Astron Observ, Key Lab Res Galaxies & Cosmol, Shanghai 200030, Peoples R China. [Moran, Sean] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Heckman, Timothy M.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Dave, Romeel] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Guo, Qi] Univ Durham, Inst Computat Cosmol, Dept Phys, Durham DH1 3LE, England. [Guo, Qi] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. RP Fu, J (reprint author), Max Planck Inst Astrophys, D-85741 Garching, Germany. EM fujian@mpa-garching.mpg.de OI Henriques, Bruno/0000-0002-1392-489X FU National Science Foundation of China [11173044]; Shanghai Committee of Science and Technology [12ZR1452700] FX We are grateful to the comments from the anonymous referee. JF acknowledges the support from the National Science Foundation of China No. 11173044 and the Shanghai Committee of Science and Technology grant No. 12ZR1452700. NR 110 TC 22 Z9 23 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 SEP PY 2013 VL 434 IS 2 BP 1531 EP 1548 DI 10.1093/mnras/stt1117 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207XO UT WOS:000323638200046 ER PT J AU McGarvey, JC Bourg, NA Thompson, JR McShea, WJ Shen, XL AF McGarvey, Jennifer C. Bourg, Norman A. Thompson, Jonathan R. McShea, William J. Shen, Xiaoli TI Effects of Twenty Years of Deer Exclusion on Woody Vegetation at Three Life-History Stages in a Mid-Atlantic Temperate Deciduous Forest SO NORTHEASTERN NATURALIST LA English DT Article ID WHITE-TAILED DEER; ODOCOILEUS-VIRGINIANUS ZIMMERMAN; BROWSING PRESSURE; ACORN CROPS; GREAT-LAKES; SUGAR MAPLE; GROWTH; PLANT; USA; REGENERATION AB Chronic browsing by Odocoileus virginianus (White-tailed Deer) has potential to alter the life history of trees within Mid-Atlantic forests, including seedling size and abundance in the short term to overstory composition in the long term. Most studies quantify the effects of deer browse using small plots (<1 ha) and short time frames (<10 years), which may misrepresent larger-scale and longer-term impacts. We maintained a 4-ha deer exclusion plot for 20 years in a mesic northern Virginia temperate deciduous forest to examine the impacts of browsing on forest trees at multiple life-history stages. We compared the abundance and species composition, as well as seedling height, of woody stems across the seedling, small-sapling, and large-sapling size classes inside the deer exclosure and within an adjacent reference area. There were no significant differences in seedling abundance or community composition, but seedling height was on average 2.25 times greater in the exclosure than the reference plot. Small-sapling (1-5 cm DBH) stem count was 4.1 times greater inside the exclosure, with all species more abundant in the exclosure except Asimina triloba (Pawpaw) and Carya tomentosa (Mockernut Hickory). Differences were smaller in the large-sapling size class (5-10 cm DBH), with relative total large-sapling stem count only 1.25 times greater in the exclosure. Browsing pressure appeared to influence the composition and size structure of smaller stems in the past 20 years, but has had little effect on larger stems. While the lack of replication limited the scope of inference of our study, our findings suggest that natural delays in mature tree recruitment in a closed-canopy forest may mask the full impact of deer herbivory for decades. C1 [McGarvey, Jennifer C.; Bourg, Norman A.; Thompson, Jonathan R.; McShea, William J.; Shen, Xiaoli] Smithsonian Inst, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [McGarvey, Jennifer C.] Univ Virginia, Dept Environm Sci, Charlottesville, VA 22903 USA. RP Thompson, JR (reprint author), Smithsonian Inst, Smithsonian Conservat Biol Inst, 1500 Remount Rd, Front Royal, VA 22630 USA. EM thompsonjr@si.edu OI Bourg, Norman/0000-0002-7443-1992 FU HSBC Climate Partnership; SIGEO Initiative; Smithsonian Institution FX Establishment of the SCBI SIGEO plot by William McShea and Norman Bourg was funded by the HSBC Climate Partnership, the SIGEO Initiative and the Smithsonian Institution. Numerous technicians, interns, and volunteers of the Conservation Ecology Center at SCBI were essential in assisting with plot establishment and data collection, most notably Shawn Behling, Megan Baker, Sumana Serchan, and Chris Lewis. Support for the original fence installation was provided by Friends of the National Zoo and Earthwatch. Additional thanks to Richard Lucas, John Parker, and the anonymous reviewers for Northeastern Naturalist for their helpful comments on later drafts of the paper. NR 56 TC 7 Z9 7 U1 8 U2 111 PU HUMBOLDT FIELD RESEARCH INST PI STEUBEN PA PO BOX 9, STEUBEN, ME 04680-0009 USA SN 1092-6194 J9 NORTHEAST NAT JI Northeast. Nat PD SEP PY 2013 VL 20 IS 3 BP 451 EP 468 DI 10.1656/045.020.0301 PG 18 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 217QU UT WOS:000324375700008 ER PT J AU Kilpatrick, AM Peters, RJ Dupuis, AP Jones, MJ Daszak, P Marra, PP Kramer, LD AF Kilpatrick, A. Marm Peters, Ryan J. Dupuis, Alan P., II Jones, Matthew J. Daszak, Peter Marra, Peter P. Kramer, Laura D. TI Predicted and observed mortality from vector-borne disease in wildlife: West Nile virus and small songbirds SO BIOLOGICAL CONSERVATION LA English DT Article DE Disease; Population; Birds; Epidemiology; West Nile virus; Conservation ID INFECTIOUS-DISEASE; DIPTERA-CULICIDAE; EMERGING DISEASE; BRIDGE VECTOR; AVIAN HOSTS; BIRDS; CULEX; TRANSMISSION; MOSQUITOS; IMPACT AB Numerous diseases of wildlife have recently emerged due to trade and travel. However, the impact of disease on wild animal populations has been notoriously difficult to detect and demonstrate, due to problems of attribution and the rapid disappearance of bodies after death. Determining the magnitude of avian mortality from West Nile virus (WNV) is emblematic of these challenges. Although correlational analyses have shown population declines coincident with the arrival of the virus, strong inference of WNV as a cause of mortality or a population decline requires additional evidence. We show how integrating field data on mosquito feeding patterns, avian abundance, and seroprevalence can be used to predict relative mortality from vector-borne pathogens. We illustrate the method with a case study on WNV in three species of small songbirds, tufted titmouse (Baeolophus bicolor), Carolina wrens (Thryothorus ludovicianus), and northern cardinals (Cardinalis cardinalis). We then determined mortality, infectiousness, and behavioral response of wrens and titmouse following infection with WNV in laboratory experiments and compared them to a previous study on WNV mortality in cardinals. In agreement with predictions, we found titmouse had the highest mortality from WNV infection, with 100% of 11 birds perishing within 7 days after infection. Mortality in wrens was significantly lower at 27% (3/11), but still substantial. Viremia profiles indicated that both species were highly infectious for WNV and could play roles in WNV amplification. These findings suggest that WNV may be killing many small-bodied birds, despite the absence of large numbers of dead birds being observed and testing positive for WNV. More broadly, they illustrate the utility of a framework for predicting relative mortality in hosts from vector-borne disease. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Kilpatrick, A. Marm; Peters, Ryan J.] Univ Calif Santa Cruz, Santa Cruz, CA 95060 USA. [Peters, Ryan J.; Dupuis, Alan P., II; Jones, Matthew J.; Kramer, Laura D.] New York State Dept Hlth, Wadsworth Ctr, Slingerlands, NY 12159 USA. [Kilpatrick, A. Marm; Daszak, Peter] Ecohlth Alliance, New York, NY 10001 USA. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Kilpatrick, AM (reprint author), Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, EE Biol EMS, UCSC, Santa Cruz, CA 95060 USA. EM akilpatr@ucsc.edu FU NSF [EF-0914866]; NIH [1R01AI090159-01]; NIAID [NO1-AI-25490] FX We thank Will Janousek for assistance capturing and transporting birds, the Smithsonian's Neighborhood Nestwatch program and residents, the staff of Rock Creek Park (Meadowside Nature Center), Fort Dupont Park, the Smithsonian National Museum of Natural History, the National Gallery of Art and the Hirshhorn museum for permission to use their property. We are indebted to Montgomery County Parks and the Patuxent National Wildlife Refuge for permission to use birds from these lands for this study. Funding was provided by NSF Grant EF-0914866, NIH Grant 1R01AI090159-01, and NIAID Contract #NO1-AI-25490. Birds were collected under USFWS permit MB177891-1. Experimental infection studies were approved by the Wadsworth Center, New York State Department of Health, animal use protocol 09-412. NR 51 TC 6 Z9 6 U1 1 U2 49 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 SEP PY 2013 VL 165 BP 79 EP 85 DI 10.1016/j.biocon.2013.05.015 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 210YQ UT WOS:000323871700010 PM 23956457 ER PT J AU McCauley, DJ Power, EA Bird, DW McInturff, A Dunbar, RB Durham, WH Micheli, F Young, HS AF McCauley, Douglas J. Power, Eleanor A. Bird, Douglas W. McInturff, Alex Dunbar, Robert B. Durham, William H. Micheli, Fiorenza Young, Hillary S. TI Conservation at the edges of the world SO BIOLOGICAL CONSERVATION LA English DT Review DE Remote; Ecosystem service; Tourism; Community; Biodiversity; Conservation; GIS; Protected area ID BIODIVERSITY CONSERVATION; CONNECTIVITY; ECOTOURISM; MANAGEMENT; DEGRADATION; ECOSYSTEMS; SERVICES; ISLANDS; TOURISM; PEOPLE AB Remote areas harbor some of the world's most undisturbed ecosystems. Major conservation gains can be made by effectively protecting nature in these remote zones. Conducting conservation work in remote settings presents both unique challenges and promising opportunities. We discuss how five commonly used approaches for conservation (buy and protect conservation; conservation motivated by the intrinsic values of nature; ecosystem service based conservation; ecotourism driven conservation; and conservation enabled by community planning) can be optimally applied to protect ecosystems in these special settings. In this discussion we draw examples from two model remote sites: Palmyra and Tabuaeran Atolls. Spatial analyses conducted using population density as a proxy for remoteness indicate that many existing recognized protected areas already include remote regions, but that the vast majority of the overall remote zones on the planet are not yet formally protected. Initiating discussions that directly consider both the roadblocks and opportunities for conservation in remote areas will help increase our odds of successfully protecting biodiversity in these unique and strategically important contexts. (C) 2013 Elsevier Ltd. All rights reserved. C1 [McCauley, Douglas J.; Micheli, Fiorenza] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Power, Eleanor A.; Bird, Douglas W.; Durham, William H.] Stanford Univ, Dept Anthropol, Stanford, CA 94305 USA. [McInturff, Alex; Dunbar, Robert B.] Stanford Univ, Dept Environm Earth Syst Sci, Stanford, CA 94305 USA. [Young, Hillary S.] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Young, Hillary S.] Harvard Univ, Ctr Environm, Cambridge, MA 02138 USA. [Young, Hillary S.] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. RP McCauley, DJ (reprint author), Univ Calif Berkeley, Dept Environm Sci Policy & Management, 130 Mulford Hall, Berkeley, CA 94720 USA. EM mccauley@berkeley.edu FU Woods Institute for the Environment; National Science Foundation FX We thank the Woods Institute for the Environment and the National Science Foundation for funding support. This represents contribution number PARC-0096 from the Palmyra Atoll Research Consortium. NR 56 TC 12 Z9 12 U1 2 U2 95 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 SEP PY 2013 VL 165 BP 139 EP 145 DI 10.1016/j.biocon.2013.05.026 PG 7 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 210YQ UT WOS:000323871700016 ER PT J AU Baker, DM Rodriguez-Martinez, RE Fogel, ML AF Baker, D. M. Rodriguez-Martinez, R. E. Fogel, M. L. TI Tourism's nitrogen footprint on a Mesoamerican coral reef SO CORAL REEFS LA English DT Article DE Mesoamerican barrier reef; Coastal aquifers; Stable isotope; Nitrogen; Eutrophication; Coral; Sewage; Tourism; Gorgonian; Monitoring; Gorgonia ventalina ID GROUNDWATER DISCHARGE; SPATIAL PATTERNS; SEWAGE POLLUTION; WATER-QUALITY; COASTAL ZONE; DELTA-N-15; MEXICO; ECOSYSTEM; YUCATAN; FLORIDA AB Globally, the eutrophication of coastal marine environments is a worsening problem that is accelerating the loss of biodiversity and ecosystem services. Coral reefs are among the most sensitive to this change, as chronic inputs of agricultural and wastewater effluents and atmospheric deposition disrupt their naturally oligotrophic state. Often, anthropogenic alteration of the coastal nitrogen pool can proceed undetected as rapid mixing with ocean waters can mask chronic and ephemeral nitrogen inputs. Monitoring nitrogen stable isotope values (delta N-15) of benthic organisms provides a useful solution to this problem. Through a 7-yr monitoring effort in Quintana Roo, Mexico, we show that delta N-15 values of the common sea fan Gorgonia ventalina were more variable near a developed (Akumal) site than at an undeveloped (Mahahual) site. Beginning in 2007, the global recession decreased tourist visitations to Akumal, which corresponded with a pronounced 1.6 aEuro degrees decline in sea fan delta N-15 through 2009, at which time delta N-15 values were similar to those from Mahahual. With the recovery of tourism, delta N-15 values increased to previous levels. Overall, 84 % of the observed variation in delta N-15 was explained by tourist visitations in the preceding year alone, indicating that variable nitrogen source contributions are correlated with sea fan delta N-15 values. We also found that annual precipitation accounted for some variation in delta N-15, likely due to its role in groundwater flushing into the sea. Together, these factors accounted for 96 % of the variation in delta N-15. Using a mixing model, we estimate that sewage can account for up to 42 % of nitrogen in sea fan biomass. These findings illustrate the high connectivity between land-based activities and coral reef productivity and the measurable impact of the tourism industry on the ecosystem it relies on. C1 [Baker, D. M.] Natl Museum Nat Hist, Marine Sci Network, Smithsonian Inst, Washington, DC 20004 USA. [Baker, D. M.; Fogel, M. L.] Carnegie Inst Sci, Geophys Lab, Washington, DC 20015 USA. [Rodriguez-Martinez, R. E.] Univ Nacl Autonoma Mexico, Unidad Acad Puerto Morelos, Inst Ciencias Mar & Limnol, Cancun 77500, QR, Mexico. RP Baker, DM (reprint author), Univ Hong Kong, Sch Biol Sci, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China. EM dbaker@ciw.edu FU Coral Disease Working Group of the Global Environment Facility Coral Targeted Research program; W.M. Keck Foundation; U.S. Environmental Protection Agency Science to Achieve Results fellowship; Smithsonian Marine Science Network Fellowship FX Special thanks to CD Harvell, E Jordan-Dahlgren, MA Maldonado, AG Jordan-Garza, L. Vazquez, P Sanchez-Navarro, and the Centro Ecologico Akumal for logistical support. J Garcia Barbabosa and the staff of Bucaneros del Caribe, and the staff of La Posada de los 40 Canones assisted with sample collection in Mahahual. We thank CW Kwan for statistical advising. This work was supported by the Coral Disease Working Group of the Global Environment Facility Coral Targeted Research program, the W.M. Keck Foundation to MLF, a U.S. Environmental Protection Agency Science to Achieve Results fellowship to DMB, and a Smithsonian Marine Science Network Fellowship to DMB. The authors claim no conflict of interest with this work. NR 44 TC 11 Z9 11 U1 8 U2 138 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0722-4028 J9 CORAL REEFS JI Coral Reefs PD SEP PY 2013 VL 32 IS 3 BP 691 EP 699 DI 10.1007/s00338-013-1040-2 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 197TQ UT WOS:000322874500009 ER PT J AU Fowler, AE Muirhead, JR Taylor, RB AF Fowler, Amy E. Muirhead, Jim R. Taylor, Richard B. TI EARLY STAGES OF A NEW ZEALAND INVASION BY CHARYBDIS JAPONICA (A. MILNE-EDWARDS, 1861) (BRACHYURA: PORTUNIDAE) FROM ASIA: BEHAVIORAL INTERACTIONS WITH A NATIVE CRAB SPECIES SO JOURNAL OF CRUSTACEAN BIOLOGY LA English DT Article DE competition; introduced; invasive; marine; Ovalipes catharus; prey ID CARCINUS-MAENAS; SHORE CRAB; GREEN CRAB; SUCCESS; BIODIVERSITY; HEMIGRAPSUS; AGGRESSION; RESISTANCE; PREDATION; HABITATS AB The Asian paddle crab, Charybdis japonica (A. Milne-Edwards, 1861), is a relatively recent invader (approx. 10 years) to northeastern New Zealand, and its large size and aggressive nature makes it a potentially formidable competitor with native species. The only endemic, similarly sized, New Zealand paddle crab, Ovalipes catharus (White and Doubleday, 1843), overlaps frequently with C. japonica in both habitat and diet. To understand their probable interactions in the field, we performed a series of experimental behavioral trials in a closed laboratory system to determine whether the crabs interact antagonistically over a shared prey resource (Perna canaliculus (Gmelin, 1791) - green-lipped mussel). In interspecific trials, C. japonica frequently displaced both sexes of O. catharus from the prey, while O. catharus usually failed to acquire prey from feeding C. japonica. In addition, male C. japonica dominated both male and female O. catharus in one-on-one competition for food, regardless of which crab possessed the food initially. Overall, male C. japonica behaved aggressively towards O. catharus and conspecifics of equal size when competing for a prey item; O. catharus showed low levels of aggression throughout all trials and increased time spent evading C. japonica as compared to C. japonica's high levels of aggression. Our research highlights the importance of understanding how aggressive behavior may influence establishment success of invading species. C1 [Fowler, Amy E.] Univ Auckland, Leigh Marine Lab, Warkworth 0941, New Zealand. [Muirhead, Jim R.; Taylor, Richard B.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Fowler, AE (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM fowlera@si.edu FU J. William Fulbright New Zealand Graduate scholarship; University of Auckland J. William Fulbright scholarship FX This research was supported by a J. William Fulbright New Zealand Graduate scholarship and University of Auckland J. William Fulbright scholarship to A.E.F. and was completed under University of Auckland Animal Ethics permit R737. Field support was provided by A. Fukunaga and C. Bedford. N. Herbert, D. Cook and M. Birch provided experimental equipment and assisted in experimental design. M. Minton was invaluable for his statistical advice. We sincerely thank J. Canning-Clode, A.M.H. Blakeslee, C.L. McLay and two anonymous reviewers for their comments, which significantly improved this manuscript. NR 55 TC 2 Z9 2 U1 5 U2 37 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 SEP PY 2013 VL 33 IS 5 BP 672 EP 680 DI 10.1163/1937240X-00002177 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 210SU UT WOS:000323855600009 ER PT J AU Evans, JD Brown, SJ Hackett, KJ Robinson, G Richards, S Lawson, D Elsik, C Coddington, J Edwards, O Emrich, S Gabaldon, T Goldsmith, M Hanes, G Misof, B Munoz-Torres, M Niehuis, O Papanicolaou, A Pfrender, M Poelchau, M Purcell-Miramontes, M Robertson, HM Ryder, O Tagu, D Torres, T Zdobnov, E Zhang, GJ Zhou, X AF Evans, Jay D. Brown, Susan J. Hackett, Kevin J. Robinson, Gene Richards, Stephen Lawson, Daniel Elsik, Christine Coddington, Jonathan Edwards, Owain Emrich, Scott Gabaldon, Toni Goldsmith, Marian Hanes, Glenn Misof, Bernard Munoz-Torres, Monica Niehuis, Oliver Papanicolaou, Alexie Pfrender, Michael Poelchau, Monica Purcell-Miramontes, Mary Robertson, Hugh M. Ryder, Oliver Tagu, Denis Torres, Tatiana Zdobnov, Evgeny Zhang, Guojie Zhou, Xin CA i5K Consortium TI The i5K Initiative:Advancing Arthropod Genomics for Knowledge, Human Health,Agriculture, and the Environment i5K CONSORTIUM SO JOURNAL OF HEREDITY LA English DT Article DE comparative genomics; disease vector; agriculture; insect evolution; genome sequencing ID SEQUENCE AB Insects and their arthropod relatives including mites, spiders, and crustaceans play major roles in the world's terrestrial, aquatic, and marine ecosystems. Arthropods compete with humans for food and transmit devastating diseases. They also comprise the most diverse and successful branch of metazoan evolution, with millions of extant species. Here, we describe an international effort to guide arthropod genomic efforts, from species prioritization to methodology and informatics. The 5000 arthropod genomes initiative (i5K) community met formally in 2012 to discuss a roadmap for sequencing and analyzing 5000 high-priority arthropods and is continuing this effort via pilot projects, the development of standard operating procedures, and training of students and career scientists, With university, governmental, and industry support, the i5K Consortium aspires to deliver sequences and analytical tools for each of the arthropod branches and each of the species having beneficial and negative effects on humankind. C1 [Evans, Jay D.; Hackett, Kevin J.; Hanes, Glenn] USDA ARS, Beltsville, MD USA. [Brown, Susan J.] Kansas State Univ, Manhattan, KS 66506 USA. [Robinson, Gene; Robertson, Hugh M.] Univ Illinois, Urbana, IL 61801 USA. [Richards, Stephen] Baylor Coll Med, Human Genome Sequencing Ctr, Houston, TX 77030 USA. [Lawson, Daniel] European Bioinformat Inst Hinxton, Hinxton, England. [Elsik, Christine] Univ Missouri, Columbia, MO USA. [Coddington, Jonathan] Smithsonian Inst NMNH, Washington, DC USA. [Edwards, Owain] CSIRO, Ctr Environm & Life Sci, Floreat, Australia. [Emrich, Scott; Pfrender, Michael] Univ Notre Dame, South Bend, IN USA. [Gabaldon, Toni] Ctr Genom Regulat, Barcelona, Spain. [Goldsmith, Marian] Univ Rhode Isl, Providence, RI 02908 USA. [Misof, Bernard; Niehuis, Oliver] Ctr Mol Biodivers Res, ZFMK, Bonn, Germany. [Munoz-Torres, Monica] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Genom Div, Berkeley, CA 94720 USA. [Papanicolaou, Alexie] CSIRO Ecosyst Sci, Black Mt, Australia. [Poelchau, Monica] Georgetown Univ, Dept Biol, Washington, DC 20057 USA. [Purcell-Miramontes, Mary] Natl Inst Food & Agr, USDA, Washington, DC USA. [Ryder, Oliver] San Diego Zoo, Inst Conservat Res, San Diego, CA USA. [Tagu, Denis] INRA UMR 1349 IGEPP, Rennes, France. [Torres, Tatiana] Univ Sao Paulo, Sao Paulo, Brazil. [Zdobnov, Evgeny] Univ Geneva, Sch Med, CH-1211 Geneva, Switzerland. [Zhang, Guojie; Zhou, Xin] BGI Shenzhen, Shenzhen, Peoples R China. RP Evans, JD (reprint author), ARS, USDA, Bee Res Lab, Beltsville, MD 20705 USA. EM jay.evans@ars.usda.gov; kevin.hackett@ars.usda.gov; generobi@illinois.edu; stephenr@hgsc.bcm.edu; lawson@ebi.ac.uk; elsikc@missouri.edu; coddington@si.edu; owain.edwards@csixo.au; semrich@nd.edu; toni.gabaldon@crg.es; mki101@uri.edu; Glenn.Hanes@ars.usda.gov; b.misof.zfmk@uni-bonn.de; mcmunozt@lbl.gov; o.niehuis.zfmk@uni-bonn.de; alexie.papanicolaou@csito.au; pfrender.1@nd.edu; mpoel-chau@gmail.com; mpurcell@nifa.usda.gov; hughrobe@life.uiuc.edu; oryder@sandiegozoo.org; denis.tagu@rennes.inra.fr; tttorres@ib.usp.br; evgeny.zdobnov@unige.ch; zhanggj@genomics.org.cn; xinzhou@genomics.org.cn RI Torres, Tatiana/B-6431-2012; UMR IGEPP, INRA/A-4054-2011; Papanicolaou, Alexie/A-1618-2011; Gabaldon, Toni/A-7336-2008; Zhou, Xin/D-4025-2009; Zdobnov, Evgeny/K-1133-2012; Elsik, Christine/C-4120-2017; Evans, Jay/C-8408-2012; Zhang, Guojie/B-6188-2014; Edwards, Owain/B-9707-2008 OI Torres, Tatiana/0000-0002-4286-3504; Papanicolaou, Alexie/0000-0002-3635-6848; Gabaldon, Toni/0000-0003-0019-1735; Zhou, Xin/0000-0002-1407-7952; Elsik, Christine/0000-0002-4248-7713; Evans, Jay/0000-0002-0036-4651; Zhang, Guojie/0000-0001-6860-1521; FU American Genetic Association; Arthropod Genomics Center (Kansas State University); US Department of Agriculture (National Institute for Food and Agriculture and Agricultural Research Service) FX American Genetic Association; the Arthropod Genomics Center (Kansas State University); and the US Department of Agriculture (National Institute for Food and Agriculture and Agricultural Research Service). NR 4 TC 64 Z9 66 U1 4 U2 35 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 0022-1503 EI 1465-7333 J9 J HERED JI J. Hered. PD SEP-OCT PY 2013 VL 104 IS 5 BP 595 EP 600 DI 10.1093/jhered/est050 PG 6 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 203LJ UT WOS:000323294400001 ER PT J AU Hong, T AF Hong, Terry TI A True Novel SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2013 VL 138 IS 14 BP 101 EP 101 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 211NZ UT WOS:000323916400067 ER PT J AU Hong, T AF Hong, Terry TI Furious Cool: Richard Pryor and the World That Made Him SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian Inst, Washington, DC 20560 USA. RP Hong, T (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD SEP 1 PY 2013 VL 138 IS 14 BP 112 EP 112 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 211NZ UT WOS:000323916400114 ER PT J AU Kipping, DM Spiegel, DS Sasselov, DD AF Kipping, David M. Spiegel, David S. Sasselov, Dimitar D. TI A simple, quantitative method to infer the minimum atmospheric height of small exoplanets SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: analytical; methods: statistical; techniques: photometric; techniques: radial velocities; planetary systems ID SUPER-EARTH GJ1214B; METAL-RICH ATMOSPHERE; GJ 1214B; TRANSMISSION SPECTRUM; EXTRASOLAR PLANET; SPECTROSCOPY; TRANSITS; SPITZER; STAR; GAS AB Amongst the many hundreds of transiting planet candidates discovered by the Kepler mission, one finds a large number of candidates with sizes between that of the Earth and Neptune. The composition of these worlds is not immediately obvious with no Solar system analogue to draw upon and there exists some ambiguity as to whether a given candidate is a rocky super-Earth or a gas-enveloped mini-Neptune. The potential scientific value and observability of the atmospheres of these two classes of worlds varies significantly, and given the sheer number of candidates in this size range, there is evidently a need for a quick, simple metric to rank whether the planets have an extended atmosphere or not. In this work, we propose a way to calculate the 'minimum atmospheric height' (R-MAH) using only a planet's radius and mass as inputs. We assume and exploit the boundary condition that the bulk composition of a solid/liquid super-Earth cannot be composed of a material lighter than that of water. Mass-radius loci above a pure-water composition planet correspond to R-MAH > 0. The statistical confidence of a planet maintaining an extended atmosphere can be therefore easily calculated to provide a simple ranking of target planets for follow-up observations. We also discuss how this metric can be useful in the interpretation of the spectra of observed planetary atmospheres. C1 [Kipping, David M.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spiegel, David S.] Inst Adv Study, Astrophys Dept, Princeton, NJ 08540 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu FU NASA; NSF [AST-0807444]; Keck Fellowship FX DMK is supported by the NASA Carl Sagan Fellowships. DSS gratefully acknowledges support from NSF grant AST-0807444 and the Keck Fellowship, and the Friends of the Institute. We are very grateful to Guillem Anglada-Escude and collaborators for kindly sharing their posteriors with us for GJ 1214b and to Josh Carter for useful conversations on Kepler-36. Special thanks to the anonymous reviewers for their helpful comments. NR 32 TC 9 Z9 9 U1 0 U2 4 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 SEP PY 2013 VL 434 IS 3 BP 1883 EP 1888 DI 10.1093/mnras/stt1050 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207YE UT WOS:000323639900005 ER PT J AU Abramowski, A Acero, F Aharonian, F Akhperjanian, AG Anguner, E Anton, G Balenderan, S Balzer, A Barnacka, A Becherini, Y Tjus, JB Bernlohr, K Birsin, E Bissaldi, E Biteau, J Boisson, C Bolmont, J Bordas, P Brucker, J Brun, F Brun, P Bulik, T Carrigan, S Casanova, S Cerruti, M Chadwick, PM Chalme-Calvet, R Chaves, RCG Cheesebrough, A Chretien, M Colafrancesco, S Cologna, G Conrad, J Couturier, C Dalton, M Daniel, MK Davids, ID Degrange, B Deil, C deWilt, P Dickinson, HJ Djannati-Atai, A Domainko, W Drury, LO Dubus, G Dutson, K Dyks, J Dyrda, M Edwards, T Egberts, K Eger, P Espigat, P Farnier, C Fegan, S Feinstein, F Fernandes, MV Fernandez, D Fiasson, A Fontaine, G Forster, A Fussling, M Gajdus, M Gallant, YA Garrigoux, T Gast, H Giebels, B Glicenstein, JF Goring, D Grondin, MH Grudzinska, M Haffner, S Hague, JD Hahn, J Harris, J Heinzelmann, G Henri, G Hermann, G Hervet, O Hillert, A Hinton, JA Hofmann, W Hofverberg, P Holler, M Horns, D Jacholkowska, A Jahn, C Jamrozy, M Janiak, M Jankowsky, F Jung, I Kastendieck, MA Katarzynski, K Katz, U Kaufmann, S Khelifi, B Kieffer, M Klepser, S Klochkov, D Kluzniak, W Kneiske, T Kolitzus, D Komin, N Kosack, K Krakau, S Krayzel, F Kruger, PP Laffon, H Lamanna, G Lefaucheur, J Lemoine-Goumard, M Lenain, JP Lennarz, D Lohse, T Lopatin, A Lu, CC Marandon, V Marcowith, A Maurin, G Maxted, N Mayer, M McComb, TJL Medina, MC Mehault, J Menzler, U Meyer, M Moderski, R Mohamed, M Moulin, E Murach, T Naumann, CL de Naurois, M Nedbal, D Niemiec, J Nolan, SJ Oakes, L Ohm, S Wilhelmi, ED Opitz, B Ostrowski, M Oya, I Panter, M Parsons, RD Arribas, MP Pekeur, NW Pelletier, G Perez, J Petrucci, PO Peyaud, B Pita, S Poon, H Puhlhofer, G Punch, M Quirrenbach, A Raab, S Raue, M Reimer, A Reimer, O Renaud, M de los Reyes, R Rieger, F Rob, L Rosier-Lees, S Rowell, G Rudak, B Rulten, CB Sahakian, V Sanchez, DA Santangelo, A Schlickeiser, R Schussler, F Schulz, A Schwanke, U Schwarzburg, S Schwemmer, S Sol, H Spengler, G Spiess, F Stawarz, L Steenkamp, R Stegmann, C Stinzing, F Stycz, K Sushch, I Szostek, A Tavernet, JP Terrier, R Tluczykont, M Trichard, C Valerius, K van Eldik, C Vasileiadis, G Venter, C Viana, A Vincent, P Volk, HJ Volpe, F Vorster, M Wagner, SJ Wagner, P Ward, M Weidinger, M White, R Wierzcholska, A Willmann, P Wornlein, A Wouters, D Zacharias, M Zajczyk, A Zdziarski, AA Zech, A Zechlin, HS Perkins, JS Ojha, R Stevens, J Edwards, PG Kadler, M AF Abramowski, A. Acero, F. Aharonian, F. Akhperjanian, A. G. Anguener, E. Anton, G. Balenderan, S. Balzer, A. Barnacka, A. Becherini, Y. Tjus, J. Becker Bernloehr, K. Birsin, E. Bissaldi, E. Biteau, J. Boisson, C. Bolmont, J. Bordas, P. Brucker, J. Brun, F. Brun, P. Bulik, T. Carrigan, S. Casanova, S. Cerruti, M. Chadwick, P. M. Chalme-Calvet, R. Chaves, R. C. G. Cheesebrough, A. Chretien, M. Colafrancesco, S. Cologna, G. Conrad, J. Couturier, C. Dalton, M. Daniel, M. K. Davids, I. D. Degrange, B. Deil, C. deWilt, P. Dickinson, H. J. Djannati-Atai, A. Domainko, W. Drury, L. O'C. Dubus, G. Dutson, K. Dyks, J. Dyrda, M. Edwards, T. Egberts, K. Eger, P. Espigat, P. Farnier, C. Fegan, S. Feinstein, F. Fernandes, M. V. Fernandez, D. Fiasson, A. Fontaine, G. Foerster, A. Fuessling, M. Gajdus, M. Gallant, Y. A. Garrigoux, T. Gast, H. Giebels, B. Glicenstein, J. F. Goering, D. Grondin, M-H. Grudzinska, M. Haeffner, S. Hague, J. D. Hahn, J. Harris, J. Heinzelmann, G. Henri, G. Hermann, G. Hervet, O. Hillert, A. Hinton, J. A. Hofmann, W. Hofverberg, P. Holler, M. Horns, D. Jacholkowska, A. Jahn, C. Jamrozy, M. Janiak, M. Jankowsky, F. Jung, I. Kastendieck, M. A. Katarzynski, K. Katz, U. Kaufmann, S. Khelifi, B. Kieffer, M. Klepser, S. Klochkov, D. Kluzniak, W. Kneiske, T. Kolitzus, D. Komin, Nu. Kosack, K. Krakau, S. Krayzel, F. Krueger, P. P. Laffon, H. Lamanna, G. Lefaucheur, J. Lemoine-Goumard, M. Lenain, J-P. Lennarz, D. Lohse, T. Lopatin, A. Lu, C-C. Marandon, V. Marcowith, A. Maurin, G. Maxted, N. Mayer, M. McComb, T. J. L. Medina, M. C. Mehault, J. Menzler, U. Meyer, M. Moderski, R. Mohamed, M. Moulin, E. Murach, T. Naumann, C. L. de Naurois, M. Nedbal, D. Niemiec, J. Nolan, S. J. Oakes, L. Ohm, S. Wilhelmi, E. de Ona Opitz, B. Ostrowski, M. Oya, I. Panter, M. Parsons, R. D. Arribas, M. Paz Pekeur, N. W. Pelletier, G. Perez, J. Petrucci, P-O. Peyaud, B. Pita, S. Poon, H. Puehlhofer, G. Punch, M. Quirrenbach, A. Raab, S. Raue, M. Reimer, A. Reimer, O. Renaud, M. de los Reyes, R. Rieger, F. Rob, L. Rosier-Lees, S. Rowell, G. Rudak, B. Rulten, C. B. Sahakian, V. Sanchez, D. A. Santangelo, A. Schlickeiser, R. Schuessler, F. Schulz, A. Schwanke, U. Schwarzburg, S. Schwemmer, S. Sol, H. Spengler, G. Spiess, F. Stawarz, L. Steenkamp, R. Stegmann, C. Stinzing, F. Stycz, K. Sushch, I. Szostek, A. Tavernet, J-P. Terrier, R. Tluczykont, M. Trichard, C. Valerius, K. van Eldik, C. Vasileiadis, G. Venter, C. Viana, A. Vincent, P. Voelk, H. J. Volpe, F. Vorster, M. Wagner, S. J. Wagner, P. Ward, M. Weidinger, M. White, R. Wierzcholska, A. Willmann, P. Woernlein, A. Wouters, D. Zacharias, M. Zajczyk, A. Zdziarski, A. A. Zech, A. Zechlin, H-S. Perkins, J. S. Ojha, R. Stevens, J. Edwards, P. G. Kadler, M. CA HESS Collaboration TI HESS and Fermi-LAT discovery of gamma-rays from the blazar 1ES 1312-423 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiation mechanisms: non-thermal; galaxies: active; BL Lacertae objects: individual: 1ES 1312-423; galaxies: jets; gamma-rays: galaxies ID BL-LACERTAE OBJECTS; LARGE-AREA TELESCOPE; ATMOSPHERIC CHERENKOV TELESCOPES; SPECTRAL ENERGY-DISTRIBUTIONS; MEDIUM-SENSITIVITY SURVEY; SOURCE CATALOG; BACKGROUND-RADIATION; COMPLETE SAMPLE; TEV BLAZARS; RADIO AB A deep observation campaign carried out by the High Energy Stereoscopic System (HESS) on Centaurus A enabled the discovery of gamma-rays from the blazar 1ES 1312-423, 2 degrees away from the radio galaxy. With a differential flux at 1 TeV of phi(1 TeV) = (1.9 +/- 0.6(stat) +/- 0.4(sys)) x 10(-13) cm(-2) s(-1) TeV-1 corresponding to 0.5 per cent of the Crab nebula differential flux and a spectral index Gamma = 2.9 +/- 0.5(stat) +/- 0.2(sys), 1ES 1312-423 is one of the faintest sources ever detected in the very high energy (E > 100 GeV) extragalactic sky. A careful analysis using three and a half years of Fermi Large Area Telescope (Fermi-LAT) data allows the discovery at high energies (E > 100 MeV) of a hard spectrum (Gamma = 1.4 +/- 0.4(stat) +/- 0.2(sys)) source coincident with 1ES 1312-423. Radio, optical, UV and X-ray observations complete the spectral energy distribution of this blazar, now covering 16 decades in energy. The emission is successfully fitted with a synchrotron self-Compton model for the non-thermal component, combined with a blackbody spectrum for the optical emission from the host galaxy. C1 [Abramowski, A.; Fernandes, M. V.; Heinzelmann, G.; Horns, D.; Kastendieck, M. A.; Kneiske, T.; Meyer, M.; Opitz, B.; Raue, M.; Spiess, F.; Tluczykont, M.; Zechlin, H-S.] Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany. [Acero, F.; Feinstein, F.; Fernandez, D.; Gallant, Y. A.; Marcowith, A.; Renaud, M.; Vasileiadis, G.; Zajczyk, A.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS, IN2P3,CC 72, F-34095 Montpellier 5, France. [Aharonian, F.; Bernloehr, K.; Brun, F.; Carrigan, S.; Casanova, S.; Chaves, R. C. G.; Deil, C.; Domainko, W.; Edwards, T.; Eger, P.; Foerster, A.; Gast, H.; Grondin, M-H.; Hague, J. D.; Hahn, J.; Hermann, G.; Hillert, A.; Hofmann, W.; Hofverberg, P.; Krueger, P. P.; Lennarz, D.; Lu, C-C.; Marandon, V.; Wilhelmi, E. de Ona; Panter, M.; Parsons, R. D.; Poon, H.; de los Reyes, R.; Rieger, F.; Sanchez, D. A.; Viana, A.; Voelk, H. J.; Volpe, F.] Max Planck Inst Kernphys, D-69029 Heidelberg, Germany. [Aharonian, F.; Drury, L. O'C.] Dublin Inst Adv Studies, Dublin 2, Ireland. [Aharonian, F.; Akhperjanian, A. G.; Sahakian, V.] Natl Acad Sci Republ Armenia, Yerevan 375019, Armenia. [Akhperjanian, A. G.; Sahakian, V.] Yerevan Phys Inst, Yerevan 375036, Armenia. [Anguener, E.; Bernloehr, K.; Birsin, E.; Gajdus, M.; Lohse, T.; Murach, T.; Oakes, L.; Oya, I.; Arribas, M. Paz; Schwanke, U.; Spengler, G.; Sushch, I.; Wagner, P.] Humboldt Univ, Inst Phys, D-12489 Berlin, Germany. [Anton, G.; Brucker, J.; Goering, D.; Haeffner, S.; Jahn, C.; Jung, I.; Katz, U.; Lopatin, A.; Raab, S.; Stinzing, F.; Valerius, K.; van Eldik, C.; Willmann, P.; Woernlein, A.] Univ Erlangen Nurnberg, Inst Phys, D-91058 Erlangen, Germany. [Balenderan, S.; Chadwick, P. M.; Cheesebrough, A.; Daniel, M. K.; Harris, J.; McComb, T. J. L.; Nolan, S. J.; Ward, M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Balzer, A.; Klepser, S.; Schulz, A.; Stegmann, C.; Stycz, K.] DESY, D-15735 Zeuthen, Germany. [Balzer, A.; Fuessling, M.; Holler, M.; Mayer, M.; Stegmann, C.] Univ Potsdam, Inst Phys & Astron, D-14476 Golm, Germany. [Barnacka, A.; Dyks, J.; Janiak, M.; Kluzniak, W.; Moderski, R.; Rudak, B.; Zajczyk, A.; Zdziarski, A. A.] Nicolaus Copernicus Astron Ctr, PL-00716 Warsaw, Poland. [Becherini, Y.; Cologna, G.; Grondin, M-H.; Jankowsky, F.; Kaufmann, S.; Mohamed, M.; Quirrenbach, A.; Schwemmer, S.; Wagner, S. J.] Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany. [Becherini, Y.; Djannati-Atai, A.; Espigat, P.; Lefaucheur, J.; Pita, S.; Punch, M.; Terrier, R.] Univ Paris Diderot, APC, CNRS, IN2P3,CEA,Irfu,Observat Paris,Sorbonne Paris Cite, F-75205 Paris 13, France. [Becherini, Y.; Biteau, J.; Degrange, B.; Fegan, S.; Fontaine, G.; Giebels, B.; Khelifi, B.; Laffon, H.; de Naurois, M.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Tjus, J. Becker; Krakau, S.; Menzler, U.; Schlickeiser, R.; Weidinger, M.; Zacharias, M.] Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany. [Bissaldi, E.; Egberts, K.; Kolitzus, D.; Perez, J.; Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Boisson, C.; Cerruti, M.; Hervet, O.; Rulten, C. B.; Sol, H.; Zech, A.] Univ Paris Diderot, CNRS, Observ Paris, LUTH, F-92190 Meudon, France. [Bolmont, J.; Chalme-Calvet, R.; Chretien, M.; Couturier, C.; Garrigoux, T.; Jacholkowska, A.; Kieffer, M.; Lenain, J-P.; Naumann, C. L.; Tavernet, J-P.; Vincent, P.] Univ Paris 07, Univ Paris 06, LPNHE, CNRS,IN2P3, F-75252 Paris 5, France. [Bordas, P.; Klochkov, D.; Puehlhofer, G.; Santangelo, A.; Schwarzburg, S.] Univ Tubingen, Inst Astron & Astrophys, D-72076 Tubingen, Germany. [Brun, P.; Chaves, R. C. G.; Glicenstein, J. F.; Kosack, K.; Medina, M. C.; Moulin, E.; Peyaud, B.; Schuessler, F.; Wouters, D.] CEA Saclay, DSM, Irfu, F-91191 Gif Sur Yvette, France. [Bulik, T.; Grudzinska, M.] Univ Warsaw, Astron Observ, PL-00478 Warsaw, Poland. [Casanova, S.; Krueger, P. P.; Pekeur, N. W.; Sushch, I.; Venter, C.; Vorster, M.] North West Univ, Unit Space Phys, ZA-2520 Potchefstroom, South Africa. [Cerruti, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Colafrancesco, S.] Univ Witwatersrand, Sch Phys, ZA-2050 Johannesburg, South Africa. [Conrad, J.; Dickinson, H. J.; Farnier, C.] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, SE-10691 Stockholm, Sweden. [Dalton, M.; Laffon, H.; Lemoine-Goumard, M.; Mehault, J.] Univ Bordeaux 1, Ctr Etud Nuc Bordeaux Gradignan, CNRS, IN2P3, F-33175 Gradignan, France. [Davids, I. D.; Steenkamp, R.] Univ Namibia, Dept Phys, Windhoek, Namibia. [deWilt, P.; Maxted, N.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Dubus, G.; Henri, G.; Pelletier, G.; Petrucci, P-O.] UJF Grenoble 1, CNRS, IPAG, INSU, F-38041 Grenoble, France. [Dutson, K.; Hinton, J. A.; Ohm, S.; White, R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Dyrda, M.; Niemiec, J.] Inst Fizyki Jadrowej PAN, PL-31342 Krakow, Poland. [Fiasson, A.; Komin, Nu.; Krayzel, F.; Lamanna, G.; Maurin, G.; Rosier-Lees, S.; Trichard, C.] Univ Savoie, Lab Annecy Le Vieux Phys Particules, CNRS, IN2P3, F-74941 Annecy Le Vieux, France. [Jamrozy, M.; Ostrowski, M.; Szostek, A.; Wierzcholska, A.] Uniwersytet Jagiellonski, Obserwatorium Astronomiczne, PL-30244 Krakow, Poland. [Katarzynski, K.; Stawarz, L.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Ohm, S.] Charles Univ Prague, Inst Particle & Nucl Phys, Fac Math & Phys, CZ-18000 Prague 8, Czech Republic. [Ohm, S.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Perkins, J. S.; Kadler, M.] NASA, Goddard Space Flight Ctr, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.; Kadler, M.] NASA, Goddard Space Flight Ctr, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Ojha, R.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA. [Ojha, R.] Catholic Univ Amer, Inst Astrophys & Computat Sci, Washington, DC 20064 USA. [Stevens, J.] CSIRO Astron & Space Sci, Narrabri, NSW 2390, Australia. [Edwards, P. G.] CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Kadler, M.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. RP Abramowski, A (reprint author), Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany. EM yvonne.becherini@lsw.uni-heidelberg.de; biteau@in2p3.fr; david.sanchez@mpi-hd.mpg.de; jeremy.s.perkins@nasa.gov RI Meyer, Manuel/E-2697-2016; Bissaldi, Elisabetta/K-7911-2016; Drury, Luke/B-1916-2017; Moulin, Emmanuel/B-5959-2017; Daniel, Michael/A-2903-2010; Komin, Nukri/J-6781-2015; Casanova, Sabrina/J-8935-2013; Couturier, Camille/K-7585-2013; Tjus, Julia/G-8145-2012; Anton, Gisela/C-4840-2013; Katz, Uli/E-1925-2013; Fontaine, Gerard/D-6420-2014; van Eldik, Christopher/C-3901-2013; Venter, Christo/E-6884-2011; Reimer, Olaf/A-3117-2013; Schussler, Fabian/G-5313-2013; Katarzynski, Krzysztof/G-4528-2014; Jamrozy, Marek/F-4507-2015 OI Meyer, Manuel/0000-0002-0738-7581; Bissaldi, Elisabetta/0000-0001-9935-8106; Drury, Luke/0000-0002-9257-2270; Moulin, Emmanuel/0000-0003-4007-0145; de los Reyes Lopez, Raquel/0000-0003-0485-9552; Daniel, Michael/0000-0002-8053-7910; Chadwick, Paula/0000-0002-1468-2685; Kneiske, Tanja M./0000-0002-3210-6200; mohamed, mahmoud/0000-0002-4625-6242; Kruger, Paulus/0000-0003-0664-8521; Komin, Nukri/0000-0003-3280-0582; Casanova, Sabrina/0000-0002-6144-9122; Couturier, Camille/0000-0002-0168-1106; Anton, Gisela/0000-0003-2039-4724; Katz, Uli/0000-0002-7063-4418; van Eldik, Christopher/0000-0001-9669-645X; Venter, Christo/0000-0002-2666-4812; Reimer, Olaf/0000-0001-6953-1385; Schussler, Fabian/0000-0003-1500-6571; FU German Ministry for Education and Research (BMBF); Max Planck Society; French Ministry for Research; CNRS-IN2P3; Astroparticle Interdisciplinary Programme of the CNRS; UK Particle Physics and Astronomy Research Council (PPARC); IPNP of the Charles University; South African Department of Science and Technology; National Research Foundation; University of Namibia; Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France; Commonwealth of Australia; NASA [NNH09ZDA001N]; NASA post-doctoral Programme at the Goddard Space Flight Center FX The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of HESS is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the French Ministry for Research, the CNRS-IN2P3 and the Astroparticle Interdisciplinary Programme of the CNRS, the UK Particle Physics and Astronomy Research Council (PPARC), the IPNP of the Charles University, the South African Department of Science and Technology and National Research Foundation, and by the University of Namibia. We appreciate the excellent work of the technical support staff in Berlin, Durham, Hamburg, Heidelberg, Palaiseau, Paris, Saclay, and in Namibia in the construction and operation of the equipment.; Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research was funded in part by NASA through Fermi Guest Investigator grant NNH09ZDA001N (proposal number 31263). This research was supported by an appointment to the NASA post-doctoral Programme at the Goddard Space Flight Center, administered by Oak Ridge Associated Universities through a contract with NASA. NR 82 TC 6 Z9 7 U1 3 U2 25 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 SEP PY 2013 VL 434 IS 3 BP 1889 EP 1901 DI 10.1093/mnras/stt1081 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207YE UT WOS:000323639900006 ER PT J AU Roy, R Kumar, B Maund, JR Schady, P Olivares, EF Malesani, D Leloudas, G Nandi, S Tanvir, N Milisavljevic, D Hjorth, J Misra, K Kumar, B Pandey, SB Sagar, R Chandola, HC AF Roy, Rupak Kumar, Brijesh Maund, Justyn R. Schady, Patricia Olivares, E. Felipe Malesani, Daniele Leloudas, Giorgos Nandi, Sumana Tanvir, Nial Milisavljevic, Dan Hjorth, Jens Misra, Kuntal Kumar, Brajesh Pandey, S. B. Sagar, Ram Chandola, H. C. TI SN 2007uy-metamorphosis of an aspheric Type Ib explosion SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2007uy; galaxies: individual: NGC 2770 ID CORE-COLLAPSE SUPERNOVA; EXPANDING PHOTOSPHERE METHOD; GAMMA-RAY BURST; HUBBLE-SPACE-TELESCOPE; LIGHT CURVES; IC SUPERNOVA; IA SUPERNOVAE; STRIPPED-ENVELOPE; RADIO SUPERNOVAE; X-RAY AB The supernovae (SNe) of Type Ibc are rare and the detailed characteristics of these explosions have been studied only for a few events. Unlike Type II SNe, the progenitors of Type Ibc have never been detected in pre-explosion images. So, to understand the nature of their progenitors and the characteristics of the explosions, investigation of proximate events is necessary. Here we present the results of multiwavelength observations of Type Ib SN 2007uy in the nearby (similar to 29.5 Mpc) galaxy NGC 2770. Analysis of the photometric observations revealed this explosion as an energetic event with peak absolute R-band magnitude -18.5 +/- 0.16, which is about 1 mag brighter than the mean value (-17.6 +/- 0.6) derived for well observed Type Ibc events. The SN is highly extinguished, E(B - V) = 0.63 +/- 0.15 mag, mainly due to foreground material present in the host galaxy. From optical light curve modelling we determine that about 0.3 M-circle dot radioactive Ni-56 is produced and roughly 4.4 M-circle dot material is ejected during this explosion with liberated energy similar to 15 x 10(51) erg, indicating the event to be an energetic one. Through optical spectroscopy, we have noticed a clear aspheric evolution of several line-forming regions, but no dependency of asymmetry is seen on the distribution of Ni-56 inside the ejecta. The SN shock interaction with the circumstellar material is clearly noticeable in radio follow-up, presenting a synchrotron self-absorption dominated light curve with a contribution of free-free absorption during the early phases. Assuming a Wolf-Rayet (WR) star, with wind velocity greater than or similar to 10(3) km s(- 1), as a progenitor, we derive a lower limit to the mass-loss rate inferred from the radio data as M 2.4 10(-5) M-circle dot yr(-1), which is consistent with the results obtained for other Type Ibc SNe bright at radio frequencies. C1 [Roy, Rupak; Kumar, Brijesh; Nandi, Sumana; Misra, Kuntal; Kumar, Brajesh; Pandey, S. B.; Sagar, Ram] Aryabhatta Res Inst Observat Sci, Manora Peak 263002, Nainital, India. [Maund, Justyn R.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Schady, Patricia; Olivares, E. Felipe] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Malesani, Daniele; Leloudas, Giorgos; Hjorth, Jens] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. [Leloudas, Giorgos] Stockholm Univ, Albanova Univ Ctr, Dept Phys, Oskar Klein Ctr, S-10691 Stockholm, Sweden. [Tanvir, Nial] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Milisavljevic, Dan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chandola, H. C.] Kumaun Univ, Dept Phys, Naini Tal 263002, India. RP Roy, R (reprint author), Aryabhatta Res Inst Observat Sci, Manora Peak 263002, Nainital, India. EM roy@aries.res.in RI Hjorth, Jens/M-5787-2014; OI Hjorth, Jens/0000-0002-4571-2306; Maund, Justyn/0000-0003-0733-7215 FU ESO programs [080.C-0833, 080.D-0229, 081.D-0173, 082.D-0292]; DNRF; Swedish Research Council [623-2011-7117]; COSPAR fellowship program; DST-RFBR [INT/RFBR/P-25, INT/RFBR/P-100] FX We thank all the observers at ARIES who provided their valuable time and support for the observations of this event. The work is based on observations made with the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. This work is partly based on the data obtained from the ESO Science Archive Facility, and data were collected under ESO programs 080.C-0833 (PI Elias-Rosa), 080.D-0229 (PI Della Valle), 081.D-0173 (PI Mazzali) and 082.D-0292 (PI Mazzali). We are thankful to the observing staffs of NOT, UKIRT, NTT, MMT and VLT for their kind cooperation in observation of SN 2007uy. This work is based on the data obtained from the ESO Science Archive Facility. For this research work the VLA radio data have been used. The VLA is operated by the National Radio Astronomy Observatory, a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. DARK is funded by the DNRF. GL is supported by the Swedish Research Council through grant No. 623-2011-7117. RR is thankful to the COSPAR fellowship program under which, he got the opportunity to visit DARK and initiated the entire project. SBP and RR acknowledge DST-RFBR grants INT/RFBR/P-25 (2008-2010) and INT/RFBR/P-100 (2011-2013) for the present work. This research has made use of Swift/UVOT data obtained through the High Energy Astrophysics Science Archive Research Center (HEASARC) Online Service, provided by the NASA/Goddard Space Flight Center. The authors would also like to thank the anonymous referee for the comments and suggestions which helped in improvement of the paper. NR 110 TC 11 Z9 11 U1 0 U2 3 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 SEP PY 2013 VL 434 IS 3 BP 2032 EP 2050 DI 10.1093/mnras/stt1148 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207YE UT WOS:000323639900018 ER PT J AU Zhu, YC Narayan, R AF Zhu, Yucong Narayan, Ramesh TI Thermal stability in turbulent accretion discs SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; convection; turbulence ID ACTIVE GALACTIC NUCLEI; X-RAY SOURCES; BLACK-HOLES; VERTICAL STRUCTURE; LOCAL SIMULATIONS; ENERGY-TRANSPORT; BINARY-SYSTEMS; DISKS; INSTABILITY; MODELS AB The standard thin accretion disc model predicts that discs around stellar mass black holes become radiation-pressure dominated and thermally unstable once their luminosity exceeds L greater than or similar to 0.02L(Edd). Observationally, discs in the high/soft state of X-ray binaries show little variability in the range 0.01L(Edd) < L < 0.5L(Edd), implying that these discs in nature are in fact quite stable. In an attempt to reconcile this conflict, we investigate one-zone disc models including turbulent and convective modes of vertical energy transport. We find both mixing mechanisms to have a stabilizing effect, leading to an increase in the L threshold up to which the disc is thermally stable. In the case of stellar mass black hole systems, convection alone leads to only a minor increase in this threshold, up to similar to 5 per cent of Eddington. However, turbulent mixing has a much greater effect - the threshold rises up to 20 per cent Eddington under reasonable assumptions. In optimistic models with superefficient turbulent mixing, we even find solutions that are completely thermally stable for all accretion rates. Similar results are obtained for supermassive black holes, except that all critical accretion rates are a factor of similar to 10 lower in Eddington ratio. C1 [Zhu, Yucong; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Zhu, YC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM yzhu@cfa.harvard.edu; rnarayan@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AE16G] FX The authors would like to thank Robert Penna, Aleksander Sadowski and Dmitrios Psaltis for insightful discussions about disc convection. We thank the anonymous referee for providing illuminating comments and helping us craft a much clearer paper. YZ also thanks Tanmoy Laskar for helpful suggestions for improving the presentation of the manuscript. YZ was supported by the Smithsonian Institution Endowment Funds. This work was supported in part by NASA grant NNX11AE16G. NR 51 TC 5 Z9 5 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 SEP PY 2013 VL 434 IS 3 BP 2262 EP 2274 DI 10.1093/mnras/stt1161 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207YE UT WOS:000323639900033 ER PT J AU Rivilla, VM Martin-Pintado, J Sanz-Forcada, J Jimenez-Serra, I Rodriguez-Franco, A AF Rivilla, V. M. Martin-Pintado, J. Sanz-Forcada, J. Jimenez-Serra, I. Rodriguez-Franco, A. TI X-ray embedded stars as driving sources of outflow-driven turbulence in OMC1-S SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE turbulence; stars: formation; stars: massive; stars: pre-main sequence; ISM: jets and outflows; X-rays: stars ID YOUNG STELLAR OBJECTS; ORION ULTRADEEP PROJECT; RADIATION-HYDRODYNAMIC SIMULATIONS; SPECTRAL ENERGY-DISTRIBUTIONS; R2 MOLECULAR CLOUD; LOW-MASS STAR; NEBULA CLUSTER; TRAPEZIUM CLUSTER; OMC-1 SOUTH; GRAVITATIONAL COLLAPSE AB Outflows arising from very young stars affect their surroundings and influence the star formation in the parental core. Multiple molecular outflows and Herbig-Haro (HH) objects have been observed in Orion, many of them originating from the embedded massive star-forming region known as OMC1-S. The detection of the outflow-driving sources is commonly difficult, because they are still hidden behind large extinction, preventing their direct observation at optical and even near- and mid-IR wavelengths. With the aim of improving the identification of the driving sources of the multiple outflows detected in OMC1-S, we used the catalogue provided by deep X-ray observations, which have unveiled the very embedded population of pre-main-sequence stars. We compared the position of stars observed by the Chandra Orion Ultra-Deep Project (COUP) in OMC1-S with the morphology of the molecular outflows and the directions of measured proper motions of HH optical objects. We find that six out of seven molecular outflows reported in OMC1-S (detection rate of 86 per cent) have an extincted X-ray COUP star located at the expected position of the driving source. In several cases, X-rays detected the possible driving sources for the first time. This clustered embedded population revealed by Chandra is very young, with an estimated average age of a few 10(5) yr. It is also likely responsible for the multiple HH objects, which are the optical correspondence of flows arising from the cloud. We show that the molecular outflows driven by the members of the OMC1-S cluster can account for the observed turbulence at core scales and regulate the star formation efficiency. We discuss the effects of outflow feedback in the formation of massive stars, concluding that the injected turbulence in OMC1-S is compatible with a competitive accretion scenario. C1 [Rivilla, V. M.; Martin-Pintado, J.; Sanz-Forcada, J.; Rodriguez-Franco, A.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. [Jimenez-Serra, I.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jimenez-Serra, I.] European So Observ, D-85748 Garching, Germany. RP Rivilla, VM (reprint author), Ctr Astrobiol CSIC INTA, Ctra Torrejon Ajalvir,Km 4, E-28850 Madrid, Spain. EM ryvendel@gmail.com RI Sanz-Forcada, Jorge/C-3176-2017; Martin-Pintado, Jesus/H-6107-2015 OI Sanz-Forcada, Jorge/0000-0002-1600-7835; Martin-Pintado, Jesus/0000-0003-4561-3508 FU MICINN [AYA2010-21697-C05-01, FIS2012-39162-C06-01]; Astro-Madrid [CAM S2009/ESP-1496]; CSIC [JAE-Predoc2008]; European Union [PIIF-GA-2011-301538] FX We thank the referee, Dr Thomas Stanke, for his critical reading of the original version of this paper and his helpful suggestions. This work has been partially funded by MICINN grants AYA2010-21697-C05-01 and FIS2012-39162-C06-01, and Astro-Madrid (CAM S2009/ESP-1496) and CSIC grant JAE-Predoc2008. IJ-S acknowledges the funding received from the People Programme (Marie Curie Actions) of the European Union's Seventh Framework Programme (FP7/2007-2013) under REA grant agreement number PIIF-GA-2011-301538. NR 94 TC 7 Z9 7 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2013 VL 434 IS 3 BP 2313 EP 2328 DI 10.1093/mnras/stt1173 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207YE UT WOS:000323639900037 ER PT J AU Tombesi, F Reeves, JN Reynolds, CS Garcia, J Lohfink, A AF Tombesi, F. Reeves, J. N. Reynolds, C. S. Garcia, J. Lohfink, A. TI An outburst scenario for the X-ray spectral variability in 3C 111 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion, accretion discs; black hole physics; line: identification; plasmas; galaxies: active; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; ACCRETION DISC OUTFLOWS; LINE RADIO GALAXIES; ULTRA-FAST OUTFLOWS; ADVECTION-DOMINATED ACCRETION; SHELL ABSORPTION-LINES; XMM-NEWTON OBSERVATION; SPINNING BLACK-HOLE; SEYFERT-GALAXIES; SUZAKU VIEW AB We present a combined Suzaku and Swift BAT broad-band E = 0.6-200 keV spectral analysis of three 3C 111 observations obtained in 2010. The data are well described with an absorbed power-law continuum and a weak (R similar or equal to 0.2) cold reflection component from distant material. We constrain the continuum cutoff at E-C similar or equal to 150-200 keV, which is in accordance with X-ray Comptonization corona models and supports claims that the jet emission is only dominant at much higher energies. Fe xxvi Ly alpha emission and absorption lines are also present in the first and second observations, respectively. The modelling and interpretation of the emission line is complex and we explore three possibilities. If originating from ionized-disc reflection, this should be emitted at r(in) >= 50 r(g) or, in the lamp-post configuration, the illuminating source should be at a height of h >= 30 r(g) above the black hole. Alternatively, the line could be modelled with a hot collisionally ionized plasma with temperature kT = 22.0(-3.2)(+6.1) keV or a photoionized plasma with log xi = 4.52(-0.16)(+0.10)erg s(-1) cm and column density N-H > 3 x 10(23) cm(-2). However, the first and second scenarios are less favoured on statistical and physical grounds, respectively. The blueshifted absorption line in the second observation can be modelled as an ultrafast outflow (UFO) with ionization parameter log xi = 4.47(-0.04)(+0.76)erg s(-1) cm, column density N-H = (5.3(-1.3)(+1.8)) x 10(22) cm(-2) and outflow velocity v(out) = 0.104 +/- 0.006c. Interestingly, the parameters of the photoionized emission model remarkably match those of the absorbing UFO, supporting the possibility that the same material could be responsible for both emission and absorption. We suggest an outburst scenario in which an accretion disc wind, initially lying out of the line of sight and observed in emission, then crosses our view to the source and it is observed in absorption as a mildly relativistic UFO. C1 [Tombesi, F.] NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. [Tombesi, F.; Reynolds, C. S.; Garcia, J.; Lohfink, A.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Reeves, J. N.] Keele Univ, Astrophys Grp, Sch Phys & Geog Sci, Keele ST5 5BG, Staffs, England. [Garcia, J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Tombesi, F (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. EM ftombesi@astro.umd.edu RI XRAY, SUZAKU/A-1808-2009 FU National Aeronautics and Space Administration [NNX12AH40G]; Astrophysics Data Analysis Program, part of the ROSES FX The authors thank the referee for the thorough reading and the constructive comments that led to improvements in the paper. FT thank K. Fukumura, D. Kazanas, R. Nemmen, R. F. Mushotzky, S. B. Kraemer, M. Cappi and H. L. Marshall for the useful discussions. FT acknowledges partial support for this work by the National Aeronautics and Space Administration under Grant No. NNX12AH40G issued through the Astrophysics Data Analysis Program, part of the ROSES 2010. NR 127 TC 7 Z9 7 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD SEP PY 2013 VL 434 IS 3 BP 2707 EP 2717 DI 10.1093/mnras/stt1213 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 207YE UT WOS:000323639900071 ER PT J AU Adams, ER Ciardi, DR Dupree, AK Gautier, TN Kulesa, C McCarthy, D AF Adams, E. R. Ciardi, D. R. Dupree, A. K. Gautier, T. N., III Kulesa, C. McCarthy, D. TI ADAPTIVE OPTICS IMAGES OF KEPLER OBJECTS OF INTEREST (vol 144, 42, 2012) SO ASTRONOMICAL JOURNAL LA English DT Correction C1 [Adams, E. R.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ciardi, D. R.] NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Gautier, T. N., III] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kulesa, C.; McCarthy, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. NR 1 TC 1 Z9 1 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD SEP PY 2013 VL 146 IS 3 AR 71 DI 10.1088/0004-6256/146/3/71 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 203OO UT WOS:000323302700028 ER PT J AU Bowler, BP Liu, MC Shkolnik, EL Dupuy, TJ AF Bowler, Brendan P. Liu, Michael C. Shkolnik, Evgenya L. Dupuy, Trent J. TI PLANETS AROUND LOW-MASS STARS. III. A YOUNG DUSTY L DWARF COMPANION AT THE DEUTERIUM-BURNING LIMIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE brown dwarfs; stars: individual (2MASS J01225093-2439505); stars: low-mass ID NEAR-INFRARED SPECTRA; ALL-SKY SURVEY; VERY-LOW MASS; EXTRASOLAR GIANT PLANETS; COLOR-MAGNITUDE DIAGRAMS; DORADUS MOVING GROUP; ORBITING HR 8799; SOLAR-TYPE STARS; BINARY T DWARF; FIELD M-DWARFS AB We report the discovery of an L-type companion to the young M3.5V star 2MASS J01225093-2439505 at a projected separation of 1 ''.45 (approximate to 52 AU) as part of our adaptive optics imaging search for extrasolar giant planets around young low-mass stars. 2MASS 0122-2439 B has very red near-infrared colors similar to the HR 8799 planets and the reddest known young/dusty L dwarfs in the field. Moderate-resolution (R approximate to 3800) 1.5-2.4 mu m spectroscopy reveals a near-infrared spectral type of L4-L6 and an angular H-band shape, confirming its cool temperature and young age. The kinematics of 2MASS 0122-2439 AB are marginally consistent with members of the similar to 120 Myr AB Dor young moving group based on the photometric distance to the primary (36 +/- 4 pc) and our radial velocity measurement of 2MASS 0122-2439 A from Keck/HIRES. We adopt the AB Dor group age for the system, but the high energy emission, lack of Li I lambda 6707 absorption, and spectral shape of 2MASS 0122-2439 B suggest a range of similar to 10-120 Myr is possible. The age and luminosity of 2MASS 0122-2439 B fall in a strip where "hot-start" evolutionary model mass tracks overlap as a result of deuterium burning. Several known substellar companions also fall in this region (2MASS J0103-5515 ABb, AB Pic b, kappa And b, G196-3 B, SDSS 2249+0044 B, LP 261-75 B, HD 203030 B, and HN Peg B), but their dual-valued mass predictions have largely been unrecognized. The implied mass of 2MASS 0122-2439 B is approximate to 12-13 M-Jup or approximate to 22-27 M-Jup if it is an AB Dor member, or possibly as low as 11 M-Jup if the wider age range is adopted. Evolutionary models predict an effective temperature for 2MASS 0122-2439 B that corresponds to spectral types near the L/T transition (approximate to 1300-1500 K) for field objects. However, we find a mid-L near-infrared spectral type, indicating that 2MASS 0122-2439 B represents another case of photospheric dust being retained to cooler temperatures at low surface gravities, as seen in the spectra of young (8-30 Myr) planetary companions. Altogether, the low mass, low temperature, and red colors of 2MASS 0122-2439 B make it a bridge between warm planets like beta Pic b and cool, very dusty ones like HR 8799 bcde. C1 [Bowler, Brendan P.; Liu, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Shkolnik, Evgenya L.] Lowell Observ, Flagstaff, AZ 86001 USA. [Dupuy, Trent J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bowler, BP (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. EM bpbowler@ifa.hawaii.edu FU NASA [NNX11AC31G]; NSF [AST09-09222]; NASA/GALEX [NNX12AC18G]; National Aeronautics and Space Administration; National Science Foundation FX We thank our anonymous referee for helpful comments; Fred Vrba and the USNO group for sharing their parallax for LP 261-75 B; Katelyn Allers, Zahed Wahhaj, Davy Kirkpatrick, David Lafreniere, and Jennifer Patience for the low-gravity spectra used in this work; Yosuke Minowa for assistance with the IRCS observations; Eric Nielsen for his compilation of YMG members; and Katelyn Allers for assistance with the LP 261-75 B observations. It is a pleasure to thank the Keck support astronomers and operating assistants who helped make this work possible: Joel Aycock, Randy Campbell, Marc Kassis, Jim Lyke, Terry Stickel, and Hien Tran. B. P. B. and M. C. L. have been supported by NASA grant NNX11AC31G and NSF grant AST09-09222. E. S. has been supported by NASA/GALEX grant NNX12AC18G. We utilized data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration (NASA). NASA's Astrophysics Data System Bibliographic Services, the VizieR catalog access tool, and the SIMBAD database operated at CDS, Strasbourg, France, were invaluable resources for this work. Finally, mahalo nui loa to the kama'aina of Hawai'i for their support of Keck and the Mauna Kea observatories. We are grateful to conduct observations from this mountain. NR 135 TC 48 Z9 48 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 55 DI 10.1088/0004-637X/774/1/55 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700055 ER PT J AU Castro, D Slane, P Carlton, A Figueroa-Feliciano, E AF Castro, Daniel Slane, Patrick Carlton, Ashley Figueroa-Feliciano, Enectali TI FERMI-LAT OBSERVATIONS OF SUPERNOVA REMNANTS INTERACTING WITH MOLECULAR CLOUDS: W41, MSH 17-39, AND G337.7-0.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma rays: ISM; ISM: individual objects (W41, MSH 17-39, G337.7-0.1); ISM: supernova remnants ID COSMIC-RAY ACCELERATION; LARGE-AREA TELESCOPE; SNR RX J1713.7-3946; MHZ MASER EMISSION; HIGH-ENERGY; GAMMA-RAYS; POLARIZATION OBSERVATIONS; PARTICLE-ACCELERATION; SWIFT J1834.9-0846; NONTHERMAL RADIO AB We report the detection of gamma-ray emission coincident with three supernova remnants (SNRs) using data from the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. W41, G337.7-0.1, and MSH 17-39 are SNRs known to be interacting with molecular clouds, as evidenced by observations of hydroxyl (OH) maser emission at 1720 MHz in their directions and other observational information. 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 G337.7-0.1 and MSH 17-39 and an extended source coincident with W41. We model their broadband emission (radio to gamma-ray) using a simple one-zone model, and after considering scenarios in which the MeV-TeV sources originate from either pi(0)-decay or leptonic emission, we conclude that the gamma-rays are most likely produced through the hadronic channel. C1 [Castro, Daniel; Figueroa-Feliciano, Enectali] MIT Kavli Ctr Astrophys & Space Res, Cambridge, MA 02139 USA. [Slane, Patrick; Carlton, Ashley] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Castro, D (reprint author), MIT Kavli Ctr Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. OI , /0000-0002-7463-6007 FU NASA [NNX10AP70G]; National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory [SV3-73016]; National Aeronautics Space Administration [NAS8-03060] FX The authors thank Stefan Funk, Elizabeth Hays, and Joshua Lande for their advise regarding Fermi-LAT data analysis. We also thank Dale Frail for conversations about SNR-MC interaction. Additionally, the authors thank the referee for constructive comments and recommendations that have strengthened the paper. This work was partially funded by NASA Fermi grant NNX10AP70G.; D.C. also acknowledges support for this work provided by the National Aeronautics and Space Administration through the Smithsonian Astrophysical Observatory contract SV3-73016 to MIT for Support of the Chandra X-Ray Observatory, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. P.O.S. acknowledges partial support from NASA contract NAS8-03060. NR 71 TC 22 Z9 22 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 SEP 1 PY 2013 VL 774 IS 1 AR UNSP 36 DI 10.1088/0004-637X/774/1/36 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700036 ER PT J AU Chakraborti, S Ray, A Smith, R Ryder, S Yadav, N Sutaria, F Dwarkadas, VV Chandra, P Pooley, D Roy, R AF Chakraborti, Sayan Ray, Alak Smith, Randall Ryder, Stuart Yadav, Naveen Sutaria, Firoza Dwarkadas, Vikram V. Chandra, Poonam Pooley, David Roy, Rupak TI THE PROGENITOR OF SN 2011ja: CLUES FROM CIRCUMSTELLAR INTERACTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; radio continuum: general; shock waves; stars: mass-loss; supernovae: individual (SN 2011ja); X-rays: general ID X-RAY-EMISSION; II-P SUPERNOVAE; RADIO-EMISSION; MASS-LOSS; IC SUPERNOVAE; LIGHT CURVES; ABSORPTION; 2004ET; EXPLOSION; SN-2004ET AB Massive stars, possibly red supergiants, which retain extended hydrogen envelopes until core collapse, produce Type II plateau (IIP) supernovae. The ejecta from these explosions shocks the circumstellar matter originating from the mass loss of the progenitor during the final phases of its life. This interaction accelerates particles to relativistic energies which then lose energy via synchrotron radiation in the shock-amplified magnetic fields and inverse Compton scattering against optical photons from the supernova. These processes produce different signatures in the radio and X-ray parts of the electromagnetic spectrum. Observed together, they allow us to break the degeneracy between shock acceleration and magnetic field amplification. In this work, we use X-rays observations from the Chandra and radio observations from the Australia Telescope Compact Array to study the relative importance of processes which accelerate particles and those which amplify magnetic fields in producing the non-thermal radiation from SN 2011ja. We use radio observations to constrain the explosion date. Multiple Chandra observations allow us to probe the history of variable mass loss from the progenitor. The ejecta expands into a low-density bubble followed by interaction with a higher density wind from a red supergiant consistent with M-ZAMS greater than or similar to 12M(circle dot). Our results suggest that a fraction of Type IIP supernovae may interact with circumstellar media set up by non-steady winds. C1 [Chakraborti, Sayan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Ray, Alak; Yadav, Naveen] Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. [Smith, Randall] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ryder, Stuart] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Sutaria, Firoza] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Dwarkadas, Vikram V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Chandra, Poonam] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [Pooley, David] Sam Houston State Univ, Dept Phys, Huntsville, TX 77340 USA. [Roy, Rupak] Aryabhatta Res Inst Observat Sci, Manora Peak, Nainital, India. RP Chakraborti, S (reprint author), Harvard Univ, Soc Fellows, 78 Mt Auburn St, Cambridge, MA 02138 USA. EM schakraborti@fas.harvard.edu OI Yadav, Naveen/0000-0002-4107-9443 FU Commonwealth of Australia; National Aeronautics and Space Administration by the Chandra X-Ray Observatory Center [13500809]; National Aeronautics Space Administration [NAS8-03060]; Twelfth Five Year Plan Program at TIFR [12P-407]; CSIR FX This research has made use of data obtained using the Chandra X-Ray Observatory through an advance target of opportunity program and software provided by the Chandra X-Ray Center (CXC) in the application packages CIAO and ChIPS. We thank CXC Director Harvey Tananbaum for the second epoch of Chandra observation which was made possible using the Director's Discretionary Time. The ATCA is part of the Australia Telescope National Facility which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. We thank the staff of the GMRT that made GMRT observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number 13500809 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. A.R. thanks the Department of Physics at West Virginia University for hospitality and the Twelfth Five Year Plan Program 12P-407 at TIFR. N.Y. is supported by the CSIR S.P. Mukherjee Fellowship. NR 64 TC 8 Z9 8 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 30 DI 10.1088/0004-637X/774/1/30 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700030 ER PT J AU Chornock, R Berger, E Fox, DB Lunnan, R Drout, MR Fong, WF Laskar, T Roth, KC AF Chornock, Ryan Berger, Edo Fox, Derek B. Lunnan, Ragnhild Drout, Maria R. Fong, Wen-fai Laskar, Tanmoy Roth, Katherine C. TI GRB 130606A AS A PROBE OF THE INTERGALACTIC MEDIUM AND THE INTERSTELLAR MEDIUM IN A STAR-FORMING GALAXY IN THE FIRST Gyr AFTER THE BIG BANG SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark ages, reionization, first stars; galaxies: abundances; gamma-ray burst: individual (GRB 130606A); intergalactic medium ID GAMMA-RAY-BURST; GUNN-PETERSON TROUGH; DIGITAL SKY SURVEY; LY-ALPHA FOREST; METAL ABSORPTION-LINES; SIMILAR-TO 5-6; Z-GREATER-THAN-5.7 QUASARS; Z-SIMILAR-TO-6 QUASARS; PHOTOMETRIC REDSHIFT; ADDITIONAL QUASARS AB We present high signal-to-noise ratio Gemini and MMT spectroscopy of the optical afterglow of the gamma-ray burst (GRB) 130606A at redshift z = 5.913, discovered by Swift. This is the first high-redshift GRB afterglow to have spectra of comparable quality to those of z approximate to 6 quasars. The data exhibit a smooth continuum at near-infrared wavelengths that is sharply cut off blueward of 8410 angstrom due to absorption from Ly alpha at redshift z approximate to 5.91, with some flux transmitted through the Lya forest between 7000 and 7800 angstrom. We use column densities inferred from metal absorption lines to constrain the metallicity of the host galaxy between a lower limit of [Si/H] greater than or similar to -1.7 and an upper limit of [S/H] less than or similar to -0.5 set by the non-detection of S II absorption. We demonstrate consistency between the dramatic evolution in the transmission fraction of Ly alpha seen in this spectrum over the redshift range z = 4.9-5.85 with that previously measured from observations of high-redshift quasars. There is an extended redshift interval of Delta z = 0.12 in the Ly alpha forest at z = 5.77 with no detected transmission, leading to a 3 sigma upper limit on the mean Ly alpha transmission fraction of less than or similar to 0.2% (or tau(eff)(GP) (Ly alpha) > 6.4). This is comparable to the lowest-redshift Gunn-Peterson troughs found in quasar spectra. Some Ly beta and Ly gamma transmission is detected in this redshift window, indicating that it is not completely opaque, and hence that the intergalactic medium (IGM) is nonetheless mostly ionized at these redshifts. We set a 2 sigma upper limit of 0.11 on the neutral fraction of the IGM at the redshift of the GRB from the lack of a Ly alpha red damping wing, assuming a model with a constant neutral density. GRB 130606A thus for the first time realizes the promise of GRBs as probes of the first galaxies and cosmic reionization. C1 [Chornock, Ryan; Berger, Edo; Lunnan, Ragnhild; Drout, Maria R.; Fong, Wen-fai; Laskar, Tanmoy] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fox, Derek B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Roth, Katherine C.] Gemini Observ, Hilo, HI 96720 USA. RP Chornock, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rchornock@cfa.harvard.edu OI Lunnan, Ragnhild/0000-0001-9454-4639 FU National Science Foundation [AST-1107973]; NASA/Swift AO8 grant [NNX13AJ64G]; NSF on behalf of the Gemini partnership: the National Science Foundation (United States) [GN-2013A-Q-39]; Science and Technology Facilities Council (United Kingdom); National Research Council (Canada); CONICYT (Chile); Australian Research Council (Australia); Ministerio da Ciencia, Tecnologia e Inovacao (Brazil); Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina) FX We thank the Gemini and MMT staffs for their assistance in obtaining these observations. The Berger GRB group at Harvard is supported by the National Science Foundation under grant AST-1107973 and by NASA/Swift AO8 grant NNX13AJ64G. Based in part on observations obtained under Program ID GN-2013A-Q-39 (PI: Cucchiara) at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). Some observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. NR 67 TC 30 Z9 30 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 26 DI 10.1088/0004-637X/774/1/26 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700026 ER PT J AU Drout, MR Soderberg, AM Mazzali, PA Parrent, JT Margutti, R Milisavljevic, D Sanders, NE Chornock, R Foley, RJ Kirshner, RP Filippenko, AV Li, W Brown, PJ Cenko, SB Chakraborti, S Challis, P Friedman, A Ganeshalingam, M Hicken, M Jensen, C Modjaz, M Perets, HB Silverman, JM Wong, DS AF Drout, M. R. Soderberg, A. M. Mazzali, P. A. Parrent, J. T. Margutti, R. Milisavljevic, D. Sanders, N. E. Chornock, R. Foley, R. J. Kirshner, R. P. Filippenko, A. V. Li, W. Brown, P. J. Cenko, S. B. Chakraborti, S. Challis, P. Friedman, A. Ganeshalingam, M. Hicken, M. Jensen, C. Modjaz, M. Perets, H. B. Silverman, J. M. Wong, D. S. TI THE FAST AND FURIOUS DECAY OF THE PECULIAR TYPE Ic SUPERNOVA 2005ek SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (SN2005ek) ID ACCRETION-INDUCED COLLAPSE; SWIFT ULTRAVIOLET/OPTICAL TELESCOPE; AUTOMATIC IMAGING TELESCOPE; HELIUM SHELL DETONATIONS; NICKEL-RICH OUTFLOWS; H-II REGIONS; IA SUPERNOVAE; WHITE-DWARFS; LIGHT CURVES; HOST GALAXIES AB We present extensive multi-wavelength observations of the extremely rapidly declining Type Ic supernova (SN Ic), SN 2005ek. Reaching a peak magnitude of MR = -17.3 and decaying by similar to 3 mag in the first 15 days post-maximum, SN 2005ek is among the fastest Type I supernovae observed to date. The spectra of SN 2005ek closely resemble those of normal SN Ic, but with an accelerated evolution. There is evidence for the onset of nebular features at only nine days post-maximum. Spectroscopic modeling reveals an ejecta mass of similar to 0.3 M-circle dot that is dominated by oxygen (similar to 80%), while the pseudo-bolometric light curve is consistent with an explosion powered by similar to 0.03 M-circle dot of radioactive Ni-56. Although previous rapidly evolving events (e. g., SN 1885A, SN 1939B, SN 2002bj, SN 2010X) were hypothesized to be produced by the detonation of a helium shell on a white dwarf, oxygen-dominated ejecta are difficult to reconcile with this proposed mechanism. We find that the properties of SN 2005ek are consistent with either the edge-lit double detonation of a low-mass white dwarf or the iron-core collapse of a massive star, stripped by binary interaction. However, if we assume that the strong spectroscopic similarity of SN 2005ek to other SNe Ic is an indication of a similar progenitor channel, then a white-dwarf progenitor becomes very improbable. SN 2005ek may be one of the lowest mass stripped-envelope core-collapse explosions ever observed. We find that the rate of such rapidly declining Type I events is at least 1%-3% of the normal SN Ia rate. C1 [Drout, M. R.; Soderberg, A. M.; Margutti, R.; Milisavljevic, D.; Sanders, N. E.; Chornock, R.; Foley, R. J.; Kirshner, R. P.; Chakraborti, S.; Challis, P.; Friedman, A.; Hicken, M.; Jensen, C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mazzali, P. A.] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool CH41 1LD, Merseyside, England. [Mazzali, P. A.] INAF Osservatorio Astron Padova, I-35122 Padua, Italy. [Mazzali, P. A.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Parrent, J. T.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Parrent, J. T.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Filippenko, A. V.; Li, W.; Cenko, S. B.; Ganeshalingam, M.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Brown, P. J.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Friedman, A.] MIT, Ctr Theoret Phys, Cambridge, MA 02139 USA. [Modjaz, M.] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Perets, H. B.] Technion Israel Inst Technol, Dept Phys, IL-32000 Haifa, Israel. [Silverman, J. M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Wong, D. S.] Univ Alberta, Dept Phys, Edmonton, AB T6G 2E1, Canada. RP Drout, MR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM mdrout@cfa.harvard.edu RI Friedman, Andrew/I-4691-2013; Perets, Hagai/K-9605-2015 OI Friedman, Andrew/0000-0003-1334-039X; Perets, Hagai/0000-0002-5004-199X FU NSF; David and Lucile Packard Foundation Fellowship for Science and Engineering; NSF Astronomy and Astrophysics Postdoctoral Fellowship [AST-1302771]; U.S. National Science Foundation (NSF) [SES 1056580]; National Science Foundation [PHYS-1066293, NSF PHY11-25915]; W. M. Keck Foundation; Harvard University Milton Fund FX M. R. D. is supported in part by the NSF through a Graduate Research Fellowship. Support for this work was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A. M. S. J.M.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1302771. A. S. F. acknowledges support from the U.S. National Science Foundation (NSF) under grant SES 1056580.; This work was supported in part by the National Science Foundation under grant No. PHYS-1066293 and the hospitality of the Aspen Center for Physics. We also acknowledge the hospitality of the Kavli Institute for Theoretical Physics and partial support by the National Science Foundation under grant No. NSF PHY11-25915.; The W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA; the observatory was made possible by the generous financial support of the W. M. Keck Foundation. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. The Hobby-Eberly Telescope (HET), is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universitat Munchen, and Georg-August-Universitat Gottingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Very Large Array is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. 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 M. Skrutskie for his continued support of the PAIRITEL project.; The supernova research of A.V.F.'s group at UC Berkeley is supported by Gary & Cynthia Bengier, the Richard & Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. KAIT and its ongoing work 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 121 TC 28 Z9 28 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 58 DI 10.1088/0004-637X/774/1/58 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700058 ER PT J AU Hainline, LJ Morgan, CW MacLeod, CL Landaal, ZD Kochanek, CS Harris, HC Tilleman, T Goicoechea, LJ Shalyapin, VN Falco, EE AF Hainline, Laura J. Morgan, Christopher W. MacLeod, Chelsea L. Landaal, Zachary D. Kochanek, C. S. Harris, Hugh C. Tilleman, Trudy Goicoechea, L. J. Shalyapin, V. N. Falco, Emilio E. TI TIME DELAY AND ACCRETION DISK SIZE MEASUREMENTS IN THE LENSED QUASAR SBS 0909+532 FROM MULTIWAVELENGTH MICROLENSING ANALYSIS SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; gravitational lensing: micro; gravitational lensing: strong; quasars: individual (SBS 0909+532) ID DARK-MATTER HALOS; GRAVITATIONAL LENS; X-RAY; EMISSION REGIONS; LIGHT CURVES; GALAXY; DECONVOLUTION; VARIABILITY; SYSTEMS; SAMPLE AB We present three complete seasons and two half-seasons of Sloan Digital Sky Survey (SDSS) r-band photometry of the gravitationally lensed quasar SBS 0909+532 from the U. S. Naval Observatory, as well as two seasons each of SDSS g-band and r-band monitoring from the Liverpool Robotic Telescope. Using Monte Carlo simulations to simultaneously measure the system's time delay and model the r-band microlensing variability, we confirm and significantly refine the precision of the system's time delay to Delta t(AB) = 50(-4)(+2) days, where the stated uncertainties represent the bounds of the formal 1 sigma confidence interval. There may be a conflict between the time delay measurement and a lens consisting of a single galaxy. While models based on the Hubble Space Telescope astrometry and a relatively compact stellar distribution can reproduce the observed delay, the models have somewhat less dark matter than we would typically expect. We also carry out a joint analysis of the microlensing variability in the r and g bands to constrain the size of the quasar's continuum source at these wavelengths, obtaining log{(r(s,r)/cm)[cos i/0.5](1/2)} = 15.3 +/- 0.3 and log{(r(s,g)/cm)[cos i/0.5](1/2)} = 14.8 +/- 0.9, respectively. Our current results do not formally constrain the temperature profile of the accretion disk but are consistent with the expectations of standard thin disk theory. C1 [Hainline, Laura J.; Morgan, Christopher W.; MacLeod, Chelsea L.; Landaal, Zachary D.] US Naval Acad, Dept Phys, Annapolis, MD 21402 USA. [Kochanek, C. S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Harris, Hugh C.; Tilleman, Trudy] US Naval Observ, Flagstaff Stn, Flagstaff, AZ 86001 USA. [Goicoechea, L. J.; Shalyapin, V. N.] Univ Cantabria, Fac Ciencias, E-39005 Santander, Spain. [Shalyapin, V. N.] Natl Acad Sci Ukraine, Inst Radiophys & Elect, UA-61085 Kharkov, Ukraine. [Falco, Emilio E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hainline, LJ (reprint author), US Naval Acad, Dept Phys, 572C Holloway Rd, Annapolis, MD 21402 USA. EM hainline@usna.edu; cmorgan@usna.edu; macleod@usna.edu; m123894@usna.edu; ckochanek@astronomy.ohio-state.edu; hch@nofs.navy.mil; trudy@nofs.navy.mil; goicol@unican.es; vshal@ukr.net; falco@cfa.harvard.edu FU National Science Foundation [AST-0907848, AST-1211146, AST-1009756]; Research Corporation for Science Advancement; Chandrasekhar X-Ray Center [11700501]; UK Science and Technology Facilities Council; Spanish Department of Science and Innovation [AYA2010-21741-C03-03]; University of Cantabria FX This material is based upon work supported by the National Science Foundation under grant Nos. AST-0907848 and AST-1211146 (to C. W. M.), and AST-1009756 (to C. S. K.). C.W.M. also gratefully acknowledges support from the Research Corporation for Science Advancement and Chandrasekhar X-Ray Center award 11700501. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The Liverpool Quasar Lens Monitoring (LQLM) program is supported by the Spanish Department of Science and Innovation grant AYA2010-21741-C03-03 (Gravitational LENses and DArk MAtter - GLENDAMA project), and the University of Cantabria. NR 40 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 69 DI 10.1088/0004-637X/774/1/69 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700069 ER PT J AU Lee, JC Hwang, HS Ko, J AF Lee, Jong Chul Hwang, Ho Seong Ko, Jongwan TI THE CALIBRATION OF STAR FORMATION RATE INDICATORS FOR WISE 22 mu m-SELECTED GALAXIES IN THE SLOAN DIGITAL SKY SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE dust, extinction; galaxies: ISM; galaxies: starburst; infrared: galaxies; stars: formation; surveys ID ACTIVE GALACTIC NUCLEI; ULTRALUMINOUS INFRARED GALAXIES; H-ALPHA; FORMING GALAXIES; DUST ATTENUATION; NEARBY GALAXIES; LOCAL UNIVERSE; DATA RELEASE; TO 3; ULTRAVIOLET AB We study star formation rate (SFR) indicators for Wide-field Infrared Survey Explorer (WISE) 22 mu m-selected, star-forming galaxies at 0.01 < z < 0.3 in the Sloan Digital Sky Survey. Using extinction-corrected H alpha luminosities and total infrared luminosities as reference SFR estimates, we calibrate WISE mid-infrared- (MIR-) related SFR indicators. Both the 12 and 22 mu m monochromatic luminosities correlate well with the reference the SFR estimates, but tend to underestimate the SFRs of metal-poor galaxies (at lower than solar metallicity), consistent with previous studies. We mitigate this metallicity dependence by using a linear combination of observed H alpha and WISE MIR luminosities for our SFR estimates. This combination provides SFR measurements as robust as those applied to Spitzer data by Kennicutt et al. However, we find that the coefficient a in L-H alpha(obs) + aL(MIR) increases with the SFR, and show that a nonlinear combination of observed Ha and MIR luminosities gives the best SFR estimates with small scatters and with little dependence on physical parameters. Such a combination of H alpha and MIR luminosities for SFR estimates is first applied to the WISE data. Using WISE data, we provide several SFR recipes that are applicable to galaxies with 0.1 less than or similar to SFR (M-circle dot yr(-1)) less than or similar to 100. C1 [Lee, Jong Chul; Ko, Jongwan] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Lee, JC (reprint author), Korea Astron & Space Sci Inst, Taejon 305348, South Korea. EM jclee@kasi.re.kr FU Smithsonian Institution; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England; American Museum of Natural History; Astrophysical Institute Potsdam; University of Basel; University of Cambridge; Case Western Reserve University; University of Chicago; Drexel University; Fermilab; Institute for Advanced Study; Johns Hopkins University; Joint Institute for Nuclear Astrophysics; Kavli Institute for Particle Astrophysics and Cosmology; Chinese Academy of Sciences (LAMOST); Los Alamos National Laboratory; Max-Planck Institute for Astronomy (MPIA); Max-Planck-Institute for Astrophysics (MPA); New Mexico State University; Ohio State University; University of Pittsburgh; University of Portsmouth; Princeton University; United States Naval Observatory; University of Washington FX We are grateful to an anonymous referee for comments that improved the original manuscript. We thank Hyunjin Shim, Kwang-Il Seon, and Margaret Geller for useful discussions. J.C.L. and J.K. are members of the Dedicated Researchers for Extragalactic AstronoMy (DREAM) in Korea Astronomy and Space Science Institute (KASI). H. S. H. acknowledges the Smithsonian Institution for the support of his post-doctoral fellowship. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory, California Institute of Technology, funded by the National Aeronautics and Space Administration. 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 71 TC 32 Z9 32 U1 1 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 62 DI 10.1088/0004-637X/774/1/62 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700062 ER PT J AU McDonald, M Benson, BA Vikhlinin, A Stalder, B Bleem, LE de Haan, T Lin, HW Aird, KA Ashby, MLN Bautz, MW Bayliss, M Bocquet, S Brodwin, M Carlstrom, JE Chang, CL Cho, HM Clocchiatti, A Crawford, TM Crites, AT Desai, S Dobbs, MA Dudley, JP Foley, RJ Forman, WR George, EM Gettings, D Gladders, MD Gonzalez, AH Halverson, NW High, FW Holder, GP Holzapfel, WL Hoover, S Hrubes, JD Jones, C Joy, M Keisler, R Knox, L Lee, AT Leitch, EM Liu, J Lueker, M Luong-Van, D Mantz, A Marrone, DP McMahon, JJ Mehl, J Meyer, SS Miller, ED Mocanu, L Mohr, JJ Montroy, TE Murray, SS Nurgaliev, D Padin, S Plagge, T Pryke, C Reichardt, CL Rest, A Ruel, J Ruhl, JE Saliwanchik, BR Saro, A Sayre, JT Schaffer, KK Shirokoff, E Song, J Suhada, R Spieler, HG Stanford, SA Staniszewski, Z Stark, AA Story, K van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zahn, O Zenteno, A AF McDonald, M. Benson, B. A. Vikhlinin, A. Stalder, B. Bleem, L. E. de Haan, T. Lin, H. W. Aird, K. A. Ashby, M. L. N. Bautz, M. W. Bayliss, M. Bocquet, S. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H. M. Clocchiatti, A. Crawford, T. M. Crites, A. T. Desai, S. Dobbs, M. A. Dudley, J. P. Foley, R. J. Forman, W. R. George, E. M. Gettings, D. Gladders, M. D. Gonzalez, A. H. Halverson, N. W. High, F. W. Holder, G. P. Holzapfel, W. L. Hoover, S. Hrubes, J. D. Jones, C. Joy, M. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Liu, J. Lueker, M. Luong-Van, D. Mantz, A. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Miller, E. D. Mocanu, L. Mohr, J. J. Montroy, T. E. Murray, S. S. Nurgaliev, D. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Rest, A. Ruel, J. Ruhl, J. E. Saliwanchik, B. R. Saro, A. Sayre, J. T. Schaffer, K. K. Shirokoff, E. Song, J. Suhada, R. Spieler, H. G. Stanford, S. A. Staniszewski, Z. Stark, A. A. Story, K. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zahn, O. Zenteno, A. TI THE GROWTH OF COOL CORES AND EVOLUTION OF COOLING PROPERTIES IN A SAMPLE OF 83 GALAXY CLUSTERS AT 0.3 < z < 1.2 SELECTED FROM THE SPT-SZ SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE early universe; galaxies: clusters: general; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID SOUTH-POLE TELESCOPE; ACTIVE GALACTIC NUCLEI; RAY LUMINOUS CLUSTERS; COLD MOLECULAR GAS; 720 SQUARE DEGREES; STAR-FORMATION; FLOW CLUSTERS; HIGH-REDSHIFT; INTRACLUSTER MEDIUM; PERSEUS CLUSTER AB We present first results on the cooling properties derived from Chandra X-ray observations of 83 high-redshift (0.3 < z < 1.2) massive galaxy clusters selected by their Sunyaev-Zel'dovich signature in the South Pole Telescope data. We measure each cluster's central cooling time, central entropy, and mass deposition rate, and compare these properties to those for local cluster samples. We find no significant evolution from z similar to 0 to z similar to 1 in the distribution of these properties, suggesting that cooling in cluster cores is stable over long periods of time. We also find that the average cool core entropy profile in the inner similar to 100 kpc has not changed dramatically since z similar to 1, implying that feedback must be providing nearly constant energy injection to maintain the observed "entropy floor" at similar to 10 keV cm(2). While the cooling properties appear roughly constant over long periods of time, we observe strong evolution in the gas density profile, with the normalized central density (rho(g),(0)/rho(crit)) increasing by an order of magnitude from z similar to 1 to z similar to 0. When using metrics defined by the inner surface brightness profile of clusters, we find an apparent lack of classical, cuspy, cool-core clusters at z > 0.75, consistent with earlier reports for clusters at z > 0.5 using similar definitions. Our measurements indicate that cool cores have been steadily growing over the 8 Gyr spanned by our sample, consistent with a constant, similar to 150M(circle dot) yr(-1) cooling flow that is unable to cool below entropies of 10 keV cm(2) and, instead, accumulates in the cluster center. We estimate that cool cores began to C1 [McDonald, M.; Bautz, M. W.; Miller, E. D.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Benson, B. A.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mantz, A.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K.; Vieira, J. D.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Hoover, S.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Vikhlinin, A.; Stalder, B.; Ashby, M. L. N.; Bayliss, M.; Foley, R. J.; Forman, W. R.; Jones, C.; Murray, S. S.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bleem, L. E.; Carlstrom, J. E.; Keisler, R.; Meyer, S. S.; Story, K.; Vieira, J. D.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [de Haan, T.; Dobbs, M. A.; Dudley, J. P.; Holder, G. P.; van Engelen, A.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Lin, H. W.] Caddo Parish Magnet High Sch, Shrevport, LA 71101 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Bayliss, M.; Nurgaliev, D.; Ruel, J.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Saro, A.; Suhada, R.; Zenteno, A.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Bocquet, S.; Desai, S.; Liu, J.; Mohr, J. J.; Zenteno, A.] Excellence Cluster Univ, D-85748 Garching, Germany. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Gladders, M. D.; High, F. W.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Mocanu, L.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H. M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Clocchiatti, A.] Pontificia Univ Catolica, Dept Astron & Astrosif, Santiago, Chile. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Lueker, M.; Reichardt, C. L.; Shirokoff, E.; Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Gettings, D.; Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Joy, M.] NASA, George C Marshall Space Flight Ctr, Dept Space Sci, Huntsville, AL 35812 USA. [Knox, L.; Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Lueker, M.; Padin, S.; Shirokoff, E.; Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.; Song, J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Dept Phys, Ctr Educ & Res Cosmol & Astrophys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. RP McDonald, M (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. EM mcdonald@space.mit.edu RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Aird, Kenneth/0000-0003-1441-9518; Reichardt, Christian/0000-0003-2226-9169; Lin, Henry/0000-0003-2767-6142 FU NASA [HST-HF51308.01-A, 12800071, 12800088, 13800883]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; National Science Foundation [ANT-0638937]; NSF Physics Frontier Center [PHY-0114422]; Kavli Foundation; Gordon and Betty Moore Foundation; NSF [AST-1009012, AST-1009649, MRI-0723073]; U.S. Department of Energy [DE-AC02-06CH11357] FX M.M. acknowledges support by NASA through a Hubble Fellowship grant HST-HF51308.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. The South Pole Telescope program is supported by the National Science Foundation through grant ANT-0638937. Partial support is also provided by the NSF Physics Frontier Center grant PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation. Support for X-ray analysis was provided by NASA through Chandra Award Nos. 12800071, 12800088, and 13800883 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA. Galaxy cluster research at Harvard is supported by NSF grant AST-1009012 and at SAO in part by NSF grants AST-1009649 and MRI-0723073. Argonne National Laboratory's work was supported under U.S. Department of Energy contract DE-AC02-06CH11357. NR 95 TC 43 Z9 43 U1 1 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR UNSP 23 DI 10.1088/0004-637X/774/1/23 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700023 ER PT J AU Ricarte, A Moldvai, N Hughes, AM Duchene, G Williams, JP Andrews, SM Wilner, DJ AF Ricarte, Angelo Moldvai, Noel Hughes, A. Meredith Duchene, Gaspard Williams, Jonathan P. Andrews, Sean M. Wilner, David J. TI RESOLVING THE MOTH AT MILLIMETER WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: individual (HD 61005); submillimeter: planetary systems ID SUN-LIKE STARS; DEBRIS DISK; PROTOPLANETARY DISKS; INTERSTELLAR-MEDIUM; BETA-PICTORIS; HR 8799; CIRCUMSTELLAR DISK; RADIATIVE-TRANSFER; AU MICROSCOPII; OPTICAL-IMAGES AB HD 61005, also known as "The Moth," is one of only a handful of debris disks that exhibit swept-back "wings" thought to be caused by interaction with the ambient interstellar medium (ISM). We present 1.3 mm Submillimeter Array observations of the debris disk around HD 61005 at a spatial resolution of 1.'' 9 that resolve the emission from large grains for the first time. The disk exhibits a double-peaked morphology at millimeter wavelengths, consistent with an optically thin ring viewed close to edge-on. To investigate the disk structure and the properties of the dust grains we simultaneously model the spatially resolved 1.3 mm visibilities and the unresolved spectral energy distribution (SED). The temperatures indicated by the SED are consistent with expected temperatures for grains close to the blowout size located at radii commensurate with the millimeter and scattered light data. We also perform a visibility-domain analysis of the spatial distribution of millimeter-wavelength flux, incorporating constraints on the disk geometry from scattered light imaging, and find suggestive evidence of wavelength-dependent structure. The millimeter-wavelength emission apparently originates predominantly from the thin ring component rather than tracing the "wings" observed in scattered light. The implied segregation of large dust grains in the ring is consistent with an ISM-driven origin for the scattered light wings. C1 [Ricarte, Angelo; Moldvai, Noel; Hughes, A. Meredith; Duchene, Gaspard] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06457 USA. [Duchene, Gaspard] UJF Grenoble 1, CNRS, INSU, Inst Planetol & Astrophys Grenoble IPAG,UMR 5274, F-38041 Grenoble 9, France. [Williams, Jonathan P.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Andrews, Sean M.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Ricarte, A (reprint author), Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA. OI Williams, Jonathan/0000-0001-5058-695X FU Miller Institute for Basic Research in Science FX We thank Holly Maness, who obtained the early data sets used in this paper and established detection. We are also grateful to Esther Buenzli for kindly providing her LOCI image used in Figure 1. A.M.H. is supported by a fellowship from the Miller Institute for Basic Research in Science. NR 47 TC 11 Z9 11 U1 1 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 80 DI 10.1088/0004-637X/774/1/80 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700080 ER PT J AU Rosenfeld, KA Andrews, SM Hughes, AM Wilner, DJ Qi, CH AF Rosenfeld, Katherine A. Andrews, Sean M. Hughes, A. Meredith Wilner, David J. Qi, Chunhua TI A SPATIALLY RESOLVED VERTICAL TEMPERATURE GRADIENT IN THE HD 163296 DISK SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; protoplanetary disks; stars: individual (HD 163296); submillimeter: general ID HERBIG-AE STAR; MAIN-SEQUENCE STARS; T-TAURI STARS; PROTOPLANETARY DISKS; ACCRETION DISKS; CIRCUMSTELLAR DISKS; YOUNG OBJECTS; SOLAR NEBULA; DM-TAU; THERMAL STRUCTURE AB We analyze sensitive, sub-arcsecond resolution ALMA science verification observations of CO emission lines in the protoplanetary disk hosted by the young, isolated Ae star HD 163296. The observed spatial morphology of the (CO)-C-12 J = 3-2 emission line is asymmetric across the major axis of the disk; the (CO)-C-12 J = 2-1 line features a much less pronounced, but similar, asymmetry. The J = 2-1 emission from (CO)-C-12 and its main isotopologues have no resolved spatial asymmetry. We associate this behavior with the direct signature of a vertical temperature gradient and layered molecular structure in the disk. This is demonstrated using both toy models and more sophisticated calculations assuming non-local thermodynamic equilibrium conditions. A model disk structure is developed to reproduce both the distinctive spatial morphology of the (CO)-C-12 J = 3-2 line as well as the J = 2-1 emission from the CO isotopologues assuming relative abundances consistent with the interstellar medium. This model disk structure has tau = 1 emitting surfaces for the (CO)-C-12 emission lines that make an angle of similar to 15 degrees with respect to the disk midplane. Furthermore, we show that the spatial and spectral sensitivity of these data can distinguish between models that have sub-Keplerian gas velocities due to the vertical extent of the disk and its associated radial pressure gradient (a fractional difference in the bulk gas velocity field of greater than or similar to 5%). C1 [Rosenfeld, Katherine A.; Andrews, Sean M.; Wilner, David J.; Qi, Chunhua] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hughes, A. Meredith] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. RP Rosenfeld, KA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA Origins of Solar Systems grant [NNX11AK63] FX We are grateful to Matt Payne, Diego Munoz, Eugene Chiang, David Knezevic, Moritz Gunther, Marc Metchnik, and Kees Dullemond for insightful conversations. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2011.0.00010. SV. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. We acknowledge support from NASA Origins of Solar Systems grant No. NNX11AK63. NR 76 TC 41 Z9 41 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 DI 10.1088/0004-637X/774/1/16 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700016 ER PT J AU Sanchis-Ojeda, R Rappaport, S Winn, JN Levine, A Kotson, MC Latham, DW Buchhave, LA AF Sanchis-Ojeda, Roberto Rappaport, Saul Winn, Joshua N. Levine, Alan Kotson, Michael C. Latham, David W. Buchhave, Lars A. TI TRANSITS AND OCCULTATIONS OF AN EARTH-SIZED PLANET IN AN 8.5 hr ORBIT SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: atmospheres; planets and satellites: detection ID ERROR-CORRECTION; HOT JUPITERS; LIGHT CURVES; KEPLER; STAR; EXOPLANET; CANDIDATES; DISCOVERY; DENSITIES; PERIODS AB We report the discovery of an Earth-sized planet (1.16 +/- 0.19 R-circle plus) in an 8.5 hr orbit around a late G-type star (KIC 8435766, Kepler-xx). The object was identified in a search for short-period planets in the Kepler database and confirmed to be a transiting planet (as opposed to an eclipsing stellar system) through the absence of ellipsoidal light variations or substantial radial-velocity variations. The unusually short orbital period and the relative brightness of the host star (m(Kep) = 11.5) enable robust detections of the changing illumination of the visible hemisphere of the planet, as well as the occultations of the planet by the star. We interpret these signals as representing a combination of reflected and reprocessed light, with the highest planet dayside temperature in the range of 2300 K-3100 K. Follow-up spectroscopy combined with finer sampling photometric observations will further pin down the system parameters and may even yield the mass of the planet. C1 [Sanchis-Ojeda, Roberto; Rappaport, Saul; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Sanchis-Ojeda, Roberto; Rappaport, Saul; Winn, Joshua N.; Levine, Alan] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Kotson, Michael C.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. RP Sanchis-Ojeda, R (reprint author), MIT, Dept Phys, Cambridge, MA 02139 USA. EM rsanchis86@gmail.com; sar@mit.edu; jwinn@mit.edu; aml@space.mit.edu OI Buchhave, Lars A./0000-0003-1605-5666 FU NASA [NAS5-26555]; Kepler mission under NASA [NNX13AB58A]; Smithsonian Astrophysical Observatory; National Aeronautics and Space Administration under the Exoplanet Exploration Program; NASA Office of Space Science [NNX09AF08G] FX We are indebted to Allyson Bieryla and Gilbert Esquerdo for their assistance with the spectroscopic follow-up observations. We also thank the referee, Nick Cowan, for a thorough critique of the manuscript. We thank Bryce Croll, Brice Demory, Amaury Triaud and Kevin Schlaufman for helpful discussions about this object, and of course we are grateful to the entire Kepler team for providing a wonderful tool for discovery. R.S.O. and J.N.W. acknowledge NASA support through the Kepler Participating Scientist Program. D. W. L. acknowledges partial support for the spectroscopic work from the Kepler mission under NASA Cooperative Agreement NNX13AB58A with the Smithsonian Astrophysical Observatory. This research has made use of the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. The data presented in this article were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-Hubble Space Telescope data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. NR 43 TC 55 Z9 55 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR UNSP 54 DI 10.1088/0004-637X/774/1/54 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700054 ER PT J AU Takahashi, S Ohashi, N Bourke, TL AF Takahashi, Satoko Ohashi, Nagayoshi Bourke, Tyler L. TI DIRECT IMAGING OF A COMPACT MOLECULAR OUTFLOW FROM A VERY LOW LUMINOSITY OBJECT: L1521F-IRS SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (L1521F-IRS); ISM: jets and outflows; ISM: molecules; stars: formation; stars: low-mass; stars: protostars ID 1ST HYDROSTATIC CORE; EVOLVED STARLESS CORE; SPITZER C2D SURVEY; CLOUD CORE; DENSE CORE; SUBMILLIMETER ARRAY; STELLAR DENSITIES; HIGH-VELOCITY; PROTOSTELLAR JET; FORMING REGION AB Studying the physical conditions of very low luminosity objects (VeLLOs; L-bol < 0.1 L-circle dot) is important for understanding the earliest evolutionary stage of protostars and brown dwarfs. We report interferometric observations of the VeLLO L1521F-IRS, in (CO)-C-12 (2-1) line emission and the 1.3 mm continuum emission, using the Submillimeter Array. With the (CO)-C-12 (2-1) high-resolution observations, we have spatially resolved a compact but poorly collimated molecular outflow associated with L1521F-IRS for the first time. The blueshifted and redshifted lobes are aligned along the east and west side of L1521F-IRS with a lobe size of approximate to 1000 AU. The estimated outflow mass, maximum outflow velocity, and outflow force are (9.0-80) x 10(-4) M-circle dot, 7.2 km s(-1), and (7.4-66) x 10(-7) M-circle dot km s(-1) yr(-1), respectively. The estimated outflow parameters such as size, mass, and momentum rate are similar to values derived for other VeLLOs, and are located at the lower end of values compared to previously studied outflows associated with low- to high-mass star-forming regions. Low-velocity less collimated (1.5 km s(-1)/1200 AU) and higher-velocity compact (4.0 km s(-1)/920 AU) outflow components are suggested by the data. These velocity structures are not consistent with those expected in the jet-driven or wind-driven outflow models, perhaps suggesting a remnant outflow from the first hydrostatic core as well as an undeveloped outflow from the protostar. Detection of an infrared source and compact millimeter continuum emission suggests the presence of the protostar, while its low bolometric luminosity (0.034-0.07 L-circle dot) and small outflow suggests that L1521F is in the earliest protostellar stage (< 10(4) yr) and contains a substellar mass object. The bolometric (or internal) luminosity of L1521F-IRS suggests that the current mass accretion rate is an order of magnitude lower than expected in the standard mass accretion model (approximate to 10(-6) M-circle dot yr(-1)), which may imply that L1521F-IRS is currently in a low activity phase. C1 [Takahashi, Satoko] Joint ALMA Observ, Santiago, Chile. [Takahashi, Satoko] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Takahashi, Satoko; Ohashi, Nagayoshi] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ohashi, Nagayoshi] Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Bourke, Tyler L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Takahashi, S (reprint author), Joint ALMA Observ, Alonso de Cordova 3107, Santiago, Chile. EM satoko.takahashi@nao.ac.jp FU Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan FX We acknowledge the staff at the Submillimeter Array for assistance with operations. The SMT is operated by the Arizona Radio Observatory (ARO), Steward Observatory, University of Arizona. S.T. acknowledges S.-W. Yen for helping the SMT 12CO (2-1) data inspection, and M. Machida and N. Hirano, and Y.-N. Su for fruitful scientific comments. We also thank our referee for the constructive comments that helped to improve this manuscript. S.T. is financially supported by a postdoctoral fellowship at the Institute of Astronomy and Astrophysics, Academia Sinica, Taiwan. NR 66 TC 15 Z9 15 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD SEP 1 PY 2013 VL 774 IS 1 AR 20 DI 10.1088/0004-637X/774/1/20 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205FA UT WOS:000323426700020 ER PT J AU Deck, KM Holman, MJ Agol, E Carter, JA Lissauer, JJ Ragozzine, D Winn, JN AF Deck, Katherine M. Holman, Matthew J. Agol, Eric Carter, Joshua A. Lissauer, Jack J. Ragozzine, Darin Winn, Joshua N. TI RAPID DYNAMICAL CHAOS IN AN EXOPLANETARY SYSTEM (vol 755, pg L21, 2012) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Deck, Katherine M.; Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.; Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Holman, Matthew J.; Carter, Joshua A.; Ragozzine, Darin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Lissauer, Jack J.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Deck, KM (reprint author), MIT, Dept Phys, 77 Massachusetts Ave, Cambridge, MA 02139 USA. NR 2 TC 0 Z9 0 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD SEP 1 PY 2013 VL 774 IS 1 AR L15 DI 10.1088/2041-8205/774/1/L15 PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208IV UT WOS:000323672400015 ER PT J AU Thacker, RW Hill, AL Hill, MS Redmond, NE Collins, AG Morrow, CC Spicer, L Carmack, CA Zappe, ME Pohlmann, D Hall, C Diaz, MC Bangalore, PV AF Thacker, Robert W. Hill, April L. Hill, Malcolm S. Redmond, Niamh E. Collins, Allen G. Morrow, Christine C. Spicer, Lori Carmack, Cheryl A. Zappe, Megan E. Pohlmann, Deborah Hall, Chelsea Diaz, Maria C. Bangalore, Purushotham V. TI Nearly Complete 28S rRNA Gene Sequences Confirm New Hypotheses of Sponge Evolution SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Assembling the Poriferan Tree of Life at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) ID CLASS DEMOSPONGIAE; PHYLOGENY; PORIFERA; SYSTEMATICS; SUPPORT; PHYLUM; RDNA AB The highly collaborative research sponsored by the NSF-funded Assembling the Porifera Tree of Life (PorToL) project is providing insights into some of the most difficult questions in metazoan systematics. Our understanding of phylogenetic relationships within the phylum Porifera has changed considerably with increased taxon sampling and data from additional molecular markers. PorToL researchers have falsified earlier phylogenetic hypotheses, discovered novel phylogenetic alliances, found phylogenetic homes for enigmatic taxa, and provided a more precise understanding of the evolution of skeletal features, secondary metabolites, body organization, and symbioses. Some of these exciting new discoveries are shared in the papers that form this issue of Integrative and Comparative Biology. Our analyses of over 300 nearly complete 28S ribosomal subunit gene sequences provide specific case studies that illustrate how our dataset confirms new hypotheses of sponge evolution. We recovered monophyletic clades for all 4 classes of sponges, as well as the 4 major clades of Demospongiae (Keratosa, Myxospongiae, Haploscleromorpha, and Heteroscleromorpha), but our phylogeny differs in several aspects from traditional classifications. In most major clades of sponges, families within orders appear to be paraphyletic. Although additional sampling of genes and taxa are needed to establish whether this pattern results from a lack of phylogenetic resolution or from a paraphyletic classification system, many of our results are congruent with those obtained from 18S ribosomal subunit gene sequences and complete mitochondrial genomes. These data provide further support for a revision of the traditional classification of sponges. C1 [Thacker, Robert W.; Carmack, Cheryl A.; Zappe, Megan E.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Hill, April L.; Hill, Malcolm S.; Spicer, Lori; Pohlmann, Deborah; Hall, Chelsea] Univ Richmond, Dept Biol, Richmond, VA 23173 USA. [Redmond, Niamh E.; Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Collins, Allen G.] NOAA, Natl Systemat Lab, Fisheries Serv, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. [Morrow, Christine C.] Queens Univ Belfast, Sch Biol Sci, MBC, Belfast BT9 7BL, Antrim, North Ireland. [Diaz, Maria C.] Museo Marino Margarita, Boca Del Rio, Nueva Esparta, Venezuela. [Bangalore, Purushotham V.] Univ Alabama Birmingham, Dept Comp & Informat Sci, Birmingham, AL 35294 USA. RP Thacker, RW (reprint author), Univ Alabama Birmingham, Dept Biol, 1300 Univ Blvd, Birmingham, AL 35294 USA. EM thacker@uab.edu RI Hill, Malcolm/B-6204-2015; OI Morrow, Christine/0000-0001-5686-8747 FU NIAID NIH HHS [P30 AI027767] NR 29 TC 19 Z9 19 U1 0 U2 37 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 SEP PY 2013 VL 53 IS 3 BP 373 EP 387 DI 10.1093/icb/ict071 PG 15 WC Zoology SC Zoology GA 205MQ UT WOS:000323448800001 PM 23748742 ER PT J AU Redmond, NE Morrow, CC Thacker, RW Diaz, MC Boury-Esnault, N Cardenas, P Hajdu, E Lobo-Hajdu, G Picton, BE Pomponi, SA Kayal, E Collins, AG AF Redmond, N. E. Morrow, C. C. Thacker, R. W. Diaz, M. C. Boury-Esnault, N. Cardenas, P. Hajdu, E. Lobo-Hajdu, G. Picton, B. E. Pomponi, S. A. Kayal, E. Collins, A. G. TI Phylogeny and Systematics of Demospongiae in Light of New Small-Subunit Ribosomal DNA (18S) Sequences SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Assembling the Poriferan Tree of Life at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) ID GLASS SPONGES PORIFERA; PHYLUM PORIFERA; MOLECULAR PHYLOGENY; ANIMAL PHYLOGENY; GENE-SEQUENCES; FOSSIL RECORD; EVOLUTION; HEXACTINELLIDA; CLASSIFICATION; VERONGIDA AB The most diverse and species-rich class of the phylum Porifera is Demospongiae. In recent years, the systematics of this clade, which contains more than 7000 species, has developed rapidly in light of new studies combining molecular and morphological observations. We add more than 500 new, nearly complete 18S sequences (an increase of more than 200%) in an attempt to further enhance understanding of the phylogeny of Demospongiae. Our study specifically targets representation of type species and genera that have never been sampled for any molecular data in an effort to accelerate progress in classifying this diverse lineage. Our analyses recover four highly supported subclasses of Demospongiae: Keratosa, Myxospongiae, Haploscleromorpha, and Heteroscleromorpha. Within Keratosa, neither Dendroceratida, nor its two families, Darwinellidae and Dictyodendrillidae, are monophyletic and Dictyoceratida is divided into two lineages, one predominantly composed of Dysideidae and the second containing the remaining families (Irciniidae, Spongiidae, Thorectidae, and Verticillitidae). Within Myxospongiae, we find Chondrosida to be paraphyletic with respect to the Verongida. We amend the latter to include species of the genus Chondrosia and erect a new order Chondrillida to contain remaining taxa from Chondrosida, which we now discard. Even with increased taxon sampling of Haploscleromorpha, our analyses are consistent with previous studies; however, Haliclona species are interspersed in even more clades. Haploscleromorpha contains five highly supported clades, each more diverse than previously recognized, and current families are mostly polyphyletic. In addition, we reassign Janulum spinispiculum to Haploscleromorpha and resurrect Reniera filholi as Janulum filholi comb. nov. Within the large clade Heteroscleromorpha, we confirmed 12 recently identified clades based on alternative data, as well as a sister-group relationship between the freshwater Spongillida and the family Vetulinidae. We transfer Stylissa flabelliformis to the genus Scopalina within the family Scopalinidae, which is of uncertain position. Our analyses uncover a large, strongly supported clade containing all heteroscleromorphs other than Spongillida, Vetulinidae, and Scopalinidae. Within this clade, there is a major division separating Axinellidae, Biemnida, Tetractinellida, Bubaridae, Stelligeridae, Raspailiidae, and some species of Petromica, Topsentia, and Axinyssa from Agelasida, Polymastiidae, Placospongiidae, Clionaidae, Spirastrellidae, Tethyidae, Poecilosclerida, Halichondriidae, Suberitidae, and Trachycladus. Among numerous results: (1) Spirophorina and its family Tetillidae are paraphyletic with respect to a strongly supported Astrophorina within Tetractinellida; (2) Agelasida is the earliest diverging lineage within the second clade listed above; and (3) Merlia and Desmacella appear to be the earliest diverging lineages of Poecilosclerida. C1 [Redmond, N. E.; Collins, A. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Morrow, C. C.] Queens Univ Belfast, Sch Biol Sci, MBC, Belfast BT9 7BL, Antrim, North Ireland. [Thacker, R. W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Diaz, M. C.] Museo Marino Margarita, Boca Del Rio, Nueva Esparta, Venezuela. [Boury-Esnault, N.] Univ Aix Marseille, Marine Endoume Stn, IMBE CNRS UMR7263, F-13007 Marseille, France. [Cardenas, P.] Uppsala Univ, Dept Systemat Biol, Evolutionary Biol Ctr, S-75236 Uppsala, Sweden. [Hajdu, E.] Univ Fed Rio de Janeiro, Museu Nacl, Dept Invertebrados, Rio De Janeiro, RJ, Brazil. [Lobo-Hajdu, G.] Univ Fed Rio de Janeiro, IBRAG, Dept Genet, Rio De Janeiro, RJ, Brazil. [Picton, B. E.] Natl Museums Northern Ireland, Dept Nat Sci, Holywood BT18 0EU, North Ireland. [Pomponi, S. A.] Florida Atlantic Univ, Harbor Branch Oceanog Inst, Ft Pierce, FL 34946 USA. [Kayal, E.] Smithsonian Inst, Natl Museum Nat Hist, Lab Analyt Biol, Washington, DC 20560 USA. [Collins, A. G.] NOAA, Natl Systemat Lab, Fisheries Serv, Washington, DC 20560 USA. RP Redmond, NE (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM collinsa@si.edu RI Lobo-Hajdu, G/A-6709-2008; Hajdu, Eduardo/C-3863-2009; OI Lobo-Hajdu, G/0000-0001-7792-9609; Morrow, Christine/0000-0001-5686-8747; Picton, Bernard/0000-0002-1500-2215 NR 111 TC 43 Z9 43 U1 4 U2 44 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD SEP PY 2013 VL 53 IS 3 BP 388 EP 415 DI 10.1093/icb/ict078 PG 28 WC Zoology SC Zoology GA 205MQ UT WOS:000323448800002 PM 23793549 ER PT J AU Morrow, CC Redmond, NE Picton, BE Thacker, RW Collins, AG Maggs, CA Sigwart, JD Allcock, AL AF Morrow, Christine C. Redmond, Niamh E. Picton, Bernard E. Thacker, Robert W. Collins, Allen G. Maggs, Christine A. Sigwart, Julia D. Allcock, A. Louise TI Molecular Phylogenies Support Homoplasy of Multiple Morphological Characters Used in the Taxonomy of Heteroscleromorpha (Porifera: Demospongiae) SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Assembling the Poriferan Tree of Life at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) ID SEQUENCE ALIGNMENT; RIBOSOMAL-RNA; SPONGES; SYSTEMATICS; SCLEROSPONGES; EVOLUTION; ACCURACY; NUCLEAR; MODELS; MUSCLE AB Sponge classification has long been based mainly on morphocladistic analyses but is now being greatly challenged by more than 12 years of accumulated analyses of molecular data analyses. The current study used phylogenetic hypotheses based on sequence data from 18S rRNA, 28S rRNA, and the CO1 barcoding fragment, combined with morphology to justify the resurrection of the order Axinellida Levi, 1953. Axinellida occupies a key position in different morphologically derived topologies. The abandonment of Axinellida and the establishment of Halichondrida Vosmaer, 1887 sensu lato to contain Halichondriidae Gray, 1867, Axinellidae Carter, 1875, Bubaridae Topsent, 1894, Heteroxyidae Dendy, 1905, and a new family Dictyonellidae van Soest et al., 1990 was based on the conclusion that an axially condensed skeleton evolved independently in separate lineages in preference to the less parsimonious assumption that asters (star-shaped spicules), acanthostyles (club-shaped spicules with spines), and sigmata (C-shaped spicules) each evolved more than once. Our new molecular trees are congruent and contrast with the earlier, morphologically based, trees. The results show that axially condensed skeletons, asters, acanthostyles, and sigmata are all homoplasious characters. The unrecognized homoplasious nature of these characters explains much of the incongruence between molecular-based and morphology-based phylogenies. We use the molecular trees presented here as a basis for re-interpreting the morphological characters within Heteroscleromorpha. The implications for the classification of Heteroscleromorpha are discussed and a new order Biemnida ord. nov. is erected. C1 [Morrow, Christine C.; Maggs, Christine A.; Sigwart, Julia D.] Queens Univ Belfast, Sch Biol Sci, MBC, Belfast BT9 7BL, Antrim, North Ireland. [Redmond, Niamh E.; Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Natl Systemat Lab, Washington, DC 20013 USA. [Picton, Bernard E.] Natl Museums Northern Ireland, Holywood BT18 0EU, North Ireland. [Thacker, Robert W.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Allcock, A. Louise] Natl Univ Ireland Galway, Sch Nat Sci, Galway, Ireland. [Allcock, A. Louise] Natl Univ Ireland Galway, Ryan Inst, Galway, Ireland. RP Morrow, CC (reprint author), Queens Univ Belfast, Sch Biol Sci, MBC, 97 Lisburn Rd, Belfast BT9 7BL, Antrim, North Ireland. EM christinemorrow@gmail.com RI Allcock, Louise/A-7359-2012; OI Allcock, Louise/0000-0002-4806-0040; Morrow, Christine/0000-0001-5686-8747; Picton, Bernard/0000-0002-1500-2215; Maggs, Christine/0000-0003-0495-7064 NR 69 TC 15 Z9 15 U1 4 U2 24 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 SEP PY 2013 VL 53 IS 3 BP 428 EP 446 DI 10.1093/icb/ict065 PG 19 WC Zoology SC Zoology GA 205MQ UT WOS:000323448800004 PM 23753661 ER PT J AU Klautau, M Azevedo, F Condor-Lujan, B Rapp, HT Collins, A Russo, CAD AF Klautau, Michelle Azevedo, Fernanda Condor-Lujan, Baslavi Rapp, Hans Tore Collins, Allen de Moraes Russo, Claudia Augusta TI A Molecular Phylogeny for the Order Clathrinida Rekindles and Refines Haeckel's Taxonomic Proposal for Calcareous Sponges SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Assembling the Poriferan Tree of Life at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) ID PORIFERA; CALCINEA; CLASSIFICATION; EVOLUTION; NUCULA; COAST; DNA AB Most biological groups are still longing for a phylogenetically sound taxonomic organization. In this article, we aimed to verify the consistency of morphological characters in calcarean sponges of the well-known non-monophyletic order Clathrinida using a molecular phylogeny. For this we included 50 species, including six type species, currently assigned to eight different genera. A maximum likelihood topology was generated for the nuclear ITS marker using the General Time Reversible model and the bootstrap reliability test. Our topology indicated 10 clathrinid clades that included species with consistent morphological characters. In the present study, we defined nine of these clades as clathrinid genera, including four newly described and two newly diagnosed genera. Recent studies have indicated that not much phylogenetic information may be found in morphology, but our findings contradict this general assertion. Our study confirms the suitability of skeleton and body anastomosis as valid characters in a phylogenetically sound taxonomy for the order. Interestingly, we have also found that, apart from the Calcinea/Calcaronea split and a few minor details, Haeckel's original proposal is remarkably similar to our own, which was based on a molecular phylogeny 140 years later. C1 [Klautau, Michelle; Azevedo, Fernanda; Condor-Lujan, Baslavi] Univ Fed Rio de Janeiro, Inst Biol, Dept Zool, BR-21941902 Rio De Janeiro, RJ, Brazil. [Rapp, Hans Tore] Univ Bergen, Dept Biol, N-5020 Bergen, Norway. [Rapp, Hans Tore] Univ Bergen, Ctr Geobiol, N-5020 Bergen, Norway. [Collins, Allen] NOAA, Natl Systemat Lab, Fisheries Serv, Washington, DC 20560 USA. [Collins, Allen] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [de Moraes Russo, Claudia Augusta] Univ Fed Rio de Janeiro, Inst Biol, Dept Genet, BR-21941902 Rio De Janeiro, RJ, Brazil. RP Klautau, M (reprint author), Univ Fed Rio de Janeiro, Inst Biol, Dept Zool, BR-21941902 Rio De Janeiro, RJ, Brazil. EM mklautau@biologia.ufrj.br RI Russo, Claudia/I-1217-2012; Klautau, Michelle/I-2041-2012 OI Russo, Claudia/0000-0002-1252-9206; Klautau, Michelle/0000-0002-5959-0776 NR 32 TC 12 Z9 12 U1 0 U2 11 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 EI 1557-7023 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD SEP PY 2013 VL 53 IS 3 BP 447 EP 461 DI 10.1093/icb/ict039 PG 15 WC Zoology SC Zoology GA 205MQ UT WOS:000323448800005 PM 23704365 ER PT J AU Hajdu, E de Paula, TS Redmond, NE Cosme, B Collins, AG Lobo-Hajdu, G AF Hajdu, Eduardo de Paula, Thiago S. Redmond, Niamh E. Cosme, Bruno Collins, Allen G. Lobo-Hajdu, Gisele TI Mycalina: Another Crack in the Poecilosclerida Framework SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Assembling the Poriferan Tree of Life at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) ID CLADORHIZIDAE POECILOSCLERIDA; MOLECULAR PHYLOGENY; RIBOSOMAL-RNA; DEMOSPONGIAE; PORIFERA; SPONGES; MITOCHONDRIAL; HYPOTHESES; NUCLEAR; ORIGIN AB This is the first phylogenetic analysis integrating both morphological and molecular data of the sponge suborder Mycalina (Poecilosclerida), which was erected in 1994. A cladistic analysis of morphology supported the monophyly of Cladorhizidae (including Euchelipluma), Guitarridae (excluding Euchelipluma), Isodictyidae, Latrunculiidae, and Podospongiidae but rejected monophyly for Desmacellidae, Esperiopsidae, Hamacanthidae, and Mycalidae. Analyses of partial 16S and partial 28S rRNA datasets combined, as well as that of a complete 18S rDNA dataset, suggest that Mycalina is not monophyletic; Biemnidae is only distantly related to other poecilosclerids; Merlia and Desmacella branch near the base of a diverse Poecilosclerida clade; Mycalidae is monophyletic (excluding Mycale [Anomomycale] titubans in 18S); and Esperiopsidae and Isodictyidae form a clade. Analyses of the two molecular datasets differed on the monophyly of Podospongiidae and about the relationship of Podospongiidae to Isodictyidae + Esperiopsidae. C1 [Hajdu, Eduardo] Univ Fed Rio de Janeiro, Museu Nacl, BR-20940040 Rio De Janeiro, RJ, Brazil. [de Paula, Thiago S.; Cosme, Bruno; Lobo-Hajdu, Gisele] Univ Estado Rio de Janeiro, Dept Genet, Inst Biol Roberto Alcantara Gomes, PHLC, BR-20550013 Rio De Janeiro, RJ, Brazil. [Redmond, Niamh E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Collins, Allen G.] NOAA, Natl Systemat Lab, Fisheries Serv, Washington, DC 20560 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Hajdu, E (reprint author), Univ Fed Rio de Janeiro, Museu Nacl, Quinta da Boa Vista S-N, BR-20940040 Rio De Janeiro, RJ, Brazil. EM eduardo.hajdu@gmail.com RI Lobo-Hajdu, G/A-6709-2008; de Paula, Thiago/B-4301-2014; Hajdu, Eduardo/C-3863-2009; Cosme, Bruno/R-8115-2016 OI Lobo-Hajdu, G/0000-0001-7792-9609; de Paula, Thiago/0000-0003-4468-4996; Cosme, Bruno/0000-0002-1985-2540 NR 50 TC 6 Z9 7 U1 1 U2 12 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 SEP PY 2013 VL 53 IS 3 BP 462 EP 472 DI 10.1093/icb/ict074 PG 11 WC Zoology SC Zoology GA 205MQ UT WOS:000323448800006 PM 23798622 ER PT J AU Diaz, MC Thacker, RW Redmond, NE Matterson, KO Collins, AG AF Diaz, Maria C. Thacker, Robert W. Redmond, Niamh E. Matterson, Kenan O. Collins, Allen G. TI Phylogenetic Novelties and Geographic Anomalies among Tropical Verongida SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Article; Proceedings Paper CT Symposium on Assembling the Poriferan Tree of Life at the Annual Meeting of the Society-for-Integrative-and-Comparative-Biology (SICB) CY JAN 03-07, 2013 CL San Francisco, CA SP Soc Integrat & Comparat Biol (SICB) ID MARINE SPONGES; PORIFERA; CHITIN AB Exploring marine sponges from shallow tropical reefs of the Caribbean and western Central Pacific, as part of large biodiversity (Moorea Biocode Project) and evolutionary (Porifera Tree of Life) research projects, we encountered 13 skeleton-less specimens, initially divided in two morphological groups, which had patterns of coloration and oxidation typical of taxa of the order Verongida (Demospongiae). The first group of samples inhabited open and cryptic habitats of shallow (15-20 m) Caribbean reefs at Bocas del Toro Archipelago, Panama. The second group inhabited schiophilous (e.g., inner coral framework and crevices) habitats on shallow reefs (0.5-20 m deep) in Moorea Island, French Polynesia. We applied an integrative approach by combining analyses of external morphology, histological observations, 18S rDNA, and mtCOI to determine the identity and the relationships of these unknown taxa within the order Verongida. Molecular analyses revealed that none of the species studied belonged to Hexadella (Ianthellidae, Verongida), the only fibreless genus of the Order Verongida currently recognized. The species from the Caribbean locality of Bocas del Toro (Panama) belong to the family Ianthellidae and is closely related to the Pacific genera Ianthella and Anomoianthella, both with well-developed fiber reticulations. We suggest the erection of a new generic denomination to include this novel eurypylous, fibreless ianthellid. The species collected in Moorea were all diplodal verongid taxa, with high affinities to a clade containing Pseudoceratina, Verongula, and Aiolochroia, a Pacific and two Caribbean genera, respectively. These unknown species represented at least three different taxa distinguished by DNA sequence analysis and morphological characteristics. Two new genera and a new species of Pseudoceratina are here proposed to accommodate these novel biological discoveries. The evolutionary and ecological meaning of having or lacking a fiber skeleton within Verongida is challenged under the evidence of the existence of fibreless genera within various verongid clades. Furthermore, the discovery of a fibreless Peudoceratina suggests that the possession of a spongin-chitin fiber reticulation is an "ecological" plastic trait that might be lost under certain conditions, such us growing within another organism's skeletal framework. These results raise new questions about the ecological and evolutionary significance of the development of a fiber skeleton and of sponges' adaptability to various environmental conditions. C1 [Diaz, Maria C.] Museo Marino, Nueva Esparta, Venezuela. [Thacker, Robert W.; Matterson, Kenan O.] Univ Alabama Birmingham, Dept Biol, Birmingham, AL 35294 USA. [Redmond, Niamh E.] Smithsonian Inst, NMNH, Washington, DC 20560 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Collins, Allen G.] NOAA, Natl Systemat Lab, Fisheries Serv, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC USA. RP Diaz, MC (reprint author), Museo Marino, Blvd Boca Del Rio, Nueva Esparta, Venezuela. EM taxochica@gmail.com; thacker@uab.edu NR 23 TC 6 Z9 6 U1 1 U2 16 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD SEP PY 2013 VL 53 IS 3 BP 482 EP 494 DI 10.1093/icb/ict033 PG 13 WC Zoology SC Zoology GA 205MQ UT WOS:000323448800008 PM 23624868 ER PT J AU Laliberte, E Turner, BL Zemunik, G Wyrwoll, KH Pearse, SJ Lambers, H AF Laliberte, Etienne Turner, Benjamin L. Zemunik, Graham Wyrwoll, Karl-Heinz Pearse, Stuart J. Lambers, Hans TI Nutrient limitation along the Jurien Bay dune chronosequence: response to Uren & Parsons (2013) SO JOURNAL OF ECOLOGY LA English DT Letter DE calcareous dune; calcifuge; chronosequence; micronutrients; nutrient limitation; parent material; pedogenesis; plant-soil (below-ground) interactions ID SOUTH-WESTERN AUSTRALIA; SWAN COASTAL-PLAIN; SOUTHWESTERN AUSTRALIA; PLANT-COMMUNITIES; EASTERN AUSTRALIA; LUPINUS-ALBUS; YELLOW SAND; PERTH BASIN; PHOSPHORUS; PHOSPHATE AB 1. Uren & Parsons (2013) criticize our nutrient addition experiment and question the integrity of the Jurien Bay dune chronosequence. Their primary criticisms relate to (i) inconsistencies in parent material along the chronosequence and (ii) the lack of consideration of micronutrients in our glasshouse experiment. 2. We reaffirm that the Quindalup-Spearwood succession is a consistent Holocene-Middle (possibly Early) Pleistocene soil chronosequence in which parent material, topography, and present-day climate and vegetation type (i.e. Mediterranean shrubland) are held relatively constant. The older (Early Pleistocene-Late Pliocene) Bassendean Sand probably contained less carbonate initially, but nevertheless represents the endpoint of an exceptionally strong gradient in soil nutrient availability. 3. The claim that we did not consider the potential importance of micronutrients is unfounded. We included a micronutrient treatment in our experiment and discussed the importance of micronutrient availability in young calcareous substrates. 4. Synthesis. We restate that our experimental results support predictions about changes in nutrient limitation during long-term pedogenesis, and affirm that the Jurien Bay chronosequence is a valuable model system for addressing ecological questions related to pedogenesis, plant diversity and plant-soil interactions. C1 [Laliberte, Etienne; Turner, Benjamin L.; Zemunik, Graham; Pearse, Stuart J.; Lambers, Hans] Univ Western Australia, Sch Plant Biol, Perth, WA 6009, Australia. [Turner, Benjamin L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Wyrwoll, Karl-Heinz] Univ Western Australia, Sch Earth & Environm, Perth, WA 6009, Australia. RP Laliberte, E (reprint author), Univ Western Australia, Sch Plant Biol, 35 Stirling Highway, Perth, WA 6009, Australia. EM etienne.laliberte@uwa.edu.au RI Turner, Benjamin/E-5940-2011; Laliberte, Etienne/B-6855-2008; Lambers, Hans/A-1544-2008 OI Turner, Benjamin/0000-0002-6585-0722; Laliberte, Etienne/0000-0002-3167-2622; Lambers, Hans/0000-0002-4118-2272 NR 36 TC 7 Z9 7 U1 2 U2 35 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD SEP PY 2013 VL 101 IS 5 BP 1088 EP 1092 DI 10.1111/1365-2745.12123 PG 5 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 208SG UT WOS:000323699000002 ER PT J AU Chisholm, RA Muller-Landau, HC Abdul Rahman, K Bebber, DP Bin, Y Bohlman, SA Bourg, NA Brinks, J Bunyavejchewin, S Butt, N Cao, HL Cao, M Cardenas, D Chang, LW Chiang, JM Chuyong, G Condit, R Dattaraja, HS Davies, S Duque, A Fletcher, C Gunatilleke, N Gunatilleke, S Hao, ZQ Harrison, RD Howe, R Hsieh, CF Hubbell, SP Itoh, A Kenfack, D Kiratiprayoon, S Larson, AJ Lian, JY Lin, DM Liu, HF Lutz, JA Ma, KP Malhi, Y McMahon, S McShea, W Meegaskumbura, M Razman, SM Morecroft, MD Nytch, CJ Oliveira, A Parker, GG Pulla, S Punchi-Manage, R Romero-Saltos, H Sang, WG Schurman, J Su, SH Sukumar, R Sun, IF Suresh, HS Tan, S Thomas, D Thomas, S Thompson, J Valencia, R Wolf, A Yap, S Ye, WH Yuan, ZQ Zimmerman, JK AF Chisholm, Ryan A. Muller-Landau, Helene C. Abdul Rahman, Kassim Bebber, Daniel P. Bin, Yue Bohlman, Stephanie A. Bourg, Norman A. Brinks, Joshua Bunyavejchewin, Sarayudh Butt, Nathalie Cao, Honglin Cao, Min Cardenas, Dairon Chang, Li-Wan Chiang, Jyh-Min Chuyong, George Condit, Richard Dattaraja, Handanakere S. Davies, Stuart Duque, Alvaro Fletcher, Christine Gunatilleke, Nimal Gunatilleke, Savitri Hao, Zhanqing Harrison, Rhett D. Howe, Robert Hsieh, Chang-Fu Hubbell, Stephen P. Itoh, Akira Kenfack, David Kiratiprayoon, Somboon Larson, Andrew J. Lian, Juyu Lin, Dunmei Liu, Haifeng Lutz, James A. Ma, Keping Malhi, Yadvinder McMahon, Sean McShea, William Meegaskumbura, Madhava Razman, Salim Mohd Morecroft, Michael D. Nytch, Christopher J. Oliveira, Alexandre Parker, Geoffrey G. Pulla, Sandeep Punchi-Manage, Ruwan Romero-Saltos, Hugo Sang, Weiguo Schurman, Jon Su, Sheng-Hsin Sukumar, Raman Sun, I-Fang Suresh, Hebbalalu S. Tan, Sylvester Thomas, Duncan Thomas, Sean Thompson, Jill Valencia, Renato Wolf, Amy Yap, Sandra Ye, Wanhui Yuan, Zuoqiang Zimmerman, Jess K. TI Scale-dependent relationships between tree species richness and ecosystem function in forests SO JOURNAL OF ECOLOGY LA English DT Article DE biodiversity; biomass; complementarity; determinants of plant community diversity and structure; productivity; sampling effects; species diversity; trees ID TROPICAL FOREST; REGRESSION-ANALYSIS; POOR PREDICTOR; PRODUCTIVITY; DIVERSITY; BIODIVERSITY; VEGETATION; METAANALYSES; CONSERVATION; COMPETITION AB 1. The relationship between species richness and ecosystem function, as measured by productivity or biomass, is of long-standing theoretical and practical interest in ecology. This is especially true for forests, which represent a majority of global biomass, productivity and biodiversity. 2. Here, we conduct an analysis of relationships between tree species richness, biomass and productivity in 25 forest plots of area 8-50ha from across the world. The data were collected using standardized protocols, obviating the need to correct for methodological differences that plague many studies on this topic. 3. We found that at very small spatial grains (0.04ha) species richness was generally positively related to productivity and biomass within plots, with a doubling of species richness corresponding to an average 48% increase in productivity and 53% increase in biomass. At larger spatial grains (0.25ha, 1ha), results were mixed, with negative relationships becoming more common. The results were qualitatively similar but much weaker when we controlled for stem density: at the 0.04ha spatial grain, a doubling of species richness corresponded to a 5% increase in productivity and 7% increase in biomass. Productivity and biomass were themselves almost always positively related at all spatial grains. 4. Synthesis. This is the first cross-site study of the effect of tree species richness on forest biomass and productivity that systematically varies spatial grain within a controlled methodology. The scale-dependent results are consistent with theoretical models in which sampling effects and niche complementarity dominate at small scales, while environmental gradients drive patterns at large scales. Our study shows that the relationship of tree species richness with biomass and productivity changes qualitatively when moving from scales typical of forest surveys (0.04ha) to slightly larger scales (0.25 and 1ha). This needs to be recognized in forest conservation policy and management. C1 [Chisholm, Ryan A.; Muller-Landau, Helene C.; Condit, Richard; Hubbell, Stephen P.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Abdul Rahman, Kassim; Fletcher, Christine; Razman, Salim Mohd] Forest Res Inst Malaysia, Kepong 52109, Selangor Darul, Malaysia. [Bebber, Daniel P.] Earthwatch Inst, Oxford OX2 7DE, England. [Bin, Yue; Cao, Honglin; Lian, Juyu; Ye, Wanhui] Chinese Acad Sci, South China Bot Garden, Key Lab Plant Resources Conservat & Sustainable U, Guangzhou 510650, Guangdong, Peoples R China. [Bohlman, Stephanie A.] Univ Florida, Sch Forest Resources & Conservat, Gainesville, FL 32611 USA. [Bourg, Norman A.; McShea, William] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Brinks, Joshua; McMahon, Sean; Parker, Geoffrey G.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Bunyavejchewin, Sarayudh] Dept Natl Pk Wildlife & Plant Conservat, Res Off, Bangkok 10900, Thailand. [Butt, Nathalie; Malhi, Yadvinder] Univ Oxford, Sch Geog & Environm, Environm Change Inst, Oxford OX1 3QY, England. [Butt, Nathalie] Univ Queensland, ARC Ctr Excellence Environm Decis, St Lucia, Qld 4072, Australia. [Cao, Min] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming 650223, Peoples R China. [Cardenas, Dairon] Inst Amazon Invest Cient Sinchi, Bogota, Colombia. [Chang, Li-Wan; Su, Sheng-Hsin] Taiwan Forestry Res Inst, Taipei 10066, Taiwan. [Chiang, Jyh-Min] Tunghai Univ, Dept Life Sci, Taichung 40704, Taiwan. [Chuyong, George] Univ Buea, Dept Plant & Anim Sci, Buea, Swp, Cameroon. [Dattaraja, Handanakere S.; Pulla, Sandeep; Sukumar, Raman; Suresh, Hebbalalu S.] Indian Inst Sci, Ctr Ecol Sci, Bangalore 560012, Karnataka, India. [Davies, Stuart; Kenfack, David; Tan, Sylvester] Smithsonian Inst, Dept Bot, MRC 166, Washington, DC 20013 USA. [Duque, Alvaro] Univ Nacl Colombia, Medellin, Colombia. [Gunatilleke, Nimal; Gunatilleke, Savitri; Meegaskumbura, Madhava] Univ Peradeniya, Fac Sci, Dept Bot, Peradeniya 20400, Sri Lanka. [Hao, Zhanqing; Yuan, Zuoqiang] Chinese Acad Sci, Inst Appl Ecol, State Key Lab Forest & Soil Ecol, Shenyang 110164, Peoples R China. [Harrison, Rhett D.] Chinese Acad Sci, Kunming Inst Bot, Kunming 650201, Peoples R China. [Harrison, Rhett D.] World Agroforestry Inst, East Asia Off, Kunming 650201, Peoples R China. [Howe, Robert; Wolf, Amy] Univ Wisconsin Green Bay, Dept Nat & Appl Sci, Green Bay, WI 54311 USA. [Hsieh, Chang-Fu] Natl Taiwan Univ, Inst Ecol & Evolutionary Biol, Taipei 10617, Taiwan. [Hubbell, Stephen P.] Univ Calif Los Angeles, Dept Ecol & Evolutionary Biol, Los Angeles, CA 90095 USA. [Itoh, Akira] Osaka City Univ, Grad Sch Sci, Osaka 5588585, Japan. [Kiratiprayoon, Somboon] Thammasat Univ Rangsit, Fac Sci & Technol, Klongluang 12121, Patumtani, Thailand. [Larson, Andrew J.] Univ Montana, Dept Forest Management, Missoula, MT 59812 USA. [Lin, Dunmei; Liu, Haifeng; Ma, Keping; Sang, Weiguo] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Lin, Dunmei] Chinese Acad Sci, Grad Univ, Beijing 100049, Peoples R China. [Liu, Haifeng; Sang, Weiguo] Minzu Univ China, Coll Life & Environm Sci, Beijing 100081, Peoples R China. [Lutz, James A.] Utah State Univ, Wildland Resources Dept, Logan, UT 84322 USA. [Morecroft, Michael D.] Nat England, Winchester SO23 7BT, Hants, England. [Nytch, Christopher J.; Thompson, Jill; Zimmerman, Jess K.] Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00936 USA. [Oliveira, Alexandre] Univ Sao Paulo, Dept Ecol IB, BR-04582050 Sao Paulo, Brazil. [Punchi-Manage, Ruwan] Univ Gottingen, Dept Ecosyst Modeling, D-37077 Gottingen, Germany. [Romero-Saltos, Hugo; Valencia, Renato] Pontificia Univ Catolica Ecuador, Escuela Ciencias Biol, Quito, Ecuador. [Schurman, Jon; Thomas, Sean] Univ Toronto, Toronto, ON M5S 3B3, Canada. [Sun, I-Fang] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 97401, Taiwan. [Thomas, Duncan] Oregon State Univ, Dept Bot & Plant Pathol, Corvallis, OR 97331 USA. [Thompson, Jill] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Yap, Sandra] Univ Philippines Diliman, Inst Biol, Quezon City 1101, Ncr, Philippines. RP Chisholm, RA (reprint author), Smithsonian Trop Res Inst, POB 0843-03092, Balboa, Ancon, Panama. EM ryan.chis@gmail.com RI Butt, Nathalie/B-3558-2014; Thompson, Jill/K-2200-2012; Oliveira, Alexandre/G-8830-2012; Chisholm, Ryan/H-8033-2012; OI Butt, Nathalie/0000-0003-1517-6191; Thompson, Jill/0000-0002-4370-2593; Oliveira, Alexandre/0000-0001-5526-8109; Lin, Dunmei/0000-0001-6112-7783; Chiang, Jyh-Min/0000-0002-6293-1551; Bourg, Norman/0000-0002-7443-1992; Parker, Geoffrey/0000-0001-7055-6491 FU US National Science Foundation [DEB-1046113, BSR-9015961, DEB-0516066, BSR-8811902, DEB-9411973, DEB-008538, DEB-0218039, DEB-0620910]; National Natural Science Foundation of China [31011120470, 31061160188]; Smithsonian Institution Global Earth Observatories; HSBC Climate Partnership; Chinese Academy of Sciences [KZCX2-YW-430]; National Science & Technology Pillar Program of China [2008BAC39B02]; Bureau of China Foreign Expert and Ministry of Education [2008 B08044]; Council of Agriculture of Taiwan [93AS 2.4.2-FI-G1(2), 94AS-11.1.2-FI-G1(1)]; National Science Council of Taiwan [NSC92-3114-B002-009, NSC98-2313-B-029-001-MY3, NSC98-2321-B-029-002]; Forestry Bureau of Taiwan [92-00-2-06, TFBM-960226]; Taiwan Forestry Research Institute [97 AS- 7.1.1.F1-G1]; Mellon Foundation; International Institute of Tropical Forestry of the USDA Forest Service; University of Puerto Rico; 1923 Fund; Direccion de Investigaciones Universidad Nacional de Colombia; Centre for Ecology and Hydrology; German Academic Exchange Services (DAAD); Ministry of Environment & Forests (Government of India); Tamilnadu Forest Department; Sarawak Forest Department; Sarawak Forestry Corporation; Global Environment Research Fund of the Ministry of the Environment Japan [D-0901]; Japan Society for the Promotion of Science [20405011]; Pontifical Catholic University of Ecuador; government of Ecuador (Donaciones del Impuesto a la Renta); Smithsonian Tropical Research Institute; University of Aarhus of Denmark; Yosemite National Park FX This work was generated using data from the Center for Tropical Forest Science/Smithsonian Institution Global Earth Observatory network (http://www.sigeo.si.edu/). The synthesis was made possible through the financial support of the US National Science Foundation (DEB-1046113), the National Natural Science Foundation of China (31011120470), the Smithsonian Institution Global Earth Observatories and the HSBC Climate Partnership. Individual plot data collection and analysis were supported by the US National Science Foundation (BSR-9015961, DEB-0516066, BSR-8811902, DEB-9411973, DEB-008538, DEB-0218039, and DEB-0620910), the National Natural Science Foundation of China (31061160188), the Chinese Academy of Sciences (KZCX2-YW-430), the National Science & Technology Pillar Program of China (2008BAC39B02), the '111 Program' from the Bureau of China Foreign Expert and Ministry of Education (No. 2008 B08044), the Council of Agriculture of Taiwan (93AS 2.4.2-FI-G1(2) and 94AS-11.1.2-FI-G1(1)), the National Science Council of Taiwan (NSC92-3114-B002-009, NSC98-2313-B-029-001-MY3 and NSC98-2321-B-029-002), the Forestry Bureau of Taiwan (92-00-2-06 and No. TFBM-960226), the Taiwan Forestry Research Institute (97 AS- 7.1.1.F1-G1), the Mellon Foundation, the International Institute of Tropical Forestry of the USDA Forest Service, the University of Puerto Rico, Yosemite National Park, the 1923 Fund, the Direccion de Investigaciones Universidad Nacional de Colombia (Convocatoria 2010-2012), the Centre for Ecology and Hydrology, the German Academic Exchange Services (DAAD), Ministry of Environment & Forests (Government of India), the Tamilnadu Forest Department, Sarawak Forest Department, Sarawak Forestry Corporation, Global Environment Research Fund of the Ministry of the Environment Japan (D-0901), Japan Society for the Promotion of Science (#20405011), the Pontifical Catholic University of Ecuador, the government of Ecuador (Donaciones del Impuesto a la Renta), the Smithsonian Tropical Research Institute and the University of Aarhus of Denmark. We thank the hundreds of people who contributed to the collection and organization of the data from the plots, including Gordon Campbell, Gary Fewless, Maria Uriarte and Linfang Wu. We thank Stephen Pacala, Roman Carrasco and Colin Beale for discussions. None of the authors has any conflict of interest. NR 51 TC 2 Z9 2 U1 6 U2 283 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD SEP PY 2013 VL 101 IS 5 DI 10.1111/1365-2745.12132 PG 10 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 208SG UT WOS:000323699000013 ER PT J AU Cheesman, AW Winter, K AF Cheesman, Alexander W. Winter, Klaus TI Growth response and acclimation of CO2 exchange characteristics to elevated temperatures in tropical tree seedlings SO JOURNAL OF EXPERIMENTAL BOTANY LA English DT Article DE Functional trait; Panama; photosynthesis; respiration; temperature; tropical forest ID NIGHTTIME TEMPERATURES; PHENOTYPIC PLASTICITY; ALTITUDINAL VARIATION; BIOTIC ATTRITION; MOUNTAIN PASSES; CLIMATE-CHANGE; WARMER PLANET; RANGE SHIFTS; LEAF MASS; FOREST AB Predictions of how tropical forests will respond to future climate change are constrained by the paucity of data on the performance of tropical species under elevated growth temperatures. In particular, little is known about the potential of tropical species to acclimate physiologically to future increases in temperature. Seedlings of 10 neo-tropical tree species from different functional groups were cultivated in controlled-environment chambers under four day/night temperature regimes between 30/22 C and 39/31 C. Under well-watered conditions, all species showed optimal growth at temperatures above those currently found in their native range. While non-pioneer species experienced catastrophic failure or a substantially reduced growth rate under the highest temperature regime employed (i.e. daily average of 35 C), growth in three lowland pioneers showed only a marginal reduction. In a subsequent experiment, three species (Ficus insipida, Ormosia macrocalyx, and Ochroma pyramidale) were cultivated at two temperatures determined as sub- and superoptimal for growth, but which resulted in similar biomass accumulation despite a 6C difference in growth temperature. Through reciprocal transfer and temperature adjustment, the role of thermal acclimation in photosynthesis and respiration was investigated. Acclimation potential varied among species, with two distinct patterns of respiration acclimation identified. The study highlights the role of both inherent temperature tolerance and thermal acclimation in determining the ability of tropical tree species to cope with enhanced temperatures. C1 [Cheesman, Alexander W.; Winter, Klaus] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Cheesman, AW (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM Alexander.Cheesman@gmail.com RI Cheesman, Alexander/H-5918-2013 OI Cheesman, Alexander/0000-0003-3931-5766 FU Smithsonian Tropical Research Institute, through the Center for Tropical Forest Studies (CTFS); Smithsonian Institute Global Earth Observatory (SIGEO) FX This work was supported by the Smithsonian Tropical Research Institute, through the Center for Tropical Forest Studies (CTFS) and Smithsonian Institute Global Earth Observatory (SIGEO). We would like to thank Lucas Cernusak and Kelly Andersen for comments on an earlier draft of this manuscript, as well as Kelly Anderson and Stuart Dennis for statistical advice. NR 75 TC 14 Z9 14 U1 7 U2 86 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0022-0957 J9 J EXP BOT JI J. Exp. Bot. PD SEP PY 2013 VL 64 IS 12 BP 3817 EP 3828 DI 10.1093/jxb/ert211 PG 12 WC Plant Sciences SC Plant Sciences GA 207DY UT WOS:000323578700022 PM 23873999 ER PT J AU McCleery, R Oli, MK Hostetler, JA Karmacharya, B Greene, D Winchester, C Gore, J Sneckenberger, S Castleberry, SB Mengak, MT AF McCleery, R. Oli, M. K. Hostetler, J. A. Karmacharya, B. Greene, D. Winchester, C. Gore, J. Sneckenberger, S. Castleberry, S. B. Mengak, M. T. TI Are declines of an endangered mammal predation-driven, and can a captive-breeding and release program aid their recovery? SO JOURNAL OF ZOOLOGY LA English DT Article DE Key Largo woodrat; capture-mark-recapture analysis; predation; Pradel's model; survival; recruitment; release; captive breeding ID KEY-LARGO WOODRAT; NEOTOMA-FLORIDANA-SMALLI; CAPTURE-MARK-RECAPTURE; POPULATION-GROWTH RATE; ACORN MAST; SURVIVAL; RECRUITMENT; RODENT; DYNAMICS; ANIMALS AB Declines of imperiled small mammals are often attributed to predation without investigating the relative influence of survival and reproductive parameters on population growth. Accordingly, declines in the endangered Key Largo woodrat Neotoma floridana smalli (KLWR) population have been attributed to predation by feral cats Felis catus, Burmese pythons Python molurus bivittatus and raccoons Procyon lotor. We estimated survival, recruitment and realized population growth rates from four capture-mark-recapture studies to determine if the pattern of demographic variation was consistent with predation as the primary cause of KLWR declines. Additionally, we evaluated the KLWR captive-breeding and release program by comparing survival of captive-born and released KLWRs to wild-born KLWRs. The realized population growth rate of wild-born KLWRs had a strong pattern of covariation with recruitment; covariation between the realized population growth rate and apparent survival was negligible. Consistent with demographic theory, our results suggest that KLWR population dynamics were driven primarily by variation in recruitment, and that periodic reductions in recruitment led to population declines. We found that the survival curve and the first month (S-1) and first 3-month (S1-3) survival estimates for the wild-born KLWRs [S-1 = 0.929 (0.890-0.968); S1-3 = 0.942 (0.919-0.965)] were considerably higher ((2) = 33.9, 1 d.f., P < 0.001) than released KLWRs [S-1 = 0.521 (0.442-0.600); S1-3 = 0.561 (0.493-0.629)]. Low survival rates from predation limited the success of the captive-breeding and release program. This study illustrates the importance of pre-release conditioning of captive-bred animals and the importance of considering reproductive parameters in conjunction with survival estimates to understand the drivers of population decline. C1 [McCleery, R.; Oli, M. K.; Greene, D.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL 32611 USA. [Hostetler, J. A.] Smithsonian Migratory Bird Ctr, Washington, DC USA. [Karmacharya, B.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Winchester, C.; Gore, J.] Florida Fish & Wildlife Conservat Commiss, Panama City, FL USA. [Sneckenberger, S.] US Fish & Wildlife Serv, South Florida Ecol Serv Off, Vero Beach, FL USA. [Castleberry, S. B.; Mengak, M. T.] Univ Georgia, Warnell Sch Forestry & Nat Resources, Athens, GA 30602 USA. RP McCleery, R (reprint author), Univ Florida, Dept Wildlife Ecol & Conservat, Newins Zeigler Hall, Gainesville, FL 32611 USA. EM ramccleery@ufl.edu RI Hostetler, Jeffrey/A-3345-2011; OI Hostetler, Jeffrey/0000-0003-3669-1758; McCleery, Robert/0000-0001-7018-005X FU USFWS [F11AP00176]; University of Florida Institute for Food and Agricultural Science FX Special thanks to Phil Frank, Steve Klett, the field technicians, volunteers and USFWS employees whose hard work was invaluable to this project. The findings and conclusions in this article are those of the authors and do not necessarily represent the views of the US Fish and Wildlife Service. Funding was provided by the USFWS (Agreement No. F11AP00176) and the University of Florida Institute for Food and Agricultural Science. NR 50 TC 7 Z9 7 U1 4 U2 81 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0952-8369 J9 J ZOOL JI J. Zool. PD SEP PY 2013 VL 291 IS 1 BP 59 EP 68 DI 10.1111/jzo.12046 PG 10 WC Zoology SC Zoology GA 206SE UT WOS:000323541900008 ER PT J AU Larjavaara, M Muller-Landau, HC AF Larjavaara, Markku Muller-Landau, Helene C. TI Measuring tree height: a quantitative comparison of two common field methods in a moist tropical forest SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE Barro Colorado Island; Central America; clinometer; hypsometer; inclinometer; lowland forest; rain forest; tree stature ID RAIN-FOREST; ALLOMETRY; CANOPY AB 1. Tree height is a key variable for estimating tree biomass and investigating tree life history, but it is difficult to measure in forests with tall, dense canopies and wide crowns. The traditional method, which we refer to as the 'tangent method', involves measuring horizontal distance to the tree and angles from horizontal to the top and base of the tree, while standing at a distance of perhaps one tree height or greater. Laser rangefinders enable an alternative method, which we refer to as the 'sine method'; it involves measuring the distances to the top and base of the tree, and the angles from horizontal to these, and can be carried out from under the tree or from some distance away. 2. We quantified systematic and random errors of these two methods as applied by five technicians to a size-stratified sample of 74 trees between 5.7 and 39.2m tall in a Neotropical moist forest in Panama. We measured actual heights using towers adjacent to these trees. 3. The tangent method produced unbiased height estimates, but random error was high, and in 6 of the 370measurements, heights were overestimated by more than 100%. 4. The sine method was faster to learn, displayed less variation in heights among technicians, and had lower random error, but resulted in systematic underestimation by 20% on average. 5. We recommend the sine method for most applications in tropical forests. However, its underestimation, which is likely to vary with forest and instrument type, must be corrected if actual heights are needed. C1 [Larjavaara, Markku] Finnish Forest Res Inst, FI-01301 Vantaa, Finland. [Muller-Landau, Helene C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Larjavaara, M (reprint author), Finnish Forest Res Inst, Jokiniemenkuja 1,Box 18, FI-01301 Vantaa, Finland. EM markku.larjavaara@gmail.com OI Larjavaara, Markku/0000-0002-3484-889X FU HSBC Climate Partnership; Smithsonian Institution Global Earth Observatories for the CTFS-SIGEO Global Forest Carbon Research Initiative; US National Science Foundation [0756920, 0201307]; Frank Levinson Family Foundation FX We thank Ervan Rutishauser, Denis Valle and another reviewer for comments on the manuscript; Ron McRoberts and Bram van Putten for advice on statistical terminology; and L. Aguilar, M. Gaitan, P. Ramos, P. Villarreal and D. Zuniga for assistance in the field. We gratefully acknowledge the financial support of the HSBC Climate Partnership and the Smithsonian Institution Global Earth Observatories for the CTFS-SIGEO Global Forest Carbon Research Initiative (www.ctfs.si.edu/group/Carbon). US National Science Foundation (Award Number: 0756920, 0201307) and the Frank Levinson Family Foundation funding for the towers made this study possible. M.L. & H.C.M. developed the idea for the study, M.L. organized the fieldwork, H.C.M. & M.L. analysed the data, and M.L. & H.C.M. wrote the paper. NR 27 TC 29 Z9 29 U1 3 U2 47 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD SEP PY 2013 VL 4 IS 9 BP 793 EP 801 DI 10.1111/2041-210X.12071 PG 9 WC Ecology SC Environmental Sciences & Ecology GA 209ED UT WOS:000323736200001 ER PT J AU Clough, GW AF Clough, G. Wayne TI From the Castle SO SMITHSONIAN LA English DT Editorial Material C1 Smithsonian Inst, Washington, DC 20560 USA. RP Clough, GW (reprint author), Smithsonian Inst, Washington, DC 20560 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU SMITHSONIAN ASSOC PI WASHINGTON PA 900 JEFFERSON DR, WASHINGTON, DC 20560 USA SN 0037-7333 J9 SMITHSONIAN JI Smithsonian PD SEP PY 2013 VL 44 IS 5 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 209YW UT WOS:000323797500007 ER PT J AU Martinez, C Madrinan, S Zavada, M Jaramillo, CA AF Martinez, Camila Madrinan, Santiago Zavada, Michael Jaramillo, Carlos Alberto TI Tracing the fossil pollen record of Hedyosmum (Chloranthaceae), an old lineage with recent Neotropical diversification SO GRANA LA English DT Article DE Asteropollis; Clavainaperturites microclavatus; Miocene; Neotropics ID CRETACEOUS ANGIOSPERM POLLEN; REPRODUCTIVE STRUCTURES; BASAL ANGIOSPERMS; FLOWERING PLANTS; EARLY EVOLUTION; SOUTH-AMERICA; LATE MIOCENE; SCALE DATA; COLOMBIA; PALEOBOTANY AB Chloranthaceae represent one of the oldest angiosperm lineages. Hedyosmum, with 45 species, is the only Neotropical genus in the family. The first appearance of Hedyosmum-like pollen was in the Early Cretaceous (approximate to 112Ma). The next unequivocal record of Hedyosmum-like pollen (Clavainaperturites microclavatus) occurred in the early Miocene. The main objective of this study was to determine the relationship between the fossil C. microclavatus and extant representatives of Hedyosmum. Pollen was examined using light, scanning and transmission electron microscopy. Based on a phylogenetic analysis of pollen traits of Chloranthaceae, we concluded that C. microclavatus is related to Hedyosmum. The abundant Neogene fossil evidence of C. microclavatus from South America showed that the ancestor of extant Hedyosmum migrated to tropical South America during the early Miocene and occupied initially lowlands. A comparison of the C. microclavatus fossil record from both Panama and Colombia/Venezuela suggests that the first Neotropical migration of Hedyosmum was from South America to Central America. The abundant Plio-Pleistocene C. microclavatus from Andean regions supports the hypothesis of a recent radiation of the genus as a consequence of the uplift of the tropical Andes. The biogeographic history of Hedyosmum provides an example of recent enrichment of the Neotropical flora. C1 [Martinez, Camila; Jaramillo, Carlos Alberto] Smithsonian Trop Res Inst, Ancon, Panama. [Martinez, Camila; Madrinan, Santiago] Univ Los Andes, Lab Bot & Sistemat, Bogota, Colombia. [Zavada, Michael] Seton Hall Univ, Dept Biol, S Orange, NJ 07079 USA. RP Jaramillo, CA (reprint author), Smithsonian Trop Res Inst, Roosvelt Ave,Tupper Bldg 401, Ancon, Panama. EM jaramilloc@si.edu RI Madrinan, Santiago/A-1149-2010 OI Madrinan, Santiago/0000-0002-0807-6523 FU Smithsonian Paleobiology Endowment Fund; Unrestricted Endowments SI Grants; University of Yale; Smithsonian Tropical Research Institute FX The authors thank James Doyle (University of California, Davis) for detailed reviews of several versions of this manuscript; James Richardson (Royal Botanic Garden, Edinburgh) and Alexandre Antonelli (Gothenburg Botanic Garden) for valuable comments; Fabio Gonzales (Universidad Nacional de Colombia, Bogota), Fabiany Herrera (STRI), Monica Carvalho (STRI) and Silane da Silva (INPA) for sending samples; the herbaria COL, US, MO, PMA, COAH and INPA for providing samples; Hong-Zhi Kong for providing the dated phylogeny of Chloranthaceae; and Mayandi Sivaguru, Alejandra Restrepo and Surangi Punyasena from the University of Illinois, Urbana, and I. Romero, for sharing photographs of fossil pollen samples. This project was supported by the Smithsonian Paleobiology Endowment Fund, the Unrestricted Endowments SI Grants, the University of Yale Edward P. Bass Distinguished Visiting Environmental Scholar, and a Short Term Fellowship from the Smithsonian Tropical Research Institute. NR 75 TC 5 Z9 5 U1 1 U2 17 PU TAYLOR & FRANCIS AS PI OSLO PA KARL JOHANS GATE 5, NO-0154 OSLO, NORWAY SN 0017-3134 J9 GRANA JI Grana PD SEP 1 PY 2013 VL 52 IS 3 BP 161 EP 180 DI 10.1080/00173134.2012.760646 PG 20 WC Plant Sciences SC Plant Sciences GA 205VY UT WOS:000323474100001 ER PT J AU Merrill, RM Naisbit, RE Mallet, J Jiggins, CD AF Merrill, R. M. Naisbit, R. E. Mallet, J. Jiggins, C. D. TI Ecological and genetic factors influencing the transition between host-use strategies in sympatric Heliconius butterflies SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE coexistence; genetic linkage; host-plant use; Lepidoptera; speciation ID PASSION-VINE BUTTERFLIES; ENEMY-FREE-SPACE; REPRODUCTIVE ISOLATION; PLANT SPECIALIZATION; ADAPTIVE RADIATION; HYBRID STERILITY; SEXUAL SELECTION; WARNING-COLOR; SPECIATION; EVOLUTION AB Shifts in host-plant use by phytophagous insects have played a central role in their diversification. Evolving host-use strategies will reflect a trade-off between selection pressures. The ecological niche of herbivorous insects is partitioned along several dimensions, and if populations remain in contact, recombination will break down associations between relevant loci. As such, genetic architecture can profoundly affect the coordinated divergence of traits and subsequently the ability to exploit novel habitats. The closely related species Heliconius cydno and H.melpomene differ in mimetic colour pattern, habitat and host-plant use. We investigate the selection pressures and genetic basis underlying host-use differences in these two species. Host-plant surveys reveal that H.melpomene specializes on a single species of Passiflora. This is also true for the majority of other Heliconius species in secondary growth forest at our study site, as expected under a model of interspecific competition. In contrast, H.cydno, which uses closed-forest habitats where both Heliconius and Passiflora are less common, appears not to be restricted by competition and uses a broad selection of the available Passiflora. However, other selection pressures are likely involved, and field experiments reveal that early larval survival of both butterfly species is highest on Passiflora menispermifolia, but most markedly so for H.melpomene, the specialist on that host. Finally, we demonstrate an association between host-plant acceptance and colour pattern amongst interspecific hybrids, suggesting that major loci underlying these important ecological traits are physically linked in the genome. Together, our results reveal ecological and genetic associations between shifts in habitat, host use and mimetic colour pattern that have likely facilitated both speciation and coexistence. C1 [Merrill, R. M.; Jiggins, C. D.] Univ Cambridge, Dept Zool, Cambridge CB2 1ST, England. [Merrill, R. M.] Smithsonian Trop Res Inst, Balboa, Panama. [Naisbit, R. E.] Univ Fribourg, Dept Biol, CH-1700 Fribourg, Switzerland. [Mallet, J.] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. RP Merrill, RM (reprint author), Univ Cambridge, Dept Zool, Cambridge CB2 1ST, England. EM r.merrill@zoo.cam.ac.uk RI Naisbit, Russell/B-9658-2011; Jiggins, Chris/B-9960-2008; mallet, james/B-5114-2008 OI Naisbit, Russell/0000-0003-0190-9323; Jiggins, Chris/0000-0002-7809-062X; FU Smithsonian Tropical Research Institute; Junior Research Fellowship at King's College, Cambridge; BBSRC; Swiss National Science Foundation; Leverhulme Trust; NERC FX We are grateful to Moises Abanto and Timothy Thurman for help in the insectaries. We thank the Smithsonian Tropical Research Institute for support and the Ministerio del Ambiente for permission to collect butterflies in Panama. RMM is supported by a Junior Research Fellowship at King's College, Cambridge, and REN was supported by a studentship from the BBSRC and by the Swiss National Science Foundation. We also thank the BBSRC and Leverhulme Trust for funding awarded to CDJ and the BBSRC and NERC for funding awarded to JM. NR 68 TC 7 Z9 7 U1 6 U2 72 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD SEP PY 2013 VL 26 IS 9 BP 1959 EP 1967 DI 10.1111/jeb.12194 PG 9 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 203TQ UT WOS:000323316800011 PM 23961921 ER PT J AU Wirshing, HH Feldheim, KA Baker, AC AF Wirshing, Herman H. Feldheim, Kevin A. Baker, Andrew C. TI Vectored dispersal of Symbiodinium by larvae of a Caribbean gorgonian octocoral SO MOLECULAR ECOLOGY LA English DT Article DE Caribbean; dispersal; octocoral; population genetics; specificity; Symbiodinium ID POPULATION GENETIC-STRUCTURE; MULTILOCUS GENOTYPE DATA; SEA FAN CORAL; FLORIDA-KEYS; ALGAL SYMBIOSIS; PSEUDOPTEROGORGIA-ELISABETHAE; MARINE POPULATIONS; GENUS SYMBIODINIUM; ALLELE FREQUENCIES; CONNECTIVITY AB The ability of coral reefs to recover from natural and anthropogenic disturbance is difficult to predict, in part due to uncertainty regarding the dispersal capabilities and connectivity of their reef inhabitants. We developed microsatellite markers for the broadcast spawning gorgonian octocoral Eunicea (Plexaura) flexuosa (four markers) and its dinoflagellate symbiont, Symbiodinium B1 (five markers), and used them to assess genetic connectivity, specificity and directionality of gene flow among sites in Florida, Panama, Saba and the Dominican Republic. Bayesian analyses found that most E. flexuosa from the Florida reef tract, Saba and the Dominican Republic were strongly differentiated from many E. flexuosa in Panama, with the exception of five colonies from Key West that clustered with colonies from Panama. In contrast, Symbiodinium B1 was more highly structured. At least seven populations were detected that showed patterns of isolation by distance. The symbionts in the five unusual Key West colonies also clustered with symbionts from Panama, suggesting these colonies are the result of long-distance dispersal. Migration rate tests indicated a weak signal of northward immigration from the Panama population into the lower Florida Keys. As E. flexuosa clonemates only rarely associated with the same Symbiodinium B1 genotype (and vice versa), these data suggest a dynamic host-symbiont relationship in which E. flexuosa is relatively well dispersed but likely acquires Symbiodinium B1 from highly structured natal areas prior to dispersal. Once vectored by host larvae, these symbionts may then spread through the local population, and/or host colonies may acquire different local symbiont genotypes over time. C1 [Wirshing, Herman H.; Baker, Andrew C.] Univ Miami, Rosenstiel Sch Marine & Atmospher Sci, Div Marine Biol & Fisheries, Miami, FL 33149 USA. [Feldheim, Kevin A.] Field Museum Nat Hist, Pritzker Lab Mol Systemat & Evolut, Chicago, IL 60605 USA. RP Wirshing, HH (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM wirshingh@si.edu RI Johnson, Selena/K-3541-2013 FU Pritzker Foundation; University of Miami's Rosenstiel School FX Special thanks to S. Gray, L. Krimsky, S. Manley, J. Sanchez and P. Etnoyer for their assistance in the field and boat captaining. K. Darois, K. Lynch and H. Tieslink contributed invaluable support in the laboratory. D. Crawford and A. Wilson provided indispensible advice and suggestions on early drafts of the manuscript. Microsatellite enrichment was carried out in the Pritzker Laboratory for Molecular Systematics and Evolution operated with support from the Pritzker Foundation. This work was partially funded by Knight and Rowlands Fellowships at the University of Miami's Rosenstiel School. NR 96 TC 6 Z9 6 U1 1 U2 29 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 J9 MOL ECOL JI Mol. Ecol. PD SEP PY 2013 VL 22 IS 17 BP 4413 EP 4432 DI 10.1111/mec.12405 PG 20 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 206GI UT WOS:000323506400006 PM 23980762 ER PT J AU Hurt, C Silliman, K Anker, A Knowlton, N AF Hurt, C. Silliman, K. Anker, A. Knowlton, N. TI Ecological speciation in anemone-associated snapping shrimps (Alpheus armatus species complex) SO MOLECULAR ECOLOGY LA English DT Article DE Alpheus; Brazil; Caribbean; host-shift; isolation migration; sea anemone; symbiosis; sympatric speciation ID GENUS ALPHEUS; REPRODUCTIVE ISOLATION; PHYLOGENETIC EVIDENCE; BARTHOLOMEA-ANNULATA; POPULATION-GENETICS; HOST-SPECIFICITY; SEA; PANAMA; ISTHMUS; CORAL AB Divergent natural selection driven by competition for limited resources can promote speciation, even in the presence of gene flow. Reproductive isolation is more likely to result from divergent selection when the partitioned resource is closely linked to mating. Obligate symbiosis and host fidelity (mating on or near the host) can provide this link, creating ideal conditions for speciation in the absence of physical barriers to dispersal. Symbiotic organisms often experience competition for hosts, and host fidelity ensures that divergent selection for a specific host or host habitat can lead to speciation and strengthen pre-existing reproductive barriers. Here, we present evidence that diversification of a sympatric species complex occurred despite the potential for gene flow and that partitioning of host resources (both by species and by host habitat) has contributed to this diversification. Four species of snapping shrimps (Alpheus armatus, A. immaculatus, A. polystictus and A. roquensis) are distributed mainly sympatrically in the Caribbean, while the fifth species (A. rudolphi) is restricted to Brazil. All five species are obligate commensals of sea anemones with a high degree of fidelity and ecological specificity for host species and habitat. We analysed sequence data from 10 nuclear genes and the mitochondrial COI gene in 11-16 individuals from each of the Caribbean taxa and from the only available specimen of the Brazilian taxon. Phylogenetic analyses support morphology-based species assignments and a well-supported Caribbean clade. The Brazilian A. rudolphi is recovered as an outgroup to the Caribbean taxa. Isolation-migration coalescent analysis provides evidence for historical gene flow among sympatric sister species. Our data suggest that both selection for a novel host and selection for host microhabitat may have promoted diversification of this complex despite gene flow. C1 [Hurt, C.; Silliman, K.] Univ Miami, Cox Sci Ctr, Miami, FL 33146 USA. [Anker, A.] Univ Fed Ceara, Inst Ciencias Mar Labomar, BR-60165081 Fortaleza, Ceara, Brazil. [Knowlton, N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Knowlton, N.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biodivers & Conservat, San Diego, CA 92093 USA. RP Hurt, C (reprint author), Tennessee Technol Univ, Pennebaker Hall, Cookeville, TN 38505 USA. EM hurtc@bio.miami.edu FU CAPES of the Brazilian Government FX We are grateful to Kristen Hultgren (University of Seattle) and Jane Indorf (University of Miami) who reviewed the manuscript and made a number of useful suggestions and corrections. Paulo P.G. Pachelle (Universidade Federal do Ceara) provided a very valuable specimen of A. rudolphi. Additional photographs were kindly provided by Frederic Fasquel (Fig. 1D,E) and Marcio Lisa (Fig. 1F). One of the authors (AA) was supported by CAPES of the Brazilian Government in the form of a postdoctoral fellowship. NR 63 TC 5 Z9 6 U1 5 U2 77 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0962-1083 EI 1365-294X J9 MOL ECOL JI Mol. Ecol. PD SEP PY 2013 VL 22 IS 17 BP 4532 EP 4548 DI 10.1111/mec.12398 PG 17 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 206GI UT WOS:000323506400014 PM 23859595 ER PT J AU Geller, J Meyer, C Parker, M Hawk, H AF Geller, J. Meyer, C. Parker, M. Hawk, H. TI Redesign of PCR primers for mitochondrial cytochrome c oxidase subunit I for marine invertebrates and application in all-taxa biotic surveys SO MOLECULAR ECOLOGY RESOURCES LA English DT Article DE biotic surveys; cytochrome c oxidase subunit I; DNA barcoding; Moorea; universal primers ID DNA; BARCODE; LIFE; SEQUENCES; PATTERNS AB DNA barcoding is a powerful tool for species detection, identification and discovery. Metazoan DNA barcoding is primarily based upon a specific region of the cytochrome c oxidase subunit I gene that is PCR amplified by primers HCO2198 and LCO1490 (Folmer primers') designed by Folmer etal. (Molecular Marine Biology and Biotechnology, 3, 1994, 294). Analysis of sequences published since 1994 has revealed mismatches in the Folmer primers to many metazoans. These sequences also show that an extremely high level of degeneracy would be necessary in updated Folmer primers to maintain broad taxonomic utility. In primers jgHCO2198 and jgLCO1490, we replaced most fully degenerated sites with inosine nucleotides that complement all four natural nucleotides and modified other sites to better match major marine invertebrate groups. The modified primers were used to amplify and sequence cytochrome c oxidase subunit I from 9105 specimens from Moorea, French Polynesia and San Francisco Bay, California, USA representing 23 phyla, 42 classes and 121 orders. The new primers, jgHCO2198 and jgLCO1490, are well suited for routine DNA barcoding, all-taxon surveys and metazoan metagenomics. C1 [Geller, J.; Hawk, H.] Moss Landing Marine Labs, Moss Landing, CA 95309 USA. [Meyer, C.; Parker, M.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Geller, J (reprint author), Moss Landing Marine Labs, 8272 Moss Landing Rd, Moss Landing, CA 95309 USA. EM geller@mlml.calstate.edu FU California Department of Fish and Wildlife (San Francisco); Gordon and Betty Moore Foundation (Moorea) FX This work was supported by the California Department of Fish and Wildlife (San Francisco) and the Gordon and Betty Moore Foundation (Moorea). The Smithsonian Environmental Research Center Marine Invasions Laboratory made specimen collections in San Francisco Bay, and we particularly thank Gail Ashton, Christopher Brown, Tracy Campbell, Linda McCann and Greg Ruiz. Michelle Marraffini, Kristin Meagher and Gillian Rhett provided additional laboratory and computer assistance at MLML. We also acknowledge a multitude of Moorea Biocode Project participants for their field and collections efforts. Comments by two reviewers significantly improved our manuscript. NR 19 TC 82 Z9 83 U1 6 U2 86 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-098X J9 MOL ECOL RESOUR JI Mol. Ecol. Resour. PD SEP PY 2013 VL 13 IS 5 BP 851 EP 861 DI 10.1111/1755-0998.12138 PG 11 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 198WK UT WOS:000322953400010 PM 23848937 ER PT J AU Betancur, R Li, CH Munroe, TA Ballesteros, JA Orti, G AF Betancur-R., Ricardo Li, Chenhong Munroe, Thomas A. Ballesteros, Jesus A. Orti, Guillermo TI Addressing Gene Tree Discordance and Non-Stationarity to Resolve a Multi-Locus Phylogeny of the Flatfishes (Teleostei: Pleuronectiformes) SO SYSTEMATIC BIOLOGY LA English DT Article DE Base compositional bias; Carangimorphariae; compositional attraction; concatenation; gene tree-species tree; multi-locus data set; non-homogeneous models; non-stationarity; Pleuronectiformes; systematic error ID BEETLE MITOCHONDRIAL PHYLOGENOMICS; RAY-FINNED FISH; MAXIMUM-LIKELIHOOD; COMPOSITIONAL HETEROGENEITY; SEQUENCE EVOLUTION; SPECIES TREES; DNA SEQUENCES; ULTRACONSERVED ELEMENTS; MOLECULAR SYSTEMATICS; PROTEIN EVOLUTION AB Non-homogeneous processes and, in particular, base compositional non-stationarity have long been recognized as a critical source of systematic error. But only a small fraction of current molecular systematic studies methodically examine and effectively account for the potentially confounding effect of non-stationarity. The problem is especially overlooked in multi-locus or phylogenomic scale analyses, in part because no efficient tools exist to accommodate base composition heterogeneity in large data sets. We present a detailed analysis of a data set with 20 genes and 214 taxa to study the phylogeny of flatfishes (Pleuronectiformes) and their position among percomorphs. Most genes vary significantly in base composition among taxa and fail to resolve flatfish monophyly and other emblematic groups, suggesting that non-stationarity may be causing systematic error. We show a strong association between base compositional bias and topological discordance among individual gene partitions and their inferred trees. Phylogenetic methods applying non-homogeneous models to accommodate non-stationarity have relatively minor effect to reduce gene tree discordance, suggesting that available computer programs applying these methods do not scale up efficiently to the data set of modest size analysed in this study. By comparing phylogenetic trees obtained with species tree (STAR) and concatenation approaches, we show that gene tree discordance in our data set is most likely due to base compositional biases than to incomplete lineage sorting. Multi-locus analyses suggest that the combined phylogenetic signal from all loci in a concatenated data set overcomes systematic biases induced by non-stationarity at each partition. Finally, relationships among flatfishes and their relatives are discussed in the light of these results. We find support for the monophyly of flatfishes and confirm findings from previous molecular phylogenetic studies suggesting their close affinity with several carangimorph groups (i.e., jack and allies, barracuda, archerfish, billfish and swordfish, threadfin, moonfish, beach salmon, and snook and barramundi). C1 [Betancur-R., Ricardo; Ballesteros, Jesus A.; Orti, Guillermo] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Li, Chenhong] Shanghai Ocean Univ, Coll Fisheries & Life Sci, Shanghai 201306, Peoples R China. [Munroe, Thomas A.] NOAA, Natl Systemat Lab NMFS, Smithsonian Inst NHB, Washington, DC 20013 USA. RP Orti, G (reprint author), George Washington Univ, Dept Biol Sci, 2023 G St NW, Washington, DC 20052 USA. EM gorti@gwu.edu FU GWU Selective Excellence in Diversity of Life program; National Science Foundation [DEB-1004765] FX This research was partially funded by GWU Selective Excellence in Diversity of Life program (to R.B.R.); and the National Science Foundation [grant DEB-1004765 (Euteleost Tree of Life) to G.O. and C.L.]. NR 117 TC 31 Z9 32 U1 5 U2 55 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 SEP PY 2013 VL 62 IS 5 BP 763 EP 785 DI 10.1093/sysbio/syt039 PG 23 WC Evolutionary Biology SC Evolutionary Biology GA 203MO UT WOS:000323297500009 PM 23749787 ER PT J AU Garcia-Robledo, C Kuprewicz, EK Staines, CL Kress, WJ Erwin, TL AF Garcia-Robledo, Carlos Kuprewicz, Erin K. Staines, Charles L. Kress, W. John Erwin, Terry L. TI Using a comprehensive DNA barcode library to detect novel egg and larval host plant associations in a Cephaloleia rolled-leaf beetle (Coleoptera: Chrysomelidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Bromeliaceae; Cephaloleia histrionica; COI; herbivory; mitochondrial DNA; Pitcairnia arcuata; Zingiberales ID INSECT HERBIVORES; SPECIES IDENTIFICATION; CASSIDINAE; GENERALIST; SPECIALIST; SUCCESS; GINGERS; ADULTS AB To fully understand the ecology and evolution of plant-herbivore interactions, information regarding the life history of both immature and adult insect stages is essential. However, most knowledge of plant-herbivore associations is derived from observations of adults. One reason for this bias is that species identification of immature stages is usually challenging. DNA barcodes can be used to identify immature stages to the species level. This technique compares short sequences of the appropriate DNA barcode loci [e.g. mitochondrial cytochrome c oxidase subunit I (COI) gene for insects] of an unidentified specimen with a known DNA barcode library. The accuracy of DNA-based identifications depends on the comprehensiveness of the DNA barcode library. We generated a comprehensive DNA barcode library for a community of rolled-leaf beetles (Coleoptera: Chrysomelidae) in a premontane tropical forest in Costa Rica. The DNA barcode COI accurately identified all beetle species included in the study. Using this DNA barcode library, we identified eggs and larvae of Cephaloleia histrionicaBaly with 100% confidence. This new record of C.histrionica is unique in that this species completes its life cycle on a bromeliad, whereas most Cephaloleia species are associated with plants from the order Zingiberales. The life cycle, diet breadth, immature stages, and sexual dimorphism are described for C.histrionica.(c) 2013 The Linnean Society of London, Biological Journal of the Linnean Society, 2013, 110, 189-198. C1 [Garcia-Robledo, Carlos; Staines, Charles L.; Erwin, Terry L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. [Garcia-Robledo, Carlos; Kuprewicz, Erin K.; Kress, W. John] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20560 USA. [Kuprewicz, Erin K.] Duke Univ, Org Trop Studies, Durham, NC 27708 USA. RP Garcia-Robledo, C (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM garciac@si.edu FU Smithsonian Postdoctoral Fellowship; National Geographic-Waitt Institute [W149-11]; Heliconia Society International; Rubenstein Fellowship - Encyclopedia of Life FX The authors thank the staff of Selva Tica-Rara Avis Reserves, I. Lopez (Smithsonian Institution) and J. Hurtado (TEAM project Barva Transect, Conservation International) for logistical support. We thank S. Nagi and D. Erickson (Smithsonian Institution) for assistance during the laboratory work. S. Whittaker (Smithsonian Institution) provided advice with respect to obtaining SEM images. Comments by Hugh Loxdale and an anonymous reviewer improved the manuscript substantially. This research was funded by a Smithsonian Postdoctoral Fellowship, a National Geographic-Waitt Institute grant (W149-11), a Heliconia Society International grant, and a Rubenstein Fellowship - Encyclopedia of Life to C.G. NR 36 TC 9 Z9 9 U1 3 U2 39 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 SEP PY 2013 VL 110 IS 1 BP 189 EP 198 DI 10.1111/bij.12115 PG 10 WC Evolutionary Biology SC Evolutionary Biology GA 200BF UT WOS:000323040200014 ER PT J AU Olson, SL Hearty, PJ AF Olson, Storrs L. Hearty, Paul J. TI Periodicity of extinction and recolonization of the West Indian topshell Cittarium pica in the Quaternary of Bermuda (Gastropoda: Trochoidea) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Coenobita clypeatus; Gulf Stream velocity; hermit crabs; larval transportation; marine istotope stages 1-11; paleoceanography ID ATLANTIC THERMOHALINE CIRCULATION; LAST INTERGLACIAL PERIOD; SEA-LEVEL HIGHSTAND; NORTH-ATLANTIC; COENOBITA-CLYPEATUS; LATE PLEISTOCENE; IBERIAN MARGIN; HERMIT-CRAB; GULF-STREAM; BAHAMAS AB Hermit-crab transported shells of the West Indian top shell Cittarium pica occur in numerous terrestrial fossil deposits on Bermuda, which is the most remote outpost of this Caribbean species. Cittarium is so far known only from deposits of interglacial ages corresponding to marine isotope stages (MIS) 11, 9, 5e, and 1 (Holocene). In at least the cases of MIS 11 and 5e, Cittarium appears at the very beginning of the interglacial. The species is definitely absent from well-stratified cave deposits of the last glacial (MIS 4-2). It is hypothesized that colder sea-surface temperatures (SSTs) during glacial periods caused Cittarium to be extirpated on Bermuda, and that it has made at least four independent colonizations of the island in the past 400000 years. Because of the limited larval life of Cittarium, the window for colonization may be a very narrow period at the onset of interglacials when the SST has risen sufficiently to make Bermuda habitable but the velocity of the Gulf Stream is still sufficiently rapid to transport viable larvae from the Bahamas.(c) 2013 The Linnean Society of London, Biological Journal of the Linnean Society, 2013, 110, 235-243. C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Hearty, Paul J.] Univ N Carolina, Dept Environm Studies, Wilmington, NC 28403 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM olsons@si.edu NR 62 TC 2 Z9 2 U1 0 U2 14 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 SEP PY 2013 VL 110 IS 1 BP 235 EP 243 DI 10.1111/bij.12119 PG 9 WC Evolutionary Biology SC Evolutionary Biology GA 200BF UT WOS:000323040200018 ER PT J AU Patrick, CJ AF Patrick, Christopher J. TI The effect of shredder community composition on the production and quality of fine particulate organic matter SO FRESHWATER SCIENCE LA English DT Article DE leaf decomposition; particle production; FPOM; shredder; processing chain ecology; biodiversity ID HYDROPSYCHE-SPARNA TRICHOPTERA; LEAF-LITTER; STREAM DETRITIVORE; ECOSYSTEM FUNCTION; FOREST STREAM; CELLULOSE DIGESTION; HEADWATER STREAMS; CURRENT KNOWLEDGE; FECAL PELLETS; INSECT FECES AB Decomposition of senesced primary production starts processing chains in aquatic systems. Shredding macroinvertebrates convert coarse particulate organic matter (CPOM) to fine particulate organic matter (FPOM) that supports 2 other feeding groups, collecting and filtering macroinvertebrates. This linkage is often invoked by aquatic ecologists, but the effect of detritivore assemblage composition on production of FPOM is relatively understudied. I manipulated detritivore assemblage composition (Limnephilus sp., Caecidotea sp., and Hyalella azteca) in aquatic mesocosms stocked with green speckled alder leaves (Alnus incana rugosa). I measured production rate, size distribution, and stoichiometry of FPOM produced through time. Detritivore species richness had a positive effect on FPOM production resulting from inclusion of the functionally dominant shredder, Limnephilus sp., in mixed-species treatments (e. g., sampling effect). Mixed-species treatments had significantly faster particle production than predicted from single-species treatments. The significant increases in particle production in mixed-species treatments could have resulted from release of Limnephilus sp. from intraspecific competition, facilitation between shredders, or both processes. FPOM size distribution and C:N varied significantly among treatments and was affected by species interactions in mixed-species treatments. The presence of Limnephilus sp. significantly skewed the FPOM size distribution and increased the mass of particles >250 mu m by similar to 60%. These results suggest that the specific shredding insects in an assemblage could strongly affect production of FPOM and the size distribution and stoichiometry of FPOM produced by the benthos of a stream. C1 [Patrick, Christopher J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Patrick, Christopher J.] Univ Notre Dame, Notre Dame, IN 46656 USA. RP Patrick, CJ (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM patrickc@si.edu FU University of Notre Dame Environmental Research Center FX Gary Belovsky, Jason McLachlan, Jennifer Tank, and Todd Crowl provided feedback and critiques of this work through its inception and execution. Gary Belovsky, Michael Cramer, and David Richardson provided helpful critiques of this manuscript. Matt Barnes and Jamin Dryer helped during the field survey. This work was funded by the University of Notre Dame Environmental Research Center. NR 58 TC 4 Z9 5 U1 8 U2 75 PU SOC FRESWATER SCIENCE PI WACO PA 5400 BOSQUE BLVD, STE 680, WACO, TX 76710 USA SN 2161-9565 J9 FRESHW SCI JI Freshw. Sci. PD SEP PY 2013 VL 32 IS 3 BP 1026 EP 1035 DI 10.1899/12-090.1 PG 10 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 197DB UT WOS:000322828300024 ER PT J AU Verde, L Protopapas, P Jimenez, R AF Verde, Licia Protopapas, Pavlos Jimenez, Raul TI Planck and the local Universe: Quantifying the tension SO PHYSICS OF THE DARK UNIVERSE LA English DT Article DE Cosmology; Hubble parameter; Age of the Universe; Cosmic Microwave Background; Bayesian methods ID GLOBULAR-CLUSTERS; HUBBLE CONSTANT; COSMOLOGICAL PARAMETERS; AGES AB We use the latest Planck constraints, and in particular constraints on the derived parameters (Hubble constant and age of the Universe) for the local universe and compare them with local measurements of the same quantities. We propose a way to quantify whether cosmological parameters constraints from two different experiments are in tension or not. Our statistic, T, is an evidence ratio and therefore can be interpreted with the widely used Jeffrey's scale. We find that in the framework of the Lambda CDM model, the Planck inferred two dimensional, joint, posterior distribution for the Hubble constant and age of the Universe is in "strong" tension with the local measurements; the odds being similar to 1: 50. We explore several possibilities for explaining this tension and examine the consequences both in terms of unknown errors and deviations from the Lambda CDM model. In some one-parameter Lambda CDM model extensions, tension is reduced whereas in other extensions, tension is instead increased. In particular, small total neutrino masses are favored and a total neutrino mass above 0.15 eV makes the tension "highly significant" (odds similar to 1: 150). A consequence of accepting this interpretation of the tension is that the degenerate neutrino hierarchy is highly disfavored by cosmological data and the direct hierarchy is slightly favored over the inverse. (C) 2013 The Authors. Published by Elsevier B.V. C1 [Verde, Licia; Jimenez, Raul] Univ Barcelona, UB IEEC, ICREA, Barcelona 08034, Spain. [Verde, Licia; Jimenez, Raul] Univ Barcelona, UB IEEC, ICC, Barcelona 08034, Spain. [Verde, Licia; Jimenez, Raul] CERN, Dept Phys, Theory Grp, CH-1211 Geneva 23, Switzerland. [Protopapas, Pavlos] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Protopapas, Pavlos] Harvard Univ, Sch Engn & Appl Sci, Inst Appl Computat Sci, Cambridge, MA 02138 USA. RP Verde, L (reprint author), Univ Barcelona, UB IEEC, ICREA, Marti i Franques 1, Barcelona 08034, Spain. EM liciaverde@gmail.com OI Jimenez, Raul/0000-0002-3370-3103; Verde, Licia/0000-0003-2601-8770 FU European Research Council under the European Community's Seventh Framework Programme [FP7-IDEASPhys]; Mineco grant [FPA2011-29678-C02-02]; ESA Member States; NASA; Canada; ESA; CNES (France); CNRS/INSU-IN2P3-INP (France); ASI (Italy); CNR (Italy); INAF (Italy); DoE (USA); STFC (UK); UKSA (UK); CSIC (Spain); MICINN (Spain); JA (Spain); Tekes (Finland); AoF (Finland); CSC (Finland); NASA (USA); DLR (Germany); MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); PRACE (EU) FX LV is supported by European Research Council under the European Community's Seventh Framework Programme grant FP7-IDEASPhys. LSS. LV and RJ acknowledge Mineco grant FPA2011-29678-C02-02. We thank Hiranya Peiris and Arthur Kosowsky for discussions and comments on an early version of this work. We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA), part of the High Energy Astrophysics Science Archive Center (HEASARC). HEASARC /LAMBDA is a service of the Astrophysics Science Division at the NASA Goddard Space Flight Center. This work is based on observations obtained with Planck (http://www.esa.int/Planck), an ESA science mission with instruments and contributions directly funded by ESA Member States, NASA, and Canada. The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). We acknowledge the use of the Planck Legacy Archive. NR 31 TC 28 Z9 28 U1 0 U2 2 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 2212-6864 J9 PHYS DARK UNIVERSE JI Phys. Dark Universe PD SEP PY 2013 VL 2 IS 3 BP 166 EP 175 DI 10.1016/j.dark.2013.09.002 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AR6NT UT WOS:000343700800006 ER PT J AU Eriksson, PG Banerjee, S Catuneanu, O Corcoran, PL Eriksson, KA Hiatt, EE Laflamme, M Lenhardt, N Long, DGF Miall, AD Mints, MV Pufahl, PK Sarkar, S Simpson, EL Williams, GE AF Eriksson, Patrick G. Banerjee, Santanu Catuneanu, Octavian Corcoran, Patricia L. Eriksson, Kenneth A. Hiatt, Eric E. Laflamme, Marc Lenhardt, Nils Long, Darrel G. F. Miall, Andrew D. Mints, Michael V. Pufahl, Peir K. Sarkar, Subir Simpson, Edward L. Williams, George E. TI Secular changes in sedimentation systems and sequence stratigraphy SO GONDWANA RESEARCH LA English DT Article DE Fragmentary sedimentary record; Actualism; Secular change in rates and intensities of processes; Earth mechanics; Palaeoatmospheric evolution; Great oxidation events; Global magmatic slowdown; Glacial events; Biological evolution; Sequence stratigraphy ID BILLION YEARS AGO; BARBERTON GREENSTONE-BELT; PERMIAN MASS EXTINCTION; GREAT OXIDATION EVENT; PROTEROZOIC KAIMUR FORMATION; SNOWBALL EARTH HYPOTHESIS; LOW-LATITUDE GLACIATION; MOUNT BRUCE SUPERGROUP; BIOLOGICAL SOIL CRUSTS; ARCHAEAN MOODIES GROUP AB The ephemeral nature of most sedimentation processes and the fragmentary character of the sedimentary record are of first-order importance. Despite a basic uniformity of external controls on sedimentation resulting in markedly similar lithologies, facies, fades associations and depositional elements within the rock record across time, there are a number of secular changes, particularly in rates and intensities of processes that resulted in contrasts between preserved Precambrian and Phanerozoic successions. Secular change encompassed (1) variations in mantle heat, rates of plate drift and of continental crustal growth, the gravitational effects of the Moon, and in rates of weathering, erosion, transport, deposition and diagenesis; (2) a decreasing planetary rotation rate over time; (3) no vegetation in the Precambrian, but prolific microbial mats, with the opposite pertaining to the Phanerozoic; (4) the long-term evolution of the hydrosphere-atmosphere-biosphere system. A relatively abrupt and sharp turning point was reached in the Neoarchaean, with spikes in mantle plume flux and tectonothermal activity and possibly concomitant onset of the supercontinent cycle. Substantial and irreversible change occurred subsequently in the Palaeoproterozoic, whereby the dramatic change from reducing to oxidizing volcanic gases ushered in change to an oxic environment, to be followed at ca. 2.4-2.3 Ga by the "Great Oxidation Event" (GOE); rise in atmospheric oxygen was accompanied by expansion of oxygenic photosynthesis in the cyanobacteria. A possible global tectono-thermal "slowdown" from ca. 2.45-2.2 Ga may have separated a preceding plate regime which interacted with a higher energy mantle from a ca. 2.2-2.0 Ga Phanerozoic-style plate tectonic regime; the "slowdown" period also encompassed the first known global-scale glaciation and overlapped with the GOE. While large palaeodeserts emerged from ca. 2.0-1.8 Ga, possibly associated with the evolution of the supercontinent cycle, widespread euxinia by ca. 1.85 Ga ushered in the "boring billion" year period. A second time of significant and irreversible change, in the Neoproterozoic, saw a second major oxidation event and several low palaeolatitude Cryogenian (740-630 Ma) glaciations. With the veracity of the "Snowball Earth" model for Neoproterozoic glaciation being under dispute, genesis of Pre-Ediacaran low-palaeolatitude glaciation remains enigmatic. Ediacaran (635-542 Ma) glaciation with a wide palaeolatitudinal range contrasts with the circum-polar nature of Phanerozoic glaciation. The observed change from low latitude to circum-polar glaciation parallels advent and diversification of the Metazoa and the Neoproterozoic oxygenation (ca. 580 Ma), and was succeeded by the Ediacaran-Cambrian transition which ushered in biomineralization, with all its implications for the chemical sedimentary record. (C) 2012 International Association for Gondwana Research. Published by Elsevier B.V. All rights reserved. C1 [Eriksson, Patrick G.; Lenhardt, Nils] Univ Pretoria, Dept Geol, ZA-0002 Pretoria, South Africa. [Banerjee, Santanu] Indian Inst Technol, Dept Earth Sci, Bombay 400076, Maharashtra, India. [Catuneanu, Octavian] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Corcoran, Patricia L.] Univ Western Ontario, Dept Earth Sci, London, ON N6A 5B7, Canada. [Eriksson, Kenneth A.] Virginia Tech, Dept Geol Sci, Blacksburg, VA 24061 USA. [Hiatt, Eric E.] Univ Wisconsin, Dept Geol, Oshkosh, WI 54901 USA. [Laflamme, Marc] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Long, Darrel G. F.] Laurentian Univ, Dept Earth Sci, Sudbury, ON P3E 2C6, Canada. [Miall, Andrew D.] Univ Toronto, Dept Geol, Toronto, ON M5S 3B1, Canada. [Mints, Michael V.] Russian Acad Sci, Inst Geol, Lab Early Precambrian Tecton, Moscow 109017, Russia. [Pufahl, Peir K.] Acadia Univ, Dept Earth & Environm Sci, Wolfville, NS B4P 2R6, Canada. [Sarkar, Subir] Jadavpur Univ, Dept Geol Sci, Kolkata 700032, India. [Simpson, Edward L.] Kutztown Univ Penn, Dept Phys Sci, Kutztown, PA 19530 USA. [Williams, George E.] Univ Adelaide, Adelaide, SA 5005, Australia. RP Eriksson, PG (reprint author), Univ Pretoria, Dept Geol, ZA-0002 Pretoria, South Africa. EM pat.eriksson@up.ac.za RI Lenhardt, Nils/F-4773-2010; OI Mints, Michael V./0000-0001-7015-6586; Hiatt, Eric/0000-0002-0004-2492; Long, Darrel/0000-0002-1014-9090 FU National Geographic Society [6003-97]; NSERC; PetroCanada Young Innovator Award; University of Wisconsin-Oshkosh University Research Program Grant; Smithsonian Institution Postdoctoral Fellowship; NASA National Astrobiology Institute Grant; University of Pretoria; National Research Foundation of South Africa FX Ed Simpson and Ken Eriksson acknowledge research support by the National Geographic Society grant 6003-97, and wish to thank Mr. Nico Oosthuyzen for permission to work in the Songimvelo game preserve and Mr. Roelf Le Roux of Barberton Mines for aid on various aspects of their work in the famous Barberton greenstone belt. Peir K. Pufahl, Eric E. Hiatt and Marc Laflamme were supported by a NSERC Discovery Grant and PetroCanada Young Innovator Award to PKP, a University of Wisconsin-Oshkosh University Research Program Grant to EEH, a Smithsonian Institution Postdoctoral Fellowship and NASA National Astrobiology Institute Grant to ML. Nils Lenhard acknowledges a University of Pretoria Research Development Program (RDP) Grant. Pat Eriksson thanks this same University, and the National Research Foundation of South Africa for research funding, and Thino Rajab for her drafting skills. We acknowledge two anonymous reviewers and guest editor Tim Kusky, for their sage advice. NR 401 TC 26 Z9 27 U1 5 U2 71 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1342-937X EI 1878-0571 J9 GONDWANA RES JI Gondwana Res. PD SEP PY 2013 VL 24 IS 2 SI SI BP 468 EP 489 DI 10.1016/j.gr.2012.09.008 PG 22 WC Geosciences, Multidisciplinary SC Geology GA 186PW UT WOS:000322057600003 ER PT J AU Moffett, MW AF Moffett, Mark W. TI Human Identity and the Evolution of Societies SO HUMAN NATURE-AN INTERDISCIPLINARY BIOSOCIAL PERSPECTIVE LA English DT Article DE Coalitions; Fission-fusion; Hunter-gatherers; Language; Outgroups; Nationalism; Social learning; Symbols; Tribes; Xenophobia ID FISSION-FUSION DYNAMICS; HUMAN SOCIAL EVOLUTION; MODERN HUMAN-BEHAVIOR; WHALES ORCINUS-ORCA; HUNTER-GATHERERS; WILD CHIMPANZEES; GROUP-SIZE; INTERGROUP CONFLICT; MATERIAL CULTURE; NEOCORTEX SIZE AB Human societies are examined as distinct and coherent groups. This trait is most parsimoniously considered a deeply rooted part of our ancestry rather than a recent cultural invention. Our species is the only vertebrate with society memberships of significantly more than 200. We accomplish this by using society-specific labels to identify members, in what I call an anonymous society. I propose that the human brain has evolved to permit not only the close relationships described by the social brain hypothesis, but also, at little mental cost, the anonymous societies within which such alliances are built. The human compulsion to discover or invent labels to "mark" group memberships may originally have been expressed in hominins as vocally learned greetings only slightly different in function from chimpanzee pant hoots (now known to be society-specific). The weight of evidence suggests that at some point, conceivably early in the hominin line, the distinct groups composed of several bands that were typical of our ancestors came to be distinguished by their members on the basis of multiple labels that were socially acquired in this way, the earliest of which would leave no trace in the archaeological record. Often overlooked as research subjects, these sizable fission-fusion communities, in recent egalitarian hunter-gatherers sometimes 2,000 strong, should consistently be accorded the status of societies, in the same sense that this word is used to describe tribes, chiefdoms, and other cultures arising later in our history. The capacity of hunter-gatherer societies to grow sufficiently populous that not all members necessarily recognize one another would make the transition to larger agricultural societies straightforward. Humans differ from chimpanzees in that societal labels are essential to the maintenance of societies and the processes giving birth to new ones. I propose that anonymous societies of all kinds can expand only so far as their labels can remain sufficiently stable. C1 Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Moffett, MW (reprint author), Smithsonian Inst, Natl Museum Nat Hist, 10th St & Constitut Ave, Washington, DC 20013 USA. EM naturalist@erols.com NR 386 TC 13 Z9 13 U1 7 U2 83 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1045-6767 EI 1936-4776 J9 HUM NATURE-INT BIOS JI Hum. Nat.-Interdiscip. Biosoc. Perspect. PD SEP PY 2013 VL 24 IS 3 BP 219 EP 267 DI 10.1007/s12110-013-9170-3 PG 49 WC Anthropology; Social Sciences, Biomedical SC Anthropology; Biomedical Social Sciences GA 194UF UT WOS:000322657500001 PM 23813244 ER PT J AU Zhou, Z Hong, DY Niu, Y Li, GD Nie, ZL Wen, J Sun, H AF Zhou, Zhuo Hong, Deyuan Niu, Yang Li, Guodong Nie, Zelong Wen, Jun Sun, Hang TI Phylogenetic and biogeographic analyses of the Sino-Himalayan endemic genus Cyananthus (Campanulaceae) and implications for the evolution of its sexual system SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cyananthus; Sino-Himalaya; Sexual system evolution; Phylogeny; Biogeography ID QINGHAI-TIBETAN PLATEAU; TRNL-F SEQUENCES; MOLECULAR PHYLOGENY; CHLOROPLAST DNA; DELAVAYI CAMPANULACEAE; RHEUM POLYGONACEAE; GEOGRAPHIC RANGE; ASTERACEAE; RADIATION; DIVERSIFICATION AB Cyananthus (Campanulaceae) is a small genus consisting of ca. 20 species endemic to the Sino-Himalayan region. Based on phylogenetic analysis using nuclear ribosomal ITS and four plastid markers (matIC, rbcL, psbA-trnH and trnG-S), our results strongly support the monophyly of Cyananthus and its close relationship with the Codonopsis clade of the platycodonoids. Three major clades are supported, corresponding to the three sections of the genus, with sect. Cyananthus, which mainly occurs in the Himalayas, being a sister to the clade comprising the other two sections (sect. Stenolobi and sect. Annul) distributed primarily in the Hengduan Mountain region. We also observed that Cyananthus exhibits variation in its sexual system, possessing both hermaphroditic and gynodioecious species. Character evolution analyses using Mesquite suggest that gynodioecy evolved from hermaphroditism only once in sect. Stenolobi, but that there is a reversal in C. forrnosus. Molecular dating and biogeographic analysis with LAGRANGE support dispersal from the Himalayas to the Hengduan Mountains during the early evolution of Cyananthus. The extensive uplift of the Qinghai-Tibetan Plateau and the Hengduan Mountains played an important role in the subsequent diversification of the genus. (C) 2013 Elsevier Inc. All rights reserved. C1 [Zhou, Zhuo; Niu, Yang; Li, Guodong; Nie, Zelong; Sun, Hang] Chinese Acad Sci, Kunming Inst Bot, Key Lab Biodivers & Biogeog, Kunming 650201, Yunnan, Peoples R China. [Hong, Deyuan] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. [Zhou, Zhuo; Niu, Yang; Li, Guodong] Univ Chinese Acad Sci, Beijing 100049, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. RP Wen, J (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, Washington, DC 20013 USA. EM wenj@si.edu; hsun@mail.kib.ac.cn RI Nie, Ze-Long/N-8471-2015 OI Nie, Ze-Long/0000-0001-8065-3981 FU National Natural Science Foundation of China (NSFC) [40930209, 31200183, U 1136601]; Chinese Academy of Sciences [XDB03030112]; Hundred Talents Program of the Chinese Academy of Sciences [2011312D11022] FX The study was supported by grants-in-aid from the National Natural Science Foundation of China (NSFC, 40930209, 31200183, U 1136601), Strategic Priority Research Program (B) of the Chinese Academy of Sciences (XDB03030112), Hundred Talents Program of the Chinese Academy of Sciences (2011312D11022 to H. Sun) and the John D. and Catherine T. MacArthur Foundation to J. Wen, R. Ree, and G. Mueller. Lab assistance was provided by Dr. H.G. Zha in the Kunming Institute of Botany and Lee Weigt, Jeff Hunt and Gabe Johnson at the Laboratory of Analytical Biology of the Smith-sonian Institution. We thank X.X. Wang, B. Xu and J.W. Zhang for help with collecting samples, and L.M. Lu for assistance on creating graphics. We also thank Sees-editing Ltd. help for English editing of the manuscript. NR 108 TC 20 Z9 21 U1 4 U2 47 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD SEP PY 2013 VL 68 IS 3 BP 482 EP 497 DI 10.1016/j.ympev.2013.04.027 PG 16 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 176PG UT WOS:000321316000010 PM 23669010 ER PT J AU Lu, LM Wang, W Chen, ZD Wen, J AF Lu, Limin Wang, Wei Chen, Zhiduan Wen, Jun TI Phylogeny of the non-monophyletic Cayratia Juss. (Vitaceae) and implications for character evolution and biogeography SO MOLECULAR PHYLOGENETICS AND EVOLUTION LA English DT Article DE Cayratia; Cyphostemma; Long-distance dispersal; Out-of-Africa; Phylogeny; Tetrastigma; Vitaceae ID GRAPE FAMILY VITACEAE; LONG-DISTANCE DISPERSAL; OUT-OF-AFRICA; MOLECULAR PHYLOGENY; VITIS VITACEAE; SEQUENCE DATA; HISTORICAL BIOGEOGRAPHY; PARTHENOCISSUS VITACEAE; TROPICAL FLORAS; DNA-SEQUENCES AB Cayratia consists of ca. 60 species primarily distributed in the tropical and subtropical regions of Asia, Australia, and Africa. It is an excellent candidate for exploring the evolution of intercontinental disjunct distributions in the Old World. Previous phylogenetic work of Vitaceae with a few species of Cayratia sampled showed that Cayratia was not monophyletic and was closely related to Cyphostemma and Tetrastigma. We herein expanded taxon sampling of Cayratia (25/60 species) with its allied genera Cyphostemma (39/150 species), Tetrastigma (27/95 species), and other related genera from Vitaceae represented, employing five plastid markers (atpB-rbcL, rps16, trnC-petN, trnH-psbA, and trnL-F), to investigate the phylogeny, character evolution and biogeography of Cayratia. The phylogenetic analyses have confirmed the monophyly of the Cayratia-Cyphostemma-Tetrastigma (CCT) clade and resolved Cayratia into three lineages: the African Cayratia clade, subg. Cayratia, and subg. Discypharia. The African Cayratia was supported as the first diverging lineage within the CCT clade and Tetrastigma is resolved as sister to subg. Discypharia. Character optimizations suggest that the presence/absence of a membrane enclosing the ventral infolds in seeds is an important character for the taxonomy of Cayratia. The presence of bracts on the lower part of the inflorescence axis is inferred to have arisen only once in Cayratia, but this character evolved several times in Tetrastigma. Both the branching pattern of tendrils and the leaf architecture are suggested as important infrageneric characters, but should be used cautiously because some states evolved multiple times. Ancestral area reconstruction and molecular dating suggest that the CCT clade originated from continental Africa in the late Cretaceous, and it then reached Asia twice independently in the late Cretaceous and late Oligocene, respectively. Several dispersals are inferred from Asia to Australia since the Eocene. (C) 2013 Elsevier Inc. All rights reserved. C1 [Lu, Limin; Wang, Wei; Chen, Zhiduan] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. [Lu, Limin] Chinese Acad Sci, Grad Sch, Beijing 100049, Peoples R China. [Wen, Jun] Smithsonian Inst, Natl Museum Nat Hist, Dept Bot, MRC166, Washington, DC 20013 USA. RP Chen, ZD (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing 100093, Peoples R China. EM zhiduan@ibcas.ac.cn; wenj@si.edu FU US National Science Foundation [DEB 0743474]; National Museum of Natural History, the Smithsonian Institution; Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution FX This study was supported by the US National Science Foundation (Grant DEB 0743474 to S.R. Manchester and J. Wen), and the Small Grants Program of the National Museum of Natural History, the Smithsonian Institution. We are grateful to Miao Sun for collecting seed materials from the PE herbarium, Zelong Nie for assistance in data analyses, and Robert Kiapranis, Michael Lovave, Thomas Magun, Quentin Luke, Elizabeth Widjaja, Leng-guan Saw, Tingshuang Yi, and Marc Appelhans for field assistance and/or sample collection. We also thank Minqing Zou for sequencing two important species during the revision of the manuscript. Laboratory work was done at and partially supported by the Laboratory of Analytical Biology of the National Museum of Natural History, the Smithsonian Institution. NR 100 TC 14 Z9 15 U1 3 U2 42 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1055-7903 EI 1095-9513 J9 MOL PHYLOGENET EVOL JI Mol. Phylogenet. Evol. PD SEP PY 2013 VL 68 IS 3 BP 502 EP 515 DI 10.1016/j.ympev.2013.04.023 PG 14 WC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity SC Biochemistry & Molecular Biology; Evolutionary Biology; Genetics & Heredity GA 176PG UT WOS:000321316000012 PM 23669013 ER PT J AU Meyer, KA Mackay, DH van Ballegooijen, AA Parnell, CE AF Meyer, K. A. Mackay, D. H. van Ballegooijen, A. A. Parnell, C. E. TI Solar Magnetic Carpet III: Coronal Modelling of Synthetic Magnetograms SO SOLAR PHYSICS LA English DT Article DE Sun: magnetic fields; Sun: magnetic carpet ID QUIET-SUN; LOOP OSCILLATIONS; BRIGHT POINTS; TRANSVERSE OSCILLATIONS; VELOCITY FIELDS; RECONNECTION; EVOLUTION; INTRANETWORK; NETWORK; CHROMOSPHERE AB This article is the third in a series working towards the construction of a realistic, evolving, non-linear force-free coronal-field model for the solar magnetic carpet. Here, we present preliminary results of 3D time-dependent simulations of the small-scale coronal field of the magnetic carpet. Four simulations are considered, each with the same evolving photospheric boundary condition: a 48-hour time series of synthetic magnetograms produced from the model of Meyer et al. (Solar Phys. 272, 29, 2011). Three simulations include a uniform, overlying coronal magnetic field of differing strength, the fourth simulation includes no overlying field. The build-up, storage, and dissipation of magnetic energy within the simulations is studied. In particular, we study their dependence upon the evolution of the photospheric magnetic field and the strength of the overlying coronal field. We also consider where energy is stored and dissipated within the coronal field. The free magnetic energy built up is found to be more than sufficient to power small-scale, transient phenomena such as nanoflares and X-ray bright points, with the bulk of the free energy found to be stored low down, between 0.5 -aEuro parts per thousand 0.8 Mm. The energy dissipated is currently found to be too small to account for the heating of the entire quiet-Sun corona. However, the form and location of energy-dissipation regions qualitatively agree with what is observed on small scales on the Sun. Future MHD modelling using the same synthetic magnetograms may lead to a higher energy release. C1 [Meyer, K. A.; Mackay, D. H.; Parnell, C. E.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meyer, KA (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. EM karen@mcs.st-and.ac.uk OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU Leverhulme Trust; STFC; Royal Society; EU FX KAM and DHM gratefully acknowledge the support of the Leverhulme Trust and the STFC. DHM would like to thank the Royal Society for their support through the Research Grant Scheme. DHM and CEP acknowledge support from the EU under FP7. NR 56 TC 4 Z9 4 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD SEP PY 2013 VL 286 IS 2 BP 357 EP 384 DI 10.1007/s11207-013-0272-1 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 145IC UT WOS:000319007700005 ER PT J AU Le Chat, G Zaslavsky, A Meyer-Vernet, N Issautier, K Belheouane, S Pantellini, F Maksimovic, M Zouganelis, I Bale, SD Kasper, JC AF Le Chat, G. Zaslavsky, A. Meyer-Vernet, N. Issautier, K. Belheouane, S. Pantellini, F. Maksimovic, M. Zouganelis, I. Bale, S. D. Kasper, J. C. TI Interplanetary Nanodust Detection by the Solar Terrestrial Relations Observatory/WAVES Low Frequency Receiver SO SOLAR PHYSICS LA English DT Article DE Interplanetary dust; Nanodust; In situ dust detection; Radio antennas; STEREO/WAVES ID PLASMA-WAVE INSTRUMENT; DUST PARTICLES; RING PLANE; GRAIN IMPACTS; COMET HALLEY; VOYAGER-2; VEGA-2; RADIO; NEPTUNE; URANUS AB New measurements using radio and plasma-wave instruments in interplanetary space have shown that nanometer-scale dust, or nanodust, is a significant contributor to the total mass in interplanetary space. Better measurements of nanodust will allow us to determine where it comes from and the extent to which it interacts with the solar wind. When one of these nanodust grains impacts a spacecraft, it creates an expanding plasma cloud, which perturbs the photoelectron currents. This leads to a voltage pulse between the spacecraft body and the antenna. Nanodust has a high charge/mass ratio, and therefore can be accelerated by the interplanetary magnetic field to the speed of the solar wind: significantly faster than the Keplerian orbital speeds of heavier dust. The amplitude of the signal induced by a dust grain grows much more strongly with speed than with mass of the dust particle. As a result, nanodust can produce a strong signal despite its low mass. The WAVES instruments on the twin Solar TErrestrial RElations Observatory spacecraft have observed interplanetary nanodust particles since shortly after their launch in 2006. After describing a new and improved analysis of the last five years of STEREO/WAVES Low Frequency Receiver data, we present a statistical survey of the nanodust characteristics, namely the rise time of the pulse voltage and the flux of nanodust. We show that previous measurements and interplanetary dust models agree with this survey. The temporal variations of the nanodust flux are also discussed. C1 [Le Chat, G.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. [Le Chat, G.; Kasper, J. C.] NASA, Lunar Sci Inst, Moffett Field, CA USA. [Le Chat, G.; Zaslavsky, A.; Meyer-Vernet, N.; Issautier, K.; Belheouane, S.; Pantellini, F.; Maksimovic, M.] Univ Paris Diderot, Univ Paris 06, CNRS, LESIA,Observ Paris, F-92195 Meudon, France. [Zouganelis, I.] Univ Paris 06, LPP, Ecole Polytech, CNRS, F-94107 St Maur Des Fosses, France. [Bale, S. D.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. RP Le Chat, G (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA USA. EM glechat@head.cfa.harvard.edu RI Bale, Stuart/E-7533-2011; Kasper, Justin/D-1152-2010 OI Bale, Stuart/0000-0002-1989-3596; Kasper, Justin/0000-0002-7077-930X FU CNES; CNRS; NASA FX We thank the team who designed and built the instrument. The S/WAVES data used here are produced by an international consortium of the Observatoire de Paris (France), the University of Minnesota (USA), the University of California Berkeley (USA), and NASA Goddard Space Flight Center (USA). The French contribution was funded by CNES and CNRS, and the USA institutions were funded by NASA. NR 28 TC 9 Z9 9 U1 1 U2 20 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-0938 J9 SOL PHYS JI Sol. Phys. PD SEP PY 2013 VL 286 IS 2 BP 549 EP 559 DI 10.1007/s11207-013-0268-x PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 145IC UT WOS:000319007700016 ER PT J AU Mueller, T O'Hara, RB Converse, SJ Urbanek, RP Fagan, WF AF Mueller, Thomas O'Hara, Robert B. Converse, Sarah J. Urbanek, Richard P. Fagan, William F. TI Social Learning of Migratory Performance SO SCIENCE LA English DT Article ID DECISION-MAKING; ORIENTATION; MOVE; INFORMATION; EVOLUTION; GENETICS; MODELS; BIRDS AB Successful bird migration can depend on individual learning, social learning, and innate navigation programs. Using 8 years of data on migrating whooping cranes, we were able to partition genetic and socially learned aspects of migration. Specifically, we analyzed data from a reintroduced population wherein all birds were captive bred and artificially trained by ultralight aircraft on their first lifetime migration. For subsequent migrations, in which birds fly individually or in groups but without ultralight escort, we found evidence of long-term social learning, but no effect of genetic relatedness on migratory performance. Social learning from older birds reduced deviations from a straight-line path, with 7 years of experience yielding a 38% improvement in migratory accuracy. C1 [Mueller, Thomas; Fagan, William F.] Univ Maryland, Dept Biol, College Pk, MD 20742 USA. [Mueller, Thomas; O'Hara, Robert B.] Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Main, Germany. [Mueller, Thomas; O'Hara, Robert B.] Goethe Univ Frankfurt, D-60325 Frankfurt, Main, Germany. [Mueller, Thomas] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. [Converse, Sarah J.] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Urbanek, Richard P.] US Fish & Wildlife Serv, Necedah Natl Wildlife Refuge, Necedah, WI 54646 USA. RP Mueller, T (reprint author), Univ Maryland, Dept Biol, College Pk, MD 20742 USA. EM muellert@gmail.com RI O'Hara, Robert/A-7499-2008; OI O'Hara, Robert/0000-0001-9737-3724; Converse, Sarah J/0000-0002-3719-5441 FU NSF [1062411]; Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz programme (Hesse, Germany); Robert Bosch Foundation FX T.M. and W.F.F. were supported by NSF Advances in Biological Informatics award 1062411, T. M. and R.B.O. were supported by the Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz programme (Hesse, Germany), and T. M. was supported by the Robert Bosch Foundation. Data were provided by the Whooping Crane Eastern Partnership and K. Jones and are deposited in the Dryad Repository: http://doi.org/10.5061/dryad.1r0f7. We thank F. Hailer, S. Servanty, E. Grant, J. Calabrese, R. Reynolds, S. Via, E. L. Neuschulz, C. Rushing, D. Bennu, and three anonymous reviewers for helpful comments and discussions. NR 31 TC 45 Z9 45 U1 16 U2 153 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD AUG 30 PY 2013 VL 341 IS 6149 BP 999 EP 1002 DI 10.1126/science.1237139 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 208BZ UT WOS:000323652300042 PM 23990559 ER PT J AU Coverdale, TC Axelman, EE Brisson, CP Young, EW Altieri, AH Bertness, MD AF Coverdale, Tyler C. Axelman, Eric E. Brisson, Caitlin P. Young, Eric W. Altieri, Andrew H. Bertness, Mark D. TI New England Salt Marsh Recovery: Opportunistic Colonization of an Invasive Species and Its Non-Consumptive Effects SO PLOS ONE LA English DT Article ID MEDIATED INDIRECT INTERACTIONS; POTENTIAL CONSERVATION VALUE; DIE-OFF; GLOBAL CHANGE; FOOD-WEB; ECOSYSTEM; MANAGEMENT; SHIFTS; VULNERABILITY; BIODIVERSITY AB Predator depletion on Cape Cod (USA) has released the herbivorous crab Sesarma reticulatum from predator control leading to the loss of cordgrass from salt marsh creek banks. After more than three decades of die-off, cordgrass is recovering at heavily damaged sites coincident with the invasion of green crabs (Carcinus maenas) into intertidal Sesarma burrows. We hypothesized that Carcinus is dependent on Sesarma burrows for refuge from physical and biotic stress in the salt marsh intertidal and reduces Sesarma functional density and herbivory through consumptive and non-consumptive effects, mediated by both visual and olfactory cues. Our results reveal that in the intertidal zone of New England salt marshes, Carcinus are burrow dependent, Carcinus reduce Sesarma functional density and herbivory in die-off areas and Sesarma exhibit a generic avoidance response to large, predatory crustaceans. These results support recent suggestions that invasive Carcinus are playing a role in the recovery of New England salt marshes and assertions that invasive species can play positive roles outside of their native ranges. C1 [Coverdale, Tyler C.; Axelman, Eric E.; Brisson, Caitlin P.; Young, Eric W.; Bertness, Mark D.] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Coverdale, TC (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM Tyler_Coverdale@Brown.edu OI Brisson, Caitlin/0000-0001-8567-1863; Coverdale, Tyler/0000-0003-0910-9187 FU NSF BIO [OCE-0927090] FX This work was funded by NSF BIO OCE-0927090. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 42 TC 5 Z9 5 U1 2 U2 75 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD AUG 29 PY 2013 VL 8 IS 8 AR e73823 DI 10.1371/journal.pone.0073823 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 209DO UT WOS:000323734600077 PM 24009763 ER PT J AU Yan, YQ Blume, D AF Yan, Yangqian Blume, D. TI Harmonically trapped Fermi gas: Temperature dependence of the Tan contact SO PHYSICAL REVIEW A LA English DT Article ID CLUSTERS; HELIUM AB Ultracold atomic gases with short-range interactions are characterized by a number of universal species-independent relations. Many of these relations involve the two-body Tan contact. Employing the canonical ensemble, we determine the Tan contact for small harmonically trapped two-component Fermi gases at unitarity over a wide range of temperatures, including the zero and high-temperature regimes. A cluster expansion that describes the properties of the N-particle system in terms of those of smaller subsystems is introduced and shown to provide an accurate description of the contact in the high-temperature regime. Finite-range corrections are quantified and the role of the Fermi statistics is elucidated by comparing results for Fermi, Bose, and Boltzmann statistics. C1 [Yan, Yangqian; Blume, D.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. [Blume, D.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Yan, YQ (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. FU National Science Foundation (NSF) [PHY-1205443, OCI-1053575]; WSU HPC; Smithsonian Astrophysical Observatory FX Support by the National Science Foundation (NSF) through Grant No. PHY-1205443 is gratefully acknowledged. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF Grant No. OCI-1053575, and the WSU HPC. This work was additionally supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 52 TC 9 Z9 9 U1 2 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD AUG 27 PY 2013 VL 88 IS 2 AR 023616 DI 10.1103/PhysRevA.88.023616 PG 9 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 207NI UT WOS:000323607900009 ER PT J AU Smith, AB Zamora, S AF Smith, Andrew B. Zamora, Samuel TI Cambrian spiral-plated echinoderms from Gondwana reveal the earliest pentaradial body plan SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE phylogeny; body plans; Echinodermata; evolution; Cambrian explosion ID SKELETAL HOMOLOGIES; GUIZHOU PROVINCE; WEST GONDWANA; KAILI BIOTA; DIVERSIFICATION; REPLACEMENTS; CHINA; SHOW AB Echinoderms are unique among animal phyla in having a pentaradial body plan, and their fossil record provides critical data on how this novel organization came about by revealing intermediate stages. Here, we report a spiral-plated animal from the early Cambrian of Morocco that is the most primitive pentaradial echinoderm yet discovered. It is intermediate between helicoplacoids (a bizarre group of spiral-bodied echinoderms) and crown-group pentaradiate echinoderms. By filling an important gap, this fossil reveals the common pattern that underpins the body plans of the two major echinoderm clades (pelmatozoans and eleutherozoans), showing that differential growth played an important role in their divergence. It also adds to the striking disparity of novel body plans appearing in the Cambrian explosion. C1 [Smith, Andrew B.] Nat Hist Museum, Dept Earth Sci, London SW7 5BD, England. [Zamora, Samuel] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Smith, AB (reprint author), Nat Hist Museum, Dept Earth Sci, Cromwell Rd, London SW7 5BD, England. EM a.smith@nhm.ac.uk RI Smith, Andrew/B-9849-2009 FU Smithsonian Institution (Springer fund); National Geographic Project [GEFNE5-11]; [CGL2011-24516] FX S.Z. was funded by the Smithsonian Institution (Springer fund) and project CGL2011-24516. Fieldwork was supported by National Geographic Project grant no. GEFNE5-11. NR 26 TC 6 Z9 6 U1 0 U2 24 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 AUG 22 PY 2013 VL 280 IS 1765 AR 20131197 DI 10.1098/rspb.2013.1197 PG 6 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 175TH UT WOS:000321255700025 PM 23804624 ER PT J AU Fair, JM Ryder, TB Loiselle, BA Blake, JG Larson, TE Davis, P Syme, J Perkins, GB Heikoop, JM AF Fair, Jeanne M. Ryder, Thomas B. Loiselle, Bette A. Blake, John G. Larson, Toti E. Davis, Paul Syme, James Perkins, George B. Heikoop, Jeffrey M. TI Estimates of dietary overlap for six species of Amazonian manakin birds using stable isotopes SO ISOTOPES IN ENVIRONMENTAL AND HEALTH STUDIES LA English DT Article; Proceedings Paper CT 8th International Conference on Applications of Stable Isotope Techniques to Ecological Studies (ISOECOL) CY AUG 20-24, 2012 CL Brest, FRANCE DE birds; carbon-13; diet; feather; isotope ecology; manakin; Monte Carlo models; moult; nitrogen-15 ID INCORPORATING CONCENTRATION-DEPENDENCE; FRUIT-EATING BIRDS; INDIVIDUAL SPECIALIZATION; SEASONAL-CHANGES; NITROGEN ISOTOPES; FORAGING ECOLOGY; CLIMATE-CHANGE; MIXING MODELS; NESTLING DIET; CARBON AB We used stable isotope ratios to determine the metabolic routing fraction of carbon and nitrogen in feathers in addition to faecal analysis to estimate diet overlap of six sympatric species of manakins in the eastern lowland forest of Ecuador. Collectively, all species varied from-23.7 to-32.7 parts per thousand for C-13, and from 6.0 to 9.9 parts per thousand for N-15, with Machaeropterus regulus showing isotopic differences from the other species. We developed a mixing model that explicitly addresses the routing of carbon and nitrogen to feathers. Interestingly, these results suggest a higher proportion of nitrogen and carbon derived from insects than anticipated based on feeding observations and faecal analysis. A concentration-dependent mixing isotopic model was also used to look at dietary proportions. While larvae and arachnids had higher N-15 values, these two groups may also be preferred prey of manakins and may be more assimilated into tissues, leading to a potential overestimation of the contribution to diet. This study supports the finding that manakin species, previously thought be primarily frugivorous, contain a significant amount of arthropods in their diet. C1 [Fair, Jeanne M.] Los Alamos Natl Lab, Environm Stewardship, Los Alamos, NM USA. [Ryder, Thomas B.] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Loiselle, Bette A.; Blake, John G.] Univ Florida, Dept Wildlife Ecol & Conservat, Gainesville, FL USA. [Larson, Toti E.; Perkins, George B.; Heikoop, Jeffrey M.] Los Alamos Natl Lab, Div Earth & Environm Sci, Los Alamos, NM 87545 USA. [Davis, Paul; Syme, James] EnviroLogic Inc, Durango, CO USA. RP Fair, JM (reprint author), Los Alamos Natl Lab, Environm Stewardship, Los Alamos, NM USA. EM jmfair@lanl.gov RI Heikoop, Jeffrey/C-1163-2011; Loiselle, Bette/O-7106-2016; OI Loiselle, Bette/0000-0003-1434-4173; Larson, Toti/0000-0002-2291-5979; Heikoop, Jeffrey/0000-0001-7648-3385 FU National Science Foundation [IBN 0235141, IOB 0508189, OISE 0513341]; International Center for Tropical Ecology at the University of Missouri, St Louis; Association of Field Ornithologist's Alexander Bergstrom Award; National Geographic Society [7113-01] FX Thanks to R. Duraes, W. P. Tori, J. R. Hidalgo, and F. Narvaez who helped collect the data. We give special thanks to David and Consuelo Romo, Kelly Swing, Jaime Guerra, and all the TBS staff for their logistical and field support. IACUC protocol number 5-12-20. This research was conducted in accordance with permit number 13-IC-FAU-DFN, Distrito Forestal Napo, Tena, Ecuador. We are grateful to Terry Erwin of the Smithsonian National Museum of Natural History for collecting and donating the arthropod samples from TBS. We thank the Ministerio de Ambiente for allowing us to conduct our research at the TBS. Funding was provided by the National Science Foundation (IBN 0235141, IOB 0508189, OISE 0513341), the International Center for Tropical Ecology at the University of Missouri, St Louis, the Association of Field Ornithologist's Alexander Bergstrom Award, and the National Geographic Society (7113-01). We also thank L. Marsh and H. Hinojosa for comments on an earlier draft. NR 70 TC 3 Z9 3 U1 6 U2 36 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 1025-6016 EI 1477-2639 J9 ISOT ENVIRON HEALT S JI Isot. Environ. Health Stud. PD AUG 20 PY 2013 VL 49 IS 3 BP 420 EP 435 DI 10.1080/10256016.2013.784702 PG 16 WC Chemistry, Inorganic & Nuclear; Environmental Sciences SC Chemistry; Environmental Sciences & Ecology GA 266HV UT WOS:000328015600014 PM 23781884 ER PT J AU Alexander, DM Stern, D Del Moro, A Lansbury, GB Assef, RJ Aird, J Ajello, M Ballantyne, DR Bauer, FE Boggs, SE Brandt, WN Christensen, FE Civano, F Comastri, A Craig, WW Elvis, M Grefenstette, BW Hailey, CJ Harrison, FA Hickox, RC Luo, B Madsen, KK Mullaney, JR Perri, M Puccetti, S Saez, C Treister, E Urry, CM Zhang, WW Bridge, CR Eisenhardt, PRM Gonzalez, AH Miller, SH Tsai, CW AF Alexander, D. M. Stern, D. Del Moro, A. Lansbury, G. B. Assef, R. J. Aird, J. Ajello, M. Ballantyne, D. R. Bauer, F. E. Boggs, S. E. Brandt, W. N. Christensen, F. E. Civano, F. Comastri, A. Craig, W. W. Elvis, M. Grefenstette, B. W. Hailey, C. J. Harrison, F. A. Hickox, R. C. Luo, B. Madsen, K. K. Mullaney, J. R. Perri, M. Puccetti, S. Saez, C. Treister, E. Urry, C. M. Zhang, W. W. Bridge, C. R. Eisenhardt, P. R. M. Gonzalez, A. H. Miller, S. H. Tsai, C. W. TI THE NuSTAR EXTRAGALACTIC SURVEY: A FIRST SENSITIVE LOOK AT THE HIGH-ENERGY COSMIC X-RAY BACKGROUND POPULATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: high-redshift; infrared: galaxies; X-rays: diffuse background; X-rays: general ID ACTIVE GALACTIC NUCLEI; DEEP FIELD-SOUTH; BL-LACERTAE OBJECTS; MS SOURCE CATALOGS; ALL-SKY SURVEY; RESOLUTION SPECTRAL TEMPLATES; HOST-GALAXY PROPERTIES; STAR-FORMING GALAXIES; POINT-SOURCE CATALOGS; HEAVILY OBSCURED AGN AB We report on the first 10 identifications of sources serendipitously detected by the Nuclear Spectroscopic Telescope Array (NuSTAR) to provide the first sensitive census of the cosmic X-ray background source population at greater than or similar to 10 keV. We find that these NuSTAR-detected sources are approximate to 100 times fainter than those previously detected at greater than or similar to 10 keV and have a broad range in redshift and luminosity (z = 0.020-2.923 and L10-40 keV approximate to 4 x 10(41)-5 x 10(45) erg s(-1)); the median redshift and luminosity are z approximate to 0.7 and L10-40 keV approximate to 3 x 10(44) erg s(-1), respectively. We characterize these sources on the basis of broad-band approximate to 0.5-32 keV spectroscopy, optical spectroscopy, and broad-band ultraviolet-to-mid-infrared spectral energy distribution analyses. We find that the dominant source population is quasars with L10-40 keV > 10(44) erg s(-1), of which approximate to 50% are obscured with N-H greater than or similar to 10(22) cm(-2). However, none of the 10 NuSTAR sources are Compton thick (N-H greater than or similar to 10(24) cm(-2)) and we place a 90% confidence upper limit on the fraction of Compton-thick quasars (L10-40 keV > 10(44) erg s(-1)) selected at greater than or similar to 10 keV of less than or similar to 33% over the redshift range z = 0.5-1.1. We jointly fitted the rest-frame approximate to 10-40 keV data for all of the non-beamed sources with L10-40 keV > 10(43) erg s(-1) to constrain the average strength of reflection; we find R < 1.4 for Gamma = 1.8, broadly consistent with that found for local active galactic nuclei (AGNs) observed at greater than or similar to 10 keV. We also constrain the host-galaxy masses and find a median stellar mass of approximate to 10(11) M-circle dot, a factor approximate to 5 times higher than the median stellar mass of nearby high-energy selected AGNs, which may be at least partially driven by the order of magnitude higher X-ray luminosities of the NuSTAR sources. Within the low source-statistic limitations of our study, our results suggest that the overall properties of the NuSTAR sources are broadly similar to those of nearby high-energy selected AGNs but scaled up in luminosity and mass. C1 [Alexander, D. M.; Del Moro, A.; Lansbury, G. B.; Aird, J.; Mullaney, J. R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Stern, D.; Assef, R. J.; Eisenhardt, P. R. M.; Tsai, C. W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Ajello, M.; Boggs, S. E.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Ballantyne, D. R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, F. E.; Saez, C.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Brandt, W. N.; Luo, B.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Christensen, F. E.; Craig, W. W.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Civano, F.; Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Comastri, A.] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Grefenstette, B. W.; Harrison, F. A.; Madsen, K. K.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Hailey, C. J.] Columbia Astrophys Lab, Columbia, NY 10027 USA. [Perri, M.; Puccetti, S.] ASI Sci Data Ctr, I-00044 Frascati, Italy. [Perri, M.; Puccetti, S.] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Urry, C. M.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Bridge, C. R.; Miller, S. H.] CALTECH, Pasadena, CA 91125 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. RP Alexander, DM (reprint author), Univ Durham, Dept Phys, Durham DH1 3LE, England. RI Urry, Claudia/G-7381-2011; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Alexander, David/0000-0002-5896-6313; Puccetti, Simonetta/0000-0002-2734-7835; Urry, Claudia/0000-0002-0745-9792; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Perri, Matteo/0000-0003-3613-4409 FU Leverhulme Trust; Science and Technology Facilities Council (STFC); SAO grant [GO2-13164X]; NASA Postdoctoral Program at the Jet Propulsion Laboratory; NSF award [AST 1008067]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06/2007]; Anillo project [ACT1101]; FONDECYT [1101024, 1120061]; Caltech NuSTAR [44A-1092750]; NASA ADP grant [NNX10AC99G]; ASI/INAF grant [I/037/12/0]; CONICYT-Chile under grant FONDECYT [3120198]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We acknowledge financial support from the Leverhulme Trust (D.M.A. and J.R.M.), the Science and Technology Facilities Council (STFC; D.M.A., A.D.M., and G.B.L.), the SAO grant GO2-13164X (M.A.), NASA Postdoctoral Program at the Jet Propulsion Laboratory (R.J.A.), NSF award AST 1008067 (D.R.B.), Center of Excellence in Astrophysics and Associated Technologies (PFB 06/2007; F.E.B. and E.T.), the Anillo project ACT1101 (F.E.B. and E.T.), FONDECYT Regular 1101024 (F.E.B.), Caltech NuSTAR subcontract 44A-1092750 (W.N.B. and B.L.), NASA ADP grant NNX10AC99G (W.N.B. and B.L.), ASI/INAF grant I/037/12/0 (A.C. and S.P.), CONICYT-Chile under grant FONDECYT 3120198 (C.S.), and FONDECYT regular grant 1120061 (E.T.). We thank the referee for a constructive and positive report. We also thank Michael Koss for the discussion of Swift-BAT results, and Mark Brodwin, Daniel Gettings, John Gizis, Richard Walters, Jingwen Wu, and Dominika Wylezalek for supporting the ground-based follow-up observations. This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of the NuSTAR Data Analysis Software (NuSTAR-DAS) jointly developed by the ASI Science Data Center (ASDC, Italy) and the California Institute of Technology (USA). NR 136 TC 35 Z9 35 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 125 DI 10.1088/0004-637X/773/2/125 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100044 ER PT J AU Asgari-Targhi, M van Ballegooijen, AA Cranmer, SR DeLuca, EE AF Asgari-Targhi, M. van Ballegooijen, A. A. Cranmer, S. R. DeLuca, E. E. TI THE SPATIAL AND TEMPORAL DEPENDENCE OF CORONAL HEATING BY ALFVEN WAVE TURBULENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); Sun: corona; turbulence; waves ID MAGNETIC-FIELD; SOLAR-WIND; MAGNETOHYDRODYNAMIC TURBULENCE; TRANSITION REGION; MODEL; LOOPS; DYNAMICS; NANOFLARES; MOTIONS; CHROMOSPHERE AB The solar atmosphere may be heated by Alfven waves that propagate up from the convection zone and dissipate their energy in the chromosphere and corona. To further test this theory, we consider wave heating in an active region observed on 2012 March 7. A potential field model of the region is constructed, and 22 field lines representing observed coronal loops are traced through the model. Using a three-dimensional (3D) reduced magnetohydrodynamics code, we simulate the dynamics of Alfven waves in and near the observed loops. The results for different loops are combined into a single formula describing the average heating rate Q as a function of position within the observed active region. We suggest this expression may be approximately valid also for other active regions, and therefore may be used to construct 3D, time-dependent models of the coronal plasma. Such models are needed to understand the role of thermal non-equilibrium in the structuring and dynamics of the Sun's corona. C1 [Asgari-Targhi, M.; van Ballegooijen, A. A.; Cranmer, S. R.; DeLuca, E. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Asgari-Targhi, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 15, Cambridge, MA 02138 USA. RI DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; van Ballegooijen, Adriaan/0000-0002-5622-3540 FU NASA [NNM07AB07C]; LMSAL [SP02H1701R] FX This project is supported under contract NNM07AB07C from NASA to the Smithsonian Astrophysical Observatory (SAO) and SP02H1701R from LMSAL to SAO. NR 54 TC 32 Z9 32 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 111 DI 10.1088/0004-637X/773/2/111 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100030 ER PT J AU Baskin, NJ Knutson, HA Burrows, A Fortney, JJ Lewis, NK Agol, E Charbonneau, D Cowan, NB Deming, D Desert, JM Langton, J Laughlin, G Showman, AP AF Baskin, Nathaniel J. Knutson, Heather A. Burrows, Adam Fortney, Jonathan J. Lewis, Nikole K. Agol, Eric Charbonneau, David Cowan, Nicolas B. Deming, Drake Desert, Jean-Michel Langton, Jonathan Laughlin, Gregory Showman, Adam P. TI SECONDARY ECLIPSE PHOTOMETRY OF THE EXOPLANET WASP-5b WITH WARM SPITZER SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric ID TRANSIT TIMING VARIATIONS; PLANET HD 189733B; HOT JUPITERS; EXTRASOLAR PLANET; ATMOSPHERIC CIRCULATION; THERMAL EMISSION; PHASE VARIATIONS; STARS; MODEL; ECCENTRICITIES AB We present secondary eclipse photometry of the extrasolar planet WASP-5b taken in the 3.6 and 4.5 mu m bands with the Spitzer Space Telescope's Infrared Array Camera as part of the extended warm mission. By estimating the depth of the secondary eclipse in these two bands we can place constraints on the planet's atmospheric pressure-temperature profile and chemistry. We measure secondary eclipse depths of 0.197% +/- 0.028% and 0.237% +/- 0.024% in the 3.6 mu m and 4.5 mu m bands, respectively. For the case of a solar-composition atmosphere and chemistry in local thermal equilibrium, our observations are best matched by models showing a hot dayside and, depending on our choice of model, a weak thermal inversion or no inversion at all. We measure a mean offset from the predicted center of eclipse of 3.7 +/- 1.8 minutes, corresponding to e cos omega = 0.0025 +/- 0.0012 and consistent with a circular orbit. We conclude that the planet's orbit is unlikely to have been perturbed by interactions with another body in the system as claimed by Fukui et al. C1 [Baskin, Nathaniel J.; Knutson, Heather A.; Desert, Jean-Michel] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 05844 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lewis, Nikole K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cowan, Nicolas B.] Northwestern Univ, Ctr Interdisciplinary Explorat & Res Astrophys, Evanston, IL 60208 USA. [Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Baskin, NJ (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. OI Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145 NR 36 TC 9 Z9 9 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 124 DI 10.1088/0004-637X/773/2/124 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100043 ER PT J AU Cucchiara, A Prochaska, JX Zhu, G Menard, B Fynbo, JPU Fox, DB Chen, HW Cooksey, KL Cenko, SB Perley, D Bloom, JS Berger, E Tanvir, NR D'Elia, V Lopez, S Chornock, R de Jaeger, T AF Cucchiara, A. Prochaska, J. X. Zhu, G. Menard, B. Fynbo, J. P. U. Fox, D. B. Chen, H. -W. Cooksey, K. L. Cenko, S. B. Perley, D. Bloom, J. S. Berger, E. Tanvir, N. R. D'Elia, V. Lopez, S. Chornock, R. de Jaeger, T. TI AN INDEPENDENT MEASUREMENT OF THE INCIDENCE OF Mg II ABSORBERS ALONG GAMMA-RAY BURST SIGHT LINES: THE END OF THE MYSTERY? SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma-ray burst: general; quasars: absorption lines; techniques: spectroscopic ID DIGITAL-SKY-SURVEY; SURVEY QSO-SPECTRA; OPTICAL SPECTROSCOPY; REDSHIFT GALAXIES; ABSORPTION-LINES; HOST GALAXY; SWIFT-ERA; REAL-TIME; FOLLOW-UP; OF-SIGHT AB In 2006, Prochter et al. reported a statistically significant enhancement of very strong Mg II absorption systems intervening the sight lines to gamma-ray bursts (GRBs) relative to the incidence of such absorption along quasar sight lines. This counterintuitive result has inspired a diverse set of astrophysical explanations (e.g., dust, gravitational lensing) but none of these has obviously resolved the puzzle. Using the largest set of GRB afterglow spectra available, we reexamine the purported enhancement. In an independent sample of GRB spectra with a survey path three times larger than Prochter et al., we measure the incidence per unit redshift of >= 1 angstrom rest-frame equivalent width Mg II absorbers at z approximate to 1 to be l(z) = 0.18 +/- 0.06. This is fully consistent with current estimates for the incidence of such absorbers along quasar sight lines. Therefore, we do not confirm the original enhancement and suggest those results suffered from a statistical fluke. Signatures of the original result do remain in our full sample (l(z) shows an approximate to 1.5 enhancement over l(z)(QSO)), but the statistical significance now lies at approximate to 90% c.l. Restricting our analysis to the subset of high-resolution spectra of GRB afterglows (which overlaps substantially with Prochter et al.), we still reproduce a statistically significant enhancement of Mg II absorption. The reason for this excess, if real, is still unclear since there is no connection between the rapid afterglow follow-up process with echelle (or echellette) spectrographs and the detectability of strong Mg II doublets. Only a larger sample of such high-resolution data will shed some light on this matter. C1 [Cucchiara, A.; Prochaska, J. X.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Zhu, G.; Menard, B.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Menard, B.] Univ Tokyo, Kavli Inst Phys & Math Universe, Kashiwa, Chiba 2778583, Japan. [Fynbo, J. P. U.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [Fox, D. B.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Chen, H. -W.] Univ Chicago, Dept Astron & Astrophys, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Cooksey, K. L.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Cenko, S. B.; Bloom, J. S.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Perley, D.] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Berger, E.; Chornock, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [D'Elia, V.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Italy. [Lopez, S.; de Jaeger, T.] Univ Chile, Dept Astron, Santiago, Chile. RP Cucchiara, A (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, 1156 High St, Santa Cruz, CA 95064 USA. EM acucchia@ucolick.org RI Fynbo, Johan/L-8496-2014; Lopez, Sebastian /I-5657-2016; OI Fynbo, Johan/0000-0002-8149-8298; Lopez, Sebastian /0000-0003-0389-0902; D'Elia, Valerio/0000-0002-7320-5862; Zhu, Guangtun/0000-0002-7574-8078; Chen, Hsiao-Wen/0000-0001-8813-4182 FU FONDECYT [1100214]; Center of Excellence in Astrophysics and Associated Technologies [PFB 06]; ERC-StG [EGGS-278202]; DNRF FX A.C. thanks the anonymous referee for the valuable comments and suggestions. A.C. also thanks J.X. Prochaska for the fundamental guidances, without which this work could not be possible. A.C. also thanks B. Menard and B. Zhu for the useful comments and to have provided the best to date compilation of high signal-to-noise quasars spectra as well their Mg II search results. Gemini results are based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). S.L. has been supported by FONDECYT grant number 1100214 and received partial support from the Center of Excellence in Astrophysics and Associated Technologies (PFB 06). J.P.U.F. acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. NR 87 TC 7 Z9 7 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 82 DI 10.1088/0004-637X/773/2/82 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100001 ER PT J AU Dahle, H Gladders, MD Sharon, K Bayliss, MB Wuyts, E Abramson, LE Koester, BP Groeneboom, N Brinckmann, TE Kristensen, MT Lindholmer, MO Nielsen, A Krogager, JK Fynbo, JPU AF Dahle, H. Gladders, M. D. Sharon, K. Bayliss, M. B. Wuyts, E. Abramson, L. E. Koester, B. P. Groeneboom, N. Brinckmann, T. E. Kristensen, M. T. Lindholmer, M. O. Nielsen, A. Krogager, J. -K. Fynbo, J. P. U. TI SDSS J2222+2745: A GRAVITATIONALLY LENSED SEXTUPLE QUASAR WITH A MAXIMUM IMAGE SEPARATION OF 15.'' 1 DISCOVERED IN THE SLOAN GIANT ARCS SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; gravitational lensing: strong; quasars: individual (SDSS J2222+2745) ID DIGITAL-SKY-SURVEY; GALAXY CLUSTERS; MASS-DISTRIBUTION; TIME-DELAY; 5TH IMAGE; J1004+4112; STATISTICS; J1029+2623; SPECTRA AB We report the discovery of a unique gravitational lens system, SDSS J2222+2745, producing five spectroscopically confirmed images of a z(s) = 2.82 quasar lensed by a foreground galaxy cluster at z(l) = 0.49. We also present photometric and spectroscopic evidence for a sixth lensed image of the same quasar. The maximum separation between the quasar images is 15.'' 1. Both the large image separations and the high image multiplicity are in themselves rare among known lensed quasars, and observing the combination of these two factors is an exceptionally unlikely occurrence in present data sets. This is only the third known case of a quasar lensed by a cluster, and the only one with six images. The lens system was discovered in the course of the Sloan Giant Arcs Survey, in which we identify candidate lenses in the Sloan Digital Sky Survey and target these for follow-up and verification with the 2.56 m Nordic Optical Telescope. Multi-band photometry obtained over multiple epochs from 2011 September to 2012 September reveals significant variability at the similar to 10%-30% level in some of the quasar images, indicating that measurements of the relative time delay between quasar images will be feasible. In this lens system, we also identify a bright (g = 21.5) giant arc corresponding to a strongly lensed background galaxy at z(s) = 2.30. We fit parametric models of the lens system, constrained by the redshift and positions of the quasar images and the redshift and position of the giant arc. The predicted time delays between different pairs of quasar images range from similar to 100 days to similar to 6 yr. C1 [Dahle, H.; Groeneboom, N.] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Dahle, H.] Univ Oslo, Ctr Math Applicat, NO-0315 Oslo, Norway. [Gladders, M. D.; Abramson, L. E.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, M. D.; Abramson, L. E.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, K.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bayliss, M. B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, M. B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Wuyts, E.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Koester, B. P.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Brinckmann, T. E.; Kristensen, M. T.; Lindholmer, M. O.; Nielsen, A.; Krogager, J. -K.; Fynbo, J. P. U.] Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen O, Denmark. RP Dahle, H (reprint author), Univ Oslo, Inst Theoret Astrophys, POB 1029, NO-0315 Oslo, Norway. EM hdahle@astro.uio.no RI Fynbo, Johan/L-8496-2014; Krogager, Jens-Kristian/E-4384-2015 OI Fynbo, Johan/0000-0002-8149-8298; Krogager, Jens-Kristian/0000-0002-4912-9388 FU Research Council of Norway; Research Corporation through a Cottrell Scholars award; University of Michigan's President's Postdoctoral Fellowship; ERC-StG [EGGS-278202]; DNRF FX H.D. acknowledges support from the Research Council of Norway. M.D.G. thanks the Research Corporation for support of this work through a Cottrell Scholars award. K.S. acknowledges support from the University of Michigan's President's Postdoctoral Fellowship. J.P.U.F. acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. We thank the NOT staff, in particular our support astronomer Stefan Geier, for excellent support, including accommodating a last-minute instrument change which allowed the spectroscopic confirmation of the D image and discovery of the E image of the quasar. NR 35 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 146 DI 10.1088/0004-637X/773/2/146 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100065 ER PT J AU Grier, CJ Martini, P Watson, LC Peterson, BM Bentz, MC Dasyra, KM Dietrich, M Ferrarese, L Pogge, RW Zu, Y AF Grier, C. J. Martini, P. Watson, L. C. Peterson, B. M. Bentz, M. C. Dasyra, K. M. Dietrich, M. Ferrarese, L. Pogge, R. W. Zu, Y. TI STELLAR VELOCITY DISPERSION MEASUREMENTS IN HIGH-LUMINOSITY QUASAR HOSTS AND IMPLICATIONS FOR THE AGN BLACK HOLE MASS SCALE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: kinematics and dynamics; galaxies: nuclei; quasars: individual (PG1411+442, PG1617+175, Mrk 509, PG 2130+099) ID ACTIVE GALACTIC NUCLEI; M-BH-SIGMA; BROAD-LINE REGION; ULTRALUMINOUS INFRARED GALAXIES; SEYFERT 1 GALAXIES; MONITORING PROJECT; DELAY MAPS; ARP 151; EVOLUTION; GROWTH AB We present new stellar velocity dispersion measurements for four luminous quasars with the Near-Infrared Integral Field Spectrometer instrument and the ALTAIR laser guide star adaptive optics system on the Gemini North 8 m telescope. Stellar velocity dispersion measurements and measurements of the supermassive black hole (BH) masses in luminous quasars are necessary to investigate the coevolution of BHs and galaxies, trace the details of accretion, and probe the nature of feedback. We find that higher-luminosity quasars with higher-mass BHs are not offset with respect to the M-BH-sigma* relation exhibited by lower-luminosity active galactic nuclei (AGNs) with lower-mass BHs, nor do we see correlations with galaxy morphology. As part of this analysis, we have recalculated the virial products for the entire sample of reverberation-mapped AGNs and used these data to redetermine the mean virial factor < f > that places the reverberation data on the quiescent M-BH-sigma* relation. With our updated measurements and new additions to the AGN sample, we obtain < f > = 4.31 +/- 1.05, which is slightly lower than, but consistent with, most previous determinations. C1 [Grier, C. J.; Martini, P.; Peterson, B. M.; Pogge, R. W.; Zu, Y.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Martini, P.; Peterson, B. M.; Pogge, R. W.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [Watson, L. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bentz, M. C.] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Dasyra, K. M.] Observ Paris, LERMA, CNRS, UMR8112, F-75014 Paris, France. [Dietrich, M.] Ohio Univ, Dept Phys & Astron, Athens, OH 45601 USA. [Ferrarese, L.] Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. RP Grier, CJ (reprint author), Ohio State Univ, Dept Astron, 140 W 18th Ave, Columbus, OH 43210 USA. OI Dasyra, Kalliopi/0000-0002-1482-2203; Zu, Ying/0000-0001-6966-6925 FU National Science Foundation [AST-1008882]; Presidential Fellowship at The Ohio State University; North American ALMA Science Center (NAASC) at NRAO; National Aeronautics and Space Administration FX The authors would like to thank Jenny Greene and Alister Graham for their helpful suggestions that improved this work. We also thank Luis Ho for pointing out a scaling error in the reported lags prior to publication. C.J.G. would like to thank Gisella De Rosa for help with some of the code used in this analysis. B.M.P., R.W.P., and C.J.G. gratefully acknowledge the support of the National Science Foundation through grant AST-1008882 to The Ohio State University. C.J.G. is also supported by a Presidential Fellowship at The Ohio State University. P.M. is grateful for support from the sabbatical visitor program at the North American ALMA Science Center (NAASC) at NRAO and the hospitality of both the NAASC and the University of Virginia while this work was completed. 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 work is based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). NR 73 TC 56 Z9 56 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 90 DI 10.1088/0004-637X/773/2/90 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100009 ER PT J AU Guarcello, MG Drake, JJ Wright, NJ Drew, JE Gutermuth, RA Hora, JL Naylor, T Aldcroft, T Fruscione, A Garcia-Alvarez, D Kashyap, VL King, R AF Guarcello, M. G. Drake, J. J. Wright, N. J. Drew, J. E. Gutermuth, R. A. Hora, J. L. Naylor, T. Aldcroft, T. Fruscione, A. Garcia-Alvarez, D. Kashyap, V. L. King, R. TI THE PROTOPLANETARY DISKS IN THE NEARBY MASSIVE STAR-FORMING REGION CYGNUS OB2 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: stars; open clusters and associations: individual (Cygnus OB2); protoplanetary disks; stars: formation; stars: pre-main sequence ID YOUNG STELLAR OBJECTS; ORION NEBULA CLUSTER; DIGITAL-SKY-SURVEY; WIDE-FIELD CAMERA; T-TAURI STARS; X REGION; DATA RELEASE; SPECTRAL CLASSIFICATION; SPATIAL-DISTRIBUTION; SPITZER OBSERVATIONS AB The formation of stars in massive clusters is one of the main modes of the star formation process. However, the study of massive star-forming regions is hampered by their typically large distances to the Sun. One exception to this is the massive star-forming region Cygnus OB2 in the Cygnus X region, at the distance of similar to 1400 pc. Cygnus OB2 hosts very rich populations of massive and low-mass stars, being the best target in our Galaxy to study the formation of stars, circumstellar disks, and planets in the presence of massive stars. In this paper, we combine a wide and deep set of photometric data, from the r band to 24 mu m, in order to select the disk-bearing population of stars in Cygnus OB2 and identify the class I, class II, and stars with transition and pre-transition disks. We selected 1843 sources with infrared excesses in an area of 1 degrees x 1 degrees centered on Cyg OB2 in several evolutionary stages: 8.4% class I, 13.1% flat-spectrum sources, 72.9% class II, 2.3% pre-transition disks, and 3.3% transition disks. The spatial distribution of these sources shows a central cluster surrounded by an annular overdensity and some clumps of recent star formation in the outer region. Several candidate subclusters are identified, both along the overdensity and in the rest of the association. C1 [Guarcello, M. G.; Drake, J. J.; Wright, N. J.; Hora, J. L.; Aldcroft, T.; Fruscione, A.; Kashyap, V. L.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Wright, N. J.; Drew, J. E.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Gutermuth, R. A.] Smith Coll, Coll Astron Dept 5, Northampton, MA 01063 USA. [Gutermuth, R. A.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Naylor, T.; King, R.] Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. [Garcia-Alvarez, D.] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain. [Garcia-Alvarez, D.] Grantecan CALP, E-38712 Brena Baja, La Palma, Spain. [Garcia-Alvarez, D.] Inst Astrofis Canarias, E-38205 Tenerife, Spain. RP Guarcello, MG (reprint author), Smithsonian Astrophys Observ, MS-67,60 Garden St, Cambridge, MA 02138 USA. RI Naylor, Tim /A-9465-2015; OI Drew, Janet/0000-0003-1192-7082 FU National Aeronautics and Space Administration; National Science Foundation; NASA [NAS8-39073]; Chandra grant [GO0-11040X]; Spanish MICINN [AYA2008-02038]; NASA Astrophysics Data Analysis Program (ADAP) [NNX11AD14G, NNX13AF08G]; Caltech/JPL [1373081, 1424329, 1440160] FX We thank the anonymous referee for the useful comments. The authors are indebted with Raffaele D'Abrusco and Ignazio Pillitteri for their precious help. This article makes use of data obtained with observations made with the Gran Telescopio CANARIAS (GTC), installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de CANARIAS, in the island of La Palma; data obtained as part of the INT Photometric H alpha Survey (IPHAS) of the northern Galactic plane carried out at the Isaac Newton Telescope (INT; all IPHAS data are processed by the Cambridge Astronomical Survey Unit, at the Institute of Astronomy in Cambridge); SDSS data, founded 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; 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; data 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. The paper is also based on data obtained as part of the UKIRT Infrared Deep Sky Survey (UKIDSS; Lawrence et al. 2007; we are grateful to Charles Williams for his support of the Apple Mac X-grid cluster in Exeter, on which the UKIRT data were reduced). UKIDSS uses the UKIRT Wide Field Camera (WFCAM; Casali et al. 2007). The photometric system is described in Hewett et al. (2006), and the calibration is described in Hodgkin et al. (2009). The pipeline processing and science archive are described in M. J. Irwin et al. (in preparation) and Hambly et al. (2008). M.G.G. is supported by the Chandra grant GO0-11040X. J.J.D., V.L.K., and T.A. are supported by NASA contract NAS8-39073 to the Chandra X-ray Center (CXC) and thank the Director, Harvey Tananbaum, and the CXC science staff for advice and support. D.G.A. acknowledges support from the Spanish MICINN through grant AYA2008-02038. R.A.G. would like to acknowledge the support of NASA Astrophysics Data Analysis Program (ADAP) grants NNX11AD14G and NNX13AF08G, and Caltech/JPL awards 1373081, 1424329, and 1440160 in support of Spitzer Space Telescope observing programs. NR 103 TC 7 Z9 7 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 135 DI 10.1088/0004-637X/773/2/135 PG 24 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100054 ER PT J AU Isenberg, PA Maruca, BA Kasper, JC AF Isenberg, Philip A. Maruca, Bennett A. Kasper, Justin C. TI SELF-CONSISTENT ION CYCLOTRON ANISOTROPY-BETA RELATION FOR SOLAR WIND PROTONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE plasmas; solar wind; waves ID PITCH-ANGLE DIFFUSION; TEMPERATURE ANISOTROPY; MAGNETIC-FIELD; CORONAL HOLE; MINOR IONS; 1 AU; WAVES; TURBULENCE; FLUCTUATIONS; INSTABILITY AB We derive a set of self-consistent marginally stable states for a system of ion-cyclotron waves propagating parallel to the large-scale magnetic field through a homogeneous proton-electron plasma. The proton distributions and the wave dispersions are related through the condition that no further ion-cyclotron resonant particle scattering or wave growth/damping may take place. The thermal anisotropy of the protons in these states therefore defines the threshold value for triggering the proton-cyclotron anisotropy instability. A number of recent papers have noted that the anisotropy of solar wind protons at 1 AU does not seem to be limited by the proton-cyclotron anisotropy threshold, even at low plasma beta. However, this puzzle seems to be due solely to the estimation of this anisotropy threshold under the assumption that the protons have a bi-Maxwellian distribution. We note that bi-Maxwellian distributions are never marginally stable to the resonant cyclotron interaction, so these estimates do not represent physically valid thresholds. The threshold anisotropies obtained from our marginally stable states are much larger, as a function of proton parallel beta, than the bi-Maxwellian estimates, and we show that the measured data remains below these more rigorous thresholds. Thus, the results of this paper resolve the apparent contradiction presented by the solar wind anisotropy observations at 1 AU: the bi-Maxwellian anisotropies are not rigorous thresholds, and so do not limit the proton distributions in the solar wind. C1 [Isenberg, Philip A.] Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. [Maruca, Bennett A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kasper, Justin C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Isenberg, PA (reprint author), Univ New Hampshire, Inst Study Earth Oceans & Space, Durham, NH 03824 USA. EM phil.isenberg@unh.edu; bmaruca@ssl.berkeley.edu; jkasper@cfa.harvard.edu FU NSF [ATM0719738, AGS 0962506]; NASA [NNX08AW07G, NNX11AJ37G]; DoE [DEFG0207ER46372] FX This work was supported in part by NSF grants ATM0719738 and AGS 0962506, NASA grants NNX08AW07G and NNX11AJ37G, and DoE grant DEFG0207ER46372. NR 44 TC 12 Z9 12 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 164 DI 10.1088/0004-637X/773/2/164 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100083 ER PT J AU Jorstad, SG Marscher, AP Smith, PS Larionov, VM Agudo, I Gurwell, M Wehrle, AE Lahteenmaki, A Nikolashvili, MG Schmidt, GD Arkharov, AA Blinov, DA Blumenthal, K Casadio, C Chigladze, RA Efimova, NV Eggen, JR Gomez, JL Grupe, D Hagen-Thorn, VA Joshi, M Kimeridze, GN Konstantinova, TS Kopatskaya, EN Kurtanidze, OM Kurtanidze, SO Larionova, EG Larionova, LV Sigua, LA MacDonald, NR Maune, JD McHardy, IM Miller, HR Molina, SN Morozova, DA Scott, T Taylor, BW Tornikoski, M Troitsky, IS Thum, C Walker, G Williamson, KE Sallum, S Consiglio, S Strelnitski, V AF Jorstad, Svetlana G. Marscher, Alan P. Smith, Paul S. Larionov, Valeri M. Agudo, Ivan Gurwell, Mark Wehrle, Ann E. Lahteenmaki, Anne Nikolashvili, Maria G. Schmidt, Gary D. Arkharov, Arkady A. Blinov, Dmitry A. Blumenthal, Kelly Casadio, Carolina Chigladze, Revaz A. Efimova, Natalia V. Eggen, Joseph R. Gomez, Jose L. Grupe, Dirk Hagen-Thorn, Vladimir A. Joshi, Manasvita Kimeridze, Givi N. Konstantinova, Tatiana S. Kopatskaya, Evgenia N. Kurtanidze, Omar M. Kurtanidze, Sofia O. Larionova, Elena G. Larionova, Liudmilla V. Sigua, Lorand A. MacDonald, Nicholas R. Maune, Jeremy D. McHardy, Ian M. Miller, H. Richard Molina, Sol N. Morozova, Daria A. Scott, Terri Taylor, Brian W. Tornikoski, Merja Troitsky, Ivan S. Thum, Clemens Walker, Gary Williamson, Karen E. Sallum, Stephanie Consiglio, Santina Strelnitski, Vladimir TI A TIGHT CONNECTION BETWEEN GAMMA-RAY OUTBURSTS AND PARSEC-SCALE JET ACTIVITY IN THE QUASAR 3C 454.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (3C 454.3); techniques: interferometric; techniques: photometric; techniques: polarimetric ID SPACE-TELESCOPE OBSERVATIONS; BASE-LINE ARRAY; GALACTIC NUCLEI; RELATIVISTIC JETS; RADIO-SOURCES; BL-LACERTAE; POLARIMETRIC OBSERVATIONS; BRIGHT BLAZARS; 2009 DECEMBER; MULTIWAVELENGTH OBSERVATIONS AB We analyze the multi-frequency behavior of the quasar 3C 454.3 during three prominent gamma-ray outbursts: 2009 Autumn, 2010 Spring, and 2010 Autumn. The data reveal a repeating pattern, including a triple flare structure, in the properties of each gamma-ray outburst, which implies similar mechanism(s) and location for all three events. The multi-frequency behavior indicates that the lower frequency events are co-spatial with the gamma-ray outbursts, although the gamma-ray emission varies on the shortest timescales. We determine that the variability from UV to IR wavelengths during an outburst results from a single synchrotron component whose properties do not change significantly over the different outbursts. Despite a general increase in the degree of optical linear polarization during an outburst, the polarization drops significantly at the peak of the gamma-ray event, which suggests that both shocks and turbulent processes are involved. We detect two disturbances (knots) with superluminal apparent speeds in the parsec-scale jet associated with the outbursts in 2009 Autumn and 2010 Autumn. The kinematic properties of the knots can explain the difference in amplitudes of the gamma-ray events, while their millimeter-wave polarization is related to the optical polarization during the outbursts. We interpret the multi-frequency behavior within models involving either a system of standing conical shocks or magnetic reconnection events located in the parsec-scale millimeter-wave core of the jet. We argue that gamma-ray outbursts with variability timescales as short as similar to 3 hr can occur on parsec scales if flares take place in localized regions such as turbulent cells. C1 [Jorstad, Svetlana G.; Marscher, Alan P.; Agudo, Ivan; Blumenthal, Kelly; Joshi, Manasvita; MacDonald, Nicholas R.; Scott, Terri; Taylor, Brian W.; Williamson, Karen E.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.; Larionov, Valeri M.; Blinov, Dmitry A.; Efimova, Natalia V.; Hagen-Thorn, Vladimir A.; Konstantinova, Tatiana S.; Kopatskaya, Evgenia N.; Larionova, Elena G.; Larionova, Liudmilla V.; Morozova, Daria A.; Troitsky, Ivan S.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Smith, Paul S.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Larionov, Valeri M.; Arkharov, Arkady A.; Efimova, Natalia V.] RAS, Main Pulkovo Astron Observ, St Petersburg 196140, Russia. [Larionov, Valeri M.; Hagen-Thorn, Vladimir A.] Isaac Newton Inst Chile, St Petersburg Branch, St Petersburg, Russia. [Agudo, Ivan; Casadio, Carolina; Gomez, Jose L.; Molina, Sol N.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Gurwell, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wehrle, Ann E.] Space Sci Inst, Boulder, CO 80301 USA. [Lahteenmaki, Anne; Tornikoski, Merja] Aalto Univ Metsahovi Radio Observ, FIN-02540 Kylmala, Finland. [Nikolashvili, Maria G.; Chigladze, Revaz A.; Kimeridze, Givi N.; Kurtanidze, Omar M.; Kurtanidze, Sofia O.; Sigua, Lorand A.] Abastumani Astrophys Observ, Mt Kanobili, Abastumani, Rep of Georgia. [Schmidt, Gary D.] Natl Sci Fdn, Arlington, VA 22230 USA. [Eggen, Joseph R.; Maune, Jeremy D.; Miller, H. Richard] Georgia State Univ, Dept Phys & Astron, Atlanta, GA 30303 USA. [Grupe, Dirk] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [McHardy, Ian M.] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England. [Taylor, Brian W.] Lowell Observ, Flagstaff, AZ 86001 USA. [Thum, Clemens] IRAM, E-18012 Granada, Spain. [Walker, Gary; Sallum, Stephanie; Consiglio, Santina; Strelnitski, Vladimir] Maria Mitchell Observ, Nantucket, MA 02554 USA. [Sallum, Stephanie] MIT, EAPS, Cambridge, MA 02139 USA. [Consiglio, Santina] Calif State Univ Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. RP Jorstad, SG (reprint author), Boston Univ, Inst Astrophys Res, 725 Commonwealth Ave, Boston, MA 02215 USA. EM jorstad@bu.edu RI Blinov, Dmitry/G-9925-2013; Lahteenmaki, Anne/L-5987-2013; Kurtanidze, Omar/J-6237-2014; Molina, Sol Natalia/F-9968-2015; Agudo, Ivan/G-1701-2015; Larionov, Valeri/H-1349-2013; Morozova, Daria/H-1298-2013; Larionova, Elena/H-7287-2013; Troitskiy, Ivan/K-7979-2013; Jorstad, Svetlana/H-6913-2013; Grishina, Tatiana/H-6873-2013; Hagen-Thorn, Vladimir/H-3983-2013; Kopatskaya, Evgenia/H-4720-2013; OI Blinov, Dmitry/0000-0003-0611-5784; Molina, Sol Natalia/0000-0002-4112-2157; Agudo, Ivan/0000-0002-3777-6182; Larionov, Valeri/0000-0002-4640-4356; Morozova, Daria/0000-0002-9407-7804; Larionova, Elena/0000-0002-2471-6500; Troitskiy, Ivan/0000-0002-4218-0148; Jorstad, Svetlana/0000-0001-9522-5453; Grishina, Tatiana/0000-0002-3953-6676; Hagen-Thorn, Vladimir/0000-0002-6431-8590; Kopatskaya, Evgenia/0000-0001-9518-337X; Larionova, Liudmila/0000-0002-0274-1481; Smith, Paul/0000-0002-5083-3663 FU NASA [NNX08AV65G, NNX10AO59G, NNX10AU15G, NNX11AO37G, NNX11AQ03G, NNX10AF88G, NNX08AW56G, NNX09AU93G, Herschel RSA 1427799, NNX11AAO85G, NAS5-00136]; NSF; BU; Lowell Observatory; UK Science and Technology Facilities Council; RFBR [12-02-00452, 12-02-31193]; Spanish Ministry of Economy and Competitiveness and the Regional Government of Andalucia (Spain) [AYA2010-14844, P09-FQM-4784]; Smithsonian Institution; Academia Sinica; Georgian National Science Foundation [GNSF/ST09/4-521]; INSU/CNRS (France); MPG (Germany); IGN (Spain); Academy of Finland FX The research at Boston University (BU) was funded in part by NASA Fermi Guest Investigator grants NNX08AV65G, NNX10AO59G, NNX10AU15G, NNX11AO37G, and NNX11AQ03G and Swift Guest Investigator grant NNX10AF88G. The VLBA is operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The PRISM camera at Lowell Observatory was developed by K. Janes et al. at BU and Lowell Observatory, with funding from the NSF, BU, and Lowell Observatory. The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, with funding from the UK Science and Technology Facilities Council. The effort at Steward Observatory was funded in part by NASA through Fermi Guest Investigator grant NNX08AW56G and NNX09AU93G. The St. Petersburg State University team acknowledges support from RFBR grants 12-02-00452 and 12-02-31193. The research at the IAA-CSIC is supported by the Spanish Ministry of Economy and Competitiveness and the Regional Government of Andalucia (Spain) through grants AYA2010-14844 and P09-FQM-4784, respectively. A. Wehrle acknowledges Guest Investigator support from NASA via Herschel RSA 1427799 and Fermi Guest Investigator grant NNX11AAO85G. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica. The Abastumani team thanks the Georgian National Science Foundation for support through grant GNSF/ST09/4-521. The Swift effort at PSU is supported by NASA contract NAS5-00136. The Calar Alto Observatory is jointly operated by the Max-Planck-Institut fur Astronomie and the Instituto de Astrofisica de Andalucia-CSIC. The IRAM 30 m telescope is supported by INSU/CNRS (France), MPG (Germany), and IGN (Spain). The Metsahovi team acknowledges support from the Academy of Finland. This study is 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/). This paper has made use of up-to-date SMARTS optical/near-infrared light curves that are available at www.astro.yale.edu/smarts/glast/home.php. NR 94 TC 50 Z9 50 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 147 DI 10.1088/0004-637X/773/2/147 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100066 ER PT J AU Naoz, S Kocsis, B Loeb, A Yunes, N AF Naoz, Smadar Kocsis, Bence Loeb, Abraham Yunes, Nicolas TI RESONANT POST-NEWTONIAN ECCENTRICITY EXCITATION IN HIERARCHICAL THREE-BODY SYSTEMS SO ASTROPHYSICAL JOURNAL LA English DT Article DE pulsars: general; stars: evolution; stars: kinematics and dynamics ID SUPERMASSIVE BLACK-HOLES; KOZAI MECHANISM; HOT JUPITERS; GRAVITATIONAL-WAVES; GLOBULAR-CLUSTERS; SECULAR EVOLUTION; ACCRETION DISKS; GALACTIC NUCLEI; TIDAL FRICTION; TRIPLE-SYSTEMS AB We study the secular, hierarchical three-body problem to first-order in a post-Newtonian expansion of general relativity (GR). We expand the first-order post-Newtonian Hamiltonian to leading-order in the ratio of the semi-major axis of the two orbits. In addition to the well-known terms that correspond to the GR precession of the inner and outer orbits, we find a new secular post-Newtonian interaction term that can affect the long-term evolution of the triple. We explore the parameter space for highly inclined and eccentric systems, where the Kozai-Lidov mechanism can produce large-amplitude oscillations in the eccentricities. The standard lore, i.e., that GR effects suppress eccentricity, is only consistent with the parts of phase space where the GR timescales are several orders of magnitude shorter than the secular Newtonian one. In other parts of phase space, however, post-Newtonian corrections combined with the three-body ones can excite eccentricities. In particular, for systems where the GR timescale is comparable to the secular Newtonian timescales, the three-body interactions give rise to a resonant-like eccentricity excitation. Furthermore, for triples with a comparable-mass inner binary, where the eccentric Kozai-Lidov mechanism is suppressed, post-Newtonian corrections can further increase the eccentricity and lead to orbital flips even when the timescale of the former is much longer than the timescale of the secular Kozai-Lidov quadrupole perturbations. C1 [Naoz, Smadar; Kocsis, Bence; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. [Naoz, Smadar] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Yunes, Nicolas] Montana State Univ, Dept Phys, Bozeman, MT 59718 USA. RP Naoz, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM snaoz@cfa.harvard.edu RI Kocsis, Bence/C-3061-2013; OI Kocsis, Bence/0000-0002-4865-7517; Naoz, Smadar/0000-0002-9802-9279 FU NASA [PF2-130096, NNX08AL43G, NNA09DB30A, NNX11AI49G, PF9-00063]; Chandra X-Ray Center; NSF [PHY-1114374, AST-0907890]; National Aeronautics Space Administration [NAS8-03060] FX We thank Alessandra Buonanno, Fred Rasio, and Gongjie Li for useful discussions, and we also thank Cole Miller for carefully reading the first draft of the paper and sending useful comments. We thank our anonymous referee for useful remarks. We thank Yoram Lithwick for the use of his allocation time on the computer cluster Quest. This research was supported in part through the computational resources and staff contributions provided by Information Technology at Northwestern University as part of its shared cluster program, Quest. S.N. acknowledge partial supported by NASA through an Einstein Post-doctoral Fellowship awarded by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract PF2-130096. This work was supported in part by NSF grant PHY-1114374 and AST-0907890, as well as NASA grants NNX08AL43G and NNA09DB30A and NNX11AI49G. B.K. acknowledges support from NASA through Einstein Postdoctoral Fellowship Award No. PF9-00063 issued by the Chandra X-Ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. N.Y. also thanks the Institute for Theory and Computation at the Harvard Smithsonian Center for Astrophysics for their hospitality. NR 78 TC 46 Z9 46 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 187 DI 10.1088/0004-637X/773/2/187 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100106 ER PT J AU Paterno-Mahler, R Blanton, EL Randall, SW Clarke, TE AF Paterno-Mahler, R. Blanton, E. L. Randall, S. W. Clarke, T. E. TI DEEP CHANDRA OBSERVATIONS OF THE EXTENDED GAS SLOSHING SPIRAL IN A2029 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A2029); galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID KELVIN-HELMHOLTZ INSTABILITIES; RELAXED GALAXY CLUSTERS; ACTIVE GALACTIC NUCLEI; COLD FRONTS; COOLING FLOWS; RADIO-SOURCES; XMM-NEWTON; MERGING CLUSTERS; PERSEUS CLUSTER; ABELL CLUSTERS AB Recent X-ray observations of galaxy clusters have shown that there is substructure present in the intracluster medium (ICM), even in clusters that are seemingly relaxed. This substructure is sometimes a result of sloshing of the ICM, which occurs in cool core clusters that have been disturbed by an off-axis merger with a sub-cluster or group. We present deep Chandra observations of the cool core cluster Abell 2029, which has a sloshing spiral extending radially outward from the center of the cluster to approximately 400 kpc at its fullest extent-the largest continuous spiral observed to date. We find a surface brightness excess, a temperature decrement, a density enhancement, an elemental abundance enhancement, and a smooth pressure profile in the area of the spiral. The sloshing gas seems to be interacting with the southern lobe of the central radio galaxy, causing it to bend and giving the radio source a wide-angle tail (WAT) morphology. This shows that WATs can be produced in clusters that are relatively relaxed on large scales. We explore the interaction between heating and cooling in the central region of the cluster. Energy injection from the active galactic nucleus is likely insufficient to offset the cooling, and sloshing may be an important additional mechanism in preventing large amounts of gas from cooling to very low temperatures. C1 [Paterno-Mahler, R.; Blanton, E. L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Paterno-Mahler, R.; Blanton, E. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Randall, S. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Clarke, T. E.] Naval Res Lab, Washington, DC 20375 USA. RP Paterno-Mahler, R (reprint author), Boston Univ, Dept Astron, 725 Commonwealth Ave, Boston, MA 02215 USA. EM rachelpm@bu.edu; eblanton@bu.edu; srandall@head.cfa.harvard.edu; tracy.clarke@nrl.navy.mil RI Blanton, Elizabeth/H-4501-2014; OI Randall, Scott/0000-0002-3984-4337 FU Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University. NR 60 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 114 DI 10.1088/0004-637X/773/2/114 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100033 ER PT J AU Shen, CC Reeves, KK Raymond, JC Murphy, NA Ko, YK Lin, J Mikic, Z Linker, JA AF Shen, Chengcai Reeves, Katharine K. Raymond, John C. Murphy, Nicholas A. Ko, Yuan-Kuen Lin, Jun Mikic, Zoran Linker, Jon A. TI NON-EQUILIBRIUM IONIZATION MODELING OF THE CURRENT SHEET IN A SIMULATED SOLAR ERUPTION SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; magnetic reconnection; Sun: coronal mass ejections (CMEs); Sun: UV radiation ID CORONAL MASS EJECTION; MAGNETIC RECONNECTION; ULTRAVIOLET-SPECTRA; SOHO OBSERVATIONS; CHARGE STATES; PLASMA; FLARES; EVOLUTION; FEATURES; SPECTROMETER AB The current sheet that extends from the top of flare loops and connects to an associated flux rope is a common structure in models of coronal mass ejections (CMEs). To understand the observational properties of CME current sheets, we generated predictions from a flare/CME model to be compared with observations. We use a simulation of a large-scale CME current sheet previously reported by Reeves et al. This simulation includes ohmic and coronal heating, thermal conduction, and radiative cooling in the energy equation. Using the results of this simulation, we perform time-dependent ionization calculations of the flow in a CME current sheet and construct two-dimensional spatial distributions of ionic charge states for multiple chemical elements. We use the filter responses from the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory and the predicted intensities of emission lines to compute the count rates for each of the AIA bands. The results show differences in the emission line intensities between equilibrium and non-equilibrium ionization. The current sheet plasma is underionized at low heights and overionized at large heights. At low heights in the current sheet, the intensities of the AIA 94 angstrom and 131 angstrom channels are lower for non-equilibrium ionization than for equilibrium ionization. At large heights, these intensities are higher for non-equilibrium ionization than for equilibrium ionization inside the current sheet. The assumption of ionization equilibrium would lead to a significant underestimate of the temperature low in the current sheet and overestimate at larger heights. We also calculate the intensities of ultraviolet lines and predict emission features to be compared with events from the Ultraviolet Coronagraph Spectrometer on the Solar and Heliospheric Observatory, including a low-intensity region around the current sheet corresponding to this model. C1 [Shen, Chengcai; Reeves, Katharine K.; Raymond, John C.; Murphy, Nicholas A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shen, Chengcai; Lin, Jun] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China. [Shen, Chengcai] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. [Ko, Yuan-Kuen] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Mikic, Zoran; Linker, Jon A.] Predict Sci Inc PSI, San Diego, CA 92121 USA. RP Shen, CC (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Reeves, Katharine/P-9163-2014; LIN, JUN/B-9890-2017; OI Murphy, Nicholas/0000-0001-6628-8033 FU NASA [NNX11AB61G, NNH11AQ13I]; NSF SHINE [AGS-1156076]; Program 973 [2011CB811403, 2013CBA01503]; NSFC [11273055]; CAS [KJCX2-EW-T07]; NASA (Heliophysics theory program); NSF (Frontiers in Earth System Dynamics) FX The authors appreciate the referee for valuable comments and suggestions that helped improve this paper. This research was supported by NASA grant NNX11AB61G, NNH11AQ13I and NSF SHINE grant AGS-1156076 to the Smithsonian Astrophysical Observatory. This work was also supported by Program 973 grants 2011CB811403 and 2013CBA01503, NSFC grant 11273055, and CAS grant KJCX2-EW-T07 to the Yunnan Astronomical Observatory. J.A.L. and Z.M. were supported by NASA (Heliophysics theory program) and NSF (Frontiers in Earth System Dynamics). NR 41 TC 10 Z9 12 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 110 DI 10.1088/0004-637X/773/2/110 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100029 ER PT J AU Wolk, SJ Rice, TS Aspin, C AF Wolk, Scott J. Rice, Thomas S. Aspin, Colin TI NEAR-INFRARED VARIABILITY AMONG YOUNG STELLAR OBJECTS IN THE STAR FORMATION REGION CYGNUS OB7 SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; infrared: stars; stars: formation; stars: pre-main sequence; stars: variables: general ID T-TAURI STARS; ORION NEBULA CLUSTER; SPECTRAL ENERGY-DISTRIBUTIONS; LOW-MASS STARS; MAGNETOSPHERIC ACCRETION; MOLECULAR CLOUD; INTERSTELLAR EXTINCTION; PHOTOMETRIC VARIABILITY; CIRCUMSTELLAR DISKS; SPITZER SURVEY AB We present an analysis of near-infrared time-series photometry in J, H, and K bands for about 100 epochs of a 1 degrees x 1 degrees region of the Lynds 1003/1004 dark cloud in the Cygnus OB7 region. Augmented by data from the Wide-field Infrared Survey Explorer, we identify 96 candidate disk bearing young stellar objects (YSOs) in the region. Of these, 30 are clearly Class I or earlier. Using the Wide-Field Imaging Camera on the United Kingdom Infrared Telescope, we were able to obtain photometry over three observing seasons, with photometric uncertainty better than 0.05 mag down to J approximate to 17. We study detailed light curves and color trajectories of similar to 50 of the YSOs in the monitored field. We investigate the variability and periodicity of the YSOs and find the data are consistent with all YSOs being variable in these wavelengths on timescales of a few years. We divide the variability into four observational classes: (1) stars with periodic variability stable over long timescales, (2) variables which exhibit short-lived cyclic behavior, (3) long-duration variables, and (4) stochastic variables. Some YSO variability defies simple classification. We can explain much of the observed variability as being due to dynamic and rotational changes in the disk, including an asymmetric or changing blocking fraction, changes to the inner disk hole size, as well as changes to the accretion rate. Overall, we find that the Class I: Class II ratio of the cluster is consistent with an age of <1 Myr, with at least one individual, wildly varying source similar to 100,000 yr old. We have also discovered a Class II eclipsing binary system with a period of 17.87 days. C1 [Wolk, Scott J.; Rice, Thomas S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Aspin, Colin] Univ Hawaii, Inst Astron, Hilo, HI 96720 USA. RP Wolk, SJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NAS8-03060]; Spitzer Science Center [1348190]; NSF REU [0757887]; National Aeronautics and Space Administration FX S.J.W. is supported by NASA contract NAS8-03060 (Chandra). T.S.R. was supported by grant 1348190 from the Spitzer Science Center. Thanks also to the NSF REU program for funding part of this research via NSF REU site grant 0757887. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this sacred mountain. NR 54 TC 17 Z9 17 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 AUG 20 PY 2013 VL 773 IS 2 AR 145 DI 10.1088/0004-637X/773/2/145 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100064 ER PT J AU Wyman, K Redfield, S AF Wyman, Katherine Redfield, Seth TI PROBING OUR HELIOSPHERIC HISTORY. I. HIGH-RESOLUTION OBSERVATIONS OF Na I AND Ca II ALONG THE SOLAR HISTORICAL TRAJECTORY SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: structure; line: profiles; local interstellar matter; Sun: heliosphere; techniques: spectroscopic ID LOCAL INTERSTELLAR-MEDIUM; ULTRA-HIGH-RESOLUTION; SCALE ATOMIC-STRUCTURE; LEO COLD CLOUD; ABSORPTION-LINES; COSMIC-RAYS; PHYSICAL-PROPERTIES; MAGNETIC-FIELD; 100 PARSECS; MILKY-WAY AB Over the course of its motion through the Galaxy, our solar system has encountered many interstellar environments of varying characteristics. Interstellar medium (ISM) density variations spanning seven orders of magnitude are commonly seen throughout the general Galactic environment, and a sufficiently dense cloud within this range has the potential to dramatically alter the structure of the heliosphere. We present observations of the ISM environments the Sun has most recently encountered based on high-resolution optical spectra toward nearby stars in the direction of the historical solar trajectory. The data were obtained with the highest-resolution spectrographs available, including the Tull Spectrograph on the Harlan J. Smith Telescope at McDonald Observatory and the Ultra-High-Resolution Facility on the Anglo-Australian Telescope at the Anglo-Australian Observatory. Observations were made of interstellar Na I and Ca II doublet absorption toward 43 bright stars within similar to 500 pc. No absorption is seen out to a distance of 120 pc (consistent with the outer boundary of the Local Bubble), but a complex collection of absorbers is seen in stars beyond 120 pc. While common absorbers are consistently seen in most sight lines, significant spatial variation is also detected, even between closely spaced sight lines. This pervasive evidence of small-scale structure not only speaks to the complexity of the morphology or physical properties of the gas in the ISM, but also emphasizes that dramatic structural changes to the heliosphere are common and it is important to understand the implications of such changes, such as the modulation in the cosmic ray flux, on planets. C1 [Wyman, Katherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wyman, Katherine; Redfield, Seth] Wesleyan Univ, Dept Astron, Van Vleck Observ, Middletown, CT 06459 USA. RP Wyman, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kwyman@cfa.harvard.edu; sredfield@wesleyan.edu OI Redfield, Seth/0000-0003-3786-3486 NR 91 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 20 PY 2013 VL 773 IS 2 AR 96 DI 10.1088/0004-637X/773/2/96 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 205EU UT WOS:000323426100015 ER PT J AU Van Bocxlaer, B Hunt, G AF Van Bocxlaer, Bert Hunt, Gene TI Morphological stasis in an ongoing gastropod radiation from Lake Malawi SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE speciation; rates of evolution; punctuated equilibrium; Viviparidae ID DARWINS FINCHES; RANDOM-WALKS; PUNCTUATED EQUILIBRIA; PHENOTYPIC EVOLUTION; ADAPTIVE RADIATION; MEASURING RATES; SELECTION; HISTORY; MODEL; DIVERSIFICATION AB Evolutionary processes leading to adaptive radiation regularly occur too fast to be accurately recorded in the fossil record but too slowly to be readily observed in living biota. The study of evolutionary radiations is thereby confronted with an epistemological gap between the timescales and approaches used by neontologists and paleontologists. Here we report on an ongoing radiation of extant Bellamya species (n = 4) from the African Rift Lake Malawi that provides an unusual opportunity to bridge this gap. The substantial molecular differentiation in this monophyletic Bellamya clade has arisen since Late Pleistocene megadroughts in the Malawi Basin caused by climate change. Morphological time-series analysis of a high-resolution, radiocarbon-dated sequence of 22 faunas spanning the Holocene documents stasis up to the middle Holocene in all traits studied (shell height, number of whorls, and two variables obtained from geometric morphometrics). Between deposition of the last fossil fauna (similar to 5 ka) and the present day, a drastic increase in morphological disparity was observed (3.7-5.8 times) associated with an increase in species diversity. Comparison of the rates of morphological evolution obtained from the paleontological time-series with phylogenetic rates indicates that the divergence in two traits could be reconstructed with the slow rates documented in the fossils, that one trait required a rate reduction (stabilizing selection), and the other faster rates (divergent selection). The combined paleontological and comparative approach taken here allows recognition that morphological stasis can be the dominant evolutionary pattern within species lineages, even in very young and radiating clades. C1 [Van Bocxlaer, Bert; Hunt, Gene] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. [Van Bocxlaer, Bert] Univ Ghent, Dept Geol & Soil Sci, Res Unit Palaeontol, B-9000 Ghent, Belgium. RP Van Bocxlaer, B (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM vanbocxlaerb@si.edu RI Hunt, Gene/B-3783-2010; Van Bocxlaer, Bert/N-1965-2016 OI Hunt, Gene/0000-0001-6430-5020; Van Bocxlaer, Bert/0000-0003-2033-326X FU Flanders Research Foundation; Ghent University Research Council; Academy of Natural Sciences in Philadelphia; Leopold III-fund; Belgian American Educational Foundation; Smithsonian Institution FX We thank the chiefs of Chipalamawamba, Kwitambo, and Kazembe for allowing us to work in outcrops near their villages; the Cultural and Museum Centre Karonga for structural support; Friedemann Schrenk, Harisson Simfukwe, Joseph Tembo, Jacques Verniers, Nore Praet, and Wout Salenbien for providing assistance in the field; Jon Ablett, Didier Van den Spiegel, Oliver Sandrock, Thomas Kristensen, Daniel Graf, and Ellen Strong for providing access to museum specimens; and Roland Schultheiss, Achilles Gautier, Pieter Kat, Ellen Strong, Thomas Ezard, two anonymous referees, and the editor for providing constructive discussion. This work was supported in part by the Flanders Research Foundation, the Ghent University Research Council, a Jessup Award from the Academy of Natural Sciences in Philadelphia, the Leopold III-fund, and Fellowships of the Belgian American Educational Foundation and the Smithsonian Institution (to B.V.B.). NR 60 TC 13 Z9 13 U1 2 U2 48 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 AUG 20 PY 2013 VL 110 IS 34 BP 13892 EP 13897 DI 10.1073/pnas.1308588110 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 203DU UT WOS:000323271400053 PM 23924610 ER PT J AU Dupree, AK Avrett, EH AF Dupree, A. K. Avrett, E. H. TI DIRECT EVALUATION OF THE HELIUM ABUNDANCES IN OMEGA CENTAURI SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE globular clusters: individual (Omega Centauri); stars: abundances; stars: atmospheres; stars: individual (LEID 54064, LEID 54084) ID HORIZONTAL-BRANCH STARS; RED GIANT STARS; GLOBULAR-CLUSTERS; MASS-LOSS; CHROMOSPHERIC LINE; RGB STARS; FIELD; NGC-2808; OUTFLOW; WIND AB A direct measure of the helium abundances from the near-infrared transition of He I at 1.08 mu m is obtained for two nearly identical red giant stars in the globular cluster Omega Centauri. One star exhibits the He I line; the line is weak or absent in the other star. Detailed non-local thermal equilibrium semi-empirical models including expansion in spherical geometry are developed to match the chromospheric H alpha, H beta, and Ca Pi K lines, in order to predict the helium profile and derive a helium abundance. The red giant spectra suggest a helium abundance of Y <= 0.22 (LEID 54064) and Y = 0.39-0.44 (LEID 54084) corresponding to a difference in the abundance Delta Y >= 0.17. Helium is enhanced in the giant star (LEID 54084) that also contains enhanced aluminum and magnesium. This direct evaluation of the helium abundances gives observational support to the theoretical conjecture that multiple populations harbor enhanced helium in addition to light elements that are products of high-temperature hydrogen burning. We demonstrate that the 1.08 mu m He I line can yield a helium abundance in cool stars when constraints on the semi-empirical chromospheric model are provided by other spectroscopic features. C1 [Dupree, A. K.; Avrett, E. H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dupree, AK (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dupree@cfa.harvard.edu; eavrett@cfa.harvard.edu NR 42 TC 18 Z9 18 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 20 PY 2013 VL 773 IS 2 AR L28 DI 10.1088/2041-8205/773/2/L28 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 198CO UT WOS:000322899600011 ER PT J AU Alo, D Correa, C Arias, C Cardenas, L AF Alo, Dominique Correa, Cristian Arias, Carlos Cardenas, Leyla TI Diversity of Aplochiton Fishes (Galaxiidea) and the Taxonomic Resurrection of A. marinus SO PLOS ONE LA English DT Article ID FRESH-WATER FISHES; SPECIES DELIMITATION; DNA BARCODES; PATAGONIAN LAKES; FALKLAND ISLANDS; GALAXIOID FISHES; ZEBRA TELEOSTEI; GLACIAL CYCLES; POPULATION; JENYNS AB Aplochiton is a small genus of galaxiid fishes endemic to Patagonia and the Falkland Islands whose taxonomy is insufficiently resolved. Recent genetic analyses confirmed the existence of only two closely related species, Aplochiton taeniatus and Aplochiton zebra, while a third controversial species, Aplochiton marinus, remained lost to synonymy with A. taeniatus. Using an integrative taxonomy framework, we studied original samples and published sequences from a broad range in western Patagonia and the Falkland Islands, and generated robust species hypotheses based on single-locus (Cytochrome Oxidase subunit I; COI) species-delineation methods and known diagnostic morphological characters analyzed in a multivariate context. Results revealed three distinct evolutionary lineages that morphologically resemble, in important respects, existing nominal species descriptions. Interestingly, the lineage associated with A. marinus was unambiguously identifiable (100% accuracy) both from the genetic and morphological viewpoints. In contrast, the morphology of A. taeniatus and A. zebra overlapped substantially, mainly due to the high variability of A. taeniatus. Discriminant function analysis aided the identification of these species with 83.9% accuracy. Hence, for their unambiguous identification, genetic screening is needed. A. marinus has seldom been documented, and when recorded, it has always been found in sites with clear marine influence. It is possible that only A. marinus preserves a life cycle related to the sea akin to the hypothesized ancestral galaxiid. We did not find evidence of claimed diadromy in A. taeniatus or A. zebra, and, therefore, these should be regarded as freshwater species. Finally, a lack of phylogeographic patterns and overrepresentation of uncommon haplotypes suggested demographic expansions in recent evolutionary time, especially of A. zebra, in line with the hypothesis of large-scale range expansion and lineage spread in western Patagonia. C1 [Alo, Dominique] Univ Austral Chile, Fac Ciencias Forestales & Recursos Nat, Inst Conservac Biodiversidad & Terr, Valdivia, Chile. [Correa, Cristian; Arias, Carlos] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Correa, Cristian; Arias, Carlos] McGill Univ, Redpath Museum, Montreal, PQ H3A 2K6, Canada. [Arias, Carlos] Smithsonian Trop Res Inst, Panama City, Panama. [Cardenas, Leyla] Univ Austral Chile, Fac Ciencias, Inst Ciencias Ambientales & Evolut, Valdivia, Chile. RP Alo, D (reprint author), Univ Austral Chile, Fac Ciencias Forestales & Recursos Nat, Inst Conservac Biodiversidad & Terr, Valdivia, Chile. EM dominiquealo@gmail.com; cristiancorrea@gmail.com OI Arias, Carlos Francisco/0000-0001-5925-0985 FU National Geographic Society (CRE grant) [8624-09]; International Development Research Centre (LACREG grant); Fondo de Investigacion Cientifica y Tecnica (FONDECYT) [11080068]; McGill School of Environment; Mejoramento Calidad y Equidad de la Educacion Superior (MECESUP) [AUS0703]; Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT); STRI; Biology department of McGill University FX This research was possible thanks to the financial support from National Geographic Society (CRE grant No. 8624-09), International Development Research Centre (LACREG grant), Fondo de Investigacion Cientifica y Tecnica (FONDECYT No. 11080068), and McGill School of Environment. During the course of this study, DA received a doctoral fellowship from Mejoramento Calidad y Equidad de la Educacion Superior (MECESUP, Project AUS0703), CC held a scholarship from Comision Nacional de Investigacion Cientifica y Tecnologica (CONICYT), and CA received fellowships from STRI and the Biology department of McGill University. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 83 TC 7 Z9 7 U1 0 U2 27 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD AUG 19 PY 2013 VL 8 IS 8 AR e71577 DI 10.1371/journal.pone.0071577 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 205ER UT WOS:000323425700071 PM 23977079 ER PT J AU Gagne, RJ AF Gagne, Raymond J. TI Four new genera of Nearctic Cecidomyiidae (Diptera) for species previously incorrectly placed SO ZOOTAXA LA English DT Article DE gall midges; conifers; Lasiopteridi; Dasineurini; Ledomyiini ID GALL MIDGES DIPTERA; BIOLOGY; MYRTACEAE AB Four new genera belonging to the tribe Dasineurini (Diptera: Cecidomyiidae: Lasiopteridi) are described for previously incorrectly placed species. The new genera are: Cembrotia Gagne, type species Janetiella coloradensis Felt; Cupressatia Gagne, type-species Janetiella siskiyou Felt; Strobilotia Gagne, type species Phytophaga carpophaga Tripp; and Rhizocecis Gagne, type species Cecidomyia rhois Coquillett. Resulting new combinations are: Cembrotia coloradensis (Felt), Cupressatia siskiyou (Felt), Cupressatia thujae (Hedlin), Strobilotia carpophaga (Tripp) and Rhizocecis rhois (Coquillett). C1 ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, Washington, DC 20013 USA. RP Gagne, RJ (reprint author), ARS, Systemat Entomol Lab, PSI, USDA,Smithsonian Inst, MRC 168,POB 37012, Washington, DC 20013 USA. EM raymond.gagne@ars.usda.gov NR 19 TC 0 Z9 1 U1 0 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 J9 ZOOTAXA JI Zootaxa PD AUG 19 PY 2013 VL 3701 IS 2 BP 148 EP 158 PG 11 WC Zoology SC Zoology GA 201NS UT WOS:000323148900002 PM 26191576 ER PT J AU Kiso, WK Selvaraj, V Nagashima, J Asano, A Brown, JL Schmitt, DL Leszyk, J Travis, AJ Pukazhenthi, BS AF Kiso, Wendy K. Selvaraj, Vimal Nagashima, Jennifer Asano, Atsushi Brown, Janine L. Schmitt, Dennis L. Leszyk, John Travis, Alexander J. Pukazhenthi, Budhan S. TI Lactotransferrin in Asian Elephant (Elephas maximus) Seminal Plasma Correlates with Semen Quality SO PLOS ONE LA English DT Article ID FERTILITY-ASSOCIATED PROTEIN; ALKALINE-PHOSPHATASE; SPERM MOTILITY; CREATINE-PHOSPHATE; MURINE SPERMATOZOA; LOXODONTA-AFRICANA; STALLION SEMEN; LACTOFERRIN; PARAMETERS; IDENTIFICATION AB Asian elephants (Elephas maximus) have highly variable ejaculate quality within individuals, greatly reducing the efficacy of artificial insemination and making it difficult to devise a sperm cryopreservation protocol for this endangered species. Because seminal plasma influences sperm function and physiology, including sperm motility, the objectives of this study were to characterize the chemistry and protein profiles of Asian elephant seminal plasma and to determine the relationships between seminal plasma components and semen quality. Ejaculates exhibiting good sperm motility (>= 65%) expressed higher percentages of spermatozoa with normal morphology (80.3 +/- 13.0 vs. 44.9 +/- 30.8%) and positive Spermac staining (51.9 +/- 14.5 vs. 7.5 +/- 14.4%), in addition to higher total volume (135.1 +/- 89.6 vs. 88.8 +/- 73.1 ml) and lower sperm concentration (473.0 +/- 511.2 vs. 1313.8 +/- 764.7x10(6) cells ml(-1)) compared to ejaculates exhibiting poor sperm motility (<= 10%; P<0.05). Comparison of seminal plasma from ejaculates with good versus poor sperm motility revealed significant differences in concentrations of creatine phosphokinase, alanine aminotransferase, phosphorus, sodium, chloride, magnesium, and glucose. These observations suggest seminal plasma influences semen quality in elephants. One-and two-dimensional (2D) gel electrophoresis revealed largely similar compositional profiles of seminal plasma proteins between good and poor motility ejaculates. However, a protein of similar to 80 kDa was abundant in 85% of ejaculates with good motility, and was absent in 90% of poor motility ejaculates (P<0.05). We used mass spectrometry to identify this protein as lactotransferrin, and immunoblot analysis to confirm this identification. Together, these findings lay a functional foundation for understanding the contributions of seminal plasma in the regulation of Asian elephant sperm motility, and for improving semen collection and storage in this endangered species. C1 [Kiso, Wendy K.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC USA. [Kiso, Wendy K.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Selvaraj, Vimal] Cornell Univ, Dept Anim Sci, Ithaca, NY 14853 USA. [Nagashima, Jennifer; Asano, Atsushi; Travis, Alexander J.] Cornell Univ, Coll Vet Med, Baker Inst Anim Hlth, Ithaca, NY 14853 USA. [Nagashima, Jennifer; Brown, Janine L.; Pukazhenthi, Budhan S.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA USA. [Schmitt, Dennis L.] Missouri State Univ, William H Darr Sch Agr, Springfield, MO USA. [Schmitt, Dennis L.] Ringling Bros Ctr Elephant Conservat, Polk City, FL USA. [Leszyk, John] Univ Massachusetts, Sch Med, Prote & Mass Spectrometry Facil, Shrewsbury, MA USA. RP Kiso, WK (reprint author), Smithsonian Conservat Biol Inst, Ctr Species Survival, Natl Zool Pk, Washington, DC USA. EM wkiso@feldinc.com FU Feld Entertainment Inc.; International Elephant Foundation; Friends of the National Zoo; Baker Institute for Animal Health FX Funding for this study was generously provided by Feld Entertainment Inc., International Elephant Foundation, Friends of the National Zoo, and the Baker Institute for Animal Health. Wendy Kiso was supported by a grant from Feld Entertainment, Inc. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 78 TC 5 Z9 5 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 AUG 16 PY 2013 VL 8 IS 8 AR e71033 DI 10.1371/journal.pone.0071033 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 207BA UT WOS:000323570200016 PM 23976974 ER PT J AU Montaser, R Paul, VJ Luesch, H AF Montaser, Rana Paul, Valerie J. Luesch, Hendrik TI Modular Strategies for Structure and Function Employed by Marine Cyanobacteria: Characterization and Synthesis of Pitinoic Acids SO ORGANIC LETTERS LA English DT Article ID PSEUDOMONAS-AERUGINOSA; GENE-EXPRESSION; THP-1 CELLS; SILYL ETHERS; INFECTION; INFLAMMATION; MACROPHAGES; CYTOKINES; OXIDATION; MOLECULE AB Novel bioactive lipids were identified from a Guamanian cyanobacterium, the Pseudomonas aeruginosa quorum sensing inhibitor pitinoic acid A (1) and the anti-inflammatory pitinoic acids B (2) and C. The structure of 2 was confirmed by synthesis, which also allowed for biological evaluation. Since 2 is an ester of pitinoic acids A and C, it represents a prodrug strategy to liberate dual biological activity for the management of P. aeruginosa infections and their associated inflammation. C1 [Montaser, Rana; Luesch, Hendrik] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. RP Luesch, H (reprint author), Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. EM luesch@cop.ufl.edu FU National Institutes of Health [P41GM086210, R01CA172310] FX We thank Dr. Qi-Yin Chen (Department of Medicinal Chemistry, University of Florida) for helpful discussions regarding the synthetic procedures and Dr. Sarath Gunasekera and Vicky Pittman (Smithsonian Marine Station) for providing additional amounts of pitinoic acid A. We thank J. R. Rocca (AMRIS, McKnight Brain Institute, University of Florida) for technical assistance with NMR data acquisition. This research was supported by the National Institutes of Health, Grants P41GM086210 and R01CA172310. This is contribution 916 from the Smithsonian Marine Station. NR 29 TC 7 Z9 7 U1 0 U2 15 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1523-7060 EI 1523-7052 J9 ORG LETT JI Org. Lett. PD AUG 16 PY 2013 VL 15 IS 16 BP 4050 EP 4053 DI 10.1021/ol401396u PG 4 WC Chemistry, Organic SC Chemistry GA 204KB UT WOS:000323363100003 PM 23915229 ER PT J AU Maruca, BA Kasper, JC AF Maruca, B. A. Kasper, J. C. TI Improved interpretation of solar wind ion measurements via high-resolution magnetic field data SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Solar wind; Ion temperature anisotropy; Wave-particle interactions; Data analysis; Instrumentation ID WAVE ACTIVITY; SPACECRAFT; EVOLUTION; PLASMAS AB The Wind spacecraft's Faraday cups (FC) continue to produce high-quality, in situ observations of thermal protons (i.e., ionized hydrogen) and a-particles (i.e., fully ionized helium) in the solar wind. By fitting a Wind/FC ion spectrum with a model velocity distribution function (VDF) for each particle species, values for density, bulk velocity, and temperature can be inferred. Incorporating measurements of the background magnetic field from the Wind Magnetic Field Investigation (MFI) allows perpendicular and parallel temperature components to be separated. Prior implementations of this analysis averaged the higher-cadence Wind/MFI measurements to match that of the Wind/FC ion spectra. However, this article summarizes recent and extensive revisions to the analysis software that, among other things, eliminate such averaging and thereby account for variations in the direction of the magnetic field over the time taken to measure the ions. A statistical comparison reveals that the old version consistently underestimates the temperature anisotropy of ion VDF's: averaging over fluctuations in the magnetic field essentially blurs the perpendicular and parallel temperature components, which makes the plasma seem artificially more isotropic. The new version not only provides a more accurate dataset of ion parameters (which is well suited to the study of microkinetic phenomena), it also demonstrates a novel technique for jointly processing particle and field data. Such methods are crucial to heliophysics as wave-particle interactions are increasingly seen as playing an important role in the dynamics of the solar wind and similar space plasmas. (C) 2013 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Maruca, B. A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Maruca, BA (reprint author), Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA. EM bmaruca@ssl.berkeley.edu; jkas-per@cfa.harvard.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU NASA [NNX08AW07G] FX The authors thank A. Szabo for assistance with Wind/MFI data and gratefully acknowledge A. J. Lazarus, J. T. Steinberg, M. R. Aellig, and all who worked on prior versions of the Wind/FC analysis code. Thanks are also extended to M. L. Stevens and S. D. Bale for fruitful discussions about this work. The analysis of Wind/FC observations at the Harvard-Smithsonian Center for Astrophysics (CfA) was supported by NASA Grant NNX08AW07G. This research has made use of the SAO/NASA Astrophysics Data System (ADS). NR 29 TC 5 Z9 5 U1 0 U2 4 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD AUG 15 PY 2013 VL 52 IS 4 BP 723 EP 731 DI 10.1016/j.asr.2013.04.006 PG 9 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 187CG UT WOS:000322093900017 ER PT J AU Gillner, S Ruger, N Roloff, A Berger, U AF Gillner, Sten Rueger, Nadja Roloff, Andreas Berger, Uta TI Low relative growth rates predict future mortality of common beech (Fagus sylvatica L.) SO FOREST ECOLOGY AND MANAGEMENT LA English DT Article DE Dendrochronology; Mortality predictions; Common beech; Crown decline; Vitality assessment ID QUERCUS-ROBUR L.; TREE MORTALITY; DROUGHT; CLIMATE; MODELS; FOREST; DEATH; RESPONSES; OAKS; PERFORMANCE AB For many tree species, growth patterns derived from tree-ring time series have been shown to be good indicators of tree mortality. Although tree rings of common beech (Fagus sylvatica) have been widely used to answer complex questions of forest ecology, there are only few studies using growth characteristics, such as growth decline or growth variability, as informative predictors of tree mortality in old-growth beech forests. To do this, we used dendrochronological data of living and dead trees from a nature reserve in eastern Germany. Using a logistic regression model, we predicted tree mortality based on growth characteristics (basal area increment; variance, autocorrelation, mean sensitivity of ring widths; growth trends) over different time horizons. Beech mortality could reliably be predicted up to 20 years in advance on the basis of relative basal area growth. Trees that grew slower in relative basal area than 0.95 cm(2)/cm y on average over a 20-year-period had a much higher mortality risk than faster-growing trees. Other statistical characteristics of the dendrochronological time series, such as the variance or autocorrelation of ring widths, the mean sensitivity or growth trends, did not convey significant additional information and did not lead to better mortality predictions. (C) 2013 Elsevier B.V. All rights reserved. C1 [Gillner, Sten; Roloff, Andreas] Tech Univ Dresden, Inst Forest Bot & Forest Zool, D-01737 Tharandt, Germany. [Rueger, Nadja] Univ Leipzig, Dept Systemat Bot & Funct Biodivers, D-04103 Leipzig, Germany. [Rueger, Nadja] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Berger, Uta] Tech Univ Dresden, Inst Forest Growth & Forest Comp Sci, D-01737 Tharandt, Germany. RP Gillner, S (reprint author), Tech Univ Dresden, Inst Forest Bot & Forest Zool, Pienner Str 7, D-01737 Tharandt, Germany. EM gillner@forst.tu-dresden.de RI Ruger, Nadja/J-6393-2015 OI Ruger, Nadja/0000-0003-2371-4172 FU Bundesministerium fur Bildung und Forschung (BMBF); Deutsche Forschungsgemeinschaft DFG [RU 1536/2-1] FX We thank E. Fritzsche for his support in the fieldwork and the staff of the Institute for Forest Botany and Zoology for their comments on the manuscript. This study was realized with the financial support by the Bundesministerium fur Bildung und Forschung (BMBF) in the project REGKLAM (www.regklam.de). We would like to give special thanks to Mr. Pielenz and the Umweltamt Dresden for their stimulus and great commitment to this study. N.R. was funded by a research grant from Deutsche Forschungsgemeinschaft DFG (RU 1536/2-1). NR 57 TC 10 Z9 12 U1 6 U2 68 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 AUG 15 PY 2013 VL 302 BP 372 EP 378 DI 10.1016/j.foreco.2013.03.032 PG 7 WC Forestry SC Forestry GA 168XN UT WOS:000320741300039 ER PT J AU Burton, MG Braiding, C Glueck, C Goldsmith, P Hawkes, J Hollenbach, DJ Kulesa, C Martin, CL Pineda, JL Rowell, G Simon, R Stark, AA Stutzki, J Tothill, NJH Urquhart, JS Walker, C Walsh, AJ Wolfire, M AF Burton, Michael G. Braiding, C. Glueck, C. Goldsmith, P. Hawkes, J. Hollenbach, D. J. Kulesa, C. Martin, C. L. Pineda, J. L. Rowell, G. Simon, R. Stark, A. A. Stutzki, J. Tothill, N. J. H. Urquhart, J. S. Walker, C. Walsh, A. J. Wolfire, M. TI The Mopra Southern Galactic Plane CO Survey SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF AUSTRALIA LA English DT Article DE Galaxy: kinematics and dynamics; Galaxy: structure; ISM: clouds; ISM: molecules; radio lines: ISM; surveys ID GIANT MOLECULAR CLOUDS; GAMMA-RAY SIGNATURES; MILKY-WAY; STAR-FORMATION; INTERSTELLAR CLOUDS; CARBON-MONOXIDE; OUTER GALAXY; RING SURVEY; DARK GAS; EMISSION AB We present the first results from a new carbon monoxide (CO) survey of the southern Galactic plane being conducted with the Mopra radio telescope in Australia. The (CO)-C-12, (CO)-C-13, and (CO)-O-18 J = 1-0 lines are being mapped over the l = 305 degrees-345 degrees, b= +/- 0.5 degrees portion of the fourth quadrant of the Galaxy, at 35 arcsec spatial and 0.1 km s(-1) spectral resolution. The survey is being undertaken with two principal science objectives: (i) to determine where and how molecular clouds are forming in the Galaxy and (ii) to probe the connection between molecular clouds and the 'missing' gas inferred from gamma-ray observations. We describe the motivation for the survey, the instrumentation and observing techniques being applied, and the data reduction and analysis methodology. In this paper, we present the data from the first degree surveyed, l = 323 degrees-324 degrees, b= +/- 0.5 degrees. We compare the data to the previous CO survey of this region and present metrics quantifying the performance being achieved; the rms sensitivity per 0.1 km s-1 velocity channel is similar to 1.5 K for (CO)-C-12 and similar to 0.7 K for the other lines. We also present some results from the region surveyed, including line fluxes, column densities, molecular masses, (CO)-C-12/(CO)-C-13 line ratios, and (CO)-C-12 optical depths. We also examine how these quantities vary as a function of distance from the Sun when averaged over the 1 square degree survey area. Approximately 2 x 10(6) M-circle dot of molecular gas is found along the G323 sightline, with an average H-2 number density of n(H2) similar to 1 cm(-3) within the Solar circle. The CO data cubes will be made publicly available as they are published. C1 [Burton, Michael G.; Braiding, C.; Tothill, N. J. H.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Glueck, C.; Simon, R.; Stutzki, J.] Univ Cologne, Inst Phys 1, KOSMA, D-50937 Cologne, Germany. [Goldsmith, P.; Pineda, J. L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Hawkes, J.; Rowell, G.] Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia. [Hollenbach, D. J.] SETI Inst, Carl Sagan Ctr, Mountain View, CA 94043 USA. [Kulesa, C.; Walker, C.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Martin, C. L.] Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tothill, N. J. H.] Univ Western Sydney, Sch Comp Engn & Math, Penrith, NSW 2751, Australia. [Urquhart, J. S.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Walsh, A. J.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Wolfire, M.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Burton, MG (reprint author), Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. EM m.burton@unsw.edu.au RI Walsh, Andrew/B-5627-2013; OI Walsh, Andrew/0000-0001-9506-0855; Burton, Michael/0000-0001-7289-1998; Rowell, Gavin/0000-0002-9516-1581; Stark, Antony/0000-0002-2718-9996 FU Commonwealth of Australia; Australian Research Council (ARC) [DP120101585] FX The Mopra radio telescope is part of the Australia Telescope National Facility, which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. Many staff of the ATNF have contributed to the success of the remote operations at Mopra. We particularly wish to acknowledge the contributions of David Brodrick, Philip Edwards, Brett Hisock, Balt Indermuehle, and Peter Mirtschin. The University of New South Wales Digital Filter Bank used for the observations with the Mopra Telescope (the UNSW-MOPS) was provided with support from the Australian Research Council (ARC). We also acknowledge ARC support through Discovery Project DP120101585. This work was also carried out, in part, at the Jet Propulsion Laboratory, California Institute of Technology. Finally, we thank the anonymous referee whose comments have helped improve this paper. NR 65 TC 3 Z9 3 U1 0 U2 5 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 1323-3580 EI 1448-6083 J9 PUBL ASTRON SOC AUST JI Publ. Astron. Soc. Aust. PD AUG 14 PY 2013 VL 30 AR e044 DI 10.1017/pasa.2013.22 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 201UU UT WOS:000323169300001 ER PT J AU Uzdin, R Dalla Torre, EG Kosloff, R Moiseyev, N AF Uzdin, Raam Dalla Torre, Emanuele G. Kosloff, Ronnie Moiseyev, Nimrod TI Effects of an exceptional point on the dynamics of a single particle in a time-dependent harmonic trap SO PHYSICAL REVIEW A LA English DT Article ID BOSE-EINSTEIN CONDENSATE; COLLECTIVE EXCITATIONS; COHERENT STATES; QUANTUM-SYSTEMS; OSCILLATOR; DEGENERACIES; HAMILTONIANS; INVARIANTS; GAS AB The time evolution of a single particle in a harmonic trap with time-dependent frequency omega(t) has been well studied. Nevertheless, here we show that when the harmonic trap is opened (or closed) as a function of time while keeping the adiabatic parameter mu = [d omega(t)/dt]/omega(2)(t) fixed, a sharp transition from an oscillatory to a monotonic exponential dynamics occurs at mu = 2. At this transition point, the time evolution has an exceptional point (EP) at all instants. This situation, where an EP of a time-dependent Hermitian Hamiltonian is obtained at any given time, is very different from other known cases. In the present case, we show that the order of the EP depends on the set of observables used to describe the dynamics. Our finding is relevant to the dynamics of a single ion in a magnetic, optical, or rf trap, and of diluted gases of ultracold atoms in optical traps. C1 [Uzdin, Raam; Dalla Torre, Emanuele G.; Kosloff, Ronnie; Moiseyev, Nimrod] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 01238 USA. [Dalla Torre, Emanuele G.] Harvard Univ, Dept Phys, Cambridge, MA 01238 USA. [Kosloff, Ronnie] Hebrew Univ Jerusalem, Fritz Haber Inst Mol Dynam, Jerusalem, Israel. [Moiseyev, Nimrod] Technion Israel Inst Technol, Schulich Fac Chem, IL-32000 Haifa, Israel. [Moiseyev, Nimrod] Technion Israel Inst Technol, Fac Phys, IL-32000 Haifa, Israel. RP Uzdin, R (reprint author), Hebrew Univ Jerusalem, Dept Phys, Jerusalem, Israel. RI Kosloff, Ronnie/D-2388-2013; OI Kosloff, Ronnie/0000-0001-6201-2523; Dalla Torre, Emanuele G./0000-0002-7219-3804 FU ITAMP FX We would like to acknowledge ITAMP for their support. This work was initialized and has been carried out as a result of the friendly and scientific atmosphere at ITAMP, which encourages informal discussions on a daily basis among the permanent and visiting members of ITAMP. We would also like to sincerely thank the anonymous referee for his/her useful comments. NR 57 TC 8 Z9 8 U1 1 U2 10 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 AUG 12 PY 2013 VL 88 IS 2 AR 022505 DI 10.1103/PhysRevA.88.022505 PG 5 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 199YI UT WOS:000323031400007 ER PT J AU Sharifi, A Kalin, L Hantush, MM Isik, S Jordan, TE AF Sharifi, Amirreza Kalin, Latif Hantush, Mohamed M. Isik, Sabahattin Jordan, Thomas E. TI Carbon dynamics and export from flooded wetlands: A modeling approach SO ECOLOGICAL MODELLING LA English DT Article DE Wetlands; Model; Carbon; Methane; CH4; DOC; Dissolved organic carbon; Carbon export; Greenhouse gas emission; Aerobic; Anaerobic; Diffusion; Ebullition ID ORGANIC-CARBON; METHANE EMISSIONS; SENSITIVITY ANALYSIS; WATER; UNCERTAINTY; ECOSYSTEMS; OXIDATION; MATTER; SOIL; VEGETATION AB Described in this article is development and validation of a process based model for carbon cycling in flooded wetlands, called WetQual-C. The model considers various biogeochemical interactions affecting C cycling, greenhouse gas emissions, organic carbon export and retention. WetQual-C couples carbon cycling with other interrelated geochemical cycles in wetlands, i.e. nitrogen and oxygen; and fully reflects the dynamics of the thin oxidized zone at the soil-water interface. Using field collected data from a small wetland receiving runoff from an agricultural watershed on the eastern shore of Chesapeake Bay, we assessed model performance and carried out a thorough sensitivity and uncertainty analysis to evaluate the credibility of the model. Overall, model performed well in capturing TOC export fluctuations and dynamics from the study wetland. Model results revealed that over a period of 2 years, the wetland removed or retained equivalent to 47 +/- 12% of the OC carbon intake, mostly via DC decomposition and DOC diffusion to sediment. The study wetland appeared as a carbon sink rather than source and proved its purpose as a relatively effective and low cost mean for improving water quality. (C) 2013 Elsevier B.V. All rights reserved. C1 [Sharifi, Amirreza; Kalin, Latif] Auburn Univ, Sch Forestry & Wildlife Sci, Auburn, AL 36849 USA. [Hantush, Mohamed M.] US EPA, Land Remediat & Pollut Control Div, Natl Risk Management Res Lab, ORD, Cincinnati, OH 45268 USA. [Isik, Sabahattin] Turgut Ozal Univ, Fac Engn, Ankara, Turkey. [Jordan, Thomas E.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Kalin, L (reprint author), Auburn Univ, Sch Forestry & Wildlife Sci, 602 Duncan Dr, Auburn, AL 36849 USA. EM Latif@auburn.edu RI ISIK, Sabahattin/G-5265-2012 FU U.S. Environmental Protection Agency through its Office of Research and Development [EP08C000066]; Auburn University, School of Forestry and Wildlife Sciences FX The U.S. Environmental Protection Agency through its Office of Research and Development partially funded and collaborated in the research described here under contract (EP08C000066) with Auburn University, School of Forestry and Wildlife Sciences. It has not been subject to the Agency review and therefore does not necessarily reflect the views of the Agency, and no official endorsement should be inferred. NR 56 TC 10 Z9 10 U1 3 U2 75 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0304-3800 EI 1872-7026 J9 ECOL MODEL JI Ecol. Model. PD AUG 10 PY 2013 VL 263 BP 196 EP 210 DI 10.1016/j.ecolmodel.2013.04.023 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 197NJ UT WOS:000322857600019 ER PT J AU Acero, F Ackermann, M Ajello, M Allafort, A Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Bottacini, E Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cecchi, C Charles, E Chaves, RCG Chekhtman, A Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S Dalton, M D'Ammando, F de Palma, F Dermer, CD Di Venere, L Silva, EDE Drell, PS Drlica-Wagner, A Falletti, L Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Gregoire, T Grenier, IA Grondin, MH Grove, JE Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hayashi, K Hays, E Hewitt, J Hill, AB Horan, D Hou, X Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, AS Kamae, T Kawano, T Kerr, M Knodlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lovellette, MN Lubrano, P Marelli, M Massaro, F Mayer, M Mazziotta, MN McEnery, JE Mehault, J Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nakamori, T Nemmen, R Nuss, E Ohsugi, T Okumura, A Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Reposeur, T Ritz, S Roth, M Rousseau, R Parkinson, PMS Schulz, A Sgro, C Siskind, EJ Smith, DA Spandre, G Spinelli, P Suson, DJ Takahashi, H Takeuchi, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tibolla, O Tinivella, M Torres, DF Tosti, G Troja, E Uchiyama, Y Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Werner, M Winer, BL Wood, KS Yang, Z AF Acero, F. Ackermann, M. Ajello, M. Allafort, A. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Bottacini, E. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cecchi, C. Charles, E. Chaves, R. C. G. Chekhtman, A. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. Dalton, M. D'Ammando, F. de Palma, F. Dermer, C. D. Di Venere, L. do Couto e Silva, E. Drell, P. S. Drlica-Wagner, A. Falletti, L. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Gregoire, T. Grenier, I. A. Grondin, M. -H. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hayashi, K. Hays, E. Hewitt, J. Hill, A. B. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, A. S. Kamae, T. Kawano, T. Kerr, M. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lovellette, M. N. Lubrano, P. Marelli, M. Massaro, F. Mayer, M. Mazziotta, M. N. McEnery, J. E. Mehault, J. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nakamori, T. Nemmen, R. Nuss, E. Ohsugi, T. Okumura, A. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Reposeur, T. Ritz, S. Roth, M. Rousseau, R. Parkinson, P. M. Saz Schulz, A. Sgro, C. Siskind, E. J. Smith, D. A. Spandre, G. Spinelli, P. Suson, D. J. Takahashi, H. Takeuchi, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tibolla, O. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Uchiyama, Y. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Werner, M. Winer, B. L. Wood, K. S. Yang, Z. TI CONSTRAINTS ON THE GALACTIC POPULATION OF TeV PULSAR WIND NEBULAE USING FERMI LARGE AREA TELESCOPE OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays: general ID GAMMA-RAY PULSARS; COMPOSITE SUPERNOVA REMNANT; YOUNG RADIO PULSAR; ENERGETIC PSR J1357-6429; BLIND FREQUENCY SEARCHES; XMM-NEWTON OBSERVATIONS; SOURCE HESS J1303-631; X-RAY; MAGNETIC-FIELD; CRAB-NEBULA AB Pulsar wind nebulae (PWNe) have been established as the most populous class of TeV gamma-ray emitters. Since launch, the Fermi Large Area Telescope (LAT) has identified five high-energy (100 MeV < E < 100 GeV) gamma-ray sources as PWNe and detected a large number of PWN candidates, all powered by young and energetic pulsars. The wealth of multi-wavelength data available and the new results provided by Fermi-LAT give us an opportunity to find new PWNe and to explore the radiative processes taking place in known ones. The TeV gamma-ray unidentified (UNID) sources are the best candidates for finding new PWNe. Using 45 months of Fermi-LAT data for energies above 10 GeV, an analysis was performed near the position of 58 TeV PWNe and UNIDs within 5. of the Galactic plane to establish new constraints on PWN properties and find new clues on the nature of UNIDs. Of the 58 sources, 30 were detected, and this work provides their gamma-ray fluxes for energies above 10 GeV. The spectral energy distributions and upper limits, in the multi-wavelength context, also provide new information on the source nature and can help distinguish between emission scenarios, i.e., between classification as a pulsar candidate or as a PWN candidate. Six new GeV PWN candidates are described in detail and compared with existing models. A population study of GeV PWN candidates as a function of the pulsar/PWN system characteristics is presented. C1 [Acero, F.; Brandt, T. J.; Ferrara, E. C.; Guiriec, S.; Harding, A. K.; Hays, E.; Hewitt, J.; McEnery, J. E.; Nemmen, R.; Perkins, J. S.; Thompson, D. J.; Troja, E.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Ackermann, M.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Buehler, R.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; do Couto e Silva, E.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Johnson, A. S.; Kamae, T.; Kerr, M.; Lande, J.; Massaro, F.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Thayer, J. G.; Thayer, J. B.; Uchiyama, Y.; Vandenbroucke, J.; Vianello, G.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.; Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Chaves, R. C. G.; Grenier, I. A.] Univ Paris Diderot, CNRS, Serv Astrophys, Lab AIM,CEA IRFU,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Bonamente, E.; Cecchi, C.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.; Marelli, M.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Chekhtman, A.] George Mason Univ, Coll Sci, Ctr Earth Observing & Space Res, Fairfax, VA 22030 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana, Sci Data Ctr, I-00044 Frascati, Italy. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Italy. [Cohen-Tanugi, J.; Falletti, L.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, CNRS, IN2P3, Lab Univers & Particules Montpellier, F-34095 Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Stockholm Univ, Oskar Klein Ctr Cosmoparticle Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [Dalton, M.; Hou, X.; Lemoine-Goumard, M.; Mehault, J.; Reposeur, T.; Rousseau, R.; Smith, D. A.] Univ Bordeaux 1, CNRS, IN2p3, CEN Bordeaux Gradignan, F-33175 Gradignan, France. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [Dermer, C. D.; Grove, J. E.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Fukazawa, Y.; Hanabata, Y.; Hayashi, K.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Higashihiroshima, Hiroshima 7398526, Japan. [Gregoire, T.; Grondin, M. -H.; Knoedlseder, J.] CNRS, IRAP, F-31028 Toulouse 4, France. [Gregoire, T.; Grondin, M. -H.; Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, F-31028 Toulouse, France. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hughes, R. E.; Winer, B. L.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Dept Phys, Columbus, OH 43210 USA. [Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Higashihiroshima, Hiroshima 7398526, Japan. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Nakamori, T.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Greenbelt, MD 20771 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Dept Phys, Santa Cruz, CA 95064 USA. [Razzano, M.; Ritz, S.; Parkinson, P. M. Saz] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.; Werner, M.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Roth, M.] Univ Washington, Dept Phys, Seattle, WA 98195 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. [Tibolla, O.] Univ Wurzburg, Inst Theoret Phys & Astrophys, D-97074 Wurzburg, Germany. [Torres, D. F.] ICREA, E-08010 Barcelona, Spain. [Vianello, G.] Consorzio Interuniv Fis Spaziale, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. RP Acero, F (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM funk@slac.stanford.edu; joshualande@gmail.com; lemoine@cenbg.in2p3.fr; rousseau@cenbg.in2p3.fr RI Massaro, Francesco/L-9102-2016; Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Saz Parkinson, Pablo Miguel/I-7980-2013; Moskalenko, Igor/A-1301-2007; Rando, Riccardo/M-7179-2013; Hays, Elizabeth/D-3257-2012; Sgro, Carmelo/K-3395-2016; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012 OI orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Mazziotta, Mario Nicola/0000-0001-9325-4672; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Marelli, Martino/0000-0002-8017-0338; Massaro, Francesco/0000-0002-1704-9850; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; Inoue, Yoshiyuki/0000-0002-7272-1136; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Pesce-Rollins, Melissa/0000-0003-1790-8018; Moskalenko, Igor/0000-0001-6141-458X; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888 FU K. A. Wallenberg Foundation; European Community [ERC-StG-259391]; Marie Curie IOF [275861] FX Royal Swedish Academy of Sciences Research Fellow, funded by a grant from the K. A. Wallenberg Foundation.; Funded by contract ERC-StG-259391 from the European Community.; Funded by a Marie Curie IOF, FP7/2007-2013, grant agreement No. 275861. NR 159 TC 28 Z9 28 U1 0 U2 19 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 77 DI 10.1088/0004-637X/773/1/77 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900077 ER PT J AU Aller, KM Kraus, AL Liu, MC Burgett, WS Chambers, KC Hodapp, KW Kaiser, N Magnier, EA Price, PA AF Aller, Kimberly M. Kraus, Adam L. Liu, Michael C. Burgett, William S. Chambers, Kenneth C. Hodapp, Klaus W. Kaiser, Nick Magnier, Eugene A. Price, Paul A. TI A PAN-STARRS plus UKIDSS SEARCH FOR YOUNG, WIDE PLANETARY-MASS COMPANIONS IN UPPER SCORPIUS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; brown dwarfs; planetary systems; stars: pre-main sequence ID BROWN DWARF CANDIDATES; NEAR-INFRARED SPECTRA; SOLAR-TYPE STARS; SKY SURVEY 2MASS; OB ASSOCIATION; HR 8799; GRAVITATIONAL-INSTABILITY; SUBSTELLAR COMPANION; CIRCUMSTELLAR DISKS; EVOLUTIONARY MODELS AB We have combined optical and NIR photometry from Pan-STARRS 1 and UKIDSS to search the young (5-10 Myr) star-forming region of Upper Scorpius for wide (approximate to 400-4000 AU) substellar companions down to similar to 5M(Jup). Our search is approximate to 4 mag deeper than previous work based on the Two Micron All Sky Survey. We identified several candidates around known stellar members using a combination of color selection and spectral energy distribution fitting. Our follow-up spectroscopy has identified two new companions as well as confirmed two companions previously identified from photometry, with spectral types of M7.5-M9 and masses of similar to 15-60 M-Jup, indicating a frequency for such wide substellar companions of similar to 0.6% +/- 0.3%. Both USco 1610-1913B and USco 1612-1800B are more luminous than expected for their spectral type compared with known members of Upper Sco. HIP 77900B has an extreme mass ratio (M-2/M-1 approximate to 0.005) and an extreme separation of 3200 AU. USco 1602-2401B also has a very large separation of 1000 AU. We have also confirmed a low-mass stellar companion, USco 1610-2502B (730 AU, M5.5). Our substellar companions appear both non-coeval with their primary stars according to evolutionary models and, as a group, are systematically more luminous than the Upper Sco cluster sequence. One possible reason for these luminosity discrepancies could be different formation processes or accretion histories for these objects. C1 [Aller, Kimberly M.; Kraus, Adam L.; Liu, Michael C.; Burgett, William S.; Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nick; Magnier, Eugene A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Kraus, Adam L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Aller, KM (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. NR 85 TC 19 Z9 19 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 63 DI 10.1088/0004-637X/773/1/63 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900063 ER PT J AU Chen, CTJ Hickox, RC Alberts, S Brodwin, M Jones, C Murray, SS Alexander, D Assef, RJ Brown, MJI Dey, A Forman, WR Gorjian, V Goulding, AD Le Floc'h, E Jannuzi, BT Mullaney, JR Pope, A AF Chen, Chien-Ting J. Hickox, Ryan C. Alberts, Stacey Brodwin, Mark Jones, Christine Murray, Stephen S. Alexander, DavidM. Assef, Roberto J. Brown, Michael J. I. Dey, Arjun Forman, William R. Gorjian, Varoujan Goulding, Andrew D. Le Floc'h, Emeric Jannuzi, Buell T. Mullaney, James R. Pope, Alexandra TI A CORRELATION BETWEEN STAR FORMATION RATE AND AVERAGE BLACK HOLE ACCRETION IN STAR-FORMING GALAXIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: starburst; infrared: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; SPECTRAL ENERGY-DISTRIBUTIONS; FORMATION RATE INDICATOR; QUASAR HOST GALAXIES; IRAC SHALLOW SURVEY; WIDE-FIELD SURVEY; SIMILAR-TO 2.5; X-RAY SURVEY; FORMATION HISTORY; GOODS-HERSCHEL AB We present a measurement of the average supermassive black hole accretion rate (BHAR) as a function of the star formation rate (SFR) for galaxies in the redshift range 0.25 < z < 0.8. We study a sample of 1767 far-IR-selected star-forming galaxies in the 9 deg(2) Bootes multi-wavelength survey field. The SFR is estimated using 250 mu m observations from the Herschel Space Observatory, for which the contribution from the active galactic nucleus (AGN) is minimal. In this sample, 121 AGNs are directly identified using X-ray or mid-IR selection criteria. We combined these detected AGNs and an X-ray stacking analysis for undetected sources to study the average BHAR for all of the star-forming galaxies in our sample. We find an almost linear relation between the average BHAR (in M-circle dot yr(-1)) and the SFR (in M-circle dot yr(-1)) for galaxies across a wide SFR range 0.85 < log SFR < 2.56 : logBHAR = (-3.72 +/- 0.52) + (1.05 +/- 0.33) log SFR. This global correlation between SFR and average BHAR is consistent with a simple picture in which SFR and AGN activity are tightly linked over galaxy evolution timescales. C1 [Chen, Chien-Ting J.; Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Alberts, Stacey; Pope, Alexandra] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Jones, Christine; Forman, William R.; Goulding, Andrew D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Alexander, DavidM.; Mullaney, James R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Assef, Roberto J.; Gorjian, Varoujan] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brown, Michael J. I.] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Dey, Arjun; Jannuzi, Buell T.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Le Floc'h, Emeric; Mullaney, James R.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA, DSM,Irfu,CNRS,CE Saclay, F-91191 Gif Sur Yvette, France. RP Chen, CTJ (reprint author), Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. EM ctchen@dartmouth.edu RI Brown, Michael/B-1181-2015; OI Brown, Michael/0000-0002-1207-9137; Chen, Chien-Ting/0000-0002-4945-5079; Alexander, David/0000-0002-5896-6313; Forman, William/0000-0002-9478-1682 FU Dartmouth Fellowship; Chandra grant [SP8-9001X, AR8-9017X] FX We are grateful to the anonymous referee for the very careful reading of the paper, and the suggestions that significantly improved this paper. We thank our colleagues on the AGES, IRAC Shallow Survey, SDWFS, NDWFS, and the XBootes teams, and the HerMES team for making the data publicly available. The first Spitzer MIPS survey of the Bootes region was obtained using GTO time provided by the Spitzer Infrared Spectrograph Team (PI: James Houck) and by M. Rieke. We thank the collaborators in that work for access to the 24 mu m catalog generated from those data by Emeric Le Floc'h. We also thank Chris S. Kochanek for useful discussions. C.-T.J.C was supported by a Dartmouth Fellowship. This work was supported in part by Chandra grants SP8-9001X and AR8-9017X. NR 92 TC 68 Z9 67 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 3 DI 10.1088/0004-637X/773/1/3 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900003 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. IV. RELATIVISTICALLY BROADENED IRON LINES SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; galaxies: active; gravitation; line: profiles; relativistic processes ID ARBITRARY MULTIPOLE MOMENTS; SAGITTARIUS A-ASTERISK; BLACK-HOLE CANDIDATES; STRONG-GRAVITY REGIME; X-RAY BINARIES; GRAVITATIONAL-WAVES; GENERAL-RELATIVITY; ACCRETION DISKS; EMISSION-LINES; KERR SPACETIME AB According to the no-hair theorem, astrophysical black holes are fully characterized by their masses and spins and are described by the Kerr metric. This theorem can be tested observationally by measuring (at least) three different multipole moments of the spacetimes of black holes. In this paper, we calculate the profiles of fluorescent iron lines emitted from the accretion flows around black hole candidates within a framework that allows us to perform the calculation as a function of its mass and spin as well as of a free parameter that measures potential deviations from the Kerr metric. We show that such deviations lead to line profiles that are significantly altered and may exhibit a modified flux ratio of the two peaks in their characteristic double-peaked shape. We also show that the disk inclination can be measured independently of the spin and the deviation parameter at low to intermediate inclination angles, as in the case of Kerr black holes. We estimate the precision that near-future X-ray missions such as Astro-H and ATHENA+ are required to achieve in order to resolve deviations from the Kerr metric in iron line profiles and show that constraints on such deviations will be strongest for rapidly spinning black holes. More generally, we show that measuring the line profile with a precision of similar to 5% at disk inclinations of 30 degrees or 60 degrees constrains the deviation parameter to order unity for values of the spin a greater than or similar to 0.5M. C1 [Johannsen, Tim] Univ Waterloo, Dept Phys & Astron, Waterloo, ON N2L 3G1, Canada. [Johannsen, Tim] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Johannsen, Tim] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada. [Johannsen, Tim; Psaltis, Dimitrios] Univ Arizona, Dept Phys, Tucson, AZ 85721 USA. [Johannsen, Tim; Psaltis, Dimitrios] Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. [Psaltis, Dimitrios] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. FU University of Arizona by the NSF [NSF 0746549]; CITA National Fellowship at the University of Waterloo; Government of Canada through Industry Canada; Province of Ontario through the Ministry of Research and Innovation FX We thank the referee, C. Reynolds, as well as L. Brenneman for useful comments. This work was supported at the University of Arizona by the NSF CAREER award NSF 0746549. T. J. was also supported by a CITA National Fellowship at the University of Waterloo. Research at Perimeter Institute is supported by the Government of Canada through Industry Canada and by the Province of Ontario through the Ministry of Research and Innovation. NR 72 TC 51 Z9 51 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 57 DI 10.1088/0004-637X/773/1/57 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900057 ER PT J AU Melott, AL Bambach, RK AF Melott, Adrian L. Bambach, Richard K. TI DO PERIODICITIES IN EXTINCTION-WITH POSSIBLE ASTRONOMICAL CONNECTIONS-SURVIVE A REVISION OF THE GEOLOGICAL TIMESCALE? SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrobiology; dust, extinctions; methods: statistical ID UNEVENLY SPACED DATA; TIME-SERIES ANALYSIS; MASS EXTINCTIONS; GENERAL TRENDS; FOSSIL RECORD; BIODIVERSITY; CYCLES; FLUCTUATION; ORIGINATION; DIVERSITY AB A major revision of the geological timescale was published in 2012. We re-examine our past finding of a 27 Myr periodicity in marine extinction rates by re-assigning dates to the extinction data used previously. We find that the spectral power in this period is somewhat increased, and persists at a narrow bandwidth, which supports our previous contention that the Nemesis hypothesis is untenable as an explanation for the periodicity that was first noted by Raup & Sepkoski in the 1980s. We enumerate a number of problems in a recent study comparing extinction rates with time series models. C1 [Melott, Adrian L.] Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. [Bambach, Richard K.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. RP Melott, AL (reprint author), Univ Kansas, Dept Phys & Astron, Lawrence, KS 66045 USA. NR 30 TC 10 Z9 10 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 6 DI 10.1088/0004-637X/773/1/6 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900006 ER PT J AU Minh, YC Liu, HB Ho, PTP Hsieh, PY Su, YN Kim, SS Wright, M AF Minh, Young Chol Liu, Hauyu Baobab Ho, Paul T. P. Hsieh, Pei-Ying Su, Yu-Nung Kim, Sungsoo S. Wright, Melvyn TI GREEN BANK TELESCOPE OBSERVATIONS OF THE NH3 (3,3) AND (6,6) TRANSITIONS TOWARD SAGITTARIUS A MOLECULAR CLOUDS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; ISM: individual objects (Sgr A); ISM: molecules; radio lines: ISM ID GALACTIC-CENTER REGION; APERTURE SYNTHESIS OBSERVATIONS; A COMPLEX; CIRCUMNUCLEAR DISK; SGR-A; GAS; PARSECS; ENVIRONMENT; AMMONIA; MORPHOLOGY AB Ammonia (3, 3) and (6, 6) transitions have been observed using the Green Bank Telescope toward the Sgr A region. The gas is mainly concentrated in 50 km s(-1) and 20 km s(-1) clouds located in a plane inclined to the galactic plane. These "main" clouds appear to be virialized and influenced by the expansion of the supernova remnant Sgr A East. The observed emission shows very complicated features in the morphology and velocity structure. Gaussian multi-component fittings of the observed spectra revealed that various "streaming" gas components exist all over the observed region. These components include those previously known as "streamers" and "ridges," but most of these components appear not to be directly connected to the major gas condensations (the 50 km s(-1) and 20 km s(-1) clouds). They are apparently located out of the galactic plane, and they may have a different origin than the major gas condensations. Some of the streaming components are expected to be sources that feed the circumnuclear disk of our Galactic center directly and episodically. They may also evolve differently than major gas condensations under the influence of the activities of the Galactic center. C1 [Minh, Young Chol] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. [Liu, Hauyu Baobab; Ho, Paul T. P.; Hsieh, Pei-Ying; Su, Yu-Nung] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kim, Sungsoo S.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Kyungki Do, South Korea. [Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. RP Minh, YC (reprint author), Korea Astron & Space Sci Inst, Daeduk Daero 776, Taejon 305348, South Korea. RI Kim, Sungsoo/A-8601-2011 OI Kim, Sungsoo/0000-0002-5570-2160 FU Mid-career Research Program through the National Research Foundation (NRF) [2011-0016898]; Ministry of Education, Science, and Technology (MEST) of Korea FX We thank the GBT staff for their capable assistance in making these observations. S.S.K.'s work was supported by the Mid-career Research Program (No. 2011-0016898) through the National Research Foundation (NRF) grant funded by the Ministry of Education, Science, and Technology (MEST) of Korea. NR 37 TC 3 Z9 3 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 31 DI 10.1088/0004-637X/773/1/31 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900031 ER PT J AU Pepper, J Siverd, RJ Beatty, TG Gaudi, BS Stassun, KG Eastman, J Collins, K Latham, DW Bieryla, A Buchhave, LA Jensen, ELN Manner, M Penev, K Crepp, JR Cargile, PA Dhital, S Calkins, ML Esquerdo, GA Berlind, P Fulton, BJ Street, R Ma, B Ge, J Wang, J Mao, QQ Richert, AJW Gould, A Depoy, DL Kielkopf, JF Marshall, JL Pogge, RW Stefanik, RP Trueblood, M Trueblood, P AF Pepper, Joshua Siverd, Robert J. Beatty, Thomas G. Gaudi, B. Scott Stassun, Keivan G. Eastman, Jason Collins, Karen Latham, David W. Bieryla, Allyson Buchhave, Lars A. Jensen, Eric L. N. Manner, Mark Penev, Kaloyan Crepp, Justin R. Cargile, Phillip A. Dhital, Saurav Calkins, Michael L. Esquerdo, Gilbert A. Berlind, Perry Fulton, Benjamin J. Street, Rachel Ma, Bo Ge, Jian Wang, Ji Mao, Qingqing Richert, Alexander J. W. Gould, Andrew Depoy, Darren L. Kielkopf, John F. Marshall, Jennifer L. Pogge, Richard W. Stefanik, Robert P. Trueblood, Mark Trueblood, Patricia TI KELT-3b: A HOT JUPITER TRANSITING A V=9.8 LATE-F STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection ID IMAGE SUBTRACTION; SUPER-EARTH; GIANT STARS; SKY SURVEY; K-DWARF; STELLAR; PLANET; EXOPLANETS; EVOLUTION; MISSION AB We report the discovery of KELT-3b, a moderately inflated transiting hot Jupiter with a mass of 1.477(-0.067)(+0.066) M-J, radius of 1.345 +/- 0.072 R-J, and an orbital period of 2.7033904 +/- 0.000010 days. The host star, KELT-3, is a V = 9.8 late F star with M-* = 1.278(-0.061)(+0.063) M-circle dot, R-* = 1.472(-0.067)(+0.065) R-circle dot, T-eff = 6306(-49)(+50) K, log(g) = 4.209(-0.031)(+0.033), and [Fe/H] = 0.044(-0.082)(+0.080), and has a likely proper motion companion. KELT-3b is the third transiting exoplanet discovered by the KELT survey, and is orbiting one of the 20 brightest known transiting planet host stars, making it a promising candidate for detailed characterization studies. Although we infer that KELT-3 is significantly evolved, a preliminary analysis of the stellar and orbital evolution of the system suggests that the planet has likely always received a level of incident flux above the empirically identified threshold for radius inflation suggested by Demory & Seager. C1 [Pepper, Joshua] Lehigh Univ, Dept Phys, Bethlehem, PA 18015 USA. [Pepper, Joshua; Siverd, Robert J.; Stassun, Keivan G.; Cargile, Phillip A.; Dhital, Saurav; Mao, Qingqing] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Beatty, Thomas G.; Gaudi, B. Scott; Gould, Andrew; Pogge, Richard W.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Eastman, Jason; Fulton, Benjamin J.; Street, Rachel] Las Cumbres Observ Global Telescope Network, Santa Barbara, CA 93117 USA. [Eastman, Jason] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Collins, Karen; Kielkopf, John F.] Univ Louisville, Dept Phys & Astron, Louisville, KY 40292 USA. [Latham, David W.; Bieryla, Allyson; Calkins, Michael L.; Esquerdo, Gilbert A.; Berlind, Perry; Stefanik, Robert P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, Lars A.] Univ Copenhagen, Niels Bohr Inst, DK-21S00 Copenhagen, Denmark. [Buchhave, Lars A.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Jensen, Eric L. N.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Manner, Mark] Spot Observ, Nunnelly, TN 37137 USA. [Penev, Kaloyan] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Dhital, Saurav] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Fulton, Benjamin J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Ma, Bo; Ge, Jian] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Wang, Ji] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Richert, Alexander J. W.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Gould, Andrew; Pogge, Richard W.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. [Depoy, Darren L.; Marshall, Jennifer L.] Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA. [Trueblood, Mark; Trueblood, Patricia] Winer Observ, Sonoita, AZ 85637 USA. RP Pepper, J (reprint author), Lehigh Univ, Dept Phys, Bldg 16, Bethlehem, PA 18015 USA. RI Mao, Qingqing/E-2043-2016; OI Richert, Alexander/0000-0002-9613-6863; Penev, Kaloyan/0000-0003-4464-1371; Jensen, Eric/0000-0002-4625-7333; Buchhave, Lars A./0000-0003-1605-5666; Pepper, Joshua/0000-0002-3827-8417; Mao, Qingqing/0000-0001-6001-6723; Eastman, Jason/0000-0003-3773-5142 FU NASA [NNG04GO70G, NNX07AP14G]; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics; National Science Foundation's PREST program [AST-0721386]; National Science Foundation through PAARE Grant [AST-0849736]; National Science Foundation through AAG Grant [AST-1009810]; NASA Kentucky Space Grant Consortium Graduate Fellowship; NSF CAREER Grant [AST-1056524]; Kepler Mission [NNX11AB99A]; NSF [NSF AST-0705139]; UCF-UF SRI program; University of Florida FX We would like to thank additional collaborators on the KELT project, including Bruce Gary, Joao Gregorio, Roberto Zambelli, and KimMcLeod. We would also like to thank Leslie Hebb, Robert Emrich, and Martin Paegert for helpful discussions. Early work on KELT-North was supported by NASA Grant NNG04GO70G. J. A. P. and K. G. S. acknowledge support from the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics. E.L.N.J. gratefully acknowledges the support of the National Science Foundation's PREST program, which helped to establish the Peter van de Kamp Observatory through grant AST-0721386. K. G. S. acknowledges the support of the National Science Foundation through PAARE Grant AST-0849736 and AAG Grant AST-1009810. K. A. C. was supported by a NASA Kentucky Space Grant Consortium Graduate Fellowship. Work by B. S. G., J. D. E., and T. G. B. was partially supported by NSF CAREER Grant AST-1056524. The TRES and KeplerCam observations were obtained with partial support from the Kepler Mission through NASA Cooperative Agreement NNX11AB99A with the Smithsonian Astrophysical Observatory (PI: D. W. L.). The Byrne Observatory at Sedgwick (BOS) is operated by the Las Cumbres Observatory Global Telescope Network and is located at the Sedgwick Reserve, a part of the University of California Natural Reserve System. EXPERT construction and follow-up observations were funded by NSF with grant NSF AST-0705139, NASA with grants NNX07AP14G (Origins), UCF-UF SRI program, and the University of Florida. This work has made use of NASA's Astrophysics Data System, the Exo-planet Orbit Database at exoplanets. org, the Extrasolar Planet Encyclopedia at exoplanet. eu (Schneider et al. 2011), and the SIMBAD database operated at CDS, Strasbourg, France. NR 54 TC 18 Z9 18 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 AUG 10 PY 2013 VL 773 IS 1 AR 64 DI 10.1088/0004-637X/773/1/64 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900064 ER PT J AU Plotkin, RM Gallo, E Jonker, PG AF Plotkin, Richard. M. Gallo, Elena Jonker, Peter G. TI THE X-RAY SPECTRAL EVOLUTION OF GALACTIC BLACK HOLE X-RAY BINARIES TOWARD QUIESCENCE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; black hole physics; X-rays: binaries ID ADVECTION-DOMINATED ACCRETION; CANDIDATE XTE J1752-223; XMM-NEWTON OBSERVATIONS; BROAD-BAND SPECTRUM; NOVA-MUSCAE 1991; LOW-HARD STATE; GX 339-4; LOW/HARD STATE; RADIO-EMISSION; MULTIWAVELENGTH OBSERVATIONS AB Most transient black hole X-ray binaries (BHXBs) spend the bulk of their time in a quiescent state, where they accrete matter from their companion star at highly sub-Eddington luminosities (we define quiescence here as a normalized Eddington ratio l(x) = L0.5-10 keV/L-Edd < 10(-5)). Here, we present Chandra X-ray imaging spectroscopy for three BHXB systems (H 1743-322, MAXI J1659-152, and XTE J1752-223) as they fade into quiescence following an outburst. Multiple X-ray observations were taken within one month of each other, allowing us to track each individual system's X-ray spectral evolution during its decay. We compare these three systems to other BHXB systems. We confirm that quiescent BHXBs have softer X-ray spectra than low-hard-state BHXBs, and that quiescent BHXB spectral properties show no dependence on the binary system's orbital parameters. However, the observed anti-correlation between X-ray photon index (Gamma) and l(x) in the low-hard state does not continue once a BHXB enters quiescence. Instead, Gamma plateaus to an average = 2.08 +/- 0.07 by the time l(x) reaches similar to 10(-5). l(x) similar to 10(-5) is thus an observationally motivated upper limit for the beginning of the quiescent spectral state. Our results are discussed in the context of different accretion flow models and across the black hole mass scale. C1 [Plotkin, Richard. M.; Gallo, Elena] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Jonker, Peter G.] SRON, Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Jonker, Peter G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jonker, Peter G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. RP Plotkin, RM (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM rplotkin@umich.edu OI Plotkin, Richard/0000-0002-7092-0326 FU National Aeronautics and Space Administration through Chandra X-Ray Observatory Center [GO1-12049A]; National Aeronautics Space Administration [NAS8-03060]; Netherlands Organisation for Scientific Research FX We thank the anonymous referee for helpful comments that improved this manuscript. We also thank Stephane Corbel for discussions regarding GX 339-4. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Nos. GO1-12049A and GO1-12049A 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. G. J. acknowledges support from the Netherlands Organisation for Scientific Research. This research has made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog, and software provided by the Chandra X-Ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. NR 169 TC 43 Z9 43 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 59 DI 10.1088/0004-637X/773/1/59 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900059 ER PT J AU Poppenhaeger, K Schmitt, JHMM Wolk, SJ AF Poppenhaeger, K. Schmitt, J. H. M. M. Wolk, S. J. TI TRANSIT OBSERVATIONS OF THE HOT JUPITER HD 189733b AT X-RAY WAVELENGTHS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; planetary systems; stars: activity; stars: coronae; stars: individual (HD 189733); X-rays: stars ID HUBBLE-SPACE-TELESCOPE; EXTRASOLAR GIANT PLANETS; ATMOSPHERIC ESCAPE; MASS-LOSS; CHROMOSPHERIC ACTIVITY; TRANSMISSION SPECTRUM; ROTATION PERIOD; YOUNG STARS; HD-189733; SYSTEM AB We present new X-ray observations obtained with Chandra ACIS-S of the HD 189733 system, consisting of a K-type star orbited by a transiting Hot Jupiter and an M-type stellar companion. We report a detection of the planetary transit in soft X-rays with a significantly deeper transit depth than observed in the optical. The X-ray data favor a transit depth of 6%-8%, versus a broadband optical transit depth of 2.41%. While we are able to exclude several possible stellar origins for this deep transit, additional observations will be necessary to fully exclude the possibility that coronal inhomogeneities influence the result. From the available data, we interpret the deep X-ray transit to be caused by a thin outer planetary atmosphere which is transparent at optical wavelengths, but dense enough to be opaque to X-rays. The X-ray radius appears to be larger than the radius observed at far-UV wavelengths, most likely due to high temperatures in the outer atmosphere at which hydrogen is mostly ionized. We furthermore detect the stellar companion HD 189733B in X-rays for the first time with an X-ray luminosity of log L-X = 26.67 erg s(-1). We show that the magnetic activity level of the companion is at odds with the activity level observed for the planet-hosting primary. The discrepancy may be caused by tidal interaction between the Hot Jupiter and its host star. C1 [Poppenhaeger, K.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Poppenhaeger, K.; Schmitt, J. H. M. M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. RP Poppenhaeger, K (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM kpoppenhaeger@cfa.harvard.edu OI Poppenhaeger, Katja/0000-0003-1231-2194 NR 64 TC 31 Z9 31 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 62 DI 10.1088/0004-637X/773/1/62 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900062 ER PT J AU Ross, NP McGreer, ID White, M Richards, GT Myers, AD Palanque-Delabrouille, N Strauss, MA Anderson, SF Shen, Y Brandt, WN Yeche, C Swanson, MEC Aubourg, E Bailey, S Bizyaev, D Bovy, J Brewington, H Brinkmann, J DeGraf, C Di Matteo, T Ebelke, G Fan, XH Ge, J Malanushenko, E Malanushenko, V Mandelbaum, R Maraston, C Muna, D Oravetz, D Pan, K Paris, I Petitjean, P Schawinski, K Schlegel, DJ Schneider, DP Silverman, JD Simmons, A Snedden, S Streblyanska, A Suzuki, N Weinberg, DH York, D AF Ross, Nicholas P. McGreer, Ian D. White, Martin Richards, Gordon T. Myers, Adam D. Palanque-Delabrouille, Nathalie Strauss, Michael A. Anderson, Scott F. Shen, Yue Brandt, W. N. Yeche, Christophe Swanson, Molly E. C. Aubourg, Eric Bailey, Stephen Bizyaev, Dmitry Bovy, Jo Brewington, Howard Brinkmann, J. DeGraf, Colin Di Matteo, Tiziana Ebelke, Garrett Fan, Xiaohui Ge, Jian Malanushenko, Elena Malanushenko, Viktor Mandelbaum, Rachel Maraston, Claudia Muna, Demitri Oravetz, Daniel Pan, Kaike Paris, Isabelle Petitjean, Patrick Schawinski, Kevin Schlegel, David J. Schneider, Donald P. Silverman, John D. Simmons, Audrey Snedden, Stephanie Streblyanska, Alina Suzuki, Nao Weinberg, David H. York, Donald TI THE SDSS-III BARYON OSCILLATION SPECTROSCOPIC SURVEY: THE QUASAR LUMINOSITY FUNCTION FROM DATA RELEASE NINE SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology: observations; galaxies: active; galaxies: luminosity function, mass function; quasars: general; surveys ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLES; HIGH-REDSHIFT QUASARS; DEEP FIELD-SOUTH; SIMILAR-TO 4; SPECTRAL ENERGY-DISTRIBUTIONS; SURVEY PHOTOMETRIC SYSTEM; BROAD-LINE QUASARS; DARK-MATTER HALOES AB We present a new measurement of the optical quasar luminosity function (QLF), using data from the Sloan Digital Sky Survey-III: Baryon Oscillation Spectroscopic Survey (SDSS-III: BOSS). From the SDSS-III Data Release Nine, a uniform sample of 22,301 i less than or similar to 21.8 quasars are selected over an area of 2236 deg(2), with confirmed spectroscopic redshifts between 2.2 < z < 3.5, filling in a key part of the luminosity-redshift plane for optical quasar studies. The completeness of the survey is derived through simulated quasar photometry, and this completeness estimate is checked using a sample of quasars selected by their photometric variability within the BOSS footprint. We investigate the level of systematics associated with our quasar sample using the simulations, in the process generating color-redshift relations and a new quasar K-correction. We probe the faint end of the QLF to M-i (z = 2.2) approximate to -24.5 and see a clear break in the QLF at all redshifts up to z = 3.5. A log-linear relation (in log Phi* - M*) for a luminosity evolution and density evolution model is found to adequately describe our data within the range 2.2 < z < 3.5; across this interval the break luminosity increases by a factor of similar to 2.6 while Phi* declines by a factor of similar to 8. At z less than or similar to 2.2 our data are reasonably well fit by a pure luminosity evolution model, and only a weak signature of "AGN downsizing" is seen, in line with recent studies of the hard X-ray luminosity function. We compare our measured QLF to a number of theoretical models and find that models making a variety of assumptions about quasar triggering and halo occupation can fit our data over a wide range of redshifts and luminosities. C1 [Ross, Nicholas P.; White, Martin; Bailey, Stephen; Schlegel, David J.; Suzuki, Nao] Lawrence Berkeley Natl Lab, Berkeley, CA 92420 USA. [McGreer, Ian D.; Fan, Xiaohui] Steward Observ, Tucson, AZ 85721 USA. [White, Martin] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Richards, Gordon T.] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Richards, Gordon T.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Myers, Adam D.] Univ Wyoming, Dept Phys & Astron, Laramie, WY 82071 USA. [Palanque-Delabrouille, Nathalie; Yeche, Christophe] CEA, Ctr Saclay, IRFU, F-91191 Gif Sur Yvette, France. [Strauss, Michael A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Anderson, Scott F.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Shen, Yue; Swanson, Molly E. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brandt, W. N.; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. N.; Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Aubourg, Eric] Univ Paris Diderot, APC, CNRS IN2P3, CEA IRFU,Observ Paris,Sorbonne Paris Cite, Paris, France. [Bizyaev, Dmitry; Brewington, Howard; Brinkmann, J.; Ebelke, Garrett; Malanushenko, Elena; Malanushenko, Viktor; Oravetz, Daniel; Pan, Kaike; Simmons, Audrey; Snedden, Stephanie] Apache Point Observ, Sunspot, NM 88349 USA. [Bovy, Jo] Inst Adv Study, Princeton, NJ 08540 USA. [DeGraf, Colin; Di Matteo, Tiziana; Mandelbaum, Rachel] Carnegie Mellon Univ, McWilliams Ctr Cosmol, Pittsburgh, PA 15213 USA. [Ge, Jian] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Maraston, Claudia] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Muna, Demitri] NYU, Ctr Cosmol & Particle Phys, Dept Phys, New York, NY 10003 USA. [Paris, Isabelle; Petitjean, Patrick] UPMC, CNRS, Inst Astrophys Paris, UMR7095, F-75014 Paris, France. [Paris, Isabelle] Univ Chile, Dept Astron, Santiago, Chile. [Schawinski, Kevin] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Silverman, John D.] Univ Tokyo, IPMU, Kashiwa, Chiba 2778568, Japan. [Streblyanska, Alina] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, Ctr Cosmol & AstroParticle Phys, Columbus, OH 43210 USA. [York, Donald] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [York, Donald] Univ Chicago, Fermi Inst, Chicago, IL 60637 USA. RP Ross, NP (reprint author), Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 92420 USA. EM npross@lbl.gov RI Mandelbaum, Rachel/N-8955-2014; Di Matteo, Tiziana/O-4762-2014; White, Martin/I-3880-2015; Brandt, William/N-2844-2015; OI Mandelbaum, Rachel/0000-0003-2271-1527; Di Matteo, Tiziana/0000-0002-6462-5734; White, Martin/0000-0001-9912-5070; Brandt, William/0000-0002-0167-2453; Bovy, Jo/0000-0001-6855-442X; Schawinski, Kevin/0000-0001-5464-0888 FU Alfred P. Sloan Foundation; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; University of Portsmouth; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; National Science Foundation; U.S. Department of Energy Office of Science; David and Lucile Packard Fellowship; NSF [AST 08-06861, AST 11-07682]; Alexander von Humboldt Foundation at the Max-Planck-Institut fur Astronomie FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington, and Yale University.; N.P.R. warmly thanks Silvia Bonoli, Federico Marulli, Nikos Fanidakis and Phil Hopkins for providing their model QLF data in a prompt manner. Matt George, Genevieve Graves, Tom Shanks, Julie Wardlow and Gabor Worseck, also provided very useful discussions. Paul Hewett was key in the K-correction discussions. I. D. M. and X. F. acknowledge support from a David and Lucile Packard Fellowship, and NSF grants AST 08-06861 and AST 11-07682. G. T. R. acknowledges the generous support of a research fellowship from the Alexander von Humboldt Foundation at the Max-Planck-Institut fur Astronomie and is grateful for the hospitality of the Astronomisches Rechen-Institut and the Institute of Astronomy, Cambridge. NR 213 TC 68 Z9 68 U1 2 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 14 DI 10.1088/0004-637X/773/1/14 PG 27 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900014 ER PT J AU Torres, G Ruiz-Rodriguez, D Badenas, M Prato, L Schaefer, GH Wasserman, LH Mathieu, RD Latham, DW AF Torres, Guillermo Ruiz-Rodriguez, Dary Badenas, Mariona Prato, L. Schaefer, G. H. Wasserman, Lawrence H. Mathieu, Robert D. Latham, David W. TI THE QUADRUPLE PRE-MAIN-SEQUENCE SYSTEM LkCa 3: IMPLICATIONS FOR STELLAR EVOLUTION MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; binaries: spectroscopic; stars: individual (LkCa3); stars: pre-main sequence; stars: rotation; techniques: radial velocities ID T-TAURI STARS; LOW-MASS STARS; CLOSE BINARY-SYSTEMS; KECK II TELESCOPE; SPECTROSCOPIC BINARIES; VLBA DETERMINATION; FORMING REGIONS; BROWN DWARFS; GG TAURI; INTERSTELLAR EXTINCTION AB We report the discovery that the pre-main-sequence (PMS) object LkCa 3 in the Taurus-Auriga star-forming region is a hierarchical quadruple system of M stars. It was previously known to be a close (similar to 0.'' 5) visual pair, with one component being a moderately eccentric 12.94 day single-lined spectroscopic binary. A re-analysis of archival optical spectra complemented by new near-infrared (NIR) spectroscopy shows both visual components to be double lined; the second one has a period of 4.06 days and a circular orbit. In addition to the orbital elements, we determine optical and NIR flux ratios, effective temperatures, and projected rotational velocities for all four stars. Using existing photometric monitoring observations of the system that had previously revealed the rotational period of the primary in the longer-period binary, we also detect the rotational signal of the primary in the 4.06 day binary, which is synchronized with the orbital motion. With only the assumption of coevality, a comparison of all of these constraints with current stellar evolution models from the Dartmouth series points to an age of 1.4 Myr and a distance of 133 pc, consistent with previous estimates for the region and suggesting that the system is on the near side of the Taurus complex. Similar comparisons of the properties of LkCa 3 and the well-known quadruple PMS system GG Tau with the widely used models from the Lyon series for a mixing length parameter of alpha(ML) = 1.0 strongly favor the Dartmouth models. C1 [Torres, Guillermo; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ruiz-Rodriguez, Dary; Prato, L.; Wasserman, Lawrence H.] Lowell Observ, Flagstaff, AZ 86001 USA. [Badenas, Mariona] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Schaefer, G. H.] CHARA Array Georgia State Univ, Mt Wilson Observ, Mt Wilson, CA 91023 USA. [Mathieu, Robert D.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. RP Torres, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gtorres@cfa.harvard.edu FU NSF; W. M. Keck Foundation; NSF [AST-1007992, AST-1009136]; NASA Keck PI Data Award [2003B, 2004A] FX We thank the anonymous referee for interesting suggestions, as well as I. Baraffe and R. White for helpful exchanges about stellar evolution models. The spectroscopic observations at the CfA were obtained with the able assistance of P. Berlind, R. Davis, L. Hartmann, E. Horine, A. Milone, and J. Peters. We are grateful to R. Davis for maintaining the CfA echelle database over the years. We also thank C. Beichman for the opportunity to obtain an additional NIRSPEC spectrum on the night of UT 2010 November 22. We thank the staff at Keck Observatory for their superb support. Data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. L. P. acknowledges support from the NASA Keck PI Data Award administered by NExScI (semesters 2003B and 2004A). Keck telescope time was also granted by NOAO through the Telescope System Instrumentation Program (TSIP). TSIP was funded by the NSF. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We recognize the Hawaiian community for the opportunity to conduct these observations from the summit of Mauna Kea. This work was partially supported by NSF grants AST-1007992 to G. T. and AST-1009136 to L. P. The research has made use of NASA's Astrophysics Data System Abstract Service, and of the SIMBAD and VizieR databases, operated at the CDS, Strasbourg, France. NR 93 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 40 DI 10.1088/0004-637X/773/1/40 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900040 ER PT J AU Wilkes, BJ Kuraszkiewicz, J Haas, M Barthel, P Leipski, C Willner, SP Worrall, DM Birkinshaw, M Antonucci, R Ashby, MLN Chini, R Fazio, GG Lawrence, C Ogle, P Schulz, B AF Wilkes, Belinda J. Kuraszkiewicz, Joanna Haas, Martin Barthel, Peter Leipski, Christian Willner, S. P. Worrall, D. M. Birkinshaw, Mark Antonucci, Robert Ashby, M. L. N. Chini, Rolf Fazio, G. G. Lawrence, Charles Ogle, Patrick Schulz, Bernhard TI REVEALING THE HEAVILY OBSCURED ACTIVE GALACTIC NUCLEUS POPULATION OF HIGH-REDSHIFT 3CRR SOURCES WITH CHANDRA X-RAY OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE quasars: general; X-rays: galaxies ID COMPACT STEEP-SPECTRUM; XMM-NEWTON OBSERVATIONS; POWERFUL RADIO GALAXIES; DIGITAL SKY SURVEY; EXTRAGALACTIC LEGACY SURVEY; DUAL-FREQUENCY OBSERVATIONS; SUPERMASSIVE BLACK-HOLES; EXTENDED GROTH STRIP; SEYFERT 2 GALAXIES; DEEP FIELD SOUTH AB Chandra observations of a complete, flux-limited sample of 38 high-redshift (1 < z < 2), low-frequency-selected (and so unbiased in orientation) 3CRR radio sources are reported. The sample includes 21 quasars (=broad-line radio galaxies) and 17 narrow-line radio galaxies (NLRGs) with matched 178 MHz radio luminosity (log L-R(5 GHz) similar to 44-45). The quasars have high radio core fraction, high X-ray luminosities (log L-X similar to 45-46), and soft X-ray hardness ratios (HR similar to -0.5) indicating low obscuration. The NLRGs have lower core fraction, lower apparent X-ray luminosities (log L-X similar to 43-45), and mostly hard X-ray hardness ratios (HR > 0) indicating obscuration (N-H similar to 10(22)-10(24) cm(-2)). These properties and the correlation between obscuration and radio core fraction are consistent with orientation-dependent obscuration as in unification models. About half the NLRGs have soft X-ray hardness ratios and/or a high [O III] emission line to X-ray luminosity ratio suggesting obscuration by Compton thick (CT) material so that scattered nuclear or extended X-ray emission dominates (as in NGC 1068). The ratios of unobscured to Compton-thin (10(22) cm(-2) < N-H(int) < 1.5 x 10(24) cm(-2)) to CT (N-H(int) > 1.5 x 10(24) cm(-2)) is 2.5:1.4:1 in this high-luminosity, radio-selected sample. The obscured fraction is 0.5, higher than is typically reported for active galactic nuclei at comparable luminosities from multi-wavelength surveys (0.1-0.3). Assuming random nuclear orientation, the unobscured half-opening angle of the disk/wind/torus structure is similar to 60 degrees and the obscuring material covers 30 degrees, similar to 12 degrees of which is CT. The multi-wavelength properties reveal that many NLRGs have intrinsic absorption 10-1000x higher than indicated by their X-ray hardness ratios, and their true L-X values are similar to 10-100x larger than the hardness-ratio absorption corrections would indicate. C1 [Wilkes, Belinda J.; Kuraszkiewicz, Joanna; Willner, S. P.; Ashby, M. L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Haas, Martin; Chini, Rolf] Ruhr Univ Bochum, Astron Inst, D-44801 Bochum, Germany. [Barthel, Peter] Univ Groningen, Kapteyn Inst, NL-9747 AD Groningen, Netherlands. [Leipski, Christian] MPIA, D-69117 Heidelberg, Germany. [Worrall, D. M.; Birkinshaw, Mark] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Antonucci, Robert] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Chini, Rolf] Univ Catolica Norte, Inst Astron, Antofagasta, Chile. [Lawrence, Charles] JPL, Pasadena, CA 91109 USA. [Ogle, Patrick] CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Schulz, Bernhard] CALTECH, IPAC, Pasadena, CA 91125 USA. RP Wilkes, BJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI Wilkes, Belinda/0000-0003-1809-2364 FU National Aeronautics and Space Administration [G08-9106X, NAS8-03060]; Chandra X-Ray Center; Smithsonian Institution Endowment, Scholarly Studies Program [40488100HH0017] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number G08-9106X, by the Chandra X-Ray Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060 (Chandra X-Ray Center) and by the Smithsonian Institution Endowment, Scholarly Studies Program, fund 40488100HH0017. The scientific results in this article are based to a significant degree on observations made by the Chandra X-Ray Observatory (CXO). We thank Mark Avara and Margaret Yellen for their early work on this project. NR 161 TC 25 Z9 25 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 15 DI 10.1088/0004-637X/773/1/15 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900015 ER PT J AU Zeng, LZ Bennett, CL Chapman, NL Chuss, DT Jimenez-Serra, I Novak, G Vaillancourt, JE AF Zeng, Lingzhen Bennett, Charles L. Chapman, Nicholas L. Chuss, David T. Jimenez-Serra, Izaskun Novak, Giles Vaillancourt, John E. TI THE SUBMILLIMETER POLARIZATION SPECTRUM OF M17 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects (M17, NGC 6618); ISM: magnetic fields; polarization; submillimeter: ISM ID MAGNETIC-FIELDS; GRAIN ALIGNMENT; MOLECULAR CLOUDS; INFRARED POLARIZATION; INTERSTELLAR GRAINS; RADIATIVE TORQUES; GALACTIC CLOUDS; SHARC-II; EMISSION; ORION AB We present 450 mu m polarimetric observations of the M17 molecular cloud obtained with the SHARP polarimeter at the Caltech Submillimeter Observatory. Across the observed region, the magnetic field orientation is consistent with previous submillimeter and far-infrared polarization measurements. Our observations are centered on a region of the molecular cloud that has been compressed by stellar winds from a cluster of OB stars. We have compared these new data with previous 350 mu m polarimetry and find an anti-correlation between the 450 and 350 mu m polarization magnitude ratio and the ratio of 21 cm to 450 mu m intensity. The polarization ratio is lower near the east end of the studied region where the cloud is exposed to stellar winds and radiation. At the west end of the region, the polarization ratio is higher. We interpret the varying polarization spectrum as evidence supporting the radiative alignment torque model for grain alignment, implying higher alignment efficiency in the region that is exposed to a higher anisotropic radiation field. C1 [Zeng, Lingzhen; Jimenez-Serra, Izaskun] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Zeng, Lingzhen; Bennett, Charles L.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Chapman, Nicholas L.; Novak, Giles] Northwestern Univ, CIERA, Evanston, IL 60208 USA. [Chapman, Nicholas L.; Novak, Giles] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Chuss, David T.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Vaillancourt, John E.] NASA, Ames Res Ctr, SOFIA Sci Ctr, Univ Space Res Assoc, Moffett Field, CA 94035 USA. RP Zeng, LZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lingzhen@cfa.harvard.edu OI Vaillancourt, John/0000-0001-8916-1828; Zeng, Lingzhen/0000-0001-6924-9072 FU National Science Foundation [AST-0838261, AST-0909030] FX We thank C. Brogan for providing the 21 cm intensity data. We are grateful to A. Chepurnov, R. Hildebrand, and A. Lazarian for illuminating discussions. This material is based upon work at the Caltech Submillimeter Observatory, which is operated by the California Institute of Technology under cooperative agreement with the National Science Foundation (AST-0838261). We thank the National Science Foundation for supporting SHARP, via grant AST-0909030 to Northwestern University. NR 36 TC 3 Z9 3 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 10 PY 2013 VL 773 IS 1 AR 29 DI 10.1088/0004-637X/773/1/29 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 193BN UT WOS:000322531900029 ER PT J AU Qi, CH Oberg, KI Wilner, DJ D'Alessio, P Bergin, E Andrews, SM Blake, GA Hogerheijde, MR van Dishoeck, EF AF Qi, Chunhua Oeberg, Karin I. Wilner, David J. D'Alessio, Paola Bergin, Edwin Andrews, Sean M. Blake, Geoffrey A. Hogerheijde, Michiel R. van Dishoeck, Ewine F. TI Imaging of the CO Snow Line in a Solar Nebula Analog SO SCIENCE LA English DT Article ID PROTOPLANETARY DISKS; STAR-FORMATION; X-RAY; ICE; CHEMISTRY; MOLECULES; WATER; PLANETESIMALS; EVOLUTION; EMISSION AB Planets form in the disks around young stars. Their formation efficiency and composition are intimately linked to the protoplanetary disk locations of "snow lines" of abundant volatiles. We present chemical imaging of the carbon monoxide (CO) snow line in the disk around TW Hya, an analog of the solar nebula, using high spatial and spectral resolution Atacama Large Millimeter/Submillimeter Array observations of diazenylium (N2H+), a reactive ion present in large abundance only where CO is frozen out. The N2H+ emission is distributed in a large ring, with an inner radius that matches CO snow line model predictions. The extracted CO snow line radius of similar to 30 astronomical units helps to assess models of the formation dynamics of the solar system, when combined with measurements of the bulk composition of planets and comets. C1 [Qi, Chunhua; Wilner, David J.; Andrews, Sean M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oeberg, Karin I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Oeberg, Karin I.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [D'Alessio, Paola] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofis, Mexico City 58089, DF, Mexico. [Bergin, Edwin] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Blake, Geoffrey A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hogerheijde, Michiel R.; van Dishoeck, Ewine F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, Ewine F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP Qi, CH (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM cqi@cfa.harvard.edu FU NASA Origins of Solar Systems [NNX11AK63]; Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica-UNAM; NSF [1008800]; Smithsonian Institution; Academia Sinica; [2004-214] FX We are grateful to S. Schnee for data calibration and reduction assistance. C. Q. thanks the Smithsonian Astrophysical Observatory (SAO) Radio Telescope Data Center (RTDC) staff for their generous computational support. C. Q., K.I.O., and D.J.W. acknowledge grant NNX11AK63 from NASA Origins of Solar Systems. P. D. acknowledges a grant from Programa de Apoyo a Proyectos de Investigacion e Innovacion Tecnologica-UNAM. E. B. acknowledges support from NSF grant 1008800. This Report makes use of the following ALMA data: ADS JAO. ALMA#2011.0.00340.S. ALMA is a partnership of the European Southern Observatory (ESO) (representing its member states), NSF (USA), and the National Institute of Natural Sciences (Japan), together with the National Research Council (Canada) and the National Science Council and Academia Sinica's Institute of Astronomy and Astrophysics (ASIAA) (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, Associated Universities, Inc. (AUI)/National Radio Astronomy Observatory, and the National Astronomical Observatory of Japan. We also make use of the Submillimeter Array (SMA) data: project #2004-214 (principal investigator, C. Q.). The SMA is a joint project between SAO and ASIAA and is funded by the Smithsonian Institution and the Academia Sinica. NR 33 TC 75 Z9 75 U1 1 U2 21 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 AUG 9 PY 2013 VL 341 IS 6146 BP 630 EP 632 DI 10.1126/science.1239560 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 197XC UT WOS:000322884800031 PM 23868917 ER PT J AU Brown, C Burslem, DFRP Illian, JB Bao, L Brockelman, W Cao, M Chang, LW Dattaraja, HS Davies, S Gunatilleke, CVS Gunatilleke, IAUN Huang, J Kassim, AR LaFrankie, JV Lian, J Lin, L Ma, K Mi, X Nathalang, A Noor, S Ong, P Sukumar, R Su, SH Sun, IF Suresh, HS Tan, S Thompson, J Uriarte, M Valencia, R Yap, SL Ye, W Law, R AF Brown, C. Burslem, D. F. R. P. Illian, J. B. Bao, L. Brockelman, W. Cao, M. Chang, L. W. Dattaraja, H. S. Davies, S. Gunatilleke, C. V. S. Gunatilleke, I. A. U. N. Huang, J. Kassim, A. R. LaFrankie, J. V. Lian, J. Lin, L. Ma, K. Mi, X. Nathalang, A. Noor, S. Ong, P. Sukumar, R. Su, S. H. Sun, I. F. Suresh, H. S. Tan, S. Thompson, J. Uriarte, M. Valencia, R. Yap, S. L. Ye, W. Law, R. TI Multispecies coexistence of trees in tropical forests: spatial signals of topographic niche differentiation increase with environmental heterogeneity SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE species coexistence; tropical forest; niche differentiation; neutral theory; spatial pattern; cross-pair overlap distribution ID LANKAN DIPTEROCARP FOREST; HABITAT ASSOCIATIONS; SPECIES COEXISTENCE; BETA-DIVERSITY; ABUNDANCE; PATTERNS; COMMUNITIES; DISPERSAL; GRADIENTS; DISTRIBUTIONS AB Neutral and niche theories give contrasting explanations for the maintenance of tropical tree species diversity. Both have some empirical support, but methods to disentangle their effects have not yet been developed. We applied a statistical measure of spatial structure to data from 14 large tropical forest plots to test a prediction of niche theory that is incompatible with neutral theory: that species in heterogeneous environments should separate out in space according to their niche preferences. We chose plots across a range of topographic heterogeneity, and tested whether pairwise spatial associations among species were more variable in more heterogeneous sites. We found strong support for this prediction, based on a strong positive relationship between variance in the spatial structure of species pairs and topographic heterogeneity across sites. We interpret this pattern as evidence of pervasive niche differentiation, which increases in importance with increasing environmental heterogeneity. C1 [Brown, C.] Univ Edinburgh, Sch Geosci, Edinburgh EH8 9XP, Midlothian, Scotland. [Brown, C.; Illian, J. B.] Univ St Andrews, Sch Math & Stat, CREEM, St Andrews KY16 9LZ, Fife, Scotland. [Burslem, D. F. R. P.] Univ Aberdeen, Inst Biol & Environm Sci, Aberdeen AB24 3UU, Scotland. [Bao, L.; Ma, K.; Mi, X.] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Brockelman, W.; Nathalang, A.] BIOTEC Cent Res Unit, Ecol Lab, Klongluang 12120, Pathum Thani, Thailand. [Cao, M.; Lin, L.] Chinese Acad Sci, Xishuangbanna Trop Bot Garden, Key Lab Trop Forest Ecol, Kunming 650223, Peoples R China. [Chang, L. W.; Su, S. H.] Taiwan Forestry Res Inst, Taipei 10066, Taiwan. [Dattaraja, H. S.; Sukumar, R.; Suresh, H. S.] Indian Inst Sci, Ctr Ecol Sci, Bangalore 560012, Karnataka, India. [Davies, S.] Harvard Univ, Ctr Trop Forest Sci, Cambridge, MA 02138 USA. [Davies, S.] Smithsonian Trop Res Inst, Panama City, Panama. [Gunatilleke, C. V. S.; Gunatilleke, I. A. U. N.] Univ Peradeniya, Dept Bot, Peradeniya 20400, Sri Lanka. [Huang, J.; Lian, J.; Ye, W.] Chinese Acad Sci, South China Bot Garden, Guangzhou 510650, Guangdong, Peoples R China. [Kassim, A. R.; Noor, S.] Forest Res Inst Malaysia, Div Forest Environm, Forest Ecol Unit, Kuala Lumpur 52109, Malaysia. [LaFrankie, J. V.; Ong, P.; Yap, S. L.] Univ Philippines Diliman, Inst Biol, Quezon City, Philippines. [Sun, I. F.] Natl Dong Hwa Univ, Dept Nat Resources & Environm Studies, Hualien 974, Taiwan. [Tan, S.] Forest Dept Sarawak, Kuching 93660, Sarawak, Malaysia. [Thompson, J.] Univ Puerto Rico, Inst Trop Ecosyst Studies, Luquillo, PR 00773 USA. [Thompson, J.] Ctr Ecol & Hydrol, Penicuik EH26 0QB, Midlothian, Scotland. [Uriarte, M.] Columbia Univ, New York, NY 10027 USA. [Valencia, R.] Pontifical Catholic Univ Ecuador, Sch Biol Sci, Plant Ecol Lab, Quito, Ecuador. [Law, R.] Univ York, York Ctr Complex Syst Anal, York YO10 5EG, N Yorkshire, England. [Law, R.] Univ York, Dept Biol, York YO10 5EG, N Yorkshire, England. RP Brown, C (reprint author), Univ Edinburgh, Sch Geosci, Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland. EM calum.brown@ed.ac.uk RI Uriarte, Maria/L-8944-2013; Thompson, Jill/K-2200-2012; Brown, Calum/D-4341-2017; OI Thompson, Jill/0000-0002-4370-2593; Brown, Calum/0000-0001-9331-1008; Burslem, David/0000-0001-6033-0990 FU Microsoft FX The CTFS plots were individually supported from a number of sources, details of which are given in the electronic supplementary material, text S2. C.B. was financially supported by a Microsoft PhD Scholarship. NR 56 TC 20 Z9 21 U1 5 U2 103 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 AUG 7 PY 2013 VL 280 IS 1764 AR 20130502 DI 10.1098/rspb.2013.0502 PG 8 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 167RA UT WOS:000320649400002 PM 23782876 ER PT J AU Okie, JG Boyer, AG Brown, JH Costa, DP Ernest, SKM Evans, AR Fortelius, M Gittleman, JL Hamilton, MJ Harding, LE Lintulaakso, K Lyons, SK Saarinen, JJ Smith, FA Stephens, PR Theodor, J Uhen, MD Sibly, RM AF Okie, Jordan G. Boyer, Alison G. Brown, James H. Costa, Daniel P. Ernest, S. K. Morgan Evans, Alistair R. Fortelius, Mikael Gittleman, John L. Hamilton, Marcus J. Harding, Larisa E. Lintulaakso, Kari Lyons, S. Kathleen Saarinen, Juha J. Smith, Felisa A. Stephens, Patrick R. Theodor, Jessica Uhen, Mark D. Sibly, Richard M. TI Effects of allometry, productivity and lifestyle on rates and limits of body size evolution SO PROCEEDINGS OF THE ROYAL SOCIETY B-BIOLOGICAL SCIENCES LA English DT Article DE slow-fast life-history continuum; evolutionary rate; metabolic theory of ecology; maximum body size; macroecology; mammal macroevolution ID MOLECULAR CLOCK; METABOLIC-RATE; COPES RULE; HISTORY; MAMMALS; TIME; TEMPERATURE; DYNAMICS; PATTERNS; RESPONSES AB Body size affects nearly all aspects of organismal biology, so it is important to understand the constraints and dynamics of body size evolution. Despite empirical work on the macroevolution and macroecology of minimum and maximum size, there is little general quantitative theory on rates and limits of body size evolution. We present a general theory that integrates individual productivity, the lifestyle component of the slow-fast life-history continuum, and the allometric scaling of generation time to predict a clade's evolutionary rate and asymptotic maximum body size, and the shape of macroevolutionary trajectories during diversifying phases of size evolution. We evaluate this theory using data on the evolution of clade maximum body sizes in mammals during the Cenozoic. As predicted, clade evolutionary rates and asymptotic maximum sizes are larger in more productive clades (e.g. baleen whales), which represent the fast end of the slow-fast lifestyle continuum, and smaller in less productive clades (e.g. primates). The allometric scaling exponent for generation time fundamentally alters the shape of evolutionary trajectories, so allometric effects should be accounted for in models of phenotypic evolution and interpretations of macroevolutionary body size patterns. This work highlights the intimate interplay between the macroecological and macroevolutionary dynamics underlying the generation and maintenance of morphological diversity. C1 [Okie, Jordan G.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Okie, Jordan G.; Brown, James H.; Hamilton, Marcus J.; Harding, Larisa E.; Smith, Felisa A.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Boyer, Alison G.] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN USA. [Brown, James H.; Hamilton, Marcus J.] Santa Fe Inst, Santa Fe, NM 87501 USA. [Costa, Daniel P.] Univ Calif Santa Cruz, Dept Ecol & Evolutionary Biol, Santa Cruz, CA 95064 USA. [Ernest, S. K. Morgan] Utah State Univ, Dept Biol, Logan, UT 84322 USA. [Ernest, S. K. Morgan] Utah State Univ, Ctr Ecol, Logan, UT 84322 USA. [Evans, Alistair R.] Monash Univ, Sch Biol Sci, Melbourne, Vic 3004, Australia. [Evans, Alistair R.] Museum Victoria, Melbourne, Vic, Australia. [Fortelius, Mikael; Lintulaakso, Kari; Saarinen, Juha J.] Univ Helsinki, Dept Geosci & Geog, Helsinki, Finland. [Gittleman, John L.; Stephens, Patrick R.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Hamilton, Marcus J.] Univ New Mexico, Dept Anthropol, Albuquerque, NM 87131 USA. [Lyons, S. Kathleen] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Theodor, Jessica] Univ Calgary, Dept Biol Sci, Calgary, AB T2N 1N4, Canada. [Uhen, Mark D.] George Mason Univ, Dept Atmospher Ocean & Earth Sci, Fairfax, VA 22030 USA. [Sibly, Richard M.] Univ Reading, Sch Biol Sci, Reading, Berks, England. RP Okie, JG (reprint author), Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. EM jordan.okie@asu.edu RI Evans, Alistair/D-4239-2011; Ernest, SK Morgan/O-2532-2015; OI Evans, Alistair/0000-0002-4078-4693; Ernest, SK Morgan/0000-0002-6026-8530; Sibly, Richard/0000-0001-6828-3543; Lintulaakso, Kari/0000-0001-9627-8821; Fortelius, Mikael/0000-0002-4851-783X FU National Science Foundation Grant Integrating Macroecological Pattern and Processes across Scales Research Coordination Network [DEB 0541625]; University of New Mexico's Program in Interdisciplinary Biological and Biomedical Sciences; Howard Hughes Medical Institute under the National Institute of Biomedical Imaging and Bioengineering Interfaces Initiative; Arizona State University's School of Earth and Space Exploration; National Aeronautics and Space Administration; NASA Astrobiology Institute FX We thank Chris Venditti, P. David Polly and an anonymous reviewer for helpful feedback. This study was supported by National Science Foundation Grant Integrating Macroecological Pattern and Processes across Scales Research Coordination Network DEB 0541625 (to F.A.S., S.K.L. and S.K.M.E., principal investigators). Financial support to J. Okie was provided by University of New Mexico's Program in Interdisciplinary Biological and Biomedical Sciences, which is funded by the Howard Hughes Medical Institute under the National Institute of Biomedical Imaging and Bioengineering Interfaces Initiative; an Exploration Postdoctoral Fellowship from Arizona State University's School of Earth and Space Exploration; and a Postdoctoral Fellowship from the National Aeronautics and Space Administration Postdoctoral Program with the NASA Astrobiology Institute, which is administered by Oak Ridge Associated Universities. This paper is IMPPS RCN publication no. 19. NR 56 TC 5 Z9 5 U1 6 U2 112 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 AUG 7 PY 2013 VL 280 IS 1764 AR 20131007 DI 10.1098/rspb.2013.1007 PG 7 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 167RA UT WOS:000320649400011 PM 23760865 ER PT J AU Petaev, MI Huang, SC Jacobsen, SB Zindler, A AF Petaev, Michail I. Huang, Shichun Jacobsen, Stein B. Zindler, Alan TI Large Pt anomaly in the Greenland ice core points to a cataclysm at the onset of Younger Dryas SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE meteorite impact; climate change; ICP-MS analysis; PGE ID PLATINUM-GROUP ELEMENTS; IMPACT; ACCUMULATION; CIRCULATION; ACCRETION; VOLCANISM; IRIDIUM; SHEET; MELT AB One explanation of the abrupt cooling episode known as the Younger Dryas (YD) is a cosmic impact or airburst at the YD boundary (YDB) that triggered cooling and resulted in other calamities, including the disappearance of the Clovis culture and the extinction of many large mammal species. We tested the YDB impact hypothesis by analyzing ice samples from the Greenland Ice Sheet Project 2 (GISP2) ice core across the Bolling-Allerod/YD boundary for major and trace elements. We found a large Pt anomaly at the YDB, not accompanied by a prominent Ir anomaly, with the Pt/Ir ratios at the Pt peak exceeding those in known terrestrial and extraterrestrial materials. Whereas the highly fractionated Pt/Ir ratio rules out mantle or chondritic sources of the Pt anomaly, it does not allow positive identification of the source. Circumstantial evidence such as very high, superchondritic Pt/Al ratios associated with the Pt anomaly and its timing, different from other major events recorded on the GISP2 ice core such as well-understood sulfate spikes caused by volcanic activity and the ammonium and nitrate spike due to the biomass destruction, hints for an extraterrestrial source of Pt. Such a source could have been a highly differentiated object like an Ir-poor iron meteorite that is unlikely to result in an airburst or trigger wide wildfires proposed by the YDB impact hypothesis. C1 [Petaev, Michail I.; Huang, Shichun; Jacobsen, Stein B.; Zindler, Alan] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Petaev, Michail I.] Harvard Smithsonian Ctr Astrophys, Div Solar Stellar & Planetary Sci, Cambridge, MA 02138 USA. RP Petaev, MI (reprint author), Harvard Univ, Dept Earth & Planetary Sci, 20 Oxford St, Cambridge, MA 02138 USA. EM mpetaev@fas.harvard.edu RI Huang, Shichun/A-3596-2008; Jacobsen, Stein/B-1759-2013 FU National Science Foundation [AGS-1007367] FX We thank Prof. Wally Broecker for encouraging this study, Dr. Mark S. Twickler for providing the GISP2 ice samples, and Dr. Robert P. Ackert for inspiring discussions. We also thank H. J. Melosh and two anonymous reviewers for helpful reviews. This work was supported by National Science Foundation Grant AGS-1007367 (to S.B.J.). NR 30 TC 18 Z9 18 U1 5 U2 43 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 AUG 6 PY 2013 VL 110 IS 32 BP 12917 EP 12920 DI 10.1073/pnas.1303924110 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 196JQ UT WOS:000322771100030 PM 23878232 ER PT J AU Schneps, MH Thomson, JM Sonnert, G Pomplun, M Chen, C Heffner-Wong, A AF Schneps, Matthew H. Thomson, Jenny M. Sonnert, Gerhard Pomplun, Marc Chen, Chen Heffner-Wong, Amanda TI Shorter Lines Facilitate Reading in Those Who Struggle SO PLOS ONE LA English DT Article ID DEVELOPMENTAL DYSLEXIA; EYE-MOVEMENTS; VISUAL-ATTENTION; LEFT MININEGLECT; FIXATED WORD; CHILDREN; INFORMATION; SLUGGISH; READERS; ADULTS AB People with dyslexia, who ordinarily struggle to read, sometimes remark that reading is easier when e-readers are used. Here, we used eye tracking to observe high school students with dyslexia as they read using these devices. Among the factors investigated, we found that reading using a small device resulted in substantial benefits, improving reading speeds by 27%, reducing the number of fixations by 11%, and importantly, reducing the number of regressive saccades by more than a factor of 2, with no cost to comprehension. Given that an expected trade-off between horizontal and vertical regression was not observed when line lengths were altered, we speculate that these effects occur because sluggish attention spreads perception to the left as the gaze shifts during reading. Short lines eliminate crowded text to the left, reducing regression. The effects of attention modulation by the hand, and of increased letter spacing to reduce crowding, were also found to modulate the oculomotor dynamics in reading, but whether these factors resulted in benefits or costs depended on characteristics, such as visual attention span, that varied within our sample. C1 [Schneps, Matthew H.; Sonnert, Gerhard; Chen, Chen; Heffner-Wong, Amanda] Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, Cambridge, MA 02138 USA. [Thomson, Jenny M.; Chen, Chen] Harvard Univ, Grad Sch Educ, Cambridge, MA 02138 USA. [Pomplun, Marc] Univ Massachusetts, Dept Comp Sci, Boston, MA 02125 USA. RP Schneps, MH (reprint author), Harvard Smithsonian Ctr Astrophys, Sci Educ Dept, 60 Garden St, Cambridge, MA 02138 USA. EM mschneps@cfa.harvard.edu OI Thomson, Jenny/0000-0002-4293-4851 FU National Science Foundation [HRD-0930962, HRD-1131039]; Youth Access Grant program at the Smithsonian Institution FX This article is based on work supported by the National Science Foundation under Grants No. HRD-0930962 and HRD-1131039, and the Youth Access Grant program at the Smithsonian Institution. Data are archived at the Harvard IQSS Dataverse Network, http://hdl.handle.net/10904/10244. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 71 TC 13 Z9 13 U1 3 U2 32 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD AUG 5 PY 2013 VL 8 IS 8 AR e71161 DI 10.1371/journal.pone.0071161 PG 16 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 218XC UT WOS:000324465000186 PM 23940709 ER PT J AU Blaimer, BB Fisher, BL AF Blaimer, Bonnie B. Fisher, Brian L. TI Taxonomy of the Crematogaster degeeri-species-assemblage in the Malagasy region (Hymenoptera: Formicidae) SO EUROPEAN JOURNAL OF TAXONOMY LA English DT Article AB We revise the species-level taxonomy of the Crematogaster (Crematogaster) degeeri-species-assemblage, a group of related ants occuring in Madagascar and the wider Malagasy region, and further provide an identification key to all species-groups of the genus Crematogaster in this region. Within the C. degeeri-assemblage, we recognize twelve species based upon morphological data from worker, queen and male ants, as well as genetic data from the barcode region of cytochrome oxidase I. Seven new species are described: Crematogaster alafara Blaimer sp. nov., C. bara Blaimer sp. nov., C. mafybe Blaimer sp. nov., C. maina Blaimer sp. nov., C. malahelo Blaimer sp. nov., C. masokely Blaimer sp. nov., C. ramamy Blaimer sp. nov. Crematogaster tricolor Gerstacker, 1859 (stat. rev.) and C. dentata Dalla Torre, 1893 (stat. nov.) are raised to species level, and the following new synonymies are proposed: Crematogaster degeeri lunaris Santschi, 1928 as a synonym of C. degeeri Forel, 1886; Crematogaster sewelli improba Forel, 1907 and C. sewelli mauritiana Forel, 1907 as synonyms of C. dentata Dalla Torre, 1893, and C. pacifica Santschi, 1919 as a synonym of C. lobata Emery, 1895. Species descriptions, images, and distribution maps and identification keys based on worker ants, as well as on queen ants where available, are presented for all twelve species. In addition, we present a molecular gene tree for cytochrome oxidase I and summarize levels of sequence divergence within and between species of the C. degeeri-species-assemblage. Our findings are discussed in the light of previous work on Malagasy Crematogaster ants. C1 [Blaimer, Bonnie B.] Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. RP Blaimer, BB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol, Washington, DC 20560 USA. EM bonnieblaimer@gmail.com NR 0 TC 1 Z9 1 U1 0 U2 2 PU MUSEUM NATL HISTOIRE NATURELLE PI PARIS PA SERVICE PUBLICATIONS SCIENTIFIQUES, 57 RUE CUVIER, 75005 PARIS, FRANCE SN 2118-9773 J9 EUR J TAXON JI Eur. J. Taxon. PD AUG 2 PY 2013 VL 51 BP 1 EP 64 DI 10.5852/ejt.2013.51 PG 64 WC Zoology SC Zoology GA 213EQ UT WOS:000324037900001 ER PT J AU de Carvalho-Sobrinho, JG de Queiroz, LP Dorr, LJ AF de Carvalho-Sobrinho, Jefferson G. de Queiroz, Luciano P. Dorr, Laurence J. TI Does Pseudobombax have prickles? Assessing the enigmatic species Pseudobombax endecaphyllum (Malvaceae: Bombacoideae) SO TAXON LA English DT Editorial Material DE Bombacaceae; Bombax; Jacaratia; Pachira; taxonomy; typification; Vellozo AB In order to better understand the taxonomy of the enigmatic Pseudobombax endecaphyllum (Vell.) A.Robyns (Malvaceae: Bombacoideae), the only species in this genus thought to have aculeate branches, we reexamined the protologues of B. endecaphyllum and Pachira decaphylla A.St.-Hil. & Naudin, the latter a name long considered to be a synonym of the former, and discovered a great deal of taxonomic confusion. We conclude that B. endecaphyllum does not belong in Pseudobombax, Pachira decaphylla was based on a mixture of elements from two plant families, and the relationship between B. endecaphyllum and Pachira decaphylla is specious. It becomes evident that B. endecaphyllum is the earliest name available for Pachira stenopetala Casar. and the new combination Pachira endecaphylla (Vell.) Carv.-Sobr. is effected. An epitype is designated for B. endecaphyllum and a lectotype is designated for Pachira decaphylla, which becomes a synonym of Pseudobombax grandiflorum var. majus A. Robyns. Most importantly, we now consider that all species of Pseudo bombax are unarmed. C1 [de Carvalho-Sobrinho, Jefferson G.; de Queiroz, Luciano P.] Univ Estadual Feira de Santana, Herbario HUEFS, BR-44036900 Feira De Santana, BA, Brazil. [Dorr, Laurence J.] Smithsonian Inst, Dept Bot, Washington, DC 20013 USA. RP de Carvalho-Sobrinho, JG (reprint author), Univ Estadual Feira de Santana, Herbario HUEFS, Ave Univ S-N, BR-44036900 Feira De Santana, BA, Brazil. EM jef.sobrinho@gmail.com RI Carvalho-Sobrinho, Jefferson/E-1480-2012; de Queiroz, Luciano Paganucci/I-1378-2012 OI Carvalho-Sobrinho, Jefferson/0000-0003-3605-0707; de Queiroz, Luciano Paganucci/0000-0001-7436-0939 NR 11 TC 1 Z9 1 U1 0 U2 3 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 EI 1996-8175 J9 TAXON JI Taxon PD AUG PY 2013 VL 62 IS 4 BP 814 EP 818 PG 5 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA AG0RV UT WOS:000335124200015 ER PT J AU Yotsu-Yamashita, M Abe, Y Kudo, Y Ritson-Williams, R Paul, VJ Konoki, K Cho, Y Adachi, M Imazu, T Nishikawa, T Isobe, M AF Yotsu-Yamashita, Mari Abe, Yuka Kudo, Yuta Ritson-Williams, Raphael Paul, Valerie J. Konoki, Keiichi Cho, Yuko Adachi, Masaatsu Imazu, Takuya Nishikawa, Toshio Isobe, Minoru TI First Identification of 5,11-Dideoxytetrodotoxin in Marine Animals, and Characterization of Major Fragment Ions of Tetrodotoxin and Its Analogs by High Resolution ESI-MS/MS SO MARINE DRUGS LA English DT Article DE tetrodotoxin; LC-MS/MS; 5,11-dideoxytetrodotoxin; biosynthesis ID INTRAMUSCULARLY ADMINISTERED TETRODOTOXIN; PUFFER AROTHRON-NIGROPUNCTATUS; IONIZATION MASS-SPECTROMETRY; FUGU-POECILONOTUS; TAKIFUGU-RUBRIPES; TRANSFER PROFILE; STEREOCONTROLLED SYNTHESIS; STRUCTURAL ASSIGNMENT; ATERGATIS-FLORIDUS; CYNOPS-ENSICAUDA AB Even though tetrodotoxin (TTX) is a widespread toxin in marine and terrestrial organisms, very little is known about the biosynthetic pathway used to produce it. By describing chemical structures of natural analogs of TTX, we can start to identify some of the precursors that might be important for TTX biosynthesis. In the present study, an analog of TTX, 5,11-dideoxyTTX, was identified for the first time in natural sources, the ovary of the pufferfish and the pharynx of a flatworm (planocerid sp. 1), by comparison with totally synthesized (-)-5,11-dideoxyTTX, using high resolution ESI-LC-MS. Based on the presence of 5,11-dideoxyTTX together with a series of known deoxy analogs, 5,6, 11-trideoxyTTX, 6,11-dideoxyTTX, 11-deoxyTTX, and 5-deoxyTTX, in these animals, we predicted two routes of stepwise oxidation pathways in the late stages of biosynthesis of TTX. Furthermore, high resolution masses of the major fragment ions of TTX, 6,11-dideoxyTTX, and 5,6,11-trideoxyTTX were also measured, and their molecular formulas and structures were predicted to compare them with each other. Although both TTX and 5,6,11-trideoxyTTX give major fragment ions that are very close, m/z 162.0660 and 162.1020, respectively, they are distinguishable and predicted to be different molecular formulas. These data will be useful for identification of TTXs using high resolution LC-MS/MS. C1 [Yotsu-Yamashita, Mari; Abe, Yuka; Kudo, Yuta; Konoki, Keiichi; Cho, Yuko] Tohoku Univ, Grad Sch Agr Sci, Sendai, Miyagi 9818555, Japan. [Ritson-Williams, Raphael] Univ Hawaii Manoa, Dept Biol, Honolulu, HI 96822 USA. [Paul, Valerie J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Adachi, Masaatsu; Imazu, Takuya; Nishikawa, Toshio] Nagoya Univ, Grad Sch Bioagr Sci, Chikusa Ku, Nagoya, Aichi 4648601, Japan. [Isobe, Minoru] Natl Tsing Hua Univ, Dept Chem, Hsinchu 30013, Taiwan. RP Yotsu-Yamashita, M (reprint author), Tohoku Univ, Grad Sch Agr Sci, Sendai, Miyagi 9818555, Japan. EM myama@biochem.tohoku.ac.jp; y.abe.woodstock@gmail.com; b3ad1305@s.tohoku.ac.jp; rrw33@hawaii.edu; Paul@si.edu; konoki@m.tohoku.ac.jp; choyuko@m.tohoku.ac.jp; madachi@agr.nagoya-u.ac.jp; imazu.takuya@b.mbox.nagoya-u.ac.jp; nisikawa@agr.nagoya-u.ac.jp; minoru@mx.nthu.edu.tw RI Konoki, Keiichi/O-9600-2014 FU Japan Society for the Promotion of Science (JSPS) [LS012]; JSPS [25-5534] FX This work was funded by the Japan Society for the Promotion of Science (JSPS), through its Funding Program for the Next Generation World-Leading Researchers (LS012) to M.Y.Y. Y.K. is grateful for financial support from JSPS Predoctoral fellowships for Young Scientists (no. 25-5534). NR 50 TC 16 Z9 17 U1 1 U2 22 PU MDPI AG PI BASEL PA POSTFACH, CH-4005 BASEL, SWITZERLAND SN 1660-3397 J9 MAR DRUGS JI Mar. Drugs PD AUG PY 2013 VL 11 IS 8 BP 2799 EP 2813 DI 10.3390/md11082799 PG 15 WC Chemistry, Medicinal SC Pharmacology & Pharmacy GA 301GR UT WOS:000330521300008 PM 23924959 ER PT J AU Hodgkison, R Ayasse, M Haberlein, C Schulz, S Zubaid, A Mustapha, WAW Kunz, TH Kalko, EKV AF Hodgkison, Robert Ayasse, Manfred Haeberlein, Christopher Schulz, Stefan Zubaid, Akbar Mustapha, Wan Aida W. Kunz, Thomas H. Kalko, Elisabeth K. V. TI Fruit bats and bat fruits: the evolution of fruit scent in relation to the foraging behaviour of bats in the New and Old World tropics SO FUNCTIONAL ECOLOGY LA English DT Article DE chemical ecology; Chiroptera; co-evolution; foraging behaviour; olfaction; Phyllostomidae; Pteropodidae; scent; seed dispersal syndromes; terpenes ID LOWLAND RAIN-FOREST; EATING BATS; CAROLLIA-PERSPICILLATA; MOLECULAR PHYLOGENY; CHEMICAL ECOLOGY; DISPERSAL AGENTS; SEED DISPERSERS; FICUS MORACEAE; FIGS; ECHOLOCATION AB 1. Frugivory among bats (Chiroptera) has evolved independently in the New and Old World tropics: within the families Phyllostomidae and Pteropodidae, respectively. Bats from both families rely primarily on olfaction for the location of fruits. However, the influence of bats on the evolution of fruit scent is almost completely unknown. 2. Using the genus Ficus as a model, the aims of this study were to explore the chemical composition of fruit scent in relation to two contrasting seed dispersal syndromes in Panama and Malaysia and to assess the influence of fruit scent on the foraging behaviour of neo- and palaeotropical fruit-eating bats (Artibeus jamaicensis and Cynopterus brachyotis, respectively). Two hypotheses were tested: (i) variation in fruit scent, between bat-and bird-dispersed figs, is independent of phylogeny and (ii) Old and New World fruit bats, which have evolved independently in each hemisphere, share the same olfactory preferences with respect to fruit scent. 3. The fruit scents of bat-and bird-dispersed fig species were sampled in the field, using dynamic headspace adsorption techniques. New and Old World fruit bats were then captured and tested on natural fig fruit scents from both hemispheres. 4. Chemical analyses, using gas chromatography (GC) and GC/mass spectrometry (MS), revealed a broad overlap in scent compounds between bat-dispersed fig species from both hemispheres. Their fruit scents were dominated by monoterpenes, which contrary to phylogenetic predictions, were completely absent from bird-dispersed species from both regions. 5. The fruit scents of bat-dispersed figs were highly attractive to neotropical bats (A. jamaicensis) in behavioural experiments, whereas those of bird-dispersed figs were completely rejected. Neotropical bats (A. jamaicensis) exhibited a significant preference for fig fruit scents dominated by monoterpenes, independent of the geographical origin of the scent. Palaeotropical bats (C. brachyotis), by contrast, rejected monoterpene-rich fruit scents from the Neotropics. 6. In a cluster analysis (which included additional, published data from the literature), the fruit scents of bat-dispersed figs were clumped by subgenus, with the exception of palaeotropical figs of the subgenus Sycomorus. C. brachyotis, from Malaysia, was the only fruit bat species that significantly preferred the fruit scents of Sycomorus figs that contained no monoterpenes. C1 [Hodgkison, Robert; Ayasse, Manfred; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. [Hodgkison, Robert; Kunz, Thomas H.] Boston Univ, Ctr Ecol & Conservat Biol, Boston, MA 02215 USA. [Haeberlein, Christopher; Schulz, Stefan] Tech Univ Carolo Wilhelmina Braunschweig, Inst Organ Chem, Braunschweig, Germany. [Zubaid, Akbar; Mustapha, Wan Aida W.] Univ Kebangsaan Malaysia, Pusat Pengajian Sains Sekitaran dan Sumber Alam, Bangi 43600, Malaysia. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. RP Hodgkison, R (reprint author), Univ Ulm, Inst Expt Ecol, D-89069 Ulm, Germany. EM rhodgkison@hotmail.com FU Smithsonian Tropical Research Institute (Panama); Lubee Bat Conservancy; Deutsche Forschungsgemeinschaft (DFG, Germany) [KA 124 8-1]; MOHE-UKMTOPDOWN [ST08FRGS00032010]; MOA [050102SF1041] FX We thank the Smithsonian Tropical Research Institute (Panama) for their support throughout this study and for extending their hospitality to Sharon Balding and Felix Hodgkison. We also thank the Department of Wildlife and National Parks (Malaysia) and the Economic Planning Unit of the Prime Minister's Department (Malaysia) for granting us permission to work in Malaysia. Finally, we gratefully acknowledge the valuable contributions of the following individuals: Ahmad Bin Dagu, for field assistance and logistical support in Malaysia; Sonja Gaessler, Larissa Albrecht and Katrin Petschl, for field assistance on BCI; Allen Herre, Adalberto Gomez, Nelida Gomez and Charlotte Jander, for sharing their knowledge of figs on BCI; Konstans Wells, for sharing information on small mammals in S. E. Asia; and Ingrid Dillon and Andrea Weiss, for administrative support and laboratory assistance at Ulm University. This research adhered to the Association of Animal Behaviour Guidelines for the Use of Animals in Research as well as the Smithsonian Tropical Research Institute's Protocol for the Humane Use of Live Vertebrates. We gratefully acknowledge the valuable contributions of three anonymous referees. The project was funded by a grant from the Lubee Bat Conservancy to THK and RH and by funds from the Deutsche Forschungsgemeinschaft (DFG, Germany) to EKVK and MA (KA 124 8-1). AZ and WAWM were funded by MOHE-UKMTOPDOWN (Grant No. ST08FRGS00032010) and MOA (Grant No. 050102SF1041). NR 60 TC 11 Z9 11 U1 11 U2 63 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0269-8463 EI 1365-2435 J9 FUNCT ECOL JI Funct. Ecol. PD AUG PY 2013 VL 27 IS 4 SI SI BP 1075 EP 1084 DI 10.1111/1365-2435.12101 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 284GK UT WOS:000329303900024 ER PT J AU Merot, C Mavarez, J Evin, A Dasmahapatra, KK Mallet, J Lamas, G Joron, M AF Merot, Claire Mavarez, Jesus Evin, Allowen Dasmahapatra, Kanchon K. Mallet, James Lamas, Gerardo Joron, Mathieu TI Genetic differentiation without mimicry shift in a pair of hybridizing Heliconius species (Lepidoptera: Nymphalidae) SO BIOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE geometric morphometrics; hybridization; multilocus genotype; reproductive isolation; speciation; wing shape ID POPULATION-STRUCTURE; MELPOMENE LINNAEUS; GENOMIC DIVERGENCE; CLADISTIC-ANALYSIS; MULLERIAN MIMICRY; SEXUAL SELECTION; MATE PREFERENCE; WARNING-COLOR; BUTTERFLIES; SPECIATION AB Butterflies in the genus Heliconius have undergone rapid adaptive radiation for warning patterns and mimicry, and are excellent models to study the mechanisms underlying diversification. In Heliconius, mimicry rings typically involve distantly related species, whereas closely related species often join different mimicry rings. Genetic and behavioural studies have n how reproductive isolation in many pairs of Heliconius taxa is largely mediated by natural and sexual selection on wing colour patterns. However, recent studies have uncovered new cases in which pairs of closely related species are near-perfect mimics of each other. Here, we provide morphometric and genetic evidence for the coexistence of two closely related, hybridizing co-mimetic species on the eastern slopes of the Andes, H.melpomene amaryllis and H.timaretassp. nov., which is described here as H.timareta thelxinoe. A joint analysis of multilocus genotyping and geometric morphometrics of wing shape shows a high level of differentiation between the two species, with only limited gene flow and mixing. Some degree of genetic mixing can be detected, but putative hybrids were rare, only one of 175 specimens being a clear hybrid. In contrast, we found phenotypic differentiation between populations of H.timareta thelxinoe, possibly indicative of strong selection for local mimicry in different communities. In this pair of species, the absence of breakdown of genetic isolation despite near-identical wing patterns implies that factors other than wing patterns keep the two taxa apart, such as chemical or behavioural signals, or ecological adaptation along a strong altitudinal gradient.(c) 2013 The Linnean Society of London, Biological Journal of the Linnean Society, 2013, 109, 830-847. C1 [Merot, Claire; Joron, Mathieu] Museum Natl Hist Nat, UMR CNRS 7205, F-75005 Paris, France. [Mavarez, Jesus] Univ Grenoble 1, LECA, F-38041 Grenoble, France. [Mavarez, Jesus] Smithsonian Trop Res Inst, Balboa, Panama. [Evin, Allowen] Univ Aberdeen, Dept Archaeol, Aberdeen AB24 3UF, Scotland. [Evin, Allowen] Museum Natl Hist Nat, UMR CNRS 7209, F-75005 Paris, France. [Dasmahapatra, Kanchon K.] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England. [Dasmahapatra, Kanchon K.; Mallet, James] UCL, Dept Genet Evolut & Environm, London WC1E 6BT, England. [Mallet, James] Harvard Univ, Dept Organism & Evolutionary Biol, Cambridge, MA 02138 USA. [Lamas, Gerardo] Univ Nacl Mayor San Marcos, Museo Hist Nat, Lima 14, Peru. RP Joron, M (reprint author), Museum Natl Hist Nat, UMR CNRS 7205, 45 Rue Buffon, F-75005 Paris, France. EM joron@mnhn.fr RI mallet, james/B-5114-2008; OI EVIN, Allowen/0000-0003-4515-1649; Lamas, Gerardo/0000-0002-3664-6730 FU URKU Estudios Amazonicos; CNRS ATIP grant; ERC FX We thank Benigno Calderon, Nicolas Chazot, Jae-Woo Chung, Mathieu Chouteau, Stephanie Galluser, Melanie McClure, Owen McMillan, Jerome Murienne, Ronald Mori Pezo, Joel Pintado, Lisa de Silva, Armando Silva Vasquez, Fraser Simpson, Cesar Ramirez and Neil Rosser for their help at various stages of fieldwork, and URKU Estudios Amazonicos for their support in Tarapoto. We thank the Ministerio de la Agricultura (ex-INRENA), the SERNANP-Bosque de Proteccion Alto Mayo and PEHCBM-Area de Conservacion Regional Cordillera Escalera for collection and export permits. We are very grateful to Chris Jiggins, Richard Merrill and Blanca Huertas for access to specimens and wings, Michel Baylac for the latest version of Rmorph and Neil Rosser for maps. We thank Marianne Elias and three anonymous reviewers for constructive and helpful comments on the manuscript. Molecular work was carried out at the Service de Systematique Moleculaire du Museum National d'Histoire Naturelle (CNRS - UMS 2700) and at the BoEM laboratory. This work was supported by a CNRS ATIP grant and an ERC Starting Grant (MimEvol) to MJ. NR 79 TC 16 Z9 16 U1 2 U2 34 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 AUG PY 2013 VL 109 IS 4 BP 830 EP 847 DI 10.1111/bij.12091 PG 18 WC Evolutionary Biology SC Evolutionary Biology GA 279JR UT WOS:000328956800008 ER PT J AU Fares, S Vargas, R Detto, M Goldstein, AH Karlik, J Paoletti, E Vitale, M AF Fares, Silvano Vargas, Rodrigo Detto, Matteo Goldstein, Allen H. Karlik, John Paoletti, Elena Vitale, Marcello TI Tropospheric ozone reduces carbon assimilation in trees: estimates from analysis of continuous flux measurements SO GLOBAL CHANGE BIOLOGY LA English DT Article DE citrus; gross primary productivity; Mediterranean forest; ozone concentration; ozone damage; Pinus ponderosa; stomatal deposition ID OPEN-TOP CHAMBERS; STOMATAL CONDUCTANCE; MULTISCALE ANALYSIS; SIERRA-NEVADA; NORWAY SPRUCE; WATER-STRESS; FOREST TREES; EXPOSURE; CO2; PHOTOSYNTHESIS AB High ground-level ozone concentrations are typical of Mediterranean climates. Plant exposure to this oxidant is known to reduce carbon assimilation. Ozone damage has been traditionally measured through manipulative experiments that do not consider long-term exposure and propagate large uncertainty by up-scaling leaf-level observations to ecosystem-level interpretations. We analyzed long-term continuous measurements (>9 site-years at 30min resolution) of environmental and eco-physiological parameters at three Mediterranean ecosystems: (i) forest site dominated by Pinus ponderosa in the Sierra Mountains in California, USA; (ii) forest site composed of a mixture of Quercus spp. and P. pinea in the Tyrrhenian sea coast near Rome, Italy; and (iii) orchard site of Citrus sinensis cultivated in the California Central Valley, USA. We hypothesized that higher levels of ozone concentration in the atmosphere result in a decrease in carbon assimilation by trees under field conditions. This hypothesis was tested using time series analysis such as wavelet coherence and spectral Granger causality, and complemented with multivariate linear and nonlinear statistical analyses. We found that reduction in carbon assimilation was more related to stomatal ozone deposition than to ozone concentration. The negative effects of ozone occurred within a day of exposure/uptake. Decoupling between carbon assimilation and stomatal aperture increased with the amount of ozone pollution. Up to 12-19% of the carbon assimilation reduction in P. ponderosa and in the Citrus plantation was explained by higher stomatal ozone deposition. In contrast, the Italian site did not show reductions in gross primary productivity either by ozone concentration or stomatal ozone deposition, mainly due to the lower ozone concentrations in the periurban site over the shorter period of investigation. These results highlight the importance of plant adaptation/sensitivity under field conditions, and the importance of continuous long-term measurements to explain ozone damage to real-world forests and calculate metrics for ozone-risk assessment. C1 [Fares, Silvano] Res Ctr Soil Plant Syst, Consiglio Ric & Sperimentaz Agr CRA, I-00184 Rome, Italy. [Vargas, Rodrigo] Univ Delaware, Delaware Environm Inst, Dept Plant & Soil Sci, Newark, DE 19716 USA. [Detto, Matteo] Smithsonian Trop Res Inst, Dpo, AA 34002 USA. [Goldstein, Allen H.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Paoletti, Elena] Inst Plant Protect, Natl Res Council, I-50019 Florence, Italy. [Vitale, Marcello] Univ Roma La Sapienza, Dept Environm Biol, I-00185 Rome, Italy. RP Fares, S (reprint author), Res Ctr Soil Plant Syst, Consiglio Ric & Sperimentaz Agr CRA, Via Navicella 2-4, I-00184 Rome, Italy. EM silvano.fares@entecra.it RI Goldstein, Allen/A-6857-2011; Fares, Silvano/H-4322-2011; Paoletti, Elena/B-8974-2009; Vargas, Rodrigo/C-4720-2008; OI Goldstein, Allen/0000-0003-4014-4896; Fares, Silvano/0000-0002-1990-0928; Paoletti, Elena/0000-0001-5324-7769; Vargas, Rodrigo/0000-0001-6829-5333; Vitale, Marcello/0000-0002-3652-7029 FU Kearney Foundation of Soil Science; University of California Agricultural Experiment Station; Office of Science, Biological and Environmental Research Program (BER), U.S. Department of Energy, through the Western Regional Center of the National Institute for Global Environmental Change (NIGEC) [DEFCO2-03ER63613]; Citrus Research Board; California Air Resources Board; European Commission FX The research in Blodgett was made possible by grants from the Kearney Foundation of Soil Science, the University of California Agricultural Experiment Station and the Office of Science, Biological and Environmental Research Program (BER), U.S. Department of Energy, through the Western Regional Center of the National Institute for Global Environmental Change (NIGEC) under Cooperative Agreement No. DEFCO2-03ER63613. We gratefully acknowledge Dr. Megan McKay for helping to collect the data.; The research in Lindcove was made possible by grants from the Citrus Research Board, the California Air Resources Board, and by the European Commission Marie Curie IOF 2008 project CITROVOC. We gratefully acknowledge Dr. Robin Weber for helping to collect the data. NR 56 TC 35 Z9 35 U1 3 U2 62 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD AUG PY 2013 VL 19 IS 8 BP 2427 EP 2443 DI 10.1111/gcb.12222 PG 17 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 276IV UT WOS:000328744900011 PM 23589473 ER PT J AU Tait, KT Hawthorne, FC Wise, MA AF Tait, Kimberly T. Hawthorne, Frank C. Wise, Michael A. TI THE CRYSTAL CHEMISTRY OF THE GRAFTONITE-BEUSITE MINERALS SO CANADIAN MINERALOGIST LA English DT Article DE Graftonite; beusite; crystal-structure refinement; electron-microprobe data ID YELLOWKNIFE PEGMATITE FIELD; GRANITIC PEGMATITE; NORTHWEST-TERRITORIES; PHOSPHATE MINERALS; SITE POPULATIONS; IRON-METEORITES; SOLID-SOLUTIONS; TRIPHYLITE; INTERGROWTHS; ASSOCIATIONS AB The crystal structures of seven members of the graftonite-beusite series, ideally (Fe2+,Mn2+,Ca)(3)(PO4)(2), monoclinic P2(1)/c, a 8.77-8.81, b 11.43-11.58, c 6.13-6.17 angstrom, beta 99.19-99.32 degrees, V 607.5-617.7 angstrom(3), have been refined to R-1 indices of 2.1-3.7% using similar to 1300-1600 unique observed reflections (vertical bar F-o vertical bar > 5 sigma F) collected using a single-crystal diffractometer equipped with MoK alpha X-radiation. The crystals used in the collection of the X-ray data were subsequently analyzed with an electron microprobe and the structural and microprobe results were used to assign site populations. The refined site-scattering values and linear variation in mean bond-length as a function of aggregate-cation radius indicate that Ca is completely ordered at the M(1) site. Similarly, Mn is ordered at the M(1) and M(3) sites, with any excess Mn occurring at M(2), and Mg is completely ordered at M(2). Detailed consideration of incident bond-valence sums at the three M sites indicates that the coordination numbers of the M(1), M(2), and M(3) sites are [8], [5], and [6], respectively, although the differences between these and [7], [5], and [5] are very small. Ca is dominant at the M(1) site in a previously refined beusite structure, and there are compositions reported here and elsewhere in which Ca is dominant at M(1) in graftonite-like compositions, indicating the potential for new mineral species in this group. C1 [Tait, Kimberly T.; Hawthorne, Frank C.] Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. [Wise, Michael A.] Smithsonian Inst, Dept Mineral Sci, Washington, DC 20560 USA. RP Hawthorne, FC (reprint author), Univ Manitoba, Dept Geol Sci, Winnipeg, MB R3T 2N2, Canada. EM frank_hawthome@umanitoba.ca RI Hawthorne, Frank/F-6864-2011 OI Hawthorne, Frank/0000-0001-6405-9931 FU Canada Research Chair in Crystallography and Mineralogy; Natural Sciences and Engineering Research Council of Canada (NSERC); NSERC FX We thank John Hughes and an anonymous reviewer for their comments on this paper. This work was supported by a Canada Research Chair in Crystallography and Mineralogy, and Research Tools and Equipment, Major Facilities Access and Discovery Grants from the Natural Sciences and Engineering Research Council of Canada (NSERC) to FCH, and an NSERC Discovery Grant to KTT. NR 33 TC 2 Z9 2 U1 0 U2 4 PU MINERALOGICAL ASSOC CANADA PI QUEBEC PA 490, RUE DE LA COURONNE, QUEBEC, QC G1K 9A9, CANADA SN 0008-4476 EI 1499-1276 J9 CAN MINERAL JI Can. Mineral. PD AUG PY 2013 VL 51 IS 4 BP 653 EP 662 DI 10.3749/canmin.51.4.653 PG 10 WC Mineralogy SC Mineralogy GA 266GA UT WOS:000328010200009 ER PT J AU Launius, RD AF Launius, Roger D. TI Pursuit of Power: NASA's Propulsion Systems Laboratory No. 1 and 2 SO PUBLIC HISTORIAN LA English DT Book Review C1 [Launius, Roger D.] 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 1 TC 0 Z9 0 U1 0 U2 0 PU UNIV CALIFORNIA PRESS PI BERKELEY PA C/O JOURNALS & DIGITAL PUBLISHING DIVISION, 2000 CENTER ST, STE 303, BERKELEY, CA 94704-1223 USA SN 0272-3433 J9 PUBL HISTORIAN JI Public Hist. PD AUG PY 2013 VL 35 IS 3 BP 112 EP 113 PG 2 WC History SC History GA 243JN UT WOS:000326312800012 ER PT J AU Errmann, R Neuhauser, R Marschall, L Torres, G Mugrauer, M Chen, WP Hu, SCL Briceno, C Chini, R Bukowiecki, L Dimitrov, DP Kjurkchieva, D Jensen, ELN Cohen, DH Wu, ZY Pribulla, T Vanko, M Krushevska, V Budaj, J Oasa, Y Pandey, AK Fernandez, M Kellerer, A Marka, C AF Errmann, R. Neuhaeuser, R. Marschall, L. Torres, G. Mugrauer, M. Chen, W. P. Hu, S. C. -L. Briceno, C. Chini, R. Bukowiecki, L. Dimitrov, D. P. Kjurkchieva, D. Jensen, E. L. N. Cohen, D. H. Wu, Z. -Y. Pribulla, T. Vanko, M. Krushevska, V. Budaj, J. Oasa, Y. Pandey, A. K. Fernandez, M. Kellerer, A. Marka, C. TI The stellar content of the young open cluster Trumpler 37 SO ASTRONOMISCHE NACHRICHTEN LA English DT Article DE open clusters and associations: individual (Trumpler 37) ID INTERMEDIATE-MASS STARS; SOLAR-TYPE STARS; CEPHEUS OB2; RESOLUTION SPECTROSCOPY; DISK EVOLUTION; TAURUS-AURIGA; ACCRETION; VARIABILITY; EMISSION AB With an apparent cluster diameter of 1.5 degrees and an age of 4 Myr, Trumpler 37 is an ideal target for photometric monitoring of young stars as well as for the search of planetary transits, eclipsing binaries and other sources of variability. The YETI consortium has monitored Trumpler 37 throughout 2010 and 2011 to obtain a comprehensive view of variable phenomena in this region. In this first paper we present the cluster properties and membership determination as derived from an extensive investigation of the literature. We also compared the coordinate list to some YETI images. For 1872 stars we found literature data. Among them 774 have high probability of being member and 125 a medium probability. Based on infrared data we re-calculate a cluster extinction of 0.9-1.2 mag. We can confirm the age and distance to be 3-5 Myr and870 pc. Stellar masses are determined from theoretical models and the mass function is fitted with a power-law index of = 1.90 (0.1-0.4 M) and = 1.12 (1-10 M). ((c) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) C1 [Errmann, R.; Neuhaeuser, R.; Mugrauer, M.; Marka, C.] Inst Astrophys, D-07745 Jena, Germany. [Errmann, R.; Neuhaeuser, R.; Mugrauer, M.; Marka, C.] Univ Sternwarte Jena, D-07745 Jena, Germany. [Marschall, L.] Gettysburg Coll Observ, Dept Phys, Gettysburg, PA 17325 USA. [Torres, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chen, W. P.; Hu, S. C. -L.] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan. [Hu, S. C. -L.] Taipei Astron Museum, Taipei 11160, Taiwan. [Briceno, C.] Ctr Invest Astron, Merida 5101, Venezuela. [Chini, R.] Ruhr Univ Bochum, Astronom Inst, D-44801 Bochum, Germany. [Chini, R.] Univ Catolica Norte, Inst Astronom, Antofagasta, Chile. [Bukowiecki, L.] Nicholas Copernicus Univ, Torun Ctr Astron, PL-87100 Torun, Poland. [Dimitrov, D. P.] Bulg Acad Sci, Inst Astron, Sofia 1784, Bulgaria. [Dimitrov, D. P.] Bulg Acad Sci, NAO, Sofia 1784, Bulgaria. [Kjurkchieva, D.] Univ Shumen, Shumen 9700, Bulgaria. [Jensen, E. L. N.; Cohen, D. H.] Swarthmore Coll, Dept Phys & Astron, Swarthmore, PA 19081 USA. [Wu, Z. -Y.] Chinese Acad Sci, NAO, Key Lab Opt Astron, Beijing 100012, Peoples R China. [Pribulla, T.; Vanko, M.; Budaj, J.] Slovak Acad Sci, Astron Inst, Tatranska Lomnica, Slovakia. [Krushevska, V.] Natl Acad Sci Ukraine, Main Astron Observ, UA-03680 Kiev, Ukraine. [Oasa, Y.] Saitama Univ, Dept Astron & Earth Sci, Sakura, Saitama 3388570, Japan. [Pandey, A. K.] Aryabhatta Res Inst Observat Sci, Naini Tal 263129, Uttarakhand, India. [Fernandez, M.] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Kellerer, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Errmann, R (reprint author), Inst Astrophys, Schillergasschen 2-3, D-07745 Jena, Germany. EM ronny.errmann@uni-jena.de RI Dimitrov, Dinko/J-7682-2013; OI Jensen, Eric/0000-0002-4625-7333 FU National Aeronautics and Space Administration; National Science Foundation; DFG [SPP 1385, NE 515 / 34-1, MU2695/13-1]; Abbe-School of Photonics; Thuringian government [B 515-07010]; Bulgarian Scientific Foundation [DO 02-85, DDVU 02/40-2010]; National Science Foundation's PREST program [AST-0721386]; [APVV-0158-11]; [2/0094/11] FX This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This research has made use of the WEBDA database, operated at the Institute for Astronomy of the University of Vienna. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France.; RN and RE would like to thank DFG for support in the Priority Programme SPP 1385 on the "First Ten Million Years of the Solar System" in project NE 515 / 34-1. RE also thanks the Abbe-School of Photonics for support. We would like to acknowledge financial support from the Thuringian government (B 515-07010) for the STK CCD camera used in this project. TP, MV and JB thank for the support to the projects APVV-0158-11 and VEGA 2/0094/11. MM acknowledges DFG for support in program MU2695/13-1. The research was supported partly by funds of projects DO 02-85 and DDVU 02/40-2010 of the Bulgarian Scientific Foundation. E.L.N.J. and D. H. C. gratefully acknowledge the support of the National Science Foundation's PREST program, which helped to establish the Peter van de Kamp Observatory through grant AST-0721386, and of the Provost's Office of Swarthmore College for their support maintaining and operating the observatory. NR 33 TC 4 Z9 4 U1 0 U2 4 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA BOSCHSTRASSE 12, D-69469 WEINHEIM, GERMANY SN 0004-6337 EI 1521-3994 J9 ASTRON NACHR JI Astro. Nachr. PD AUG PY 2013 VL 334 IS 7 BP 673 EP 681 DI 10.1002/asna.201311890 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 237IS UT WOS:000325863500009 ER PT J AU Kita, NT Yin, QZ MacPherson, GJ Ushikubo, T Jacobsen, B Nagashima, K Kurahashi, E Krot, AN Jacobsen, SB AF Kita, Noriko T. Yin, Qing-Zhu MacPherson, Glenn J. Ushikubo, Takayuki Jacobsen, Benjamin Nagashima, Kazuhide Kurahashi, Erika Krot, Alexander N. Jacobsen, Stein B. TI 26Al-26Mg isotope systematics of the first solids in the early solar system SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID ALUMINUM-RICH INCLUSIONS; REFRACTORY INCLUSIONS; CARBONACEOUS-CHONDRITE; AL-26-MG-26 SYSTEMATICS; INITIAL AL-26/AL-27; HETEROGENEOUS DISTRIBUTION; CONTEMPORANEOUS FORMATION; CA,AL-RICH INCLUSIONS; PROTOPLANETARY DISKS; ALLENDE METEORITE AB High-precision bulk aluminum-magnesium isotope measurements of calcium-aluminum-rich inclusions (CAIs) from CV carbonaceous chondrites in several laboratories define a bulk 26Al-26Mg isochron with an inferred initial 26Al/27Al ratio of approximately 5.25x10-5, named the canonical ratio. Nonigneous CV CAIs yield well-defined internal 26Al-26Mg isochrons consistent with the canonical value. These observations indicate that the canonical 26Al/27Al ratio records initial Al/Mg fractionation by evaporation and condensation in the CV CAI-forming region. The internal isochrons of igneous CV CAIs show a range of inferred initial 26Al/27Al ratios, (4.2-5.2)x10-5, indicating that CAI melting continued for at least 0.2Ma after formation of their precursors. A similar range of initial 26Al/27Al ratios is also obtained from the internal isochrons of many CAIs (igneous and nonigneous) in other groups of carbonaceous chondrites. Some CAIs and refractory grains (corundum and hibonite) from unmetamorphosed or weakly metamorphosed chondrites, including CVs, are significantly depleted in 26Al. At least some of these refractory objects may have formed prior to injection of 26Al into the protosolar molecular cloud and its subsequent homogenization in the protoplanetary disk. Bulk aluminum and magnesium-isotope measurements of various types of chondrites plot along the bulk CV CAI isochron, suggesting homogeneous distribution of 26Al and magnesium isotopes in the protoplanetary disk after an epoch of CAI formation. The inferred initial 26Al/27Al ratios of chondrules indicate that most chondrules formed 1-3Ma after CAIs with the canonical 26Al/27Al ratio. C1 [Kita, Noriko T.; Ushikubo, Takayuki] Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. [MacPherson, Glenn J.] Smithsonian Inst, US Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Jacobsen, Benjamin] Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. [Nagashima, Kazuhide; Krot, Alexander N.] Univ Hawaii Manoa, Sch Ocean Earth Sci & Technol, Hawaii Inst Geophys & Planetol, Honolulu, HI 96822 USA. [Kurahashi, Erika] Univ Munster, Inst Mineral, D-48149 Munster, Germany. [Jacobsen, Stein B.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. RP Kita, NT (reprint author), Univ Wisconsin, Dept Geosci, WiscSIMS, Madison, WI 53706 USA. EM noriko@geology.wisc.edu RI Yin, Qing-Zhu/B-8198-2009; Kita, Noriko/H-8035-2016 OI Yin, Qing-Zhu/0000-0002-4445-5096; Kita, Noriko/0000-0002-0204-0765 FU NASA [NNX09AB88G, NNX11AJ51G, NNX11AD43G, NNX11 AK82G, NNX10AH76G]; UC Laboratory Fees Research Program [12_LR-237921] FX The authors acknowledge the organizing committee of the Workshop on "Formation of the First Solid in the Solar System" for the opportunity of this article. The constructive comments by Joel Baker and James Connelly and the careful handling by associate editor Edward Scott improved clarity of the manuscript significantly. This work is supported by NASA programs (NNX09AB88G, NK; NNX11AJ51G, QZY; NNX11AD43G, GJM; NNX11 AK82G, SBJ; NNX10AH76G, ANK) and UC Laboratory Fees Research Program 12_LR-237921 to QZY. NR 99 TC 40 Z9 40 U1 1 U2 28 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 AUG PY 2013 VL 48 IS 8 BP 1383 EP 1400 DI 10.1111/maps.12141 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237KC UT WOS:000325867500002 ER PT J AU Bullock, ES Knight, KB Richter, FM Kita, NT Ushikubo, T MacPherson, GJ Davis, AM Mendybaev, RA AF Bullock, Emma S. Knight, Kim B. Richter, Frank M. Kita, Noriko T. Ushikubo, Takayuki MacPherson, Glenn J. Davis, Andrew M. Mendybaev, Ruslan A. TI Mg and Si isotopic fractionation patterns in types B1 and B2 CAIs: Implications for formation under different nebular conditions SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID AL-RICH INCLUSIONS; REFRACTORY INCLUSIONS; CRYSTALLIZATION SEQUENCES; ALLENDE METEORITE; MELILITE; CONDENSATION; EVAPORATION; LIQUIDS; CHONDRITES; EVOLUTION AB Magnesium and silicon isotopic profiles across melilite grains in two type B1 and two type B2 calcium-aluminum-rich inclusions (CAIs) reveal differing but constant enrichments in heavy isotopes everywhere except 1000m from the CAI margins. There is no close correlation in the B1s or the B2s between isotopic composition and akermanite content of the melilite, a measure of progressive igneous crystallization, yet such a correlation might be expected in a type B2: without a melilite mantle (as in B1s) to seal the interior off and prevent further evaporation, the melt would have maintained communication with the external gas. These observations indicate a model in which B1s and B2s solidified under differing conditions. The B2s solidified under lower hydrogen pressures (PH210-4-10-5 bars) than did B1s (PH2>10-4 bars), so surface volatilization was slower in the B2s and internal chemical and isotopic equilibrium was maintained over the interval of melilite crystallization. The outermost zones of the CAIs (1000m from the edge) are not consistently enriched in heavy isotopes relative to the interiors, as might be expected from diffusion-limited surface evaporation of the melt. In all cases, the magnesium in the CAI margins is lighter than in the interiors. In one case, silicon in the margin also is lighter, but locally in some CAIs, it is isotopically heavier near the surface. If melt evaporation played a role in the formation of these outer zones, a later event in many cases caused isotopic re-equilibration with an external and isotopically near-normal reservoir. C1 [Bullock, Emma S.; MacPherson, Glenn J.] Smithsonian Inst, US Natl Museum Nat Hist, Washington, DC 20560 USA. [Knight, Kim B.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Richter, Frank M.; Davis, Andrew M.; Mendybaev, Ruslan A.] Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. [Kita, Noriko T.; Ushikubo, Takayuki] Univ Wisconsin, Dept Geosci, Madison, WI 53706 USA. [Davis, Andrew M.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. RP Bullock, ES (reprint author), Smithsonian Inst, US Natl Museum Nat Hist, Washington, DC 20560 USA. EM bullockE@si.edu RI Kita, Noriko/H-8035-2016; OI Kita, Noriko/0000-0002-0204-0765; Davis, Andrew/0000-0001-7955-6236 FU NASA [NNX09AG39G, NNX09AB88G, NNX11AD43G, NNX09AG38G]; NSF [EAR03-19230, EAR07-44079] FX The manuscript was greatly improved by careful and thoughtful reviews by Drs. Christine Floss (Assoc. Ed.), Yunbin Guan, Julie Paque, and Steve Simon. This work was supported by NASA grants NNX09AG39G (A. M. D., PI), NNX09AB88G (N. K., PI), NNX11AD43G (G. J. M., PI), and NNX09AG38G (F. R., PI). WiscSIMS is partly supported by NSF (EAR03-19230, EAR07-44079). NR 34 TC 7 Z9 7 U1 2 U2 15 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 AUG PY 2013 VL 48 IS 8 BP 1440 EP 1458 DI 10.1111/maps.12158 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237KC UT WOS:000325867500006 ER PT J AU MacPherson, GJ Andronicos, CL Bindi, L Distler, VV Eddy, MP Eiler, JM Guan, YB Hollister, LS Kostin, A Kryachko, V Steinhardt, WM Yudovskaya, M Steinhardt, PJ AF MacPherson, Glenn J. Andronicos, Christopher L. Bindi, Luca Distler, Vadim V. Eddy, Michael P. Eiler, John M. Guan, Yunbin Hollister, Lincoln S. Kostin, Alexander Kryachko, Valery Steinhardt, William M. Yudovskaya, Marina Steinhardt, Paul J. TI Khatyrka, a new CV3 find from the Koryak Mountains, Eastern Russia SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID NATURAL QUASI-CRYSTAL; CHONDRITES; ORIGIN AB A new meteorite find, named Khatyrka, was recovered from eastern Siberia as a result of a search for naturally occurring quasicrystals. The meteorite occurs as clastic grains within postglacial clay-rich layers along the banks of a small stream in the Koryak Mountains, Chukotka Autonomous Okrug of far eastern Russia. Some of the grains are clearly chondritic and contain Type IA porphyritic olivine chondrules enclosed in matrices that have the characteristic platy olivine texture, matrix olivine composition, and mineralogy (olivine, pentlandite, nickel-rich iron-nickel metal, nepheline, and calcic pyroxene [diopside-hedenbergite solid solution]) of oxidized-subgroup CV3 chondrites. A few grains are fine-grained spinel-rich calcium-aluminum-rich inclusions with mineral oxygen isotopic compositions again typical of such objects in CV3 chondrites. The chondritic and CAI grains contain small fragments of metallic copper-aluminum-iron alloys that include the quasicrystalline phase icosahedrite. One grain is an achondritic intergrowth of Cu-Al metal alloys and forsteritic olivine +/- diopsidic pyroxene, both of which have meteoritic (CV3-like) oxygen isotopic compositions. Finally, some grains consist almost entirely of metallic alloys of aluminum+copper +/- iron. The Cu-Al-Fe metal alloys and the alloy-bearing achondrite clast are interpreted to be an accretionary component of what otherwise is a fairly normal CV3 (oxidized) chondrite. This association of CV3 chondritic grains with metallic copper-aluminum alloys makes Khatyrka a unique meteorite, perhaps best described as a complex CV3 (ox) breccia. C1 [MacPherson, Glenn J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. [Andronicos, Christopher L.] Purdue Univ, Dept Earth & Atmospher Sci, W Lafayette, IN 47907 USA. [Bindi, Luca] Univ Florence, Dipartimento Sci Terra, I-50121 Florence, Italy. [Distler, Vadim V.; Kryachko, Valery; Yudovskaya, Marina] Russian Acad Sci, Inst Geol Ore Deposits, Moscow 119017, Russia. [Eddy, Michael P.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Eiler, John M.; Guan, Yunbin] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Hollister, Lincoln S.] Princeton Univ, Dept Geosci, Princeton, NJ 08544 USA. [Kostin, Alexander] BHP Billiton, Geosci Technol, Houston, TX 77056 USA. [Steinhardt, William M.] Harvard Univ, Dept Earth & Planetary Sci, Cambridge, MA 02138 USA. [Steinhardt, Paul J.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Steinhardt, Paul J.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. RP MacPherson, GJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. EM macphers@si.edu RI Yudovskaya, Marina/K-3980-2013 FU NSF MRSEC program through New York University [DMR-0820341]; MIUR; Dept. of Mineral Sciences FX The expedition to Chukotka was supported by a grant from an anonymous donor to Princeton University (PJS, Principal Investigator). The research was supported, in part, by the NSF MRSEC program through New York University (grant DMR-0820341; PJS); the MIUR, PRIN 2009 project "Modularity, microstructures and non-stoichiometry in minerals" (LB); and the Chairman's Discretionary Fund, Dept. of Mineral Sciences, SI (GJM). We have benefitted from comments and many contributions to detailed imaging studies of the samples by N. Yao. The expedition was enabled by a co-operative agreement between Princeton University and the Institute of Geology of Ore Deposits, Mineralogy, Petrography and Geochemistry (IGEM) of the Russian Academy of Science (RAS). The expedition also hugely benefitted from the logistical aid provided by Olga Komelkova, Victor Komelkov, and Bogdan Makovskii, all from Anadyr, who organized and provided all transportation and provisions both in base camp in the Koryak Mountains and en route between the base camp and Anadyr. We also are grateful to Prof. A. J. T. Jull, George Burr, and the rest of the team at the Accelerator Mass Spectrometry Laboratory, University of Arizona, for their excellent work in producing the 14C age dates of the blue clay layer. Finally, this manuscript benefitted greatly from constructive reviews by Drs. Michael Weisberg, Misha Petaev, and Associate Editor Adrian Brearley. NR 24 TC 16 Z9 16 U1 2 U2 13 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 AUG PY 2013 VL 48 IS 8 BP 1499 EP 1514 DI 10.1111/maps.12170 PG 16 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237KC UT WOS:000325867500009 ER PT J AU Kralj-Fiser, S Schneider, JM Kuntner, M AF Kralj-Fiser, Simona Schneider, Jutta M. Kuntner, Matjaz TI Challenging the Aggressive Spillover Hypothesis: Is Pre-Copulatory Sexual Cannibalism a Part of a Behavioural Syndrome? SO ETHOLOGY LA English DT Review ID SOCIALLY POLYMORPHIC SPIDER; ORB-WEAVING SPIDERS; WEB SPIDER; FITNESS CONSEQUENCES; SPERM COMPETITION; DOLOMEDES-TRITON; NEPHILID SPIDERS; PRAYING-MANTIS; FISHING SPIDER; MATE CHOICE AB Pre-copulatory cannibalism - females devouring males during courtship - may bring no benefit to either sex. The aggressive spillover hypothesis' (ASH) posits that pre-copulatory cannibalism represents a spillover of female aggressiveness from the juvenile foraging context, when aggressiveness is advantageous, to the adult mating context, when aggressiveness may be non-adaptive or maladaptive. The ASH suggests that individuals exhibit limited plasticity in aggressive behaviours because they are genetically canalised for indiscriminate aggressiveness towards prey and conspecifics, including males. Hence, a tendency to employ pre-copulatory cannibalism is a part of the female aggression syndrome, an assertion generally accepted in the personality field. We here re-evaluate the previous findings in the light of personality criteria, which we propose for ASH validation: between-individual differences, repeatability and heritability in tendency for pre-copulatory attacks (and pre-copulatory cannibalism) and voracity towards prey, and their correlation. To re-evaluate ASH and to allow for additional or alternative explanations, we ask whether pre-copulatory cannibalism depends on female hunger, mating status, size and/or male quality. Finally, we ask whether cannibalistic females have a reduced reproductive success as predicted by the ASH. While repeatability and heritability in voracity towards prey and its correlation with the tendency to engage in pre-copulatory cannibalism were found in certain systems, we lack any evidence for repeatability and heritability in pre-copulatory cannibalistic attempts and for its maladaptiveness. Rather than only resorting to the ASH, foraging and mate choice hypotheses may also explain pre-copulatory cannibalism. We suggest clarifying the use of the terms sexual cannibalism (effect) and female aggressiveness or tendency to attack and devour males (cause), and argue that male strategies to avoid cannibalism should be considered. We propose testing the ASH as the explanation for pre-copulatory cannibalism in those cases where female tendency to devour males correlates with actual pre-copulatory cannibalism and when all the above criteria are fulfilled. Finally, we propose future directions for studying the ASH. C1 [Kralj-Fiser, Simona] Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Ljubljana SI-1001, Slovenia. [Schneider, Jutta M.] Univ Hamburg, Biozentrum Grindel, Museum & Inst Zool, Hamburg, Germany. [Kuntner, Matjaz] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kuntner, Matjaz] Hubei Univ, Coll Life Sci, Wuhan, Hubei, Peoples R China. RP Kralj-Fiser, S (reprint author), Slovenian Acad Sci & Arts, Ctr Sci Res, Inst Biol, Novi Trg 2,POB 306, Ljubljana SI-1001, Slovenia. EM simonakf@gmail.com RI Schneider, Jutta /G-3727-2010 FU Slovenian Research Agency [Z1-4194, P1-0236] FX This research was supported by the Slovenian Research Agency, grants Z1-4194 to S. K. F. and P1-0236 to M. K. NR 57 TC 12 Z9 12 U1 7 U2 72 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0179-1613 EI 1439-0310 J9 ETHOLOGY JI Ethology PD AUG PY 2013 VL 119 IS 8 BP 615 EP 623 DI 10.1111/eth.12111 PG 9 WC Psychology, Biological; Behavioral Sciences; Zoology SC Psychology; Behavioral Sciences; Zoology GA 237FU UT WOS:000325854800001 ER PT J AU Mello, MAR Kalko, EKV Silva, WR AF Mello, Marco A. R. Kalko, Elisabeth K. V. Silva, Wesley R. TI Effects of moonlight on the capturability of frugivorous phyllostomid bats (Chiroptera: Phyllostomidae) at different time scales SO ZOOLOGIA LA English DT Article DE Activity; behavior; foraging; lunar phobia; mist netting ID FORAGING BEHAVIOR; LUNAR PHOBIA; BRAZIL; PREDATION; PATTERNS; CYCLE AB Some bat species seem to be lunar phobic, i.e., they avoid flying in bright areas or during bright periods of the night; however, the evidence is still controversial. We think that part of this controversy comes from pooling data on bat captures and moonlight intensity according to broad categories, such as moon phases, which conceal the high variability among nights. Therefore, we used detailed, long-term field data on three phyllostomid bat species, in order to test the hypothesis of lunar phobia at two different time scales: 1) among nights, by pooling data of different nights according to moon phases and testing for differences in the distribution of captures; and 2) within a night, by analyzing the relationship between capturability and moonlight intensity (measured as illuminance) in one-hour intervals for 29 individual nights. Although most captures of the studied bat species occurred in the first half of the night, their activity pattern varied largely among nights, and was not always unimodal as commonly assumed. At the larger time scale, all studied bat species showed evidence of lunar phobia, as they were more frequently captured on dark moon phases. Nevertheless, at the smaller time scale, only Carollia perspicillata (Linnaeus, 1758) was less frequently captured on brighter periods of the night. We propose that the unimodal activity pattern assumed for frugivorous phyllostomid bats may be an artifact of data organization, and that activity and lunar phobia are much more variable than previously assumed. C1 [Mello, Marco A. R.] Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Biol Geral, BR-31270901 Belo Horizonte, MG, Brazil. [Mello, Marco A. R.; Kalko, Elisabeth K. V.] Univ Ulm, Inst Expt Okol, D-89069 Ulm, Germany. [Kalko, Elisabeth K. V.] Smithsonian Trop Res Inst, Balboa, Panama. [Silva, Wesley R.] Univ Estadual Campinas, Dept Zool, Campinas, SP, Brazil. RP Mello, MAR (reprint author), Univ Fed Minas Gerais, Inst Ciencias Biol, Dept Biol Geral, Ave Antonio Carlos 6627, BR-31270901 Belo Horizonte, MG, Brazil. EM marmello@gmail.com RI Mello, Marco/B-1095-2008 OI Mello, Marco/0000-0002-9098-9427 FU Lincoln Park Zoo; Rio de Janeiro Research Foundation (Faperj) [E-26/150.662/2000]; Sao Paulo Research Foundation (Fapesp) [02/09286-0]; German Academic Exchange Service (DAAD) [290088/2004-6]; Alexander von Humboldt Foundation (AvH) [1134644]; Federal University of Minas Gerais FX We are very grateful to many people who helped us in this study. Ivan Sazima, James Roper,. Mauro Galetti, Marcelo Nogueira, Joao Vasconcellos-Neto, and Ariovaldo Cruz-Neto made important suggestions to earlier versions of the manuscript. Joao Moreira provided us with the worksheet for illuminance calculation. Fernando Fernandez helped us with fieldwork infrastructure. IBAMA, especially Dionisio Pessamilio and Rodrigo Mayerhofer, allowed us to work at Poco das Antas. This work was supported by grants to MARM from the Lincoln Park Zoo, Rio de Janeiro Research Foundation (Faperj, E-26/150.662/2000), Sao Paulo Research Foundation (Fapesp, 02/09286-0), German Academic Exchange Service (DAAD, 290088/2004-6), Alexander von Humboldt Foundation (AvH, 1134644), and Federal University of Minas Gerais. NR 35 TC 2 Z9 2 U1 3 U2 20 PU SOC BRASILEIRA ZOOLOGIA, UNIV FEDERAL PARANA PI CURITIBA PA CAIXA POSTAL 19020, CURITIBA, PARANA 81531-980, BRAZIL SN 1984-4670 J9 ZOOLOGIA-CURITIBA JI Zoologia PD AUG PY 2013 VL 30 IS 4 BP 397 EP 402 DI 10.1590/S1984-46702013000400005 PG 6 WC Zoology SC Zoology GA 234SK UT WOS:000325664400005 ER PT J AU DiMichele, WA Elrick, SD Bateman, RM AF DiMichele, William A. Elrick, Scott D. Bateman, Richard M. TI GROWTH HABIT OF THE LATE PALEOZOIC RHIZOMORPHIC TREE-LYCOPSID FAMILY DIAPHORODENDRACEAE: PHYLOGENETIC, EVOLUTIONARY, AND PALEOECOLOGICAL SIGNIFICANCE SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE arborescent lycopsids; Diaphorodendron; evolutionary-developmental change; growth architecture; Isoetales s.l.; lateral branching; lycophyte; paedomorphosis; Pennsylvanian; saltation; Scotland; Synchysidendron; USA ID AGE HERRIN COAL; GEN-NOV; ARBORESCENT LYCOPSIDS; PENNSYLVANIAN-AGE; SALTATIONAL EVOLUTION; HOPEFUL MONSTERS; LEPIDODENDRON; EURAMERICA; ARCHITECTURE; LYCOPODS AB Premise of the study: Rhizomorphic lycopsids evolved the tree habit independently of all other land plants. Newly discovered specimens allow radical revision of our understanding of the growth architectures of the extinct Paleozoic sister-genera Synchysidendron and Diaphorodendron. Methods: Detailed descriptions of six remarkable adpression specimens from the Pennsylvanian of the USA and three casts from the late Mississippian of Scotland are used to revise and reanalyze a previously published morphological cladistic matrix and to reinterpret their remarkable growth forms. Key results: Contrary to previous assertions, Synchysidendron resembled Diaphorodendron in having a distinct and relatively complex growth habit that emphasized serially homologous, closely spaced, deciduous lateral branches at the expense of reduced monocarpic crown branches. Lateral branches originated through several strongly anisotomous dichotomies before producing during extended periods large numbers of Achlamydocarpon strobili. The comparatively large diameter of abscission scars remaining on the main trunk and the emergence of branches above the horizontal plane suggest that the lateral branch systems were robust. Lateral branches were borne in two opposite rows on the main trunk and continued upward into an isotomously branched, determinate crown; their striking distichous arrangement caused preferred orientation of fallen trunks on bedding planes. Conclusions: This discovery identifies the plagiotropic growth habit, dominated by serial lateral branches, as ubiquitous in the Diaphorodendraceae and also as unequivocally primitive within Isoetales s.l., a conclusion supported by both the revised morphological cladistic analysis and relative first appearances of taxa in the fossil record. Previously assumed complete homology between crown branching in Lepidodendraceae and that of all earlier-divergent genera requires reassessment. Saltational phenotypic transitions via modification of key developmental switches remains the most credible explanation for architectural evolution in the group. The resulting architecture allowed Diaphorodendraceae to co-dominate disturbed, clastic, equatorial wetlands from the Asbian to the Early Permian. C1 [DiMichele, William A.] Natl Museum Nat Hist, Dept Paleobiol, Smithsonian Inst, Washington, DC 20560 USA. [Elrick, Scott D.] Univ Illinois, Coal Sect, Illinois Geol Survey, Champaign, IL 61820 USA. [Bateman, Richard M.] Royal Bot Gardens Kew, Jodrell Lab, Richmond TW9 3DS, Surrey, England. RP Bateman, RM (reprint author), Royal Bot Gardens Kew, Jodrell Lab, Richmond TW9 3DS, Surrey, England. EM r.bateman@kew.org NR 69 TC 11 Z9 11 U1 3 U2 13 PU BOTANICAL SOC AMER INC PI ST LOUIS PA PO BOX 299, ST LOUIS, MO 63166-0299 USA SN 0002-9122 J9 AM J BOT JI Am. J. Bot. PD AUG PY 2013 VL 100 IS 8 BP 1604 EP 1625 DI 10.3732/ajb.1200623 PG 22 WC Plant Sciences SC Plant Sciences GA 228GL UT WOS:000325173800010 PM 23935114 ER PT J AU Osmond, MM Reudink, MW Germain, RR Marra, PP Nocera, JJ Boag, PT Ratcliffe, LM AF Osmond, Matthew M. Reudink, Matthew W. Germain, Ryan R. Marra, Peter P. Nocera, Joseph J. Boag, Peter T. Ratcliffe, Laurene M. TI Relationships between carotenoid-based female plumage and age, reproduction, and mate colour in the American Redstart (Setophaga ruticilla) SO CANADIAN JOURNAL OF ZOOLOGY-REVUE CANADIENNE DE ZOOLOGIE LA English DT Article DE American Redstart; carotenoid; colour; female ornament; plumage; Setophaga ruticilla; sexual selection ID FLYCATCHER FICEDULA-HYPOLEUCA; SEXUAL SELECTION; PIED FLYCATCHER; INTRASEXUAL COMPETITION; MUTUAL ORNAMENTATION; NORTHERN CARDINALS; PARENTAL QUALITY; MIGRATORY BIRD; TREE SWALLOWS; ARRIVAL DATE AB Most studies investigating the function and evolution of ornaments have focused on males. Variation in ornaments may also reflect individual quality and convey information in females. We examined correlations between female plumage colour and reproductive variables in the sexually dichromatic songbird, the American Redstart (Setophaga ruticilla (L., 1758)). Female American Redstarts display yellow, carotenoid-based plumage patches on their tails, wings, and flanks. Using reflectance spectrometry, we quantified brightness (feather structure) and "yellowness" (hue and chroma) of tail and flank feathers to examine whether female plumage colour varies with age, reproductive success, parental care, and the plumage colour of mates. Female plumage varied with age, with adult (after-second-year) females having brighter tail feathers than first-year females. We failed to find a relationship between female plumage colour and pairing or first-egg dates. However, adult females with brighter tails visited their nests less frequently and first-year females with brighter tails fledged fewer offspring. Adult females with brighter tails also mated with males who provided less care. In addition, adult females with yellower flanks paired with males with brighter flanks and with males who provided less parental care. We suggest that plumage colouration in female American Redstarts can act as a signal of individual age and quality. C1 [Osmond, Matthew M.; Reudink, Matthew W.; Germain, Ryan R.; Nocera, Joseph J.; Boag, Peter T.; Ratcliffe, Laurene M.] Queens Univ, Dept Biol, Kingston, ON K7L 3N6, Canada. [Reudink, Matthew W.; Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20008 USA. RP Osmond, MM (reprint author), Michigan State Univ, WK Kellogg Biol Stn, Hickory Corners, MI 49060 USA. EM matthew.osmond@mail.mcgill.ca RI Boag, Peter/B-2907-2014; OI Boag, Peter/0000-0003-0050-2089; Reudink, Matthew/0000-0001-8956-5849 FU Natural Sciences and Engineering Research Council of Canada; Canadian Foundation for Innovation; National Science Foundation [0085965]; Smithsonian Institution; Queen's University; Ontario Innovation Trust; Sigma Xi; American Ornithologists' Union; Society of Canadian Ornithologists; American Museum of Natural History FX We gratefully acknowledge the hard work of the many field assistants that contributed to this study. R. Reudink, T. Murphy, and two anonymous reviewers provided insightful discussion and comments on earlier versions of the manuscript. We thank R. Montgomerie for the use of his colour analysis equipment, software, and expertise. Funding was provided by the Natural Sciences and Engineering Research Council of Canada, the Canadian Foundation for Innovation, a National Science Foundation grant to P.P.M. (0085965), the Smithsonian Institution, Queen's University, Ontario Innovation Trust, Sigma Xi, the American Ornithologists' Union, the Society of Canadian Ornithologists, and the American Museum of Natural History. NR 71 TC 7 Z9 7 U1 5 U2 48 PU CANADIAN SCIENCE PUBLISHING, NRC RESEARCH PRESS PI OTTAWA PA 1200 MONTREAL ROAD, BUILDING M-55, OTTAWA, ON K1A 0R6, CANADA SN 0008-4301 J9 CAN J ZOOL JI Can. J. Zool.-Rev. Can. Zool. PD AUG PY 2013 VL 91 IS 8 BP 589 EP 595 DI 10.1139/cjz-2013-0017 PG 7 WC Zoology SC Zoology GA 221TS UT WOS:000324683000007 ER PT J AU Schook, MW Wildt, DE Weiss, RB Wolfe, BA Archibald, KE Pukazhenthi, BS AF Schook, Mandi W. Wildt, David E. Weiss, Rachael B. Wolfe, Barbara A. Archibald, Kate E. Pukazhenthi, Budhan S. TI Fundamental Studies of the Reproductive Biology of the Endangered Persian Onager (Equus hemionus onager) Result in First Wild Equid Offspring from Artificial Insemination SO BIOLOGY OF REPRODUCTION LA English DT Article DE artificial insemination; cryopreservation; endocrine; equid; estrous cycle; onager ID SPERMATOZOAL MOTILITY PARAMETERS; DAILY SPERM OUTPUT; SEMEN CHARACTERISTICS; LUTEINIZING-HORMONE; OVARIAN ACTIVITY; ESTROUS-CYCLE; MARES; STALLIONS; PATTERNS; DONKEY AB We studied the Persian onager (Equus hemionus onager), an endangered equid subspecies. The objective was to characterize endocrine patterns and ovarian follicular dynamics of females as well as seminal traits and sperm sensitivity to cryopreservation in males as a prerequisite to testing the feasibility of artificial insemination (AI). Urinary progesterone and estrogen metabolite profiles were determined by enzyme immunoassay in 11 females. Serial ultrasonography of ovarian activity was performed for 2 mo in a subset of four females. Females were seasonally polyestrous (June-November). Ovarian morphometry via ultrasonography and urinary progesterone profiles were more reflective of reproductive events than urinary estrogen patterns, and preovulatory follicle size was smaller than reported for other equid species. There was evidence for lactational suppression of estrus for up to 1.5 yr in nursing dams. Electroejaculation allowed recovery of highly motile sperm from 7, anesthetized males on 57% of occasions. Spermatozoa, including motility and acrosomal integrity, were resilient to freeze-thawing. Artificial insemination was successful in 2 of 3 females following detection of a dominant follicle and deslorelin administration, resulting in births of a healthy female and male foal by using fresh/chilled and frozen/thawed sperm, respectively. C1 [Schook, Mandi W.; Wildt, David E.; Archibald, Kate E.; Pukazhenthi, Budhan S.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Schook, Mandi W.; Weiss, Rachael B.; Wolfe, Barbara A.] The Wilds, Cumberland, OH USA. RP Schook, MW (reprint author), Cleveland Metropk Zoo, Cleveland, OH 44109 USA. EM mmv@clevelandmetroparks.com; pukazhenthib@si.edu FU Sichel Endowment Fund; Phillip Reed, Jr., Fund FX Supported by the Sichel Endowment Fund and the Phillip Reed, Jr., Fund. Presented in part at the International Wild Equid Conference, September 18-22, 2012, University of Veterinary Medicine, Vienna, Austria. NR 85 TC 5 Z9 5 U1 2 U2 8 PU SOC STUDY REPRODUCTION PI MADISON PA 1691 MONROE ST,SUITE # 3, MADISON, WI 53711-2021 USA SN 0006-3363 J9 BIOL REPROD JI Biol. Reprod. PD AUG PY 2013 VL 89 IS 2 AR 41 DI 10.1095/biolreprod.113.110122 PG 13 WC Reproductive Biology SC Reproductive Biology GA 220JU UT WOS:000324580000004 PM 23863403 ER PT J AU Batygin, K Morbidelli, A AF Batygin, K. Morbidelli, A. TI Analytical treatment of planetary resonances SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE celestial mechanics; planets and satellites: dynamical evolution and stability; chaos ID MEAN-MOTION RESONANCE; GASEOUS PROTOPLANETARY DISK; EXTRA-SOLAR PLANETS; LARGE-SCALE CHAOS; ORBITAL RESONANCES; TIDAL EVOLUTION; GIANT PLANETS; PERTURBATIVE TREATMENT; OSCILLATOR SYSTEMS; CLOSE ENCOUNTERS AB An ever-growing observational aggregate of extrasolar planets has revealed that systems of planets that reside in or near mean-motion resonances are relatively common. While the origin of such systems is attributed to protoplanetary disk-driven migration, a qualitative description of the dynamical evolution of resonant planets remains largely elusive. Aided by the pioneering works of the last century, we formulate an approximate, integrable theory for first-order resonant motion. We utilize the developed theory to construct an intuitive, geometrical representation of resonances within the context of the unrestricted three-body problem. Moreover, we derive a simple analytical criterion for the appearance of secondary resonances between resonant and secular motion. Subsequently, we demonstrate the onset of rapid chaotic motion as a result of overlap among neighboring first-order mean-motion resonances, as well as the appearance of slow chaos as a result of secular modulation of the planetary orbits. Finally, we take advantage of the integrable theory to analytically show that, in the adiabatic regime, divergent encounters with first-order mean-motion resonances always lead to persistent apsidal anti-alignment. C1 [Batygin, K.; Morbidelli, A.] Observ Cote Azur, Dept Lagrange, F-06304 Nice, France. [Batygin, K.] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Batygin, K (reprint author), Observ Cote Azur, Dept Lagrange, F-06304 Nice, France. EM kbatygin@cfa.harvard.edu; orby@oca.eu FU Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics FX We wish to thank Jake Ketchum and Matt Holman for carefully reviewing the manuscript and providing helpful suggestions. We wish to thank Christian Beauge for a very thorough and insightful referee report that greatly enhanced the quality of this manuscript. K. B. acknowledges the generous support from the ITC Prize Postdoctoral Fellowship at the Institute for Theory and Computation, Harvard-Smithsonian Center for Astrophysics. NR 88 TC 10 Z9 10 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2013 VL 556 AR A28 DI 10.1051/0004-6361/201220907 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500028 ER PT J AU Elliott, J Kruhler, T Greiner, J Savaglio, S Olivares, F Rau, EA Postigo, AD Sanchez-Ramirez, R Wiersema, K Schady, P Kann, DA Filgas, R Nardini, M Berger, E Fox, D Gorosabel, J Klose, S Levan, A Guelbenzu, AN Rossi, A Schmidl, S Sudilovsky, V Tanvir, NR Thone, CC AF Elliott, J. Kruehler, T. Greiner, J. Savaglio, S. Olivares, F. Rau, E. A. de Ugarte Postigo, A. Sanchez-Ramirez, R. Wiersema, K. Schady, P. Kann, D. A. Filgas, R. Nardini, M. Berger, E. Fox, D. Gorosabel, J. Klose, S. Levan, A. Guelbenzu, A. Nicuesa Rossi, A. Schmidl, S. Sudilovsky, V. Tanvir, N. R. Thoene, C. C. TI The low-extinction afterglow in the solar-metallicity host galaxy of gamma-ray burst 110918A SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE gamma-ray burst: general; gamma-ray burst: individual: 110918A; ISM: general; galaxies: abundances; galaxies: photometry; galaxies: star formation ID STAR-FORMING GALAXIES; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; DUST EXTINCTION; STELLAR MASS; PHOTOMETRIC REDSHIFTS; LUMINOSITY FUNCTION; STARBURST GALAXIES; OPTICAL AFTERGLOWS; FORMATION HISTORY AB Galaxies selected through long gamma-ray bursts (GRBs) could be of fundamental importance when mapping the star formation history out to the highest redshifts. Before using them as efficient tools in the early Universe, however, the environmental factors that govern the formation of GRBs need to be understood. Metallicity is theoretically thought to be a fundamental driver in GRB explosions and energetics, but it is still, even after more than a decade of extensive studies, not fully understood. This is largely related to two phenomena: a dust-extinction bias, which prevented high-mass and thus likely high-metallicity GRB hosts from being detected in the first place, and a lack of efficient instrumentation, which limited spectroscopic studies, including metallicity measurements, to the low-redshift end of the GRB host population. The subject of this work is the very energetic GRB 110918A (E-gamma,E-iso = 1.9 x 10(54) erg), for which we measure a redshift of z = 0.984. GRB 110918A gave rise to a luminous afterglow with an intrinsic spectral slope of beta = 0.70, which probed a sight-line with little extinction (A(V)(GRB) = 0.16 mag) and soft X-ray absorption (N-H,N-X = (1.6 +/- 0.5) x 10(21) cm(-2)) typical of the established distributions of afterglow properties. However, photometric and spectroscopic follow-up observations of the galaxy hosting GRB 110918A, including optical/near-infrared photometry with the Gamma-Ray burst Optical Near-infrared Detector and spectroscopy with the Very Large Telescope/X-shooter, reveal an all but average GRB host in comparison to the z similar to 1 galaxies selected through similar afterglows to date. It has a large spatial extent with a half-light radius of R-1/2 similar to 10 kpc, the highest stellar mass for z < 1.9 (log(M-*/M-circle dot) = 10.68 +/- 0.16), and an H alpha-based star formation rate of SFRH alpha = 41(-16)(+28) M-circle dot yr(-1). We measure a gas-phase extinction of A(V)(gas) similar to 1.8 mag through the Balmer decrement and one of the largest host-integrated metallicities ever of around solar using the well-constrained ratios of [N II]/H alpha and [N II]/[O II] (12 + log (O/H) = 8.93 +/- 0.13 and 8.85(-0.18)(+0.14), respectively). This presents one of the very few robust metallicity measurements of GRB hosts at z similar to 1, and establishes that GRB hosts at z similar to 1 can also be very metal rich. It conclusively rules out a metallicity cut-off in GRB host galaxies and argues against an anti-correlation between metallicity and energy release in GRBs. C1 [Elliott, J.; Greiner, J.; Savaglio, S.; Olivares, F.; Rau, E. A.; Schady, P.; Kann, D. A.; Filgas, R.; Sudilovsky, V.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kruehler, T.; de Ugarte Postigo, A.] Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, DK-2100 Copenhagen, Denmark. [de Ugarte Postigo, A.; Sanchez-Ramirez, R.; Gorosabel, J.; Thoene, C. C.] Inst Astrofis Andalucia IAA CSIC, Granada 18008, Spain. [Wiersema, K.; Tanvir, N. R.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Kann, D. A.; Klose, S.; Guelbenzu, A. Nicuesa; Rossi, A.; Schmidl, S.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Filgas, R.] Czech Tech Univ, Inst Expt & Appl Phys, Prague 12800, Czech Republic. [Nardini, M.] Univ Milano Bicocca, I-20126 Milan, Italy. [Berger, E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fox, D.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Levan, A.] Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. [Gorosabel, J.] Univ Pais Vasco UPV EHU, ETS Ingn, Unidad Asociada Grp Ciencia Planetarias UPV EHU I, Dept Fis Aplicada 1, Bilbao 48013, Spain. [Gorosabel, J.] Ikerbasque, Basque Fdn Sci, Bilbao 48008, Spain. RP Elliott, J (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM jonnyelliott@mpe.mpg.de RI Rossi, Andrea/N-4674-2015 OI Rossi, Andrea/0000-0002-8860-6538 FU DFG [HA 1850/28-1, SA 2001/1-1, SA 2001/2-1]; National Aeronautics and Space Administration; Marie Curie Career Integration Grant Fellowship; European Commission under the Marie Curie Intra-European Fellowship Programme; Danish National Research Foundation; MPG [M.FE.A.Ext 00003]; Deutscher Akademischer Austausch-Dienst (DAAD); Dark Cosmology Centre; STFC; DFG cluster of excellence Origin and Structure of the Universe; National Science Foundation [AST-1107973]; [AYA2012-39362-C02-02]; [AYA2011-24780/ESP]; [AYA2009-14000-C03-01/ESP]; [AYA2010-21887-C04-01] FX We thank the anonymous referees for their constructive criticisms, Regis Lachaume for the WFI observations, and Mara Salvato and Ivan Baldry for helpful discussions. Part of the funding for GROND (both hardware as well as personnel) was generously granted from the Leibniz-Prize to Prof. G. Hasinger (DFG grant HA 1850/28-1). Based on observations made with the Gran Telescopio Canarias (GTC), that is installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de AstrofAnsica de Canarias on the island of La Palma. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. A.d.U.P. acknowledges support from a Marie Curie Career Integration Grant Fellowship. T. K. acknowledges support by the European Commission under the Marie Curie Intra-European Fellowship Programme. The Dark Cosmology Centre is funded by the Danish National Research Foundation. SS acknowledges support through project M.FE.A.Ext 00003 of the MPG. F.O.E. acknowledges funding of his Ph.D. through the Deutscher Akademischer Austausch-Dienst (DAAD). A.d.U.P., C. T., R. S. R., and J.G. acknowledge support from the Spanish research projects AYA2012-39362-C02-02, AYA2011-24780/ESP, AYA2009-14000-C03-01/ESP, and AYA2010-21887-C04-01. A.d.U.P. acknowledges support from The Dark Cosmology Centre. K. W. acknowledges support by the STFC. P. S. acknowledges support by DFG grant SA 2001/1-1. D. A. K. acknowledges support by the DFG cluster of excellence Origin and Structure of the Universe. S. K., A.N.G., and A. R. acknowledge support by DFG grant Kl 766/16-1. A. R., A.N.G., A. K., and D. A. K. are grateful for travel funding support through MPE. M.N. acknowledges support by DFG grant SA 2001/2-1. E. B. acknowledges support from the National Science Foundation through Grant AST-1107973. J.E. is thankful for the support from A. and G. Elliott. NR 110 TC 25 Z9 25 U1 0 U2 11 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2013 VL 556 AR A23 DI 10.1051/0004-6361/201220968 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500023 ER PT J AU Lopez-Sepulcre, A Taquet, V Sanchez-Monge, A Ceccarelli, C Dominik, C Kama, M Caux, E Fontani, F Fuente, A Ho, PTP Neri, R Shimajiri, Y AF Lopez-Sepulcre, A. Taquet, V. Sanchez-Monge, A. Ceccarelli, C. Dominik, C. Kama, M. Caux, E. Fontani, F. Fuente, A. Ho, P. T. P. Neri, R. Shimajiri, Y. TI High-angular resolution observations towards OMC-2 FIR 4: Dissecting an intermediate-mass protocluster SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: individual objects: OMC-2 FIR 4; ISM: molecules ID SUBMILLIMETER-WAVE OBSERVATIONS; STAR-FORMATION; PROTOSTELLAR ENVELOPES; PHYSICAL STRUCTURE; MOLECULAR CLOUD; STELLAR CONTENT; ORION; CORES; PROTOSTARS; EMISSION AB Context. Intermediate-mass stars are an important ingredient of our Galaxy and a key to understanding how high-and low-mass stars form in clusters. One of the closest known young intermediate-mass protoclusters is OMC-2 FIR 4, which is located at a distance of 420 pc in Orion. This region is one of the few where the complete 500-2000 GHz spectrum has been observed with the heterodyne spectrometer HIFI on board the Herschel satellite, and unbiased spectral surveys at 0.8, 1, 2, and 3 mm have been obtained with the JCMT and IRAM 30-m telescopes. Aims. We aim to disentangle the core multiplicity, to investigate the morphology of this region in order to study the formation of a low-and intermediate-mass protostar cluster, and to aid in interpretation of the single-dish line profiles already in our hands. Methods. We used the IRAM Plateau de Bure Interferometer to image OMC-2 FIR 4 in the 2-mm continuum emission, as well as in DCO+(2-1), DCN(2-1), (CS)-S-34(3-2), and several CH3OH lines. In addition, we analysed observations of the NH3(1, 1) and (2, 2) inversion transitions that used the Very Large Array of the NRAO. The resulting maps have an angular resolution that allows us to resolve structures of 5 '', which is equivalent to similar to 2000 AU. Results. Our observations reveal three spatially resolved sources within OMC-2 FIR 4, of one or several solar masses each, with hints of further unresolved substructure within them. Two of these sources have elongated shapes and are associated with dust continuum emission peaks, thus likely containing at least one molecular core each. One of them also displays radio continuum emission, which may be attributed to a young B3-B4 star that dominates the overall luminosity output of the region. The third identified source displays a DCO+(2-1) emission peak and weak dust continuum emission. Its higher abundance of DCO+ relative to the other two regions suggests a lower temperature, hence its possible association with either a younger low-mass protostar or a starless core. It may alternatively be part of the colder envelope of OMC-2 FIR 4. Conclusions. Our interferometric observations show the complexity of the intermediate-mass protocluster OMC-2 FIR 4, where multiple cores, chemical differentiation, and an ionised region all coexist within an area of only 10 000 AU. C1 [Lopez-Sepulcre, A.; Taquet, V.; Ceccarelli, C.] UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. [Sanchez-Monge, A.; Fontani, F.] Osserv Astrofis Arcetri, I-50124 Florence, Italy. [Dominik, C.; Kama, M.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1090 GE Amsterdam, Netherlands. [Dominik, C.] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6525 AJ Nijmegen, Netherlands. [Caux, E.] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France. [Caux, E.] IRAP, CNRS, F-31028 Toulouse 4, France. [Fuente, A.] Observatorio Astron Nacl, Madrid 28803, Spain. [Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Ho, P. T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neri, R.] IRAM, F-38406 St Martin Dheres, France. [Shimajiri, Y.] Natl Inst Nat Sci, Natl Astron Observ Japan, Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan. RP Lopez-Sepulcre, A (reprint author), UJF Grenoble 1, CNRS INSU, IPAG, UMR 5274, F-38041 Grenoble, France. EM ana.sepulcre@obs.ujf-grenoble.fr RI Fuente, Asuncion/G-1468-2016; OI Fuente, Asuncion/0000-0001-6317-6343; Kama, Mihkel/0000-0003-0065-7267; Fontani, Francesco/0000-0003-0348-3418 FU CNES (Centre National d'Etudes Spatiales); Agence Nationale pour la Recherche (ANR), France [ANR-08-BLAN-022]; NWO; NOVA; Leids Kerkhoven-Bosscha Fonds; COST Action on Astrochemistry; CONSOLIDER INGENIO [CSD2009-00038] FX A.L.S. and C. C. acknowledge funding from the CNES (Centre National d'Etudes Spatiales) and from the Agence Nationale pour la Recherche (ANR), France (project FORCOMS, contracts ANR-08-BLAN-022). M. K. gratefully acknowledges funding from an NWO grant, NOVA, Leids Kerkhoven-Bosscha Fonds, and the COST Action on Astrochemistry. C. D. acknowledges funding from Leids Kerkhoven-Bosscha Fonds. A. F. has been partially supported within the programme CONSOLIDER INGENIO 2010, under grant CSD2009-00038 "Molecular Astrophysics: The Herschel and ALMA Era-ASTROMOL". We are grateful to the anonymous referee and to C. M. Walmsley, whose suggestions contributed to improve the quality of the present paper. NR 51 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 AUG PY 2013 VL 556 AR A62 DI 10.1051/0004-6361/201220905 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500062 ER PT J AU Peter, H Bingert, S Klimchuk, JA de Forest, C Cirtain, JW Golub, L Winebarger, AR Kobayashi, K Korreck, KE AF Peter, H. Bingert, S. Klimchuk, J. A. de Forest, C. Cirtain, J. W. Golub, L. Winebarger, A. R. Kobayashi, K. Korreck, K. E. TI Structure of solar coronal loops: from miniature to large-scale SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE Sun: corona; magnetic fields; Sun: UV radiation; Sun: activity; methods: data analysis ID DYNAMICS-OBSERVATORY SDO; ACTIVE-REGION LOOPS; TRANSITION-REGION; MAGNETIC-FIELDS; BRIGHT POINTS; COOL LOOPS; HINODE; MODEL; TRACE; SUN AB Aims. We use new data from the High-resolution Coronal Imager (Hi-C) with its unprecedented spatial resolution of the solar corona to investigate the structure of coronal loops down to 0.2 ''. Methods. During a rocket flight, Hi-C provided images of the solar corona in a wavelength band around 193 angstrom that is dominated by emission from Fe XII showing plasma at temperatures around 1.5 MK. We analyze part of the Hi-C field-of-view to study the smallest coronal loops observed so far and search for the possible substructuring of larger loops. Results. We find tiny 1.5 MK loop-like structures that we interpret as miniature coronal loops. Their coronal segments above the chromosphere have a length of only about 1 Mm and a thickness of less than 200 km. They could be interpreted as the coronal signature of small flux tubes breaking through the photosphere with a footpoint distance corresponding to the diameter of a cell of granulation. We find that loops that are longer than 50 Mm have diameters of about 2 '' or 1.5 Mm, which is consistent with previous observations. However, Hi-C really resolves these loops with some 20 pixels across the loop. Even at this greatly improved spatial resolution, the large loops seem to have no visible substructure. Instead they show a smooth variation in cross-section. Conclusions. That the large coronal loops do not show a substructure on the spatial scale of 0.1 '' per pixel implies that either the densities and temperatures are smoothly varying across these loops or it places an upper limit on the diameter of the strands the loops might be composed of. We estimate that strands that compose the 2 '' thick loop would have to be thinner than 15 km. The miniature loops we find for the first time pose a challenge to be properly understood through modeling. C1 [Peter, H.; Bingert, S.] Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. [Klimchuk, J. A.] NASA, Heliophys Div, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [de Forest, C.] SW Res Inst, Instrumentat & Space Res Div, Boulder, CO 80302 USA. [Cirtain, J. W.; Winebarger, A. R.] NASA, George C Marshall Space Flight Ctr, MSFC, Huntsville, AL 35812 USA. [Golub, L.; Korreck, K. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 01238 USA. [Kobayashi, K.] Univ Alabama, Ctr Space & Aeronaut Res, Huntsville, AL 35812 USA. RP Peter, H (reprint author), Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. EM peter@mps.mpg.de RI Klimchuk, James/D-1041-2012 OI Klimchuk, James/0000-0003-2255-0305 FU NASA's Low Cost Access to Space program; Max-Planck/Princeton Center for Plasma Physics; NASA FX We acknowledge the High-resolution Coronal Imager instrument grant funded by the NASA's Low Cost Access to Space program. MSFC/NASA led the mission and partners include the Smithsonian Astrophysical Observatory in Cambridge, Mass.; Lockheed Martin's Solar Astrophysical Laboratory in Palo Alto, Calif.; the University of Central Lancashire in Lancashire, England; and the Lebedev Physical Institute of the Russian Academy of Sciences in Moscow. The AIA and HMI data used are provided courtesy of NASA/SDO and the AIA and HMI science teams. The AIA and HMI data have been retrieved using the German Data Center for SDO. The numerical simulation was conducted at the High Performance Computing Center Stuttgart (HLRS). This work was partially funded by the Max-Planck/Princeton Center for Plasma Physics. The work of J.A.K. was supported by the NASA Supporting Research and Technology and Guest Investigator Programs. H.P. acknowledges stimulating discussions with Robert Cameron and Aaron Birch. We thank the anonymous referee for constructive comments. NR 51 TC 38 Z9 38 U1 1 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 AUG PY 2013 VL 556 AR A104 DI 10.1051/0004-6361/201321826 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500104 ER PT J AU van der Marel, N Kristensen, LE Visser, R Mottram, JC Yildiz, UA van Dishoeck, EF AF van der Marel, N. Kristensen, L. E. Visser, R. Mottram, J. C. Yildiz, U. A. van Dishoeck, E. F. TI Outflow forces of low-mass embedded objects in Ophiuchus: a quantitative comparison of analysis methods SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE ISM: jets and outflows; ISM: molecules; stars: protostars; stars: low-mass; circumstellar matter; submillimeter: ISM ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; BIPOLAR MOLECULAR OUTFLOWS; CO LINE FORMATION; RHO-OPHIUCHI; DARK CLOUD; SUBMILLIMETER; PROTOSTARS; ENVELOPE; EVOLUTION AB Context. The outflow force of molecular bipolar outflows is a key parameter in theories of young stellar feedback on their surroundings. The focus of many outflow studies is the correlation between the outflow force, bolometric luminosity, and envelope mass. However, it is difficult to combine the results of different studies in large evolutionary plots over many orders of magnitude due to the range of data quality, analysis methods, and corrections for observational effects, such as opacity and inclination. Aims. We aim to determine the outflow force for a sample of low-luminosity embedded sources. We quantify the influence of the analysis method and the assumptions entering the calculation of the outflow force. Methods. We used the James Clerk Maxwell Telescope to map (CO)-C-12 J = 3-2 over 2' x 2' regions around 16 Class I sources of a well-defined sample in Ophiuchus at 15 '' resolution. The outflow force was then calculated using seven different methods differing, e. g., in the use of intensity-weighted emission and correction factors for inclination. Two well studied outflows (HH 46 and NGC1 333 IRAS4A) are added to the sample and included in the comparison. Results. The results from the analysis methods differ from each other by up to a factor of 6, whereas observational properties and choices in the analysis procedure affect the outflow force by up to a factor of 4. Subtraction of cloud emission and integrating over the remaining profile increases the outflow force at most by a factor of 4 compared to line wing integration. For the sample of Class I objects, bipolar outflows are detected around 13 sources including 5 new detections, where the three nondetections are confused by nearby outflows from other sources. New outflow structures without a clear powering source are discovered at the corners of some of the maps. Conclusions. When combining outflow forces from different studies, a scatter by up to a factor of 5 can be expected. Although the true outflow force remains unknown, the separation method (separate calculation of dynamical time and momentum) is least affected by the uncertain observational parameters. The correlations between outflow force, bolometric luminosity, and envelope mass are further confirmed down to low-luminosity sources. C1 [van der Marel, N.; Kristensen, L. E.; Mottram, J. C.; Yildiz, U. A.; van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Visser, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. RP van der Marel, N (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM nmarel@strw.leidenuniv.nl RI Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011 OI Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721 FU Netherlands Research School for Astronomy (NOVA); Spinoza grant; Netherlands Organisation for Scientific Research (NWO) [614.001.008] FX The authors would like to thank Sylvie Cabrit and Mario Tafalla for useful discussions, Antonio Chrysostomou who carried out part of the 12CO observations and Rowin Meijerink and Edo Loenen who carried out the 13CO observations. The James Clerk Maxwell Telescope is operated by the Joint Astronomy Centre on behalf of the Science and Technology Facilities Council of the United Kingdom, the Netherlands Organisation for Scientific Research, and the National Research Council of Canada. Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO). NR 63 TC 16 Z9 16 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 AUG PY 2013 VL 556 AR A76 DI 10.1051/0004-6361/201220717 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500076 ER PT J AU Yildiz, UA Kristensen, LE van Dishoeck, EF San Jose-Garcia, I Karska, A Harsono, D Tafalla, M Fuente, A Visser, R Jorgensen, JK Hogerheijde, MR AF Yildiz, U. A. Kristensen, L. E. van Dishoeck, E. F. San Jose-Garcia, I. Karska, A. Harsono, D. Tafalla, M. Fuente, A. Visser, R. Jorgensen, J. K. Hogerheijde, M. R. TI High-J CO survey of low-mass protostars observed with Herschel-HIFI SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE astrochemistry; stars: formation; stars: protostars; ISM: molecules; techniques: spectroscopic ID YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; PROTOSTELLAR ENVELOPES; CIRCUMSTELLAR DISKS; CHEMICAL EVOLUTION; PACS SPECTROSCOPY; MOLECULAR CLOUDS; SHOCK CHEMISTRY; BIPOLAR OUTFLOW; KEY PROGRAM AB Context. In the deeply embedded stage of star formation, protostars start to heat and disperse their surrounding cloud cores. The evolution of these sources has traditionally been traced through dust continuum spectral energy distributions (SEDs), but the use of CO excitation as an evolutionary probe has not yet been explored due to the lack of high-J CO observations. Aims. The aim is to constrain the physical characteristics (excitation, kinematics, column density) of the warm gas in low-mass protostellar envelopes using spectrally resolved Herschel data of CO and compare those with the colder gas traced by lower excitation lines. Methods. Herschel-HIFI observations of high-J lines of (CO)-C-12, (CO)-C-13, and (CO)-O-18 (up to J(u) = 10, E-u up to 300 K) are presented toward 26 deeply embedded low-mass Class 0 and Class I young stellar objects, obtained as part of the Water In Star-forming regions with Herschel (WISH) key program. This is the first large spectrally resolved high-J CO survey conducted for these types of sources. Complementary lower J CO maps were observed using ground-based telescopes, such as the JCMT and APEX and convolved to matching beam sizes. Results. The (CO)-C-12 10-9 line is detected for all objects and can generally be decomposed into a narrow and a broad component owing to the quiescent envelope and entrained outflow material, respectively. The (CO)-C-12 excitation temperature increases with velocity from similar to 60 K up to similar to 130 K. The median excitation temperatures for (CO)-C-12, (CO)-C-13, and (CO)-O-18 derived from single-temperature fits to the J(u) = 2-10 integrated intensities are similar to 70 K, 48 K and 37 K, respectively, with no significant difference between Class 0 and Class I sources and no trend with M-env or L-bol. Thus, in contrast to the continuum SEDs, the spectral line energy distributions (SLEDs) do not show any evolution during the embedded stage. In contrast, the integrated line intensities of all CO isotopologs show a clear decrease with evolutionary stage as the envelope is dispersed. Models of the collapse and evolution of protostellar envelopes reproduce the (CO)-O-18 results well, but underproduce the (CO)-C-13 and (CO)-C-12 excitation temperatures, due to lack of UV heating and outflow components in those models. The H2O 1(10) - 1(01)/CO 10-9 intensity ratio does not change significantly with velocity, in contrast to the H2O/CO 3-2 ratio, indicating that CO 10-9 is the lowest transition for which the line wings probe the same warm shocked gas as (HO)-O-2. Modeling of the full suite of (CO)-O-18 lines indicates an abundance profile for Class 0 sources that is consistent with a freeze-out zone below 25 K and evaporation at higher temperatures, but with some fraction of the CO transformed into other species in the cold phase. In contrast, the observations for two Class I sources in Ophiuchus are consistent with a constant high CO abundance profile. Conclusions. The velocity resolved line profiles trace the evolution from the Class 0 to the Class I phase through decreasing line intensities, less prominent outflow wings, and increasing average CO abundances. However, the CO excitation temperature stays nearly constant. The multiple components found here indicate that the analysis of spectrally unresolved data, such as provided by SPIRE and PACS, must be done with caution. C1 [Yildiz, U. A.; Kristensen, L. E.; van Dishoeck, E. F.; San Jose-Garcia, I.; Harsono, D.; Hogerheijde, M. R.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van Dishoeck, E. F.; Karska, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Tafalla, M.] Observ Astron Nacl IGN, Madrid 28014, Spain. [Fuente, A.] Observ Astron Nacl, Alcala De Henares 28803, Spain. [Visser, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Jorgensen, J. K.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen O, Denmark. [Jorgensen, J. K.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen K, Denmark. RP Yildiz, UA (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM yildiz@strw.leidenuniv.nl RI Jorgensen, Jes Kristian/L-7936-2014; Yildiz, Umut/C-5257-2011; Fuente, Asuncion/G-1468-2016; Kristensen, Lars/F-4774-2011; Karska, Agata/O-5311-2016 OI Jorgensen, Jes Kristian/0000-0001-9133-8047; Yildiz, Umut/0000-0001-6197-2864; Fuente, Asuncion/0000-0001-6317-6343; Kristensen, Lars/0000-0003-1159-3721; Karska, Agata/0000-0001-8913-925X FU Netherlands Research School for Astronomy (NOVA); Spinoza grant; Netherlands Organisation for Scientific Research (NWO) [614.001.008]; European Community [238258]; Netherlands Organization for Scientific Research (NWO) [600.063.310.10] FX The authors are grateful to the rest of the WISH team for stimulating discussions and to Joseph Mottram, Carolyn McCoey and the anonymous referee for valuable comments on the manuscript. They also thank the APEX, JCMT and Herschel staff as well as NL and MPIfR observers for carrying out the observations. Astrochemistry in Leiden is supported by The Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from The Netherlands Organisation for Scientific Research (NWO), and by the European Community's Seventh Framework Programme FP7/20072013 under grant agreement 238258 (LASSIE). The authors are grateful to many funding agencies and the HIFI-ICC staff who has been contributing for the construction of Herschel and HIFI for many years. HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France and the US. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland, NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA). Sweden: Chalmers University of Technology - MC2, RSS & GARD; Onsala Space Observatory; Swedish National Space Board, Stockholm University -Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Construction of CHAMP+ is a collaboration between the Max-Planck-Institut fur Radioastronomie Bonn, Germany; SRON Netherlands Institute for Space Research, Groningen, The Netherlands; The Netherlands Research School for Astronomy (NOVA); and the Kavli Institute of Nanoscience at Delft University of Technology, The Netherlands; with support from The Netherlands Organization for Scientific Research (NWO) grant 600.063.310.10. NR 81 TC 33 Z9 33 U1 0 U2 6 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2013 VL 556 AR A89 DI 10.1051/0004-6361/201220849 PG 46 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500089 ER PT J AU Zhang, Z Gilfanov, M Bogdan, A AF Zhang, Z. Gilfanov, M. Bogdan, A. TI Low-mass X-ray binary populations in galaxy outskirts: Globular clusters and supernova kicks SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE X-rays: binaries; globular clusters: general; Galaxy: halo; supernovae: general ID NEARBY EARLY-TYPE; VIRGO-CLUSTER; LUMINOSITY FUNCTIONS; RADIO PULSARS; HOST GALAXY; SYSTEMS; CHANDRA; ENVIRONMENT; CONNECTION; EMISSION AB For the first time, we have systematically explored the population of discrete X-ray sources in the outskirts of early-type galaxies. Based on a broad sample of 20 galaxies observed with Chandra we detected overdensity of X-ray sources in their outskirts. The overdensity appears as halos of resolved sources around the galaxies. These halos are broader than stellar light, extending out to at least similar to 10r(e) (r(e) is the effective radius). These halos are composed of sources fainter than similar to 5 x 10(38) erg/s, whereas the more luminous sources appear to follow the distribution of the stellar light, suggesting that the excess source population consists of neutron star binaries. Dividing the galaxy sample into four groups according to their stellar mass and specific frequency of globular clusters (GCs), we find that the extended halos are present in all groups except for the low-mass galaxies with low GC content. We propose that the extended halos may be comprised of two independent components, low-mass X-ray binaries (LMXBs) located in GCs, which are known to have a wider distribution than the stellar light, and neutron star LMXBs kicked out of the main body of the parent galaxy by supernova explosions. The available deep optical and X-ray data of NGC 4365 support this conclusion. For this galaxy we identified 60.1 +/- 10.8 excess sources in the (4-10)r(e) region of which similar to 40% are located in GCs, whereas similar to 60% are field LMXBs. We interpret the latter as kicked neutron star LMXBs. We discuss the implications of these results for the natal kick distributions of black holes and neutron stars. C1 [Zhang, Z.; Gilfanov, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. [Bogdan, A.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Zhang, Z (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany. EM zzhang@mpa-garching.mpg.de; gilfanov@mpa-garching.mpg.de FU NASA [PF1-120081, NAS8-03060]; Chandra X-ray Center FX We thank Andrew Cooper, Diederik Kruijssen, and Jingying Wang for discussions which have improved this paper. We thank Klaus Dolag for the discussion of the intracluster light in clusters of galaxies. This research has made use of Chandra archival data provided by Chandra X-ray Center, and 2MASS Large Galaxy Atlas data provided by NASA/IPAC infrared science archive. Akos Bogdan acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant number PF1-120081 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 57 TC 3 Z9 3 U1 0 U2 2 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD AUG PY 2013 VL 556 AR A9 DI 10.1051/0004-6361/201220685 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 211GH UT WOS:000323893500009 ER PT J AU Caldwell, L Bakker, VJ Sillett, TS Desrosiers, MA Morrison, SA Angeloni, LM AF Caldwell, Luke Bakker, Victoria J. Sillett, T. Scott Desrosiers, Michelle A. Morrison, Scott A. Angeloni, Lisa M. TI REPRODUCTIVE ECOLOGY OF THE ISLAND SCRUB-JAY SO CONDOR LA English DT Article DE Aphelocoma insularis; California; habitat-specific demography; nest survival; observer effects; reproductive ecology; Santa Cruz Island ID SANTA-CRUZ ISLAND; NEST-SITE SELECTION; TERRITORY SIZE; APHELOCOMA-INSULARIS; SWAINSONS WARBLERS; HABITAT STRUCTURE; POPULATION-SIZE; SONGBIRD NESTS; PREDATION RISK; SUCCESS AB We investigated the reproductive ecology of the Island Scrub-Jay (Aphelocoma insularis), which is endemic to Santa Cruz Island, California, and is a species of conservation concern. We documented daily nest survival, probability of renesting, annual fledging success, and breeding behavior, and determined how these factors varied in relation to the habitat characteristics of the jays' home ranges. Clutch sizes, feeding rates, and nest attendance were not correlated with chaparral cover or with home-range size. In contrast, nest predation, which accounted for 92% of documented nest failures, was less likely at nests that were more concealed, at nests of breeding pairs with home ranges that were smaller and had a greater proportion of taller vegetation, and at nests that were initiated earlier in the breeding season. Researchers' activity near nests increased the likelihood of predation, although the effect diminished with a nest's age. Despite relatively low nest survival, the high frequency of renesting allowed pairs to fledge an average of 1.1 +/- 0.1 young per year, or 1.8 +/- 0.2 young after the effects of the observer were accounted for. Currently, chaparral habitats on Santa Cruz Island are regenerating following the removal of exotic herbivores. This regeneration could in turn increase and improve breeding habitat for this island endemic. C1 [Caldwell, Luke; Desrosiers, Michelle A.; Angeloni, Lisa M.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Bakker, Victoria J.; Sillett, T. Scott] Natl Zool Pk, Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Washington, DC 20013 USA. [Morrison, Scott A.] Nature Conservancy, San Francisco, CA 94105 USA. RP Caldwell, L (reprint author), Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. EM lukecaldwell@hotmail.com FU Nature Conservancy; Channel Islands National Park; University of California's Santa Cruz Island Reserve; Smithsonian Institution; Colorado State University FX We thank The Nature Conservancy, Channel Islands National Park, and the University of California's Santa Cruz Island Reserve for support of the Island Scrub-Jay Conservation Initiative. This work was done at the University of California Natural Reserve System's Santa Cruz Island Reserve on property owned and managed by The Nature Conservancy. Karl Bardon, Sinead Borchert, Jenelle Dowling, Ben Griffith, Eileen Muller, Kyle Pias, and Anna Potter provided excellent assistance in the field. We are grateful to Mika Altfeld, Christina Boser, Reed Bowman, Walter Boyce, Kate Faulkner, John Fitzpatrick, Cameron Ghalambor, Brian Guerrero, Kathryn Langin, Lyndal Laughrin, Mario Pesendorfer, Helen Sofaer, Jerre Stallcup, Lotus Vermeer, and Winston Vickers for advice and logistical support, and to Brian Cohen for the map figures. We also thank Robert Curry and Claire Curry for perceptive comments that improved this paper. Funding was provided by The Nature Conservancy, the Smithsonian Institution, Channel Islands National Park, and Colorado State University. NR 62 TC 6 Z9 6 U1 3 U2 43 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 AUG PY 2013 VL 115 IS 3 BP 603 EP 613 DI 10.1525/cond.2013.120028 PG 11 WC Ornithology SC Zoology GA 213TH UT WOS:000324082600017 ER PT J AU Capper, A Flewelling, LJ Arthur, K AF Capper, Angela Flewelling, Leanne J. Arthur, Karen TI Dietary exposure to harmful algal bloom (HAB) toxins in the endangered manatee (Trichechus manatus latirostris) and green sea turtle (Chelonia mydas) in Florida, USA SO HARMFUL ALGAE LA English DT Article DE Brevetoxin; Okadaic acid; Saxitoxin; Lyngbyatoxin-A; Cyanobacteria; Dinoflagellate ID INDIAN RIVER LAGOON; CYANOBACTERIUM LYNGBYA-MAJUSCULA; RED TIDE DINOFLAGELLATE; KARENIA-BREVIS; OKADAIC ACID; MARINE CYANOBACTERIUM; SECONDARY METABOLITES; PYRODINIUM-BAHAMENSE; COASTAL WATERS; POTENTIAL ROLE AB Florida is a hotspot for cyano- and microalgal harmful algal blooms (HABs) with annual red-tide events off-shore and blooms of Lyngbya spp. commonly observed in both marine and freshwater environments. This region also provides extensive foraging habitat for large populations of herbivorous green turtles (Chelonia mydas) and manatees (Trichechus manatus latirostris). The exposure of aquatic organisms to HAB toxins is not well known and whilst acute exposures are better understood, the vulnerability of aquatic animals to chronic exposure from multiple HAB toxins over prolonged periods has rarely been addressed. This study aimed to identify the presence of toxic compounds produced by HAB species commonly found in Florida (brevetoxins, okadaic acid, saxitoxins and Lyngbya toxins) in tissues and gut samples from manatee and green sea turtles that stranded in Florida, USA. Muscle, liver and alimentary tract samples were opportunistically collected from 14 manatees and 13 green turtles that stranded on the Florida shoreline between December 2003 and February 2006. Samples from each animal were assessed for the presence of brevetoxin, okadaic acid, lyngbyatoxin-A and saxitoxin. Nine (64%) manatees and 11 (85%) turtles were found to have been exposed to one or more of the HAB toxins. Okadaic acid and saxitoxin were only found in alimentary tract samples, whereas brevetoxin was more widely distributed. No lyngbyatoxin-A was observed in any tissue samples. The majority of turtles (13) stranded on the Atlantic coast between St. Johns and Monroe counties, with one on the Gulf coast at Bay County, whereas nine manatees were stranded on the Gulf coast between Levy and Lee counties, with the remaining five between Volusia and Brevard counties on the Atlantic coast. This HAB toxin screen has identified that a large proportion of a random sample of turtles and manatees that stranded in Florida in 2003-2006 were exposed to HAB toxins. Most of the concentrations measured were low, and the toxins were directly linked to the death of only three of these animals. However, the presence of these compounds, and in some cases the presence of multiple HAB toxins in individual animals, indicates that turtles and manatees in Florida are exposed to deleterious compounds at sub-lethal levels in their environment, which could ultimately compromise their health. (C) 2013 Elsevier B.V. All rights reserved. C1 [Capper, Angela] James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. [Capper, Angela] James Cook Univ, Ctr Sustainable Trop Fisheries & Aquaculture, Townsville, Qld 4811, Australia. [Capper, Angela; Arthur, Karen] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Flewelling, Leanne J.] Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, St Petersburg, FL 33701 USA. RP Capper, A (reprint author), James Cook Univ, Sch Marine & Trop Biol, Townsville, Qld 4811, Australia. EM angela.capper@jcu.edu.au; Leanne.Flewelling@myfwc.com; karen.arthur@anu.edu.au RI CSTFA, ResearcherID/P-1067-2014; OI Capper, Angela/0000-0002-4922-0253 FU Smithsonian Marine Station Fellowship; US Dept. of Commerce [NA05 NOS 4781194]; Florida Fish and Wildlife Conservation Commission FX This research was funded by a Smithsonian Marine Station Fellowship to A.C., Grant Number NA05 NOS 4781194 from the US Dept. of Commerce (DoC, NOAA, ECOHAB programme) through UNC-CH, and the Florida Fish and Wildlife Conservation Commission. The findings, opinions and recommendations expressed in this publication are those of the authors and not necessarily those of the DoC. The authors thank veterinarians and staff at the Marine Mammal Pathobiology Laboratory and Karrie Minch and staff at the Sea Turtle Stranding and Salvage Network for their assistance with tissue acquisition and stranding data. Tissue collection and analysis was carried out in accordance with Permit No. MA773494-8 for manatees and Marine Turtle Permit No. 105 for green sea turtles. This is contribution 911 of the Smithsonian Marine Station, Fort Pierce, Florida. NR 109 TC 9 Z9 9 U1 10 U2 134 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 1568-9883 J9 HARMFUL ALGAE JI Harmful Algae PD AUG PY 2013 VL 28 BP 1 EP 9 DI 10.1016/j.hal.2013.04.009 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 210WW UT WOS:000323866800001 ER PT J AU Labandeira, CC AF Labandeira, Conrad C. TI A paleobiologic perspective on plant-insect interactions SO CURRENT OPINION IN PLANT BIOLOGY LA English DT Review ID LONG-PROBOSCID SCORPIONFLIES; NORTH-CENTRAL TEXAS; ARTHROPOD ASSOCIATIONS; FOSSIL EVIDENCE; CLIMATE-CHANGE; EARLY HISTORY; POLLINATION; HERBIVORY; ANGIOSPERMS; COEVOLUTION AB Fossil plant-insect associations (PI As) such as herbivory and pollination have become increasingly relevant to paleobiology and biology. Researchers studying fossil PI As now employ procedures for assuring unbiased representation of field specimens, use of varied analytical quantitative techniques, and address ecological and evolutionarily important issues. For herbivory, the major developments are: Late Silurian-Middle Devonian (ca. 420-385 Ma(a)) origin of herbivory; Late Pennsylvanian (318-299 Ma) expansion of herbivory; Permian (299-252 Ma) herbivore colonization of new habitats; consequences of the end-Permian (252 Ma) global crisis; early Mesozoic (ca. 235-215 Ma) rediversification of plants and herbivores; end-Cretaceous (66.5 Ma) effects on extinction; and biological effects of the Paleocene-Eocene Thermal Maximum (PETM) (55.8 Ma). For pollination, salient issues include: Permian pollination evidence; the plant hosts of mid-Mesozoic (ca. 160-110 Ma) long-proboscid pollinators; and effect of the angiosperm revolution (ca. 125-90 Ma) on earlier pollinator relationships. Multispecies interaction studies, such as contrasting damage types with insect diversity and establishing robust food webs, expand the compass and relevance of past PIAs. C1 [Labandeira, Conrad C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Labandeira, Conrad C.] Rhodes Univ, Dept Geol, ZA-6140 Grahamstown, South Africa. [Labandeira, Conrad C.] Capital Normal Univ, Coll Life Sci, Beijing 100048, Peoples R China. [Labandeira, Conrad C.] Univ Maryland, Dept Entomol, College Pk, MD 20742 USA. [Labandeira, Conrad C.] Univ Maryland, BEES Program, College Pk, MD 20742 USA. RP Labandeira, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. EM labandec@si.edu FU [DEB-0919071] FX I thank Beverley Glover and Pradeep Kachroo for an invitation to provide this manuscript. Finnegan Marsh drafted and formatted the figures. Grant DEB-0919071 to P. Wilf is acknowledged. This is Contribution 254 of the Evolution of Terrestrial Ecosystem consortium at the National Museum of Natural History, in Washington, DC. NR 57 TC 18 Z9 20 U1 9 U2 114 PU CURRENT BIOLOGY LTD PI LONDON PA 84 THEOBALDS RD, LONDON WC1X 8RR, ENGLAND SN 1369-5266 EI 1879-0356 J9 CURR OPIN PLANT BIOL JI Curr. Opin. Plant Biol. PD AUG PY 2013 VL 16 IS 4 BP 414 EP 421 DI 10.1016/j.pbi.2013.06.003 PG 8 WC Plant Sciences SC Plant Sciences GA 210XW UT WOS:000323869400004 PM 23829938 ER PT J AU Davidson, TM de Rivera, CE Canton, JT AF Davidson, Timothy M. de Rivera, Catherine E. Canton, James T. TI Small increases in temperature exacerbate the erosive effects of a non-native burrowing crustacean SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Bioerosion; Burrowing isopod; Climate change; Ecosystem engineering; Invasive species; Temperature effects ID RECENT CLIMATE-CHANGE; SPHAEROMA-QUOIANUM; BORING CRUSTACEANS; WATER TEMPERATURE; FOOD-WEB; MARINE; COMMUNITY; ECOSYSTEM; RESPONSES; PLASTICS AB Increases in temperature associated with global climate change are predicted to elicit drastic changes, especially to marine and freshwater ecosystems. Even small changes in water temperature (1-2 degrees C) may alter rates of biological activity, with concomitant effects to communities and ecosystems. The biological erosion of marine habitats and structures is a rarely considered yet important activity that is likely to be influenced by changing ocean temperatures. We conducted an experiment to test how seawater temperature affects erosion by a non-native crustacean (Sphaeroma quoianum). Aquaria were maintained at one of thirteen temperatures (7.5 degrees C-25.2 degrees C). In each aquarium, twenty isopods were encaged with an expanded polystyrene foam block (800 ml) and left to burrow. Polystyrene floats under docks are often damaged by isopods in the field. After two months, isopods created the longest burrows in the moderate seawater temperatures (13.8 degrees C-18.3 degrees C); these temperatures were 1.1-5.6 degrees C higher than the mean ambient temperatures whence they came. Shorter burrows were observed for the coldest (7.5 degrees C) and warmest seawater treatments (25.2 degrees C). These results indicate that increasing seawater temperatures can exacerbate the bioerosive effects of non-native S. quoianum until a threshold, after which the impacts diminish. Because ocean temperatures are predicted to increase 1.5-2.6 degrees C in the next 90 years, our data suggest erosion by this non-native crustacean will increase 14.7-37.6% in Coos Bay/South Slough, Oregon (where isopods were collected). However, other invaded bays on the Pacific coast of North America may also experience mean increases of biological erosion of 6.6-29.8%. Since biological activity is tightly coupled with temperature in many species, we hypothesize that the biological erosion rates of other erosive species will also increase with rising water temperatures affecting marine habitats, communities, and structures. (C) 2013 Elsevier B.V. All rights reserved. C1 [Davidson, Timothy M.; de Rivera, Catherine E.] Portland State Univ ESM, Dept Environm Sci & Management, Portland, OR 97207 USA. [Canton, James T.] Williams Coll Myst Seaport, Maritime Studies Program, Mystic, CT 06355 USA. RP Davidson, TM (reprint author), Smithsonian Trop Res Inst, Apartado Postal 0843-03092, Balboa, Ancon, Panama. EM DavidsonT@si.edu; derivera@pdx.edu; James.T.Carlton@williams.edu OI Davidson, Timothy/0000-0001-9535-7982 FU Estuarine Reserves Division, Office of Ocean and Coastal Resource Management, National Ocean Service, National Oceanic and Atmospheric Administration FX We are grateful to Anne Phillip, Dereck Guba, and Justin Ashby for their assistance during the experiment. Heejun Chang, Linda Mantel, Yangdong Pan, Gregory Ruiz, Steven Rumrill, and Mark Sytsma provided helpful advice and comments. We thank Elise Granek for her advice and for allowing the use of equipment We also thank the anonymous reviewers for their comments on this manuscript. This research was conducted in the National Estuarine Research Reserve System under an award from the Estuarine Reserves Division, Office of Ocean and Coastal Resource Management, National Ocean Service, National Oceanic and Atmospheric Administration. NR 53 TC 3 Z9 3 U1 4 U2 42 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD AUG PY 2013 VL 446 BP 115 EP 121 DI 10.1016/j.jembe.2013.05.008 PG 7 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 201JZ UT WOS:000323139200016 ER PT J AU Yarrington, CS Tyler, AC Altieri, AH AF Yarrington, Charles S. Tyler, Anna Christina Altieri, Andrew H. TI Do snails facilitate bloom-forming macroalgae in a eutrophic estuary? SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Eutrophication; Feedbacks; Herbivory; Indirect effects; Macroalgal bloom; Nutrient cycling ID ILYANASSA-OBSOLETA SAY; TEMPERATE COASTAL LAGOON; MARINE ECOSYSTEMS; MUD SNAIL; NUTRIENT REGENERATION; RELATIVE IMPORTANCE; SHALLOW ESTUARIES; GROWTH; NITROGEN; COMMUNITY AB Blooms of macroalgae are one of the most visible and problematic results of eutrophication-driven estuarine degradation because they can smother seagrass, obstruct fishing, and close beaches to tourism. Not surprisingly, high densities of herbivores are commonly associated with these blooms. Invertebrates in other systems can facilitate macrophyte growth under equilibrium conditions by releasing nutrients or reducing competitors. Based on laboratory experiments it has been suggested that the omnivorous snail Ilyanassa obsoleta likewise facilitates bloom-forming macroalgae in estuaries of the Northeastern US. If snails enhance macroalgal blooms as suggested, it would have broad implications for nutrient retention and cycling in estuaries. We tested whether snails actually do facilitate macroalgal blooms in a natural setting through community surveys, laboratory incubations, and field experiments. We confirmed in our surveys that snail densities were positively correlated with macroalgal biomass, and in laboratory incubations that snail excreta enhanced macroalgal growth and that snail activity mobilized sediment nutrients and enhanced sediment-water column coupling. Snails thus have the potential to influence nutrient recycling and retention. However, snails did not facilitate macroalgal growth in our field manipulations of snails and bloom-forming macroalgae along an estuarine eutrophication gradient. Macroalgal growth in our experiment was highly variable across the estuarine gradient and through the growing season, suggesting that large-scale variation in physical factors such as nutrients, light, or temperature plays the dominant role in limiting macroalgal blooms. The departure of our field results from predictions of laboratory studies reinforces previous warnings that laboratory experiments can be useful tools for elucidating mechanisms that drive field patterns, but are not a substitute for field experiments where they are possible. While snails do not appear to directly influence macroalgal growth, we suggest that the potential influence of snails on benthic metabolism and nutrient cycling demands further investigation in the field. (C) 2013 Elsevier B.V. All rights reserved. C1 [Yarrington, Charles S.; Tyler, Anna Christina] Rochester Inst Technol, Coll Sci, Gosnell Sch Life Sci, Rochester, NY 14623 USA. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Tyler, AC (reprint author), Rochester Inst Technol, Coll Sci, Gosnell Sch Life Sci, 85 Lomb Mem Dr, Rochester, NY 14623 USA. EM actsbi@rit.edu FU National Science Foundation [OCE 0727642] FX We thank E. Hane, H. Pough and two anonymous reviewers for their helpful comments that improved the manuscript A. Giblin, K. Foreman, R. Marino, R. Howarth and M. Hayn provided logistical support in Woods Hole. B. Bourdon, M. Bida, N. McLenaghan, C. Scheiner, J. Barnette, and A. Abdul Rahman provided invaluable assistance in the field and laboratory. Funding for this work was provided by the National Science Foundation grant number OCE 0727642 to A.C.T. [ST] NR 71 TC 3 Z9 3 U1 2 U2 38 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD AUG PY 2013 VL 446 BP 253 EP 261 DI 10.1016/j.jembe.2013.05.019 PG 9 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 201JZ UT WOS:000323139200032 ER PT J AU Long, WC Sellers, AJ Hines, AH AF Long, W. Christopher Sellers, Andrew J. Hines, Anson H. TI Mechanism by which coarse woody debris affects predation and community structure in Chesapeake Bay SO JOURNAL OF EXPERIMENTAL MARINE BIOLOGY AND ECOLOGY LA English DT Article DE Blue crab; Coarse woody debris; Community structure; Grass shrimp; Mummichog; Predation ID HABITAT COMPLEXITY; FORAGING SUCCESS; TEMPORAL VARIATION; SHALLOW-WATER; FISH HABITAT; BLUE CRABS; FOOD-WEB; STREAM; RIVER; REFUGE AB Coarse woody debris (CWD) provides a structured habitat in aquatic systems. It is associated with a higher abundance, diversity, and productivity of aquatic animals and can provide a shelter from physical stressors and predation. We investigated the effects of CWD on predation risk and community structure in two field experiments in the Rhode River, Chesapeake Bay. In the first experiment we assessed the effects of the orientation (horizontal or vertical) and complexity (simple or crossed) of CWD, and in the second experiment we investigated the effects of interstitial space (ISS). We measured predation risk in a tethering experiment for three species in each experiment: juvenile blue crab, Callinectes sapidus; mummichog (a type of killifish), Fundulus heteroditus; and grass shrimp, Palaemonetes pugio. These three species are common in nearshore Chesapeake Bay habitats but differ in their size and habitat use, allowing for a holistic examination of the function of CWD. At the end of the experiments, the benthic community inhabiting the CWD was sampled. By interpreting the community data in light of the predation experiments we were able to examine how the structural characteristics of the CWD affected predation to shape the benthic community. In the first experiment, lowest predation was experienced by blue crabs at the treatments with high complexity at the sediment surface, by mummichogs at all CWD treatments relative to control plots, and by grass shrimp in horizontally oriented treatments. In the second experiment, lowest predation was experienced by blue crabs at moderate to high ISSs, by mummichogs at intermediate ISSs, and by grass shrimp at low and high ISSs. Predation rates for each experimental species could be predicted by the size of the prey, and by both the size of their predators and the size of species that prey on the predators relative to the ISS of the structure. Community structure differed among treatments in both experiments and appeared to be driven primarily by predation risk; species whose predators were in high abundance in a treatment were less abundant themselves. This work demonstrates the importance of CWD and of wooded shorelines as important habitat for both economically and ecologically important species. It also highlights the importance of top-down forcing in the small scale community dynamics of these near-shore habitats. Published by Elsevier B.V. C1 [Long, W. Christopher; Sellers, Andrew J.; Hines, Anson H.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Long, WC (reprint author), NOAA, Kodiak Lab, Resource Assessment & Conservat Engn Div, Alaska Fisheries Sci Ctr,Natl Marine Fisheries Se, 301 Res Ct, Kodiak, AK 99615 USA. EM chris.long@noaa.gov RI Long, William/C-7074-2009 OI Long, William/0000-0002-7095-1245 FU Marine Science Network Fellowship from the Smithsonian Institution; NOAA grant through the Blue Crab Advanced Research Consortium; NSF Grant for Research Experience for Undergraduates FX We thank Lela Schlenker, Laila Melendez, Paige Roberts, Margaret Kramer, and the other members of the Smithsonian Environmental Research Center crab lab for the help with field and laboratory work, the SERC invasions lab for shrimp tethering lessons, and Robert Aguilar for the help in identifying fish and running statistics. WCL was supported by a Marine Science Network Fellowship from the Smithsonian Institution and AS was supported by an Internship funded by NOAA grant through the Blue Crab Advanced Research Consortium to AHH and NSF Grant for Research Experience for Undergraduates. Comments from Jordana Long, Ben Daily, Frank Morado, Robert Foy, and two anonymous reviewers substantially improved previous versions of the manuscript. The findings and conclusions in the paper are those of the authors and do not necessarily represent the views of the National Marine Fisheries Service, NOAA. [ST] NR 48 TC 6 Z9 6 U1 4 U2 41 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0981 J9 J EXP MAR BIOL ECOL JI J. Exp. Mar. Biol. Ecol. PD AUG PY 2013 VL 446 BP 297 EP 305 DI 10.1016/j.jembe.2013.05.021 PG 9 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 201JZ UT WOS:000323139200037 ER PT J AU Moreiras, S Marsh, E Nami, H Estrella, D Duran, V AF Moreiras, Stella Marsh, Erik Nami, Hugo Estrella, Diego Duran, Victor TI Holocene geomorphology, tectonics, and archaeology in Barrancas, arid Central Andes piedmont (33 degrees S) SO APPLIED GEOGRAPHY LA English DT Article DE Tectonics; Lagoons; Badlands; Archaeological site formation processes; Argentina ID LATE PLEISTOCENE; ARGENTINA; MENDOZA; EXCURSION AB Archaeology and geomorphology are closely linked in Barrancas, Argentina, where both disciplines are necessary to understand human environment interactions during the Holocene. The geomorphology suggests that the area was located in a distal alluvial environment of the Zonda paleo-river that drained to the east. Active tectonics during the Pliocene-Early Pleistocene caused the gradual uplift of the Lunlunta Sierras to the southwest, which led to the bifurcation of the paleo-river. For most of the Holocene, the area was seasonally flooded, suggesting a lacustrine microenvironment A long record of human occupation beginning in the Early Holocene suggests an extended period of intimate human environment interactions. Recently, the environment has shifted dramatically. Erosion has created a badlands and significantly impacted the archaeological record. Understanding geomorphological processes is central for archaeological research in general, and especially in Barrancas. This research is an integral part of the ongoing community archaeology program in the area, and for the planned creation of an archaeological reserve. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Moreiras, Stella] Consejo Nacl Invest Cient & Tecn, IANIGLA, CCT Mendoza, Mendoza, Argentina. [Marsh, Erik] UNCuyo, Lab Paleo Ecol Humana, Mendoza, Argentina. [Nami, Hugo] Consejo Nacl Invest Cient & Tecn, IGEBA, Dpto Ciencias Geol, FCEN,UBA,CABA, RA-1033 Buenos Aires, DF, Argentina. [Nami, Hugo] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Estrella, Diego] UNCuyo, Fac Filosofia & Letras, Lab Geoarqueol, Mendoza, Argentina. [Duran, Victor] UNCuyo, CONICET, Lab Geoarqueol, Mendoza, Argentina. RP Moreiras, S (reprint author), Consejo Nacl Invest Cient & Tecn, IANIGLA, CCT Mendoza, Mendoza, Argentina. EM moreiras@mendoza-conicet.gob.ar; erik.marsh@gmail.com; hgnami@fullbrightmail.org; uzphaestar@gmail.com; duranvic@logos.uncu.edu.ar NR 50 TC 2 Z9 2 U1 1 U2 5 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0143-6228 J9 APPL GEOGR JI Appl. Geogr. PD AUG PY 2013 VL 42 BP 217 EP 226 DI 10.1016/j.apgeog.2013.04.005 PG 10 WC Geography SC Geography GA 204IX UT WOS:000323360100022 ER PT J AU Sargis, EJ Woodman, N Morningstar, NC Reese, AT Olson, LE AF Sargis, Eric J. Woodman, Neal Morningstar, Natalie C. Reese, Aspen T. Olson, Link E. TI Morphological distinctiveness of Javan Tupaia hypochrysa (Scandentia, Tupaiidae) SO JOURNAL OF MAMMALOGY LA English DT Article DE cranium; digits; hand; mandible; manus; postcranium; rays; skeleton; skull; treeshrews ID TREE SHREWS; PHYLOGENETIC IMPLICATIONS; FUNCTIONAL-MORPHOLOGY; TREESHREWS MAMMALIA; SORICIDAE; BOUNDARIES; HIGHLANDS; GUATEMALA; CRYPTOTIS; SKULL AB The common treeshrew, Tupaia glis, represents a species complex with a complicated taxonomic history. It is distributed mostly south of the Isthmus of Kra on the Malay Peninsula and surrounding islands. In our recent revision of a portion of this species complex, we did not fully assess the population from Java (T. "glis" hypochrysa) because of our limited sample. Herein, we revisit this taxon using multivariate analyses in comparisons with T. glis, T. chrysogaster of the Mentawai Islands, and T. ferruginea from Sumatra. Analyses of both the manus and skull of Javan T. "glis" hypochrysa show it to be most similar to T. chrysogaster and distinct from both T. glis and T. ferruginea. Yet, the Javan population and T. chrysogaster have different mammae counts, supporting recognition of T. hypochrysa as a distinct species. The change in taxonomic status of T. hypochrysa has conservation implications for both T. glis and this Javan endemic. C1 [Sargis, Eric J.; Morningstar, Natalie C.] Yale Univ, Dept Anthropol, New Haven, CT 06520 USA. [Sargis, Eric J.; Reese, Aspen T.] Yale Univ, Dept Ecol & Evolutionary Biol, New Haven, CT 06520 USA. [Sargis, Eric J.; Reese, Aspen T.] Yale Peabody Museum Nat Hist, Div Vertebrate Zool, New Haven, CT 06520 USA. [Woodman, Neal] Smithsonian Inst, Natl Museum Nat Hist, Patuxent Wildlife Res Ctr, US Geol Survey, Washington, DC 20013 USA. [Olson, Link E.] Univ Alaska Fairbanks, Univ Alaska Museum, Fairbanks, AK 99775 USA. RP Sargis, EJ (reprint author), Yale Univ, Dept Anthropol, POB 208277, New Haven, CT 06520 USA. EM eric.sargis@yale.edu OI Woodman, Neal/0000-0003-2689-7373 FU National Science Foundation [DEB-0542532/0542725]; Alaska EPSCoR grant; United States Geological Survey's Patuxent Wildlife Research Center; Yale Peabody Museum of Natural History Summer Internship Program FX This research was supported by National Science Foundation grant DEB-0542532/0542725 and an Alaska EPSCoR grant to EJS and LEO. Additional support was provided to NW from the United States Geological Survey's Patuxent Wildlife Research Center and to NCM from the Yale Peabody Museum of Natural History Summer Internship Program. We thank the following curators, collection managers, and museums for access to the specimens in their collections: E. Westwig, D. Lunde, and R. Voss, AMNH, New York; R. Portela-Miguez, L. Tomsett, and P. Jenkins, BMNH, London; B. Stanley and L. Heaney, Field Museum of Natural History (FMNH), Chicago; J. Dines, Los Angeles County Museum of Natural History, Los Angeles (LACM); J. Chupasko and M. Omura, Museum of Comparative Zoology at Harvard University (MCZ), Cambridge, Massachusetts; C. Conroy and J. Patton, Museum of Vertebrate Zoology at University of California, Berkeley (MVZ); R. Winkler, Naturhistorisches Museum Basel (NMB); B. Herzig, A. Bibl, A. Gamauf, Naturhistorisches Museum Wien, Vienna (NMW); H. van Grouw, Nationaal Natuurhistorisch Museum, Leiden (RMNH); L. Gordon, R. Thorington, K. Helgen, and D. Lunde, USNM, Washington, DC; R. Angermann and F. Mayer, Museum fur Naturkunde (ZMB), Berlin; and M. Anderson, Zoologisk Museum University of Copenhagen (ZMUC). We are grateful to S. Raredon, Division of Fishes, Museum Support Center, USNM, for assistance with the digital X-ray system, and to R. Portela-Miguez, Department of Zoology, BMNH, for providing X-rays of the 2 BMNH T. hypochrysa specimens. We thank E. Meijaard and an anonymous reviewer for comments that improved the manuscript. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the United States government. NR 33 TC 5 Z9 5 U1 0 U2 8 PU ALLIANCE COMMUNICATIONS GROUP DIVISION ALLEN PRESS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-2372 J9 J MAMMAL JI J. Mammal. PD AUG PY 2013 VL 94 IS 4 BP 938 EP 947 DI 10.1644/13-MAMM-A-042.1 PG 10 WC Zoology SC Zoology GA 206OS UT WOS:000323532600018 ER PT J AU Sedio, BE Paul, JR Taylor, CM Dick, CW AF Sedio, Brian E. Paul, John R. Taylor, Charlotte M. Dick, Christopher W. TI Fine-scale niche structure of Neotropical forests reflects a legacy of the Great American Biotic Interchange SO NATURE COMMUNICATIONS LA English DT Article ID TROPICAL FORESTS; SPECIES COEXISTENCE; ADAPTIVE EVOLUTION; PLANT DIVERSITY; ANDEAN UPLIFT; COMMUNITY; DISPERSAL; PHYLOGENY; RUBIACEAE; PATTERNS AB The tendency of species to retain their ancestral niches may link processes that determine community assembly with biogeographic histories that span geological time scales. Biogeographic history is likely to have had a particularly strong impact on Neotropical forests because of the influence of the Great American Biotic Interchange, which followed emergence of a land connection between North and South America similar to 3 Ma. Here we examine the community structure, ancestral niches and ancestral distributions of the related, hyperdiverse woody plant genera Psychotria and Palicourea (Rubiaceae) in Panama. We find that 49% of the variation in hydraulic traits, a strong determinant of community structure, is explained by species' origins in climatically distinct biogeographic regions. Niche evolution models for a regional sample of 152 species indicate that ancestral climatic niches are associated with species' habitat distributions, and hence local community structure and composition, even millions of years after dispersal into new geographic regions. C1 [Sedio, Brian E.; Dick, Christopher W.] Univ Michigan, Dept Ecol & Evolutionary Biol, Ann Arbor, MI 49109 USA. [Paul, John R.] Colorado State Univ, Dept Biol, Ft Collins, CO 80523 USA. [Taylor, Charlotte M.] Missouri Bot Garden, St Louis, MO 63166 USA. [Dick, Christopher W.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sedio, BE (reprint author), Univ Michigan, Dept Ecol & Evolutionary Biol, 830 N Univ, Ann Arbor, MI 49109 USA. EM bsedio@umich.edu FU NSF [DEB 1010816] FX We thank R. Magill, R. Foster and the Environmental and Conservation Program of the Field Museum, as well as D. Lorence and the National Tropical Botanical Garden whose botanical collections made this study possible. We also thank A. King, S. Smith, D. Goldberg, J. Wright, J. Bemmels, the Angert Lab and the University of Michigan Plant Ecology Discussion Group for intellectual input, the Smithsonian Tropical Research Institute for support of the original fieldwork on Barro Colorado Island and J. Megahan for assistance with the artwork. This study was facilitated by the support of NSF DEB 1010816 and an NSF Graduate Research Fellowship to B.E.S. NR 45 TC 9 Z9 9 U1 5 U2 50 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD AUG PY 2013 VL 4 AR 2317 DI 10.1038/ncomms3317 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 209JQ UT WOS:000323752300002 PM 23939338 ER PT J AU Hirsch, BT Tujague, MP Di Blanco, YE Di Bitetti, MS Janson, CH AF Hirsch, Ben T. Tujague, Maria P. Di Blanco, Yamil E. Di Bitetti, Mario S. Janson, Charles H. TI Comparing capuchins and coatis: causes and consequences of differing movement ecology in two sympatric mammals SO ANIMAL BEHAVIOUR LA English DT Article DE animal movement; capuchin; Cebus apella nigritus; coati; foraging; Nasua nasua; straightness index; trapline; travel behaviour; travel cost ID CEBUS-APELLA-NIGRITUS; GROUP SPATIAL POSITION; HOME-RANGE USE; NASUA-NASUA; BEHAVIORAL ECOLOGY; MULTIPLE NUTRIENTS; VIGILANCE BEHAVIOR; FEEDING ECOLOGY; FOOD DETECTION; TRAVEL SPEED AB The mechanisms that shape animal movement decisions at the level of an individual or a group of animals can scale up to affect larger-scale ecological processes. Ecologists often use mechanistic animal movement models to understand these links, but animal movement models rarely connect empirically with an understanding of how animals actually decide to move around in their environment. To better understand this relationship, we compared the travel behaviour of two sympatric mammal species that have broadly similar diets: brown capuchin monkeys, Cebus apella nigritus, and ring-tailed coatis, Nasua nasua. According to most mechanistic animal movement models, species that exploit the same resources should show similar movement patterns. Although the fruit component of coati and capuchin diets is very similar, coatis primarily feed on invertebrates in the leaf litter or soil, while capuchins forage on invertebrate prey in the forest canopy. We found that these two species showed markedly different movement patterns: while capuchins typically travelled between fruit trees in relatively straight lines, coatis had significantly more tortuous daily travel paths and frequently visited the same fruit trees more than once per day. These circular coati travel paths would not be predicted by most foraging models. We posit that these differences in coati and capuchin movement patterns are driven by differences in arboreal and terrestrial travel costs, exploitation of fallen fruits and shifts in foraging behaviour over the course of the day. Because these seemingly small differences between the two species lead to major differences in movement behaviour, we posit that animal movement models need to better incorporate (1) travel costs, (2) both directed travel and random food search and (3) realistic diet models that include resources with different nutrient compositions. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Hirsch, Ben T.] Smithsonian Trop Res Inst, Balboa, Panama. [Hirsch, Ben T.] Ohio State Univ, Sch Environm & Nat Resources, Columbus, OH 43210 USA. [Tujague, Maria P.] Univ Nacl La Plata, Fac Ciencias Nat & Museo, CONICET, Natl Res Council, La Plata, Buenos Aires, Argentina. [Tujague, Maria P.; Di Blanco, Yamil E.; Di Bitetti, Mario S.] Univ Nacl Misiones, CONICET, Natl Res Council, Inst Biol Subtrop,Fac Ciencias Forestales, Puerto Iguazu, Misiones, Argentina. [Tujague, Maria P.; Di Blanco, Yamil E.; Di Bitetti, Mario S.] Asociac Civil Ctr Invest Bosque Atlantico CeIBA, Puerto Iguazu, Misiones, Argentina. [Janson, Charles H.] Univ Montana, Div Biol Sci, Missoula, MT 59812 USA. RP Hirsch, BT (reprint author), Ohio State Univ, Sch Environm & Nat Resources, 2021 Coffey Rd, Columbus, OH 43210 USA. EM hirschb@si.edu FU National Science Fund [BCS-0314525, BNS-9009023]; Argentine Research Council (CONICET); Idea Wild; American Society of Mammalogists; Fullbright FX We thank Alex Alcocer Aldunate, Ana Alvarez, Maria Celia Baldovino, Maria Veronica Cifre, Santiago Escobar, Carolina Ferrari, Emanuel Galetto, Elizabeth Gonzales Valentin, Rosalyn Johnson, Daniel Lambruschi, Luis Molina, Viviana Munoz, Juan Pablo Peretti, Noelia Rivas, Taylor Rubin, Fermino Silva and Mauro Tammone for help and assistance during the course of the field work. This paper has benefited tremendously thanks to comments by Margaret Crofoot, Esteban Fernandez-Juricic and two anonymous referees. We thank the Administracion de Parques Nacionales (APN) for permission to carry out work in Iguaz. This study was funded in part by National Science Fund grants (BCS-0314525 and BNS-9009023) to C.H.J. and B. T. H., an Argentine Research Council (CONICET) dissertation fellowship to M. P. T., grants from Idea Wild and American Society of Mammalogists to M. P. T., and a Fullbright to C.H.J. NR 68 TC 3 Z9 4 U1 3 U2 49 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 2013 VL 86 IS 2 BP 331 EP 338 PG 8 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 201XE UT WOS:000323175500014 ER PT J AU Ballentine, B Horton, B Brown, ET Greenberg, R AF Ballentine, Barbara Horton, Brent Brown, E. Tracy Greenberg, Russell TI Divergent selection on bill morphology contributes to nonrandom mating between swamp sparrow subspecies SO ANIMAL BEHAVIOUR LA English DT Article DE behaviour; Melospiza georgiana; morphological evolution; speciation; swamp sparrow ID MALE BIRD SONG; DARWINS FINCHES; FEMALE RESPONSE; ECOLOGICAL SPECIATION; ACOUSTIC ADAPTATION; MELOSPIZA-GEORGIANA; MITOCHONDRIAL-DNA; NATURAL-SELECTION; SEXUAL SELECTION; MARSH SPARROWS AB Traits subject to ecologically based divergent selection that also affect nonrandom mating (i.e. 'magic traits') may hasten incipient speciation. In this study, we investigated whether nonrandom mating results from ecological divergence between swamp sparrow, Melospiza georgiana, subspecies. As a by-product of adaptive divergence in bill morphology between populations of swamp sparrows, there is a corresponding divergence in features of song shown to be salient to females, potentially providing a mechanism of reproductive isolation. Thus, female mating preferences for song could result in prezygotic isolation that prevents gene flow between subspecies. In this study we tested the hypothesis that female preferences for song provide a mechanism of reproductive isolation that limits gene flow between subspecies. Using copulation solicitation assays, we found that female coastal plain swamp sparrows showed a significant preference for consubspecific songs over heterosubspecific songs. We further tested whether mating preferences in coastal populations explain observed differences in song between subspecies. We found evidence that mating preferences in coastal females may explain the evolution of some acoustic features of song. We suggest that the bill may be an example of a 'magic trait' that contributes to continued divergence of swamp sparrow subspecies. (C) 2013 The Association for the Study of Animal Behaviour. Published by Elsevier Ltd. All rights reserved. C1 [Ballentine, Barbara] Univ West Georgia, Dept Biol, Carrollton, GA USA. [Ballentine, Barbara; Horton, Brent; Brown, E. Tracy; Greenberg, Russell] Smithsonian Inst, Natl Zool Pk, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. [Horton, Brent] Emory Univ, Dept Psychol, Atlanta, GA 30322 USA. RP Ballentine, B (reprint author), Western Carolina Univ, Dept Biol, Cullowhee, NC 28723 USA. EM beballentine@email.wcu.edu FU Smithsonian Institution Endowment Grant; Friends of the National Zoo; National Zoological Park FX This project was supported by a Smithsonian Institution Endowment Grant, The Friends of the National Zoo, and The National Zoological Park. We thank members of the Migratory Bird Center for advice, support and feedback. We thank Steve Nowicki for advice on experimental design. We thank Jeff Podos, Tim Wright and two anonymous referees for helpful comments that improved the manuscript. NR 61 TC 5 Z9 5 U1 4 U2 63 PU ACADEMIC PRESS LTD- ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0003-3472 EI 1095-8282 J9 ANIM BEHAV JI Anim. Behav. PD AUG PY 2013 VL 86 IS 2 BP 467 EP 473 DI 10.1016/j.anbehav.2013.06.002 PG 7 WC Behavioral Sciences; Zoology SC Behavioral Sciences; Zoology GA 201XE UT WOS:000323175500030 ER PT J AU Kouba, AJ Lloyd, RE Houck, ML Silla, AJ Calatayud, N Trudeau, VL Clulow, J Molinia, F Langhorne, C Vance, C Arregui, L Germano, J Lermen, D Della Togna, G AF Kouba, Andrew J. Lloyd, Rhiannon E. Houck, Marlys L. Silla, Aimee J. Calatayud, Natalie Trudeau, Vance L. Clulow, John Molinia, Frank Langhorne, Cecilia Vance, Carrie Arregui, Lucia Germano, Jennifer Lermen, Dominik Della Togna, Gina TI Emerging trends for biobanking amphibian genetic resources: The hope, reality and challenges for the next decade SO BIOLOGICAL CONSERVATION LA English DT Article DE Amphibian; Biobanking; Sperm; Oocyte; Embryo; Cell culture; Assisted reproduction; Cryoconservation; Genetic resource bank (GRB) AB How to conserve our planet's rapidly disappearing biodiversity is one of the greatest challenges of our generation. Among terrestrial vertebrate taxa, amphibians are most at risk with 41% of all known species experiencing population declines and one-third threatened with extinction. Although many institutions have responded by establishing captive assurance colonies for several critically endangered amphibians, the resources provided by these conservation organizations will not be enough to save all species 'at risk' without a multi-pronged approach. Around the world, zoos, aquariums, governments, and conservation NGOs are beginning to establish amphibian gene banks to conserve, in perpetuity, the remaining extant genetic diversity for many of these critically endangered species. A suite of biomaterials has been targeted for cryoconservation including blood, cell cultures, tissues, spermatozoa, eggs, and embryos. Several international workshops on amphibian gene banking and assisted reproductive technologies have been held between 2010 and 2012, bringing together leading experts in the fields of amphibian ecology, physiology, and cryobiology to synthesize emerging trends for biobanking amphibian genetic resources, provide opportunities for collaboration, and discuss future research directions. The following review paper and summary will provide a synopsis of these international workshops, in particular the hopes, realities, and current challenges inherent to this applied research field. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Kouba, Andrew J.] Memphis Zoo, Conservat & Res Dept, Memphis, TN USA. [Lloyd, Rhiannon E.] Univ Portsmouth, Sch Pharm & Biomed Sci, Inst Biomed & Biomol Sci, Portsmouth, Hants, England. [Houck, Marlys L.; Germano, Jennifer] San Diego Zoo Global, Inst Conservat Res, Escondido, CA USA. [Silla, Aimee J.] Univ Wollongong, Sch Biol Sci, Inst Conservat Biol & Environm Management, Wollongong, NSW, Australia. [Calatayud, Natalie; Langhorne, Cecilia; Vance, Carrie] Mississippi State Univ, Dept Biochem Mol Biol Entomol & Plant Pathol, Mississippi State, MS 39762 USA. [Trudeau, Vance L.] Univ Ottawa, Dept Biol, Ctr Adv Res Environm Genom, Ottawa, ON K1N 6N5, Canada. [Clulow, John] Univ Newcastle, Sch Environm & Life Sci, Newcastle, NSW 2300, Australia. [Molinia, Frank] Landcare Res, Auckland, New Zealand. [Arregui, Lucia] Univ Autonoma Madrid, Dept Biol, E-28049 Madrid, Spain. [Lermen, Dominik] Fraunhofer Inst Biomed Engn, Dept Cell Biol & Appl Virol, D-66386 St Ingbert, Germany. [Della Togna, Gina] Smithsonian Conservat Biol Inst, Ctr Species Survival, Washington, DC USA. RP Kouba, AJ (reprint author), Memphis Zoo, Conservat & Res Dept, 2000 Prentiss Pl, Memphis, TN USA. EM akouba@memphiszoo.org RI Arregui, Lucia/C-2525-2013; OI Trudeau, Vance/0000-0002-0845-9444; Silla, Aimee/0000-0002-2277-9030 FU Institute of Museum and Library Services (IMLSs) [LG-25-09-0064-09]; Morris Animal Foundation [D08ZO-037]; Leverhulme Trust [ECF/2009/0123]; NSW Environmental Trust [2012/RD/0105]; Memphis Zoo's Conservation Action Network; Environment Canada; University of Ottawa Research Chair program; Australian Research Council; World Wildlife Fund; National Leadership Program Grant from IMLS [LG-25-08-0066] FX AK work was supported by a National Leadership Grant (LG-25-09-0064-09) from the Institute of Museum and Library Services (IMLSs) as well as a Morris Animal Foundation Grant (D08ZO-037). R.L. is grateful for funding from the Leverhulme Trust (ECF/2009/0123). AS is grateful to the NSW Environmental Trust (Grant Number: 2012/RD/0105). LA is thankful to the Memphis Zoo's Conservation Action Network for funding support. V.T. is grateful for support from Environment Canada and the University of Ottawa Research Chair program. J.C. is thankful for support from the Australian Research Council and World Wildlife Fund. MH work was supported by a National Leadership Program Grant (LG-25-08-0066) from IMLS. NR 113 TC 12 Z9 12 U1 7 U2 53 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0006-3207 J9 BIOL CONSERV JI Biol. Conserv. PD AUG PY 2013 VL 164 BP 10 EP 21 DI 10.1016/j.biocon.2013.03.010 PG 12 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 200RO UT WOS:000323086800002 ER PT J AU Davidson, BS Sattler, GD Via, S Braun, MJ AF Davidson, Brian S. Sattler, Gene D. Via, Sara Braun, Michael J. TI Reproductive isolation and cryptic introgression in a sky island enclave of Appalachian birds SO ECOLOGY AND EVOLUTION LA English DT Article DE Chickadees; hybridization; introgression; metapopulation dynamics; Poecile; reproductive isolating mechanism; speciation ID CHICKADEES PARUS-ATRICAPILLUS; BLACK-CAPPED CHICKADEE; MULTILOCUS GENOTYPE DATA; POPULATION-STRUCTURE; HYBRID ZONE; CAROLINA CHICKADEES; POECILE-ATRICAPILLUS; P-CAROLINENSIS; MITOCHONDRIAL-DNA; CLIMATE-CHANGE AB Reproductive isolation is central to the speciation process, and cases where the strength of reproductive isolation varies geographically can inform our understanding of speciation mechanisms. Although generally treated as separate species, Black-capped chickadees (Poecile atricapillus) and Carolina chickadees (P. carolinensis) hybridize and undergo genetic introgression in many areas where they come into contact across the eastern United States and in the northern Appalachian Mountains. The Great Smoky Mountains harbor the last large breeding population of atricapillus in the southern Appalachians, isolated from the species' main range by nearly 200 km. This population is believed to be reproductively isolated from local carolinensis due to an unusual, behaviorally mediated elevational range gap, which forms during the breeding season and may function as an incipient reproductive isolating mechanism. We examined the effectiveness of this putative isolating mechanism by looking for genetic introgression from carolinensis in Great Smoky Mountain atricapillus. We characterized this population and parental controls genetically using hundreds of amplified fragment length polymorphism (AFLP) loci as well as mitochondrial DNA (mtDNA) sequence data from cytochrome-b. Great Smoky Mountain atricapillus have experienced nuclear genetic introgression from carolinensis, but at much lower levels than other populations near the hybrid zone to the north. No mitochondrial introgression was detected, in contrast to northern contact areas. Thus, the seasonal elevational range gap appears to have been effective in reducing gene flow between these closely related taxa. C1 [Davidson, Brian S.; Braun, Michael J.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC 534, Suitland, MD 20746 USA. [Davidson, Brian S.; Via, Sara; Braun, Michael J.] Univ Maryland, Program Behav Ecol Evolut & Systemat, College Pk, MD 20742 USA. [Sattler, Gene D.] Liberty Univ, Dept Biol & Chem, Lynchburg, VA 24502 USA. RP Braun, MJ (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC 534,4210 Silver Hill Rd, Suitland, MD 20746 USA. EM braunm@si.edu FU Smithsonian Institution Research Endowments program; University of Maryland FX The Smithsonian Institution Research Endowments program and the University of Maryland provided support for this research. NR 68 TC 5 Z9 5 U1 0 U2 31 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD AUG PY 2013 VL 3 IS 8 BP 2485 EP 2496 DI 10.1002/ece3.604 PG 12 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 202GA UT WOS:000323200800008 ER PT J AU Pinto, CM Helgen, KM Fleischer, RC Perkins, SL AF Miguel Pinto, C. Helgen, Kristofer M. Fleischer, Robert C. Perkins, Susan L. TI Hepatozoon Parasites (Apicomplexa: Adeleorina) in Bats SO JOURNAL OF PARASITOLOGY LA English DT Article ID RIBOSOMAL-RNA GENE; MOLECULAR CHARACTERIZATION; PHYLOGENETIC INFERENCE; TISSUE-CYSTS; SEQUENCES; COCCIDIA; BRAZIL; ZONE AB We provide the first evidence of Hepatozoon parasites infecting bats. We sequenced a short fragment of the 18S rRNA gene (similar to 600 base pairs) of Hepatozoon parasites from 3 Hipposideros cervinus bats from Borneo. Phylogenies inferred by model-based methods place these Hepatozoon within a clade formed by parasites of reptiles, rodents, and marsupials. We discuss the scenario that bats might be common hosts of Hepatozoon. C1 [Miguel Pinto, C.] Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. [Miguel Pinto, C.; Perkins, Susan L.] Amer Museum Nat Hist, Sackler Inst Comparat Genom, New York, NY 10024 USA. [Miguel Pinto, C.] CUNY, Grad Ctr, New York, NY 10016 USA. [Miguel Pinto, C.] Pontificia Univ Catolica Ecuador, Ctr Invest Enfermedades Infecciosas, Quito, Ecuador. [Miguel Pinto, C.; Helgen, Kristofer M.] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Fleischer, Robert C.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. RP Pinto, CM (reprint author), Amer Museum Nat Hist, Dept Mammal, New York, NY 10024 USA. EM mpinto@amnh.org OI Perkins, Susan/0000-0002-5400-5662 FU American Society of Mammalogists; Smithsonian Institution FX CMP acknowledges the support provided by a Grant-in-Aid of the American Society of Mammalogists and a graduate student fellowship from the Smithsonian Institution. Fieldwork was supported by funding from the Smithsonian Institution and logistical support from Robert Stuebing and the Bintulu Office of Grand Perfect Sdn Bhd. NR 27 TC 5 Z9 5 U1 0 U2 10 PU AMER SOC PARASITOLOGISTS PI LAWRENCE PA 810 EAST 10TH STREET, LAWRENCE, KS 66044 USA SN 0022-3395 J9 J PARASITOL JI J. Parasitol. PD AUG PY 2013 VL 99 IS 4 BP 722 EP 724 DI 10.1645/12-18.1 PG 3 WC Parasitology SC Parasitology GA 197BG UT WOS:000322821900025 PM 23240742 ER PT J AU Scarlata, CD Elias, BA Godwin, JR Powell, RA Shepherdson, D Shipley, LA Brown, JL AF Scarlata, C. D. Elias, B. A. Godwin, J. R. Powell, R. A. Shepherdson, D. Shipley, L. A. Brown, J. L. TI Influence of environmental conditions and facility on faecal glucocorticoid concentrations in captive pygmy rabbits (Brachylagus idahoensis) SO ANIMAL WELFARE LA English DT Article DE animal welfare; captive breeding; environmental enrichment; faecal glucocorticoids; husbandry; pygmy rabbit ID URINARY CORTISOL RESPONSES; ANIMAL-WELFARE; ADRENOCORTICAL ACTIVITY; REPRODUCTIVE SUCCESS; STRESS RESPONSES; ZOO ANIMALS; ROOM CHANGE; ENRICHMENT; BEHAVIOR; AGGRESSION AB The objective of this study was to determine if housing conditions, specifically pen size and soil enrichment, had an effect on faecal glucocorticoid concentrations in the endangered pygmy rabbit (Brachylagus idahoensis). The success of the captive breeding programme has been limited, so one hypothesis is that chronic stress due to sub-optimal housing conditions may be responsible for poor fecundity. Faecal glucocorticoid concentrations were assessed in 50 females housed among several pen types at two breeding facilities. The highest glucocorticoid concentrations were found in females housed in 0.37 m(2) crates as compared to enclosures ranging from 0.96 to 75 m(2) in size. Results also indicated that enrichment of enclosures with soil had a significant influence on adrenal activity, based on a reduction in glucocorticoid excretion for females moved from non-soil pens to those with soil. Last, a significant facility effect on glucocorticoid concentrations was observed, suggesting that factors other than housing influenced adrenal activity in these rabbits. In conclusion, based on measurements of faecal glucocorticoids, pygmy rabbits are best managed in enclosures that contain soil for digging burrows. Pen size had little effect on stress hormones, except for crates where limited space and/or absence of soil was associated with higher glucocorticoid concentrations. These results underline the importance of monitoring glucocorticoid concentrations in captive breeding programmes to identify optimal husbandry and management practices. C1 [Scarlata, C. D.; Godwin, J. R.; Powell, R. A.] N Carolina State Univ, Raleigh, NC 27695 USA. [Scarlata, C. D.; Shepherdson, D.] Oregon Zoo, Portland, OR USA. [Elias, B. A.; Shipley, L. A.] Washington State Univ, Pullman, WA 99164 USA. [Brown, J. L.] Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Brown, JL (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM brownjan@si.edu FU Morris Animal Foundation; Smithsonian Institution; Friends of the National Zoo; Washington Department of Fish and Wildlife; North Carolina State University; Washington State University FX Thank you to all the pygmy rabbit keepers (M Illig, J Jackson-VonDohlen, A Williams, H Starr, R Lamson, K Walker and L Klinski) for their dedication to the rabbits and for all the hours spent collecting samples and behavioural data. In addition, thank you to N Presley, N Parker and S Putnam for their patience and technical assistance in the laboratory. The authors are grateful to H Patisaul and S Kennedy Stoskopf for insightful thoughts on the development of this study and for helpful comments on drafts of the manuscript. Funding for this project was provided by a large grant from the Morris Animal Foundation and several supporting grants from the Smithsonian Institution, Friends of the National Zoo, Washington Department of Fish and Wildlife, North Carolina State University, and Washington State University. NR 43 TC 7 Z9 7 U1 3 U2 36 PU UNIV FEDERATION ANIMAL WELFARE PI WHEATHAMPSTEAD PA OLD SCHOOL, BREWHOUSE HILL, WHEATHAMPSTEAD AL4 8AN, HERTS, ENGLAND SN 0962-7286 J9 ANIM WELFARE JI Anim. Welf. PD AUG PY 2013 VL 22 IS 3 BP 357 EP 368 DI 10.7120/09627286.22.3.357 PG 12 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 196JE UT WOS:000322769700007 ER PT J AU Queenborough, SA Metz, MR Valencia, R Wright, SJ AF Queenborough, Simon A. Metz, Margaret R. Valencia, Renato Joseph Wright, S. TI Demographic consequences of chromatic leaf defence in tropical tree communities: do red young leaves increase growth and survival? SO ANNALS OF BOTANY LA English DT Article DE Delayed greening; seedling herbivory; young leaf colour; seedlings; tropical forest ID NEOTROPICAL FOREST; RAIN-FOREST; ANTIHERBIVORE DEFENSE; DEPENDENT RECRUITMENT; SPECIES COEXISTENCE; AMAZONIAN FORESTS; JUVENILE LEAVES; USE EFFICIENCY; PLANT DEFENSE; TRADE-OFF AB Many tropical forest tree species delay greening their leaves until full expansion. This strategy is thought to provide newly flushing leaves with protection against damage by herbivores by keeping young leaves devoid of nutritive value. Because young leaves suffer the greatest predation from invertebrate herbivores, delayed greening could prevent costly tissue loss. Many species that delay greening also produce anthocyanin pigments in their new leaves, giving them a reddish tint. These anthocyanins may be fungicidal, protect leaves against UV damage or make leaves cryptic to herbivores blind to the red part of the spectrum. A comprehensive survey was undertaken of seedlings, saplings and mature trees in two diverse tropical forests: a rain forest in western Amazonia (Yasun National Park, Ecuador) and a deciduous forest in Central America (Barro Colorado Island, Panam). A test was made of whether individuals and species with delayed greening or red-coloured young leaves showed lower mortality or higher relative growth rates than species that did not. At both Yasun and Barro Colorado Island, species with delayed greening or red young leaves comprised significant proportions of the seedling and tree communities. At both sites, significantly lower mortality was found in seedlings and trees with delayed greening and red-coloured young leaves. While there was little effect of leaf colour on the production of new leaves of seedlings, diameter relative growth rates of small trees were lower in species with delayed greening and red-coloured young leaves than in species with regular green leaves, and this effect remained when the trade-off between mortality and growth was accounted for. Herbivores exert strong selection pressure on seedlings for the expression of defence traits. A delayed greening or red-coloured young leaf strategy in seedlings appears to be associated with higher survival for a given growth rate, and may thus influence the species composition of later life stages. C1 [Queenborough, Simon A.] Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. [Metz, Margaret R.] Univ Calif Davis, Dept Plant Pathol, Davis, CA 95616 USA. [Valencia, Renato] Pontifical Catholic Univ Ecuador, Sch Biol Sci, Plant Ecol Lab, Quito, Ecuador. [Joseph Wright, S.] Smithsonian Trop Res Inst, Panama City, Panama. RP Queenborough, SA (reprint author), Ohio State Univ, Dept Ecol Evolut & Organismal Biol, Columbus, OH 43210 USA. EM queenborough.1@osu.edu RI Wright, Stuart/M-3311-2013 OI Wright, Stuart/0000-0003-4260-5676 FU National Science Foundation's LTREB programme [DEB-1122634, DEB-0614525]; Center for Tropical Forest Science at the Smithsonian Tropical Research Institute; University of California, Berkeley; SENESCYT [300]; Pontifical Catholic University of Ecuador (PUCE); Environmental Sciences Program of the Smithsonian Institution FX We are extremely grateful to Lissy Coley and Tom Kursar for allowing us to use data they collected in Panama, as well as providing many insightful comments on the manuscript. We further thank Kasey Barton and two anonymous reviewers for many helpful comments on the manuscript, and Kasey Barton and Mick Hanley for inviting M. R. M. and S. A. Q. to the seedling herbivory special symposium at ESA 2012. We thank Laura Mason for help with database management. R. V. thanks PUCE for granting him a sabbatical year and the University of Aarhus for offering research facilities during this year. We appreciate the hard work of the many field assistants who have diligently surveyed the seedling and tree communities in Yasuni and BCI for many years, especially Anelio Loor, Everaldo Zambrano and Milton Zambrano at Yasuni, and A. Hernandez and R. Gonzalez at BCI. We thank the Ministerio del Medioambiente of Ecuador for permission to carry out fieldwork in Yasuni National Park and within the Yasuni Forest Dynamics Plot. Both the Yasuni and BCI Forest Dynamics Plots are associated to the Center for Tropical Forest Science, a global network of large-scale demographic tree plots. The Yasuni seedling census is supported via the National Science Foundation's LTREB programme under grants DEB-1122634 and DEB-0614525, as well as grants from the Center for Tropical Forest Science at the Smithsonian Tropical Research Institute and from the University of California, Berkeley. The Yasuni FDP was supported by SENESCYT (project 300) in 2011. The Forest Dynamics Plot of Yasuni National Park has been made possible through the generous support of the Pontifical Catholic University of Ecuador (PUCE) funds of donaciones del impuesto a la renta, the government of Ecuador, the US National Science Foundation, the Andrew W. Mellon Foundation, the Smithsonian Tropical Research Institute and the University of Aarhus of Denmark. The Environmental Sciences Program of the Smithsonian Institution supported the seedling studies at BCI. NR 62 TC 7 Z9 9 U1 2 U2 46 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 AUG PY 2013 VL 112 IS 4 SI SI BP 677 EP 684 DI 10.1093/aob/mct144 PG 8 WC Plant Sciences SC Plant Sciences GA 198WC UT WOS:000322952500005 PM 23881717 ER PT J AU Kitajima, K Cordero, RA Wright, SJ AF Kitajima, Kaoru Cordero, Roberto A. Joseph Wright, S. TI Leaf life span spectrum of tropical woody seedlings: effects of light and ontogeny and consequences for survival SO ANNALS OF BOTANY LA English DT Article DE Fracture toughness; herbivory; leaf life span; leaf density; leaf toughness; light environment; ontogenetic changes; phenotypic plasticity; seedling survival; stem density; tropical lianas; tropical trees ID RAIN-FOREST EVERGREENS; COST-BENEFIT-ANALYSIS; SHADE TOLERANCE; TREE SEEDLINGS; FRACTURE-TOUGHNESS; NEOTROPICAL FOREST; RESOURCE AVAILABILITY; CARBOHYDRATE STORAGE; ECONOMICS SPECTRUM; FUNCTIONAL TRAITS AB Leaf life span is widely recognized as a key life history trait associated with herbivory resistance, but rigorous comparative data are rare for seedlings. The goal of this study was to examine how light environment affects leaf life span, and how ontogenetic development during the first year may influence leaf fracture toughness, lamina density and stem density that are relevant for herbivory resistance, leaf life span and seedling survival. Data from three experiments encompassing 104 neotropical woody species were combined. Leaf life span, lamina and vein fracture toughness, leaf and stem tissue density and seedling survival were quantified for the first-year seedlings at standardized ontogenetic stages in shade houses and common gardens established in gaps and shaded understorey in a moist tropical forest in Panama. Mortality of naturally recruited seedlings till 1 year later was quantified in 800 1-m(2) plots from 1994 to 2011. Median leaf life span ranged widely among species, always greater in shade (ranging from 151 to 1790 d in the understorey and shade houses) than in gaps (115867 d), but with strong correlation between gaps and shade. Leaf and stem tissue density increased with seedling age, whereas leaf fracture toughness showed only a weak increase. All these traits were positively correlated with leaf life span. Leaf life span and stem density were negatively correlated with seedling mortality in shade, while gap mortality showed no correlation with these traits. The wide spectrum of leaf life span and associated functional traits reflects variation in shade tolerance of first-year seedlings among coexisting trees, shrubs and lianas in this neotropical forest. High leaf tissue density is important in enhancing leaf toughness, a known physical defence, and leaf life span. Both seedling leaf life span and stem density should be considered as key functional traits that contribute to seedling survival in tropical forest understoreys. C1 [Kitajima, Kaoru] Univ Florida, Dept Biol, Gainesville, FL 32611 USA. [Kitajima, Kaoru; Joseph Wright, S.] Smithsonian Trop Res Inst, Balboa, Panama. [Cordero, Roberto A.] Univ Nacl, Escuela Ciencias Biol, Heredia, Costa Rica. RP Kitajima, K (reprint author), Univ Florida, Dept Biol, Gainesville, FL 32611 USA. EM kitajima@ufl.edu RI Wright, Stuart/M-3311-2013; Cordero Solorzano, Roberto A./H-8273-2016 OI Wright, Stuart/0000-0003-4260-5676; Cordero Solorzano, Roberto A./0000-0001-7270-104X FU Smithsonian Tropical Research Institute; [NSF-0093033] FX We thank Sebastian Bernal, Marta Vargas, Joel Sands and Andrez Hernandez for growing, monitoring and/or measuring thousands of seedlings, and also Lisa Cowart, Jeff Hubbard, Sarah Tarrant and Ana-Maria Llorens for their assistance. The study was supported by NSF-0093033 to K. K., and by the Smithsonian Tropical Research Institute. NR 85 TC 14 Z9 15 U1 1 U2 77 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 AUG PY 2013 VL 112 IS 4 SI SI BP 685 EP 699 DI 10.1093/aob/mct036 PG 15 WC Plant Sciences SC Plant Sciences GA 198WC UT WOS:000322952500006 PM 23532047 ER PT J AU Guo, YC Ferguson, HC Giavalisco, M Barro, G Willner, SP Ashby, MLN Dahlen, T Donley, JL Faber, SM Fontana, A Galametz, A Grazian, A Huang, KH Kocevski, DD Koekemoer, AM Koo, DC McGrath, EJ Peth, M Salvato, M Wuyts, S Castellano, M Cooray, AR Dickinson, ME Dunlop, JS Fazio, GG Gardner, JP Gawiser, E Grogin, NA Hathi, NP Hsu, LT Lee, KS Lucas, RA Mobasher, B Nandra, K Newman, JA van der Wel, A AF Guo, Yicheng Ferguson, Henry C. Giavalisco, Mauro Barro, Guillermo Willner, S. P. Ashby, Matthew L. N. Dahlen, Tomas Donley, Jennifer L. Faber, Sandra M. Fontana, Adriano Galametz, Audrey Grazian, Andrea Huang, Kuang-Han Kocevski, Dale D. Koekemoer, Anton M. Koo, David C. McGrath, Elizabeth J. Peth, Michael Salvato, Mara Wuyts, Stijn Castellano, Marco Cooray, Asantha R. Dickinson, Mark E. Dunlop, James S. Fazio, G. G. Gardner, Jonathan P. Gawiser, Eric Grogin, Norman A. Hathi, Nimish P. Hsu, Li-Ting Lee, Kyoung-Soo Lucas, Ray A. Mobasher, Bahram Nandra, Kirpal Newman, Jeffery A. van der Wel, Arjen TI CANDELS MULTI-WAVELENGTH CATALOGS: SOURCE DETECTION AND PHOTOMETRY IN THE GOODS-SOUTH FIELD SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE catalogs; galaxies: high-redshift; galaxies: photometry; methods: data analysis; techniques: image processing ID ORIGINS DEEP SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; STAR-FORMATION HISTORY; SIMILAR-TO 2; GMASS ULTRADEEP SPECTROSCOPY; EXTRAGALACTIC LEGACY SURVEY; REST-FRAME ULTRAVIOLET; UV LUMINOSITY FUNCTION; HIGH-REDSHIFT GALAXIES; SPACE-TELESCOPE AB We present a UV to mid-infrared multi-wavelength catalog in the CANDELS/GOODS-S field, combining the newly obtained CANDELS HST/WFC3 F105W, F125W, and F160W data with existing public data. The catalog is based on source detection in the WFC3 F160W band. The F160W mosaic includes the data from CANDELS deep and wide observations as well as previous ERS and HUDF09 programs. The mosaic reaches a 5 sigma limiting depth (within an aperture of radius 0 ''.17) of 27.4, 28.2, and 29.7 AB for CANDELS wide, deep, and HUDF regions, respectively. The catalog contains 34,930 sources with the representative 50% completeness reaching 25.9, 26.6, and 28.1 AB in the F160W band for the three regions. In addition to WFC3 bands, the catalog also includes data from UV (U band from both CTIO/MOSAIC and VLT/VIMOS), optical (HST/ACS F435W, F606W, F775W, F814W, and F850LP), and infrared (HST/WFC3 F098M, VLT/ISAAC K s, VLT/HAWK-I K s, and Spitzer/IRAC 3.6, 4.5, 5.8, 8.0 mu m) observations. The catalog is validated via stellar colors, comparison with other published catalogs, zero-point offsets determined from the best-fit templates of the spectral energy distribution of spectroscopically observed objects, and the accuracy of photometric redshifts. The catalog is able to detect unreddened star-forming (passive) galaxies with stellar mass of 10(10) M-circle dot at a 50% completeness level to z similar to 3.4 (2.8), 4.6 (3.2), and 7.0 (4.2) in the three regions. As an example of application, the catalog is used to select both star-forming and passive galaxies at z similar to 2-4 via the Balmer break. It is also used to study the color-magnitude diagram of galaxies at 0 < z < 4. C1 [Guo, Yicheng; Barro, Guillermo; Faber, Sandra M.; Koo, David C.] Univ Calif Santa Cruz, Lick Observ, Dept Astron & Astrophys, UCO, Santa Cruz, CA 95064 USA. [Guo, Yicheng; Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Ferguson, Henry C.; Dahlen, Tomas; Huang, Kuang-Han; Koekemoer, Anton M.; Lucas, Ray A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Willner, S. P.; Ashby, Matthew L. N.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Donley, Jennifer L.] Los Alamos Natl Lab, Los Alamos, NM USA. [Fontana, Adriano; Galametz, Audrey; Grazian, Andrea; Castellano, Marco] INAF, Osservatorio Astron, I-00040 Monte Porzio Catone, Italy. [Huang, Kuang-Han; Peth, Michael] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Salvato, Mara; Wuyts, Stijn; Hsu, Li-Ting; Nandra, Kirpal] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Salvato, Mara] Excellence Cluster, D-85748 Garching, Germany. [Cooray, Asantha R.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Dickinson, Mark E.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Dunlop, James S.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Gardner, Jonathan P.] NASAs Goddard Space Flight Ctr, Astrophys Sci Div, Observat Cosmol Lab, Greenbelt, MD USA. [Gawiser, Eric] Rutgers State Univ, Dept Phys & Astron, New Brunswick, NJ 08903 USA. [Hathi, Nimish P.] Carnegie Observ, Pasadena, CA USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Mobasher, Bahram] Univ Calif Riverside, Dept Phys & Astron, Riverside, CA 92521 USA. [Newman, Jeffery A.] Univ Pittsburgh, Dept Phys & Astron, Pittsburgh, PA 15260 USA. [van der Wel, Arjen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. RP Guo, YC (reprint author), Univ Calif Santa Cruz, Lick Observ, Dept Astron & Astrophys, UCO, Santa Cruz, CA 95064 USA. EM ycguo@ucolick.org RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Castellano, Marco/0000-0001-9875-8263; Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823 FU NASA through a grant from the Space Telescope Science Institute [HST-GO-12060]; NASA [NAS5-26555]; NASA HST [GO-12060.10-A]; NSF [AST-0808133]; European Research Council; Royal Society FX We thank the anonymous referee for constructive comments that improve this article. Support for program number HST-GO-12060 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, Incorporated, under NASA contract NAS5-26555. Y.G. and the authors from UCSC acknowledge support from NASA HST grant GO-12060.10-A and NSF grant AST-0808133. J.S.D. acknowledges the support of the European Research Council via the award of an Advanced Grant and the support of the Royal Society via a Wolfson Research Merit Award. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 84 TC 120 Z9 121 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 EI 1538-4365 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD AUG PY 2013 VL 207 IS 2 AR UNSP 24 DI 10.1088/0067-0049/207/2/24 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 195NO UT WOS:000322710000006 ER PT J AU Gingerich, O AF Gingerich, Owen TI TRANSITS IN THE SEVENTEENTH CENTURY AND THE CREDENTIALLING OF KEPLERIAN ASTRONOMY SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Article C1 Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ginger@cfa.harvard.edu NR 26 TC 1 Z9 1 U1 0 U2 1 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD AUG PY 2013 VL 44 BP 303 EP 312 PN 3 PG 10 WC History & Philosophy Of Science SC History & Philosophy of Science GA 193LG UT WOS:000322560700004 ER PT J AU Gingerich, O AF Gingerich, Owen TI A Renaissance Globemaker's Toolbox: Johannes Schoner and the Revolution of Modern Science, 1475-1550 SO JOURNAL FOR THE HISTORY OF ASTRONOMY LA English DT Book Review C1 [Gingerich, Owen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Gingerich, O (reprint author), Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM ginger@cfa.harvard.edu NR 1 TC 0 Z9 0 U1 0 U2 0 PU SCIENCE HISTORY PUBLICATIONS LTD PI CAMBRIDGE PA 16 RUTHERFORD RD, CAMBRIDGE CB2 2HH, ENGLAND SN 0021-8286 J9 J HIST ASTRON JI J. Hist. Astron. PD AUG PY 2013 VL 44 BP 364 EP 365 PN 3 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 193LG UT WOS:000322560700008 ER PT J AU Hong, T AF Hong, Terry TI The Lowland SO LIBRARY JOURNAL LA English DT Book Review C1 [Hong, Terry] Smithsonian BookDragon, Washington, DC USA. RP Hong, T (reprint author), Smithsonian BookDragon, Washington, DC USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU REED BUSINESS INFORMATION PI NEW YORK PA 360 PARK AVENUE SOUTH, NEW YORK, NY 10010 USA SN 0363-0277 J9 LIBR J JI Libr. J. PD AUG PY 2013 VL 138 IS 13 BP 87 EP 87 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 201LI UT WOS:000323142700183 ER PT J AU Riley, SM AF Riley, Sheila M. TI Loss of Innocence SO LIBRARY JOURNAL LA English DT Book Review C1 [Riley, Sheila M.] Smithsonian Inst Libs, Washington, DC USA. RP Riley, SM (reprint author), Smithsonian Inst Libs, 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 AUG PY 2013 VL 138 IS 13 BP 88 EP 88 PG 1 WC Information Science & Library Science SC Information Science & Library Science GA 201LI UT WOS:000323142700191 ER PT J AU Slater, GJ Harmon, LJ AF Slater, Graham J. Harmon, Luke J. TI Unifying fossils and phylogenies for comparative analyses of diversification and trait evolution SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Editorial Material DE macroevolution; palaeontology; phylogenetic comparative methods; systematics ID MOLECULAR PHYLOGENIES; NEOGENE BRYOZOAN; BODY-SIZE; RATES; RECORD; SPECIATION; DIVERSITY; TEMPO; TIME; RECONSTRUCTION AB 1. The aim of macroevolutionary research is to understand pattern and process in phenotypic evolution and lineage diversification at and above the species level. Historically, this kind of research has been tackled separately by palaeontologists, using the fossil record, and by evolutionary biologists, using phylogenetic comparative methods. 2. Although both approaches have strengths, researchers gain most power to understand macroevolution when data from living and fossil species are analysed together in a phylogenetic framework. This merger sets up a series of challenges - for many fossil clades, well-resolved phylogenies based on morphological data are not available, while placing fossils into phylogenies of extant taxa and determining their branching times is equally challenging. Once methods for building such trees are available, modelling phenotypic and lineage diversification using combined data presents its own set of challenges. 3. The five papers in this Special Feature tackle a disparate range of topics in macroevolutionary research, from time calibration of trees to modelling phenotypic evolution. All are united, however, in implementing novel phylogenetic approaches to understand macroevolutionary pattern and process in or using the fossil record. This Special Feature highlights the benefits that may be reaped by integrating data from living and extinct species and, we hope, will spur further integrative work by empiricists and theoreticians from both sides of the macroevolutionary divide. C1 [Slater, Graham J.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20013 USA. [Slater, Graham J.] Smithsonian Inst, Div Mammals, Museum Natl Hist Nat, Washington, DC 20013 USA. [Harmon, Luke J.] Univ Idaho, Dept Biol Sci, Moscow, ID 83844 USA. [Harmon, Luke J.] Univ Idaho, Inst Bioinformat & Evolutionary Studies IBEST, Moscow, ID 83844 USA. RP Slater, GJ (reprint author), Smithsonian Inst, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM SlaterG@si.edu NR 48 TC 29 Z9 29 U1 2 U2 45 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD AUG PY 2013 VL 4 IS 8 BP 699 EP 702 DI 10.1111/2041-210X.12091 PG 4 WC Ecology SC Environmental Sciences & Ecology GA 197ZK UT WOS:000322891200001 ER PT J AU Wagner, PJ Marcot, JD AF Wagner, Peter J. Marcot, Jonathan D. TI Modelling distributions of fossil sampling rates over time, space and taxa: assessment and implications for macroevolutionary studies SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE evolutionary biology; macroevolution; phylogenetics; systematics ID NORTH-AMERICAN MAMMALS; MAXIMUM-LIKELIHOOD; TAXONOMIC DIVERSITY; DIVERGENCE TIMES; RECORD; DIVERSIFICATION; PATTERNS; EVOLUTION; PRESERVATION; HYPOTHESES AB 1. Observed patterns in the fossil record reflect not just macroevolutionary dynamics, but preservation patterns. Sampling rates themselves vary not simply over time or among major taxonomic groups, but within time intervals over geography and environment, and among species within clades. Large databases of presences of taxa in fossil-bearing collections allow us to quantify variation in per-collection sampling rates among species within a clade. We do this separately not just for different time/stratigraphic intervals, but also for different geographic or ecologic units within time/stratigraphic intervals. We then re-assess per-million-year sampling rates given the distributions of per-collection sampling rates. 2. We use simple distribution models (geometric and lognormal) to assess general models of per-locality sampling rate distributions given occurrences among appropriate fossiliferous localities. We break these down not simply by time period, but by general biogeographic units in order to accommodate variation over space as well as among species. 3. We apply these methods to occurrence data for Meso-Cenozoic mammals drawn from the Paleobiology Database and the New and Old Worlds fossil mammal database. We find that all models of distributed rates do vastly better than the best uniform sampling rates and that the lognormal in particular does an excellent job of summarizing sampling rates. We also show that the lognormal distributions vary fairly substantially among biogeographic units of the same age. 4. As an example of the utility of these rates, we assess the most likely divergence times for basal (Eocene-Oligocene) carnivoramorphan mammals from North America and Eurasia using both stratigraphic and morphological data. The results allow for unsampled taxa or unsampled portions of sampled lineages to be in either continent and also allow for the variation in sampling rates among species. We contrast five models using stratigraphic likelihoods in different ways to summarize how they might affect macroevolutionary inferences. C1 [Wagner, Peter J.] Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. [Marcot, Jonathan D.] Univ Illinois, Dept Anim Biol, Urbana, IL 61801 USA. RP Wagner, PJ (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. EM wagnerpj@si.edu RI Marcot, Jonathan/G-2427-2012 NR 63 TC 20 Z9 20 U1 0 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD AUG PY 2013 VL 4 IS 8 BP 703 EP 713 DI 10.1111/2041-210X.12088 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 197ZK UT WOS:000322891200002 ER PT J AU Hunt, G AF Hunt, Gene TI Testing the link between phenotypic evolution and speciation: an integrated palaeontological and phylogenetic analysis SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE Punctuated equilibrium; speciation; Poseidonamicus; anagenesis; cladogenesis ID MORPHOLOGICAL EVOLUTION; PUNCTUATED EQUILIBRIUM; RANDOM-WALKS; SPECIES DIVERSIFICATION; QUANTITATIVE GENETICS; GENUS POSEIDONAMICUS; NEOGENE BRYOZOAN; ATLANTIC SECTOR; TRAIT VARIANCE; SOUTHERN-OCEAN AB 1. The punctuated equilibrium model predicts that phenotypic change is concentrated into pulses associated with speciation, with little change otherwise accruing in established lineages. Palaeontological tests of this model have generally lacked an adequate phylogenetic and modelling framework, whereas tests relying on extant populations lack direct constraints on the evolutionary dynamics within lineages. 2. This study extends a modelling approach developed in comparative studies and applies it to a clade with a rich fossil record, the deep-sea ostracode genus Poseidonamicus. Using a phylogenetic framework and an independent set of shape traits plus body size, a model was fit that allows estimation of anagenetic (within-lineage) evolution, cladogenetic (speciational) change and geographic variation within species. 3. Maximum-likelihood parameter estimates suggested dominantly speciational change for only one or two shape traits, depending on model assumptions. For the remaining shape traits and body size, the contribution of anagenesis was always substantial. Confidence limits on these solutions were quite broad (although narrower when multiple traits were analysed jointly), with most traits consistent with both strongly anagenetic and strongly cladogenetic change. 4. Whereas uncertainty about phylogenetic topology and species limits has little influence on the conclusions, assuming stasis instead of Brownian motion within lineages shifted support to solutions in which speciational change was more dominant, although several traits remained dominantly explained by anagenetic evolution. 5. These results suggest that for the traits and taxa examined, anagenesis contributes substantially to long-term divergence. The uncertainty in the results highlights the analytical difficulty of decomposing anagenetic and cladogenetic sources of phenotypic evolution, even with fossil constraints. When model uncertainty is taken into account, the task of doing so using observations from entirely extant populations is even more daunting. C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Hunt, G (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. EM hunte@si.edu RI Hunt, Gene/B-3783-2010 OI Hunt, Gene/0000-0001-6430-5020 NR 74 TC 11 Z9 11 U1 1 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X EI 2041-2096 J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD AUG PY 2013 VL 4 IS 8 BP 714 EP 723 DI 10.1111/2041-210X.12085 PG 10 WC Ecology SC Environmental Sciences & Ecology GA 197ZK UT WOS:000322891200003 ER PT J AU Slater, GJ AF Slater, Graham J. TI Phylogenetic evidence for a shift in the mode of mammalian body size evolution at the Cretaceous-Palaeogene boundary SO METHODS IN ECOLOGY AND EVOLUTION LA English DT Article DE Brownian motion; body size; comparative methods; evolutionary rates; fossils; macroevolution; mammals; Ornstein-Uhlenbeck ID CONTINUOUS TRAIT EVOLUTION; FOSSIL RECORD; PHENOTYPIC DIVERSIFICATION; ECOLOGICAL LIMITS; RADIATION; TREES; EXTINCTION; RATES; TAXA; RECONSTRUCTION AB 1. Phylogenetic comparative methods provide a powerful way of addressing classic questions about tempo and mode of phenotypic evolution in the fossil record, such as whether mammals increased in body size diversity after the Cretaceous-Palaeogene (K-Pg) extinction. 2. Most often, these kinds of questions are addressed in the context of variation in evolutionary rates. Shifts in the mode of phenotypic evolution provide an alternative and, in some cases, more realistic explanation for patterns of trait diversity in the fossil record, but these kinds of processes are rarely tested for. 3. In this study, I use a time-calibrated phylogeny of living and fossil Mammaliaformes as a framework to test novel models of body size evolution derived from palaeontological theory. Specifically, I ask whether the K-Pg extinction resulted in a change in rates of body size evolution or release from a constrained adaptive zone. 4. I found that a model comprising an Ornstein-Uhlenbeck process until the K-Pg event and a Brownian motion process from the Cenozoic onwards was the best supported model for these data. Surprisingly, results indicate a lower absolute rate of body size evolution during the Cenozoic than during the Mesozoic. This is explained by release from a stationary OU process that constrained realized disparity. Despite a lower absolute rate, body size disparity has in fact been increasing since the K-Pg event. 5. The use of time-calibrated phylogenies of living and extinct taxa and realistic, process-based models provides unparalleled power in testing evolutionary hypotheses. However, researchers should take care to ensure that the models they use are appropriate to the question being tested and that the parameters estimated are interpreted in the context of the best fitting model. C1 Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Slater, GJ (reprint author), Smithsonian Inst, Dept Paleobiol, Natl Museum Nat Hist, MRC 121,POB 37012, Washington, DC 20013 USA. EM SlaterG@si.edu NR 63 TC 56 Z9 56 U1 7 U2 74 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2041-210X J9 METHODS ECOL EVOL JI Methods Ecol. Evol. PD AUG PY 2013 VL 4 IS 8 BP 734 EP 744 DI 10.1111/2041-210X.12084 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 197ZK UT WOS:000322891200005 ER PT J AU Woodhams, DC Brucker, RM AF Woodhams, Douglas C. Brucker, Robert M. TI Disease defence through generations: leaf-cutter ants and their symbiotic bacteria SO MOLECULAR ECOLOGY LA English DT Editorial Material DE ant; bacteria; coevolution; microbial ecology; symbiosis ID MICROBIAL COMMUNITIES; SOCIAL IMMUNITY; ROLES AB Microbial ecology of animals is taking on significance in the modern dialogue for the biology of species. Similar to a nuclear genome, the entire bacterial assemblage maintains an ancestral signal of the host's evolution leading to cophylogeny between the host and the microbes they harbour (Brucker & Bordenstein 2012b). The stability of such associations is of great interest as they provide a means for species to acquire new traits and genetic diversity that their own genomes lack (McFall-Ngai etal. 2013). The role of gut microbiota, for example, in host health and nutrition is widely recognized and a shared characteristic among animals. The role of bacteria colonizing the outside surfaces of animals is less well understood, but rather than random colonization, these microbes on skin, cuticles, scales and feathers in many cases provide benefits to the host. The symbiosis of leaf-cutter ants, their fungus gardens and their microbiota is a fascinating and complex system. Whether culture-independent bacterial diversity on the cuticle of leaf-cutter ants is high or highly constrained by subcuticular gland secretions is one prominent question. In this issue of Molecular Ecology, Andersen etal. (2013) show that leaf-cutting ants, Acromyrmex echinatior, maintain a dominant and colony-specific bacterium called Pseudonocardia on their cuticles (the laterocervical plates in particular). This bacterium is involved in protecting the ants and their fungal gardens from disease. Other fungus-gardening attine species as well as soil and vegetation can harbour Pseudonocardia. However, it was previously unknown how stable the bacterial strain-ant colony association was through the lifetime of the colony. C1 [Woodhams, Douglas C.] Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80302 USA. [Woodhams, Douglas C.] Smithsonian Trop Res Inst, Washington, DC 20521 USA. [Brucker, Robert M.] Vanderbilt Univ, Dept Biol Sci, Nashville, TN 37235 USA. RP Woodhams, DC (reprint author), Univ Colorado, Dept Ecol & Evolutionary Biol, Boulder, CO 80302 USA. EM dwoodhams@gmail.com NR 12 TC 0 Z9 0 U1 3 U2 118 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 AUG PY 2013 VL 22 IS 16 BP 4141 EP 4143 DI 10.1111/mec.12431 PG 3 WC Biochemistry & Molecular Biology; Ecology; Evolutionary Biology SC Biochemistry & Molecular Biology; Environmental Sciences & Ecology; Evolutionary Biology GA 197XQ UT WOS:000322886400001 PM 23927408 ER PT J AU Platais, I Gosnell, NM Meibom, S Kozhurina-Platais, V Bellini, A Veillet, C Burkhead, MS AF Platais, Imants Gosnell, Natalie M. Meibom, Soren Kozhurina-Platais, Vera Bellini, Andrea Veillet, Christian Burkhead, Martin S. TI WIYN OPEN CLUSTER STUDY. LV. ASTROMETRY AND MEMBERSHIP IN NGC 6819 SO ASTRONOMICAL JOURNAL LA English DT Article DE astrometry; open clusters and associations: individual (NGC 6819) ID YOUNG OPEN CLUSTER; XMM-NEWTON; VARIABLE-STARS; PROPER MOTIONS; CCD PHOTOMETRY; RED GIANTS; KEPLER; CATALOG; FIELD; ASTEROSEISMOLOGY AB We present proper motions and astrometric membership analysis for 15,750 stars around the intermediate-age open cluster NGC 6819. The accuracy of relative proper motions for well-measured stars ranges from similar to 0.2 mas yr(-1) within 10' of the cluster center to 1.1 mas yr(-1) outside this radius. In the proper motion vector-point diagram, the separation between the cluster members and field stars is convincing down to V similar to 18 and within 10' from the cluster center. The formal sum of membership probabilities indicates a total of similar to 2500 cluster members down to V similar to 22. We confirm the cluster membership of several variable stars, including some eclipsing binaries. The estimated absolute proper motion of NGC 6819 is mu(abs)(x) = -2.6 +/- 0.5 and mu(abs)(y) = -4.2 +/- 0.5 mas yr(-1). A cross-identification between the proper motion catalog and a list of X-ray sources in the field of NGC 6819 resulted in a number of new likely optical counterparts, including a candidate CV. For the first time we show that there is significant differential reddening toward NGC 6819. C1 [Platais, Imants] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gosnell, Natalie M.] Univ Wisconsin, Dept Astron, Madison, WI 53706 USA. [Meibom, Soren] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kozhurina-Platais, Vera; Bellini, Andrea] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Veillet, Christian] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Burkhead, Martin S.] Indiana Univ, Dept Astron, Bloomington, IN 47405 USA. RP Platais, I (reprint author), Johns Hopkins Univ, Dept Phys & Astron, 3400 North Charles St, Baltimore, MD 21218 USA. EM imants@pha.jhu.edu FU National Science Foundation [AST 09-08114] FX I. Platais gratefully acknowledges support from the National Science Foundation through grant AST 09-08114 to Johns Hopkins University. Barbara Anthony-Twarog, Gerhard Auner, Kyle Cudworth, Alison Doane, Terry Girard, Ted Gull, Jim Hesser, Burt Jones, Irina Kumkova, Arnie Phifer, Bill Schoening, and John Stauffer are all thanked for permitting us to digitize their priceless collections of photographic plates. Robert Spies is thanked for his dedication to restoring and maintaining the functionality of GAMMA II. Norbert Zacharias and Gary Wycoff are thanked for their help with the StarScan machine at the US Naval Observatory. We appreciate a pilot study by Dean McLaughlin on the dynamical status of NGC 6819. Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l'Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. NR 38 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 AUG PY 2013 VL 146 IS 2 AR 43 DI 10.1088/0004-6256/146/2/43 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 183TW UT WOS:000321841100025 ER PT J AU Supple, MA Hines, HM Dasmahapatra, KK Lewis, JJ Nielsen, DM Lavoie, C Ray, DA Salazar, C McMillan, WO Counterman, BA AF Supple, Megan A. Hines, Heather M. Dasmahapatra, Kanchon K. Lewis, James J. Nielsen, Dahlia M. Lavoie, Christine Ray, David A. Salazar, Camilo Owen McMillan, W. Counterman, Brian A. TI Genomic architecture of adaptive color pattern divergence and convergence in Heliconius butterflies SO GENOME RESEARCH LA English DT Article ID DNA-SEQUENCING DATA; MULLERIAN MIMICRY; WARNING-COLOR; HYBRID ZONES; NATURAL-SELECTION; RNA-SEQ; EVOLUTION; GENE; POPULATION; ALIGNMENT AB Identifying the genetic changes driving adaptive variation in natural populations is key to understanding the origins of biodiversity. The mosaic of mimetic wing patterns in Heliconius butterflies makes an excellent system for exploring adaptive variation using next-generation sequencing. In this study, we use a combination of techniques to annotate the genomic interval modulating red color pattern variation, identify a narrow region responsible for adaptive divergence and convergence in Heliconius wing color patterns, and explore the evolutionary history of these adaptive alleles. We use whole genome resequencing from four hybrid zones between divergent color pattern races of Heliconius erato and two hybrid zones of the co-mimic Heliconius melpomene to examine genetic variation across 2.2 Mb of a partial reference sequence. In the intergenic region near optix, the gene previously shown to be responsible for the complex red pattern variation in Heliconius, population genetic analyses identify a shared 65-kb region of divergence that includes several sites perfectly associated with phenotype within each species. This region likely contains multiple cis-regulatory elements that control discrete expression domains of optix. The parallel signatures of genetic differentiation in H. erato and H. melpomene support a shared genetic architecture between the two distantly related co-mimics; however, phylogenetic analysis suggests mimetic patterns in each species evolved independently. Using a combination of next-generation sequencing analyses, we have refined our understanding of the genetic architecture of wing pattern variation in Heliconius and gained important insights into the evolution of novel adaptive phenotypes in natural populations. C1 [Supple, Megan A.; Salazar, Camilo; Owen McMillan, W.] Smithsonian Trop Res Inst, Panama City, Panama. [Supple, Megan A.] N Carolina State Univ, Biomath Program, Raleigh, NC 27695 USA. [Hines, Heather M.; Nielsen, Dahlia M.] N Carolina State Univ, Dept Genet, Raleigh, NC 27695 USA. [Hines, Heather M.] Penn State Univ, Dept Biol, University Pk, PA 16802 USA. [Dasmahapatra, Kanchon K.] UCL, Dept Genet Evolut & Environm, London WC1E 6BT, England. [Dasmahapatra, Kanchon K.] Univ York, Dept Biol, York YO10 5DD, N Yorkshire, England. [Lewis, James J.] Cornell Univ, Dept Ecol & Evolutionary Biol, Ithaca, NY 14853 USA. [Lavoie, Christine; Ray, David A.; Counterman, Brian A.] Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA. [Salazar, Camilo] Univ Rosario, Fac Ciencias Nat & Matemat, Bogota, Colombia. RP Counterman, BA (reprint author), Mississippi State Univ, Dept Biol Sci, Mississippi State, MS 39762 USA. EM bcounterman@biology.msstate.edu RI Salazar, camilo/A-1647-2010; OI Salazar, camilo/0000-0001-9217-6588; Dasmahapatra, Kanchon Kumar/0000-0002-2840-7019 FU CNRS Nouraugues; NIH [F32 GM889942, T32 HD060555]; NSF [DEB-1257839, DEB-0844244, DEB-0715096, IOS-1305686]; Smithsonian Institution FX We wish to thank Claudia Rosales for the tremendous amount of work she did in the laboratory; Jamie Walters and Chris Jiggins for contributing sequencing data; and Chris Smith for computational support. We thank Arnaud Martin, the editor, and three reviewers for their insightful comments on previous versions of the manuscript. We also thank the following permitting agencies for permission to collect butterflies: Peruvian Ministerio de Agricultura and Instituto Nacional de Recursos Naturales (004-2008-INRENA-IFFS-DCB and 011756-AG-INRENA); Ecuadorian Ministerio del Ambiente Ecuadorian (013-09 IC-FAU-DNB/MA); French Guiana Ministere de L'Ecologie, de L'Energie, du Developpemet Durable et de la Mar (BIODAD-2010-0433); Panamanian Autoridad Nacional del Ambiente (SC/A-7-11); and Colombian Ministerio de Ambiente, Vivienda y Desarrollo Territorial (RGE0027-LAM3483). This work was funded by the following awards: CNRS Nouraugues (B.A.C.); NIH F32 GM889942 (H.M.H.) and T32 HD060555 (J.J.L.); NSF DEB-1257839 (B.A.C.), DEB-0844244 (W.O.M.), DEB-0715096 (W.O.M.), and IOS-1305686 (J.J.L.); and the Smithsonian Institution. NR 63 TC 29 Z9 29 U1 1 U2 79 PU COLD SPRING HARBOR LAB PRESS, PUBLICATIONS DEPT PI COLD SPRING HARBOR PA 1 BUNGTOWN RD, COLD SPRING HARBOR, NY 11724 USA SN 1088-9051 EI 1549-5469 J9 GENOME RES JI Genome Res. PD AUG PY 2013 VL 23 IS 8 BP 1248 EP 1257 DI 10.1101/gr.150615.112 PG 10 WC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity SC Biochemistry & Molecular Biology; Biotechnology & Applied Microbiology; Genetics & Heredity GA 193RS UT WOS:000322579800005 PM 23674305 ER PT J AU Bose, S Kumar, B Sutaria, F Kumar, B Roy, R Bhatt, VK Pandey, SB Chandola, HC Sagar, R Misra, K Chakraborti, S AF Bose, Subhash Kumar, Brijesh Sutaria, Firoza Kumar, Brajesh Roy, Rupak Bhatt, V. K. Pandey, S. B. Chandola, H. C. Sagar, Ram Misra, Kuntal Chakraborti, Sayan TI Supernova 2012aw-a high-energy clone of archetypal Type IIP SN 1999em SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE supernovae: general; supernovae: individual: SN 2012aw; supernovae: individual: SN 1999em; supernovae: individual: SN 1999gi; supernovae: individual: SN 2004et; galaxies: individual: NGC 3551 ID CORE-COLLAPSE SUPERNOVAE; O-I LAMBDA-LAMBDA-6300; PLATEAU SUPERNOVAE; LIGHT CURVES; QUANTITATIVE SPECTROSCOPY; HYDRODYNAMICAL MODELS; PHYSICAL-PROPERTIES; SPECTRAL-ANALYSIS; STANDARD STARS; DUST FORMATION AB We present densely sampled UBVRI/griz photometric and low-resolution (6-10 A) optical spectroscopic observations from 4 to 270 d after explosion of a newly discovered Type II SN 2012aw in a nearby (similar to 9.9 Mpc) galaxy M95. The light-curve characteristics of apparent magnitudes, colours, bolometric luminosity and the presence and evolution of prominent spectral features are found to have striking similarity with the archetypal IIP SNe 1999em, 1999gi and 2004et. The early time observations of SN 2012aw clearly detect minima in the light curve of V, R and I bands near 37 d after explosion and this we suggest to be an observational evidence for emergence of recombination phase. The mid-plateau M-V magnitude (-16.67 +/- 0.04) lies in between the bright (similar to-18) and subluminous (similar to-15) IIP SNe. The mass of nickel is 0.06 +/- 0.01 M-circle dot. The synow modelling of spectra indicate that the value and evolution of the photospheric velocity is similar to SN 2004et, but about similar to 600 km s(-1) higher than that of SNe 1999em and 1999gi at comparable epochs. This trend is more apparent in the line velocities of H alpha and H beta. A comparison of ejecta velocity properties with that of existing radiation-hydrodynamical simulations indicate that the energy of explosion lies in the range 1-2 x 10(51) ergs; a further comparison of nebular phase [O i] doublet luminosity with SNe 2004et and 1987A indicate that the mass of progenitor star is about 14 to 15 M-circle dot. The presence of high-velocity absorption features in the mid-to-late plateau and possibly in early phase spectra show signs of interaction between ejecta and the circumstellar matter; being consistent with its early time detection at X-ray and radio wavebands. C1 [Bose, Subhash; Kumar, Brijesh; Kumar, Brajesh; Roy, Rupak; Bhatt, V. K.; Pandey, S. B.; Sagar, Ram; Misra, Kuntal] Aryabhatta Res Inst Observat Sci, Naini Tal 263002, India. [Sutaria, Firoza] Indian Inst Astrophys, Bangalore 560034, Karnataka, India. [Kumar, Brajesh] Univ Liege, Inst Astrophys & Geophys, B-4000 Liege, Belgium. [Chandola, H. C.] Kumaun Univ, Dept Phys, Naini Tal 263002, India. [Chakraborti, Sayan] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Bose, S (reprint author), Aryabhatta Res Inst Observat Sci, Naini Tal 263002, India. EM email@subhashbose.com NR 102 TC 27 Z9 27 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 AUG PY 2013 VL 433 IS 3 BP 1871 EP 1891 DI 10.1093/mnras/stt864 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 191HK UT WOS:000322403800008 ER PT J AU Nava, L Sironi, L Ghisellini, G Celotti, A Ghirlanda, G AF Nava, L. Sironi, L. Ghisellini, G. Celotti, A. Ghirlanda, G. TI Afterglow emission in gamma-ray bursts - I. Pair-enriched ambient medium and radiative blast waves SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE gamma-ray burst: general; X-rays: general ID HIGH-ENERGY EMISSION; LORENTZ-FACTOR; LIGHT CURVES; GRB 090510; DYNAMICAL MODEL; FLUID-DYNAMICS; FIREBALL MODEL; SHOCK ORIGIN; ONSET; FERMI AB Forward shocks caused by the interaction between a relativistic blast wave and the circumburst medium are thought to be responsible for the afterglow emission in gamma-ray bursts (GRBs). We consider the hydrodynamics of a spherical relativistic blast wave expanding into the surrounding medium and we generalize the standard theory in order to account for several effects that are generally ignored. In particular, we consider the role of adiabatic and radiative losses in the hydrodynamical evolution of the shock, under the assumption that the cooling losses are fast. Our model can describe adiabatic, fully radiative and semiradiative blast waves, and can describe the effects of a time-varying radiative efficiency. The equations we present are valid for arbitrary density profiles, and also for a circumburst medium enriched with electron-positron pairs. The presence of pairs enhances the fraction of shock energy gained by the leptons, thus increasing the importance of radiative losses. Our model allows us to study whether the high-energy (> 0.1 GeV) emission in GRBs may originate from afterglow radiation. In particular, it is suitable to test whether the fast decay of the high-energy light curve observed in several Fermi Large Area Telescope GRBs can be ascribed to an initial radiative phase, followed by the standard adiabatic evolution. C1 [Nava, L.] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Obs Paris, Sorbonne Paris Cite, France. [Sironi, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ghisellini, G.; Celotti, A.; Ghirlanda, G.] Osserv Astron Brera, INAF, I-23807 Merate, Italy. [Celotti, A.] SISSA, I-34136 Trieste, Italy. RP Nava, L (reprint author), Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Obs Paris, Sorbonne Paris Cite, France. EM lara.nava@apc.univ-paris7.fr OI Ghirlanda, Giancarlo/0000-0001-5876-9259; Ghisellini, Gabriele/0000-0002-0037-1974 FU NASA [PF1-120090, NAS8-03060]; Chandra X-ray Center; PRIN-INAF grant FX LN thanks SISSA and INAF-Osservatorio Astronomico di Brera for the kind hospitality during the completion of this work. LS gratefully thanks the Osservatorio Astronomico di Brera - Merate for hospitality and stimulating discussions. LN is also grateful to Pawan Kumar for helpful discussions. LS is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We acknowledge the 2011 PRIN-INAF grant for financial support. NR 57 TC 22 Z9 22 U1 1 U2 4 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2013 VL 433 IS 3 BP 2107 EP 2121 DI 10.1093/mnras/stt872 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 191HK UT WOS:000322403800029 ER PT J AU Sadowski, A Narayan, R Sironi, L Ozel, F AF Sadowski, Aleksander Narayan, Ramesh Sironi, Lorenzo Oezel, Feryal TI Location of the bow shock ahead of cloud G2 at the Galactic Centre SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE acceleration of particles; accretion, accretion discs; black hole physics; radiation mechanisms: non-thermal ID SGR A-ASTERISK; SUPERMASSIVE BLACK-HOLE; ACCRETION FLOW; SAGITTARIUS-A; GRMHD SIMULATIONS; GAS; DYNAMICS; SCHEME; MODELS; GALAXY AB We perform detailed magnetohydrodynamic simulations of the gas cloud G2 interacting with the accretion flow around the Galactic Centre black hole Sgr A*. We take as our initial conditions a steady-state, converged solution of the accretion flow obtained earlier using the general-relativistic magnetohydrodynamic code harm. Using the observed parameters for the cloud's orbit, we compute the interaction of the cloud with the ambient gas and identify the shock structure that forms ahead of the cloud. We show that for many configurations, the cloud front crosses the orbit pericentre seven to nine months earlier than the centre-of-mass. C1 [Sadowski, Aleksander; Narayan, Ramesh; Sironi, Lorenzo; Oezel, Feryal] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Oezel, Feryal] Univ Arizona, Tucson, AZ 85721 USA. RP Sadowski, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM asadowski@cfa.harvard.edu; rnarayan@cfa.harvard.edu; lsironi@cfa.harvard.edu; fozel@email.arizona.edu OI Narayan, Ramesh/0000-0002-1919-2730 FU NASA [NNX11AE16G, PF1-120090, NAS8-03060]; Chandra X-ray Center; NSF [AST-1108753]; Radcliffe Institute for Advanced Study at Harvard University; [TG-AST120010] FX AS and RN were supported in part by NASA grant NNX11AE16G. LS is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. FO acknowledges support from NSF grant AST-1108753 and from the Radcliffe Institute for Advanced Study at Harvard University. The simulations were performed on XSEDE resources under contract No. TG-AST120010 and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 30 TC 11 Z9 11 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 AUG PY 2013 VL 433 IS 3 BP 2165 EP 2171 DI 10.1093/mnras/stt879 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 191HK UT WOS:000322403800033 ER PT J AU Brightman, M Silverman, JD Mainieri, V Ueda, Y Schramm, M Matsuoka, K Nagao, T Steinhardt, C Kartaltepe, J Sanders, DB Treister, E Shemmer, O Brandt, WN Brusa, M Comastri, A Ho, LC Lanzuisi, G Lusso, E Nandra, K Salvato, M Zamorani, G Akiyama, M Alexander, DM Bongiorno, A Capak, P Civano, F Del Moro, A Doi, A Elvis, M Hasinger, G Laird, ES Masters, D Mignoli, M Ohta, K Schawinski, K Taniguchi, Y AF Brightman, M. Silverman, J. D. Mainieri, V. Ueda, Y. Schramm, M. Matsuoka, K. Nagao, T. Steinhardt, C. Kartaltepe, J. Sanders, D. B. Treister, E. Shemmer, O. Brandt, W. N. Brusa, M. Comastri, A. Ho, L. C. Lanzuisi, G. Lusso, E. Nandra, K. Salvato, M. Zamorani, G. Akiyama, M. Alexander, D. M. Bongiorno, A. Capak, P. Civano, F. Del Moro, A. Doi, A. Elvis, M. Hasinger, G. Laird, E. S. Masters, D. Mignoli, M. Ohta, K. Schawinski, K. Taniguchi, Y. TI A statistical relation between the X-ray spectral index and Eddington ratio of active galactic nuclei in deep surveys SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; galaxies: active; galaxies: nuclei; quasars: emission lines; quasars: general; X-rays: galaxies ID FIELD-SOUTH SURVEY; SEYFERT 1 GALAXIES; NEWTON QUASAR SURVEY; MS SOURCE CATALOGS; BLACK-HOLE MASSES; COSMOS SURVEY; XMM-COSMOS; EMISSION-LINE; DATA RELEASE; LUMINOSITY AB We present an investigation into how well the properties of the accretion flow on to a supermassive black hole may be coupled to those of the overlying hot corona. To do so, we specifically measure the characteristic spectral index, Gamma, of a power-law energy distribution, over an energy range of 2-10 keV, for X-ray selected, broad-lined radio-quiet active galactic nuclei (AGN) up to z similar to 2 in Cosmic Evolution Survey (COSMOS) and Extended Chandra Deep Field South (E-CDF-S). We test the previously reported dependence between Gamma and black hole mass, full width at half-maximum (FWHM) and Eddington ratio using a sample of AGN covering a broad range in these parameters based on both the Mg ii and H alpha emission lines with the later afforded by recent near-infrared spectroscopic observations using Subaru/Fibre Multi Object Spectrograph. We calculate the Eddington ratios, lambda(Edd), for sources where a bolometric luminosity (L-Bol) has been presented in the literature, based on spectral energy distribution fitting, or, for sources where these data do not exist, we calculate L-Bol using a bolometric correction to the X-ray luminosity, derived from a relationship between the bolometric correction and L-X/L-3000. From a sample of 69 X-ray bright sources (> 250 counts), where Gamma can be measured with greatest precision, with an estimate of L-Bol, we find a statistically significant correlation between Gamma and lambda(Edd), which is highly significant with a chance probability of 6.59x 10(-8). A statistically significant correlation between Gamma and the FWHM of the optical lines is confirmed, but at lower significance than with lambda(Edd) indicating that lambda(Edd) is the key parameter driving conditions in the corona. Linear regression analysis reveals that Gamma = (0.32 +/- 0.05) log(10)lambda(Edd) + (2.27 +/- 0.06) and Gamma = (-0.69 +/- 0.11) log(10)(FWHM/km s(-1)) + (4.44 +/- 0.42). Our results on Gamma-lambda(Edd) are in very good agreement with previous results. While the Gamma-lambda(Edd) relationship means that X-ray spectroscopy may be used to estimate black hole accretion rate, considerable dispersion in the correlation does not make this viable for single sources, however could be valuable for large X-ray spectral samples, such as those to be produced by eROSITA. C1 [Brightman, M.; Brusa, M.; Lanzuisi, G.; Nandra, K.; Salvato, M.; Bongiorno, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Silverman, J. D.; Schramm, M.; Steinhardt, C.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe WPI, Chiba 2778583, Japan. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Ueda, Y.; Nagao, T.; Ohta, K.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Matsuoka, K.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Matsuoka, K.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Nagao, T.] Kyoto Univ, Hakubi Ctr Adv Res, Sakyo Ku, Kyoto 6068302, Japan. [Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Sanders, D. B.; Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Treister, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Shemmer, O.] Univ N Texas, Dept Phys, Denton, TX 76203 USA. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brusa, M.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Brusa, M.; Comastri, A.; Zamorani, G.; Mignoli, M.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ho, L. C.; Masters, D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Lusso, E.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Akiyama, M.] Tohoku Univ, Astron Inst, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Alexander, D. M.; Del Moro, A.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Bongiorno, A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Capak, P.] CALTECH, NASA, JPL Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Doi, A.] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Chuou Ku, Sagamihara, Kanagawa 2525210, Japan. [Laird, E. S.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Schawinski, K.] Yale Univ, Dept Phys, New Haven, CT 06520 USA. RP Brightman, M (reprint author), Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany. EM mbright@mpe.mpg.de RI Lanzuisi, Giorgio/K-4378-2013; Brandt, William/N-2844-2015; Mignoli, Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; OI Lanzuisi, Giorgio/0000-0001-9094-0984; Alexander, David/0000-0002-5896-6313; Brandt, William/0000-0002-0167-2453; Mignoli, Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Bongiorno, Angela/0000-0002-0101-6624; Shemmer, Ohad/0000-0003-4327-1460; Schawinski, Kevin/0000-0001-5464-0888; Zamorani, Giovanni/0000-0002-2318-301X FU Japan Society for the Promotion of Science (JSPS) FX The authors would like to thank the anonymous referee for the careful reading and constructive criticism of our manuscript. The authors would also like to thank the builders and operators of XMM-Newton and Chandra and all those involved in the COSMOS and E-CDF-S surveys. MB would like to acknowledge the financial support at the start of this project from the Japan Society for the Promotion of Science (JSPS). NR 63 TC 40 Z9 40 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2013 VL 433 IS 3 BP 2485 EP 2496 DI 10.1093/mnras/stt920 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 191HK UT WOS:000322403800059 ER PT J AU Kurokawa, H Kaltenegger, L AF Kurokawa, H. Kaltenegger, L. TI Atmospheric mass-loss and evolution of short-period exoplanets: the examples of CoRoT-7b and Kepler-10b SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: individual: CoRoT-7b; planets and satellites: individual: Kepler-10b; planets and satellites: physical evolution; stars: activity ID HOT JUPITERS; SUPER-EARTHS; PLANETARY-ATMOSPHERES; EXTRASOLAR PLANETS; LUMINOSITY; NEPTUNES; DWARFS; SYSTEM; STARS; TIME AB Short-period exoplanets potentially lose envelope masses during their evolution because of atmospheric escape caused by the intense X-ray and extreme UV (XUV) radiation from their host stars. We develop a combined model of atmospheric mass-loss calculation and thermal evolution calculation of a planet to simulate its evolution and explore the dependences on the formation history of the planet. Thermal atmospheric escape as well as the Roche lobe overflow contributes to mass-loss. The maximum initial planetary model mass depends primarily on the assumed evolution model of the stellar XUV luminosity. We adapt the model to CoRoT-7b and Kepler-10b to explore the evolution of both planets and the maximum initial mass of these planets. We take the recent X-ray observation of CoRoT-7 into account and explore the effect of different XUV evolution models on the planetary initial mass. Our calculations indicate that both hot super-Earths could be remnants of Jupiter-mass gas planets. C1 [Kurokawa, H.] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan. [Kurokawa, H.] Tokyo Inst Technol, Dept Earth & Planetary Sci, Meguro Ku, Tokyo 1528551, Japan. [Kurokawa, H.; Kaltenegger, L.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Kaltenegger, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Kurokawa, H (reprint author), Nagoya Univ, Dept Phys, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648602, Japan. EM kurokawa@geo.titech.ac.jp OI Kurokawa, Hiroyuki/0000-0003-1965-1586 FU DFG [ENP Ka 3142/1-1]; Global COE programme "From the Earth to Earths"; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan [23244027] FX The authors acknowledge support from DFG funding ENP Ka 3142/1-1. This work is also supported by Global COE programme "From the Earth to Earths" and Grants-in-Aid from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan (23244027). The authors also acknowledge Professor J. Zuluaga for fruitful discussions on the different XUV models and Dr C. Mordasini for input for the equation of state of solar composition gas. The authors appreciate the referee of this paper for many fruitful suggestions. NR 30 TC 15 Z9 15 U1 0 U2 6 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2013 VL 433 IS 4 BP 3239 EP 3245 DI 10.1093/mnras/stt965 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 191IF UT WOS:000322405900036 ER PT J AU Chuang, CH Prada, F Cuesta, AJ Eisenstein, DJ Kazin, E Padmanabhan, N Sanchez, AG Xu, XY Beutler, F Manera, M Schlegel, DJ Schneider, DP Weinberg, DH Brinkmann, J Brownstein, JR Thomas, D AF Chuang, Chia-Hsun Prada, Francisco Cuesta, Antonio J. Eisenstein, Daniel J. Kazin, Eyal Padmanabhan, Nikhil Sanchez, Ariel G. Xu, Xiaoying Beutler, Florian Manera, Marc Schlegel, David J. Schneider, Donald P. Weinberg, David H. Brinkmann, Jon Brownstein, Joel R. Thomas, Daniel TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: single-probe measurements and the strong power of f(z)Sigma(8)(z) on constraining dark energy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; cosmology: observations; distance scale; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; 2-POINT CORRELATION-FUNCTION; REDSHIFT-SPACE DISTORTIONS; DATA RELEASE; ACOUSTIC-OSCILLATIONS; COSMOLOGICAL IMPLICATIONS; TO 0.5; SCALE; SAMPLE AB We present measurements of the anisotropic galaxy clustering from the Data Release 9 (DR9) CMASS sample of the Sloan Digital Sky Survey (SDSS)-III Baryon Oscillation Spectroscopic Survey (BOSS). We analyse the broad-range shape of the monopole and quadrupole correlation functions to obtain constraints, at the effective redshift z = 0.57 of the sample, on the Hubble expansion rate H(z), the angular-diameter distance D-A(z), the normalized growth rate f (z)Sigma(8)(z), the physical matter density (m)h(2), and the biased amplitude of matter fluctuation b Sigma(8)(z). We obtain H(0.57), D-A(0.57), f (0.57)Sigma(8)(0.57), (m)h(2), b Sigma(8)(0.57) = 87.6_-6.8 boolean AND+6.7 kms(-1) Mpc(-1), 1396 +/- 73 Mpc, 0.428 +/- 0.066,0.126_-0.010+0.008, 1.19 +/- 0.14} and their covariance matrix as well. The parameters which are not well constrained by our galaxy clustering analysis are marginalized over with wide flat priors. Since no priors from other data sets [i.e. cosmic microwave background (CMB)] are adopted and no dark energy models are assumed, our results from BOSS CMASS galaxy clustering alone may be combined with other data sets, i.e. CMB, SNe, lensing or other galaxy clustering data to constrain the parameters of a given cosmological model. We show that the major power on constraining dark energy from the anisotropic galaxy clustering signal, as compared to the angular-averaged one (monopole), arises from including the normalized growth rate f (z)Sigma(8)(z). In the case of the cosmological model assuming a constant dark energy equation of state and a flat universe (wCDM), our single-probe CMASS constraints, combined with CMB (WMAP9+SPT), yield a value for the dark energy equation-of-state parameter of w = -0.90 +/- 0.11. Therefore, it is important to include f (z)Sigma(8)(z) while investigating the nature of dark energy with current and upcoming large-scale galaxy surveys. C1 [Chuang, Chia-Hsun; Prada, Francisco] Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain. [Prada, Francisco] Univ Autonoma Madrid, CSIC, E-28049 Madrid, Spain. [Prada, Francisco] CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. [Cuesta, Antonio J.; Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kazin, Eyal] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Sanchez, Ariel G.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Xu, Xiaoying] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Beutler, Florian; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Manera, Marc; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Brinkmann, Jon] Apache Point Observ, Sunspot, NM 88349 USA. [Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. RP Chuang, CH (reprint author), Univ Autonoma Madrid, CSIC, Inst Fis Teor, E-28049 Madrid, Spain. EM chuang@nhn.ou.edu FU Spanish MICINN [MultiDarkCSD2009-00064, AYA201021231- C02-01]; Comunidad de Madrid [HEPHACOS S2009/ESP-1473]; NASA Office of Space Science; ICG; SEPNet; University of Portsmouth; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; University of Arizona; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; Harvard University; Instituto de Astrofisica de Canarias; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; Princeton University; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University FX We would like to thank Graeme Addison, Chris Blake, Ryan Keisler, Savvas Nesseris, Christian Reichardt, Beth Reid, Lado Samushia and Kyle Story for useful discussions. CC and FP acknowledge support from the Spanish MICINN Consolider-Ingenio 2010 Programme under grant MultiDarkCSD2009-00064 andAYA201021231- C02-01 grant. CC and FP were also supported by the Comunidad de Madrid under grant HEPHACOS S2009/ESP-1473.; We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. The mock catalogues used were produced in SCIAMA High Performance Supercomputer (HPC) cluster, supported by the ICG, SEPNet and the University of Portsmouth.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy Office of Science. The SDSS-III web site is http://www.sdss3.org/.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University. NR 83 TC 34 Z9 34 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2013 VL 433 IS 4 BP 3559 EP 3571 DI 10.1093/mnras/stt988 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 191IF UT WOS:000322405900063 ER PT J AU Potts, R AF Potts, Richard TI Hominin evolution in settings of strong environmental variability SO QUATERNARY SCIENCE REVIEWS LA English DT Review DE Paleoclimate; Human evolution; Adaptability; Variability selection; Olorgesailie; Africa; Environment ID SOUTHERN KENYA RIFT; PLEISTOCENE OLORGESAILIE FORMATION; PLIOPLEISTOCENE AFRICAN CLIMATE; LARGE MAMMAL FAUNAS; EAST-AFRICA; TURKANA BASIN; PALEOSOL CARBONATES; TROPICAL AFRICA; LATE NEOGENE; STONE TOOLS AB Investigations into how climate change shaped human evolution have begun to focus on environmental dynamics, i.e., the nature and tempo of climate and landscape variability, an approach that de-emphasizes static reconstructions of early hominin habitats. The interaction among insolation cycles is especially apparent in the paleoenvironmental records of the East African Rift System, where the longest records of human evolution are preserved. However, environmental indicators such as deep-sea oxygen isotopes, terrestrial dust flux, paleosol carbon isotopes, and lake sediments do not point consistently to any simple trend or climate driver of evolutionary change. Comparison of environmental indicators cautions against an exclusive focus on any given end-member of environmental fluctuation (driest or wettest, warmest or coolest), and argues for the impact of the entire range of variability in shaping evolutionary change. A model of alternating high and low climate variability for tropical Africa further implies that specific environmental indicators reflect different aspects of East African environmental dynamics. The model may thus help reconcile some of the conflicting interpretations about the environmental drivers of hominin evolution. First and last appearances of hominin lineages, benchmark biogeographic events, and the emergence of key adaptations and capacities to alter the surroundings are consistently concentrated in the predicted longest intervals of high climate variability. The view that emerges is that important changes in stone technology, sociality, and other aspects of hominin behavior can now be understood as adaptive responses to heightened habitat instability. Published by Elsevier Ltd. C1 Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. RP Potts, R (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20013 USA. EM pottsr@si.edu FU Peter Buck Fund for Human Origins Research; Ruth and Vernon Taylor Foundation; NSF HOMINID Program [BCS-0218511] FX I am grateful to many colleagues for their collaboration and shared data over the past decade, particularly Kay Behrensmeyer, Alan Deino, Peter deMenocal, Craig Feibel, and Bernie Owen. Research reported here was supported by the Peter Buck Fund for Human Origins Research, the Ruth and Vernon Taylor Foundation, and NSF HOMINID Program (BCS-0218511). The Olorgesailie fieldwork is a collaborative project of the National Museums of Kenya; I especially thank I.O. Farah, E. Mbua, F.K. Manthi, and M. Muungu of the NMK for their permissions and logistical support. I am grateful to Jennifer Clark for help in preparing the figures. The manuscript was improved by comments from reviewers, including M.H. Trauth. This is a publication of the Smithsonian's Human Origins Program. NR 108 TC 43 Z9 44 U1 15 U2 119 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 AUG 1 PY 2013 VL 73 BP 1 EP 13 DI 10.1016/j.quascirev.2013.04.003 PG 13 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 190QX UT WOS:000322356400001 ER PT J AU Baeza, JA Fuentes, MS AF Antonio Baeza, J. Fuentes, M. Soledad TI Exploring phylogenetic informativeness and nuclear copies of mitochondrial DNA (numts) in three commonly used mitochondrial genes: mitochondrial phylogeny of peppermint, cleaner, and semi-terrestrial shrimps (Caridea: Lysmata, Exhippolysmata, and Merguia) SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Exhippolysmata; hermaphrodite; Hippolytidae; Merguia; ornamental ID PROTANDRIC SIMULTANEOUS HERMAPHRODITISM; MARINE SHRIMP; SPECTRAL-ANALYSIS; SOCIAL MONOGAMY; MOLECULAR PHYLOGENY; DECAPOD CRUSTACEANS; WURDEMANNI CARIDEA; SEX ALLOCATION; CONTROL REGION; GENUS ALPHEUS AB Of paramount importance to studies that profit from molecular trees is the accuracy and robustness of the reconstructed phylogenies. Causes of systematic error that can mislead phylogenetic methods include nuclear copies of mitochondrial DNA (numts) and low phylogenetic informativeness (PI). Herein, numts and PI were explored in three mitochondrial genes commonly used for phylogenetic reconstruction: 16S, 12S, and cytochrome c oxidase I (COI). Shrimps from the genera Lysmata, Exhippolysmata, and Merguia were used as a model system. COI and 12S polymerase chain reaction (PCR) products from various species; (2) double peaks, background noise, and ambiguity in sequence chromatograms of COI and 12SPCR products that produced a single clear band in other species; and (3) indels, stop codons, and considerable composition bias in COI-like cloned sequences of one problematic species (Lysmata seticaudata), was interpreted as evidence of pervasive non-functional nuclear copies of mitochondrial DNA (numts) of the targeted COI (and probably 12S) mtDNA fragment. DNA markers studied was investigated using PI profiling, spectral analysis, and neighbour-nets. Marker-specific PI profiles suggested that the COI marker has the highest information content and greatest power for resolving both shallow and deep nodes in trees depicting the phylogenetic relationship among the species studied. Nonetheless, spectral analysis of splits and neighbour-nets suggested that the 16S and 12S markers were equally or even more powerful than the COI marker for resolving nodes at all phylogenetic levels. Altogether, these analyses suggest that all three mtDNA markers are equally useful for resolving phylogenetic relationships in the shrimps studied, and that PI profiling is not necessarily useful to estimate overall gene utility. A total-evidence' phylogenetic analysis that included 34 species and used a concatenated data set of 1403 characters (from reliable 16S, 12S and COI sequences), demonstrated that the genus Lysmata is paraphyletic, and that the monophyletic clade comprising species of Lysmata and Exhippolysmata can be divided into four well-supported subclades (Neotropical, Cleaner, Cosmopolitan, and Morphovariable).(c) 2013 The Linnean Society of London C1 [Antonio Baeza, J.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. [Antonio Baeza, J.] Univ Catolica Norte, Larrondo 1281, Coquimbo, Chile. [Fuentes, M. Soledad] Algenol Biofuels, Ft Myers, FL 33928 USA. RP Baeza, JA (reprint author), Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL 34949 USA. EM baeza.antonio@gmail.com OI Baeza, Juan Antonio/0000-0002-2573-6773 FU STRI Marine postdoctoral Fellowship; SMSFP postdoctoral Fellowship; National Geographic research grant FX Many thanks to: Bill Hoffman, from the Smithsonian Marine Ecosystems Exhibit (SMEE); Valerie Paul, Raphael Ritson-Williams, Sherry Reed, Koty Sharp, and Julie Piraino, from the Smithsonian Marine Station at Fort Pierce (SMSFP); Luis Ignacio Vilchis and William A. Newman, from the Scripps Institution of Oceanography (SIO), University of California at San Diego; Jimmy O'Donnell, from the University of California at Santa Cruz; Juan Bolanos, Jesus Enrique Hernandez, and Regulo Lopez, from the Universidad de Oriente (UDO), Boca del Rio, Venezuela; Adriane A. Braga, from the Universidade Estadual Paulista (UNESP), Botucatu, Brazil; Arthur Anker, from the University of Florida, Gainsville, FL, USA; Carla Piantonni, from the National Museum of Natural History, Washington DC, USA; Arcadio Castillo, from the Smithsonian Tropical Research Institute (STRI), Panama; and Fernando Alvarez, from the Universidad Nacional Autonoma de Mexico (UNAM), Mexico City, for their help during the different steps of specimen collection and loan. Special thanks to Jeff Hunt and Lee Weigt at the Laboratory of Analytical Biology, NMNH, Washington DC for their logistical support. Thanks also to Dr J.E. Buhay and an anonymous reviewer, whose comments improved preliminary versions of this article. This study was partially funded by a National Geographic research grant. J.A.B. is grateful for the support from an STRI Marine postdoctoral Fellowship and a SMSFP postdoctoral Fellowship. The authors have no conflict of interest regarding the information provided in this article. This is Smithsonian Marine Station at Fort Pierce contribution number 919. NR 110 TC 7 Z9 7 U1 0 U2 13 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 AUG PY 2013 VL 168 IS 4 BP 699 EP 722 DI 10.1111/zoj.12044 PG 24 WC Zoology SC Zoology GA 190IS UT WOS:000322333500002 ER PT J AU Sues, HD Schoch, RR AF Sues, Hans-Dieter Schoch, Rainer R. TI Reassessment of cf. Halticosaurus orbitoangulatus from the Upper Triassic (Norian) of Germany - a pseudosuchian, not a dinosaur SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE Archosauria; Baden-Wurttemberg; Loricata; Lowenstein Formation; Paracrocodylomorpha ID SAUROPODOMORPH DINOSAURIA; EARLY EVOLUTION; ARCHOSAURS; TAXONOMY; SAURISCHIA AB The holotype of cf. Halticosaurus orbitoangulatus Huene, 1932, comprises an incomplete and macerated but associated skull of an archosaurian reptile from the middle (second) Stubensandstein (middle Lowenstein Formation; Upper Triassic: Norian) of Baden-Wurttemberg, Germany. It was originally interpreted as a theropod dinosaur but more recently it has been suggested that this taxon has crocodylomorph affinities. Detailed preparation of the holotype of cf. H. orbitoangulatus has revealed much new anatomical information and permitted reassessment of its affinities. The maxilla lacks both a distinct antorbital fossa and a medial bony lamina bordering the antorbital fenestra. The lateral surface of the dentary bears a pronounced horizontal ridge. The squamosal differs from that of basal crocodylomorphs in being L-shaped rather than arcuate in dorsal view, lacking a dorsolateral overhang, and lacking an interlocking contact with the paroccipital process as, for example, in the basal crocodylomorph Saltoposuchus connectens from the same horizon and locality. Phylogenetic analysis placed cf. H. orbitoangulatus amongst loricatan pseudosuchians (but not amongst Crocodylomorpha) rather than amongst theropod dinosaurs. The holotype of cf. H. orbitoangulatus represents a previously unrecognized taxon of loricatan pseudosuchian, which is here named Apatosuchus orbitoangulatus and set apart from other known Norian-age non-crocodylomorph loricatans by its apparently much smaller size. (C) 2013 The Linnean Society of London, C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Schoch, Rainer R.] Staatliches Museum Nat Kunde Stuttgart, D-70191 Stuttgart, Germany. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu FU Alexander von Humboldt Award for Excellence in Research and Teaching FX We thank M. Kamenz for her exquisite preparation of the holotype of Apatosuchus orbitoangulatus, which made this study possible. H.-D. S. gratefully acknowledges receipt of an Alexander von Humboldt Award for Excellence in Research and Teaching, which supported his work at the Staatliches Museum fur Naturkunde Stuttgart. We thank S. L. Nesbitt and an anonymous reviewer for helpful comments on a draft of the manuscript. TNT is a program for phylogenetic analysis made freely available by the Willi Hennig Society. NR 40 TC 1 Z9 1 U1 0 U2 1 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 AUG PY 2013 VL 168 IS 4 BP 859 EP 872 DI 10.1111/zoj.12038 PG 14 WC Zoology SC Zoology GA 190IS UT WOS:000322333500005 ER PT J AU Kawai, K Hailer, F de Guia, AP Ichikawa, H Saitoh, T AF Kawai, Kuniko Hailer, Frank Pauline de Guia, Anna Ichikawa, Hideo Saitoh, Takashi TI Refugia in Glacial Ages Led to the Current Discontinuous Distribution Patterns of the Dark Red-backed Vole Myodes rex on Hokkaido, Japan SO ZOOLOGICAL SCIENCE LA English DT Article DE Myodes rex; mitochondrial DNA control region; haplotype; distribution pattern; refugia ID MITOCHONDRIAL-DNA; CLETHRIONOMYS-GLAREOLUS; MAXIMUM-LIKELIHOOD; POPULATION-GROWTH; CONTROL REGION; POLYMORPHISM; COLONIZATION; INFERENCE; MAMMALS; ISLAND AB The terrestrial mammalian fauna of the North Japanese island, Hokkaido, is more similar to that of Southern Siberia than to the main island of Japan, Honshu. Three species of the genus Myodes (Muridae, Rodentia) are found on Hokkaido, but not on Honshu. While Myodes rufocanus and M. rutilus are widely distributed across Hokkaido as well as the Eurasian continent, M. rex, which is endemic to Hokkaido and its adjacent islands, shows a discontinuous distribution pattern. We analyzed the phylogeographic history of M. rex using the mitochondrial DNA control region in order to interpret their discontinuous distribution pattern. Phylogenetic relationships among 54 distinct haplotypes showed that M. rex can be divided into four clades that occur on the northern, central, and southern regions of the Hokkaido mainland and on Rishiri Island, respectively. The phylogroups in the northern and central regions were largely separated in space, although several areas of sympatry were found. The phylogroup in the southern region, which was clearly separated from other phylogroups, showed markedly low genetic variability. All analyzed individuals from the population on Rishiri belonged to a separate lineage. Across a range of divergence rate estimates, we dated the basal divergence of all phylogroups to the mid to late Pleistocene, with subsequent signals of population expansion within lineages. We conclude that current phylogeographic structure in M. rex likely reflects Pleistocene survival in several separate refugia in situ. Past glacial ages have thus played an important role in shaping the current distribution patterns of mammalian species on Hokkaido. C1 [Kawai, Kuniko; Ichikawa, Hideo; Saitoh, Takashi] Hokkaido Univ, Field Sci Ctr, Sapporo, Hokkaido 0600811, Japan. [Kawai, Kuniko] Smithsonian Inst, Natl Museum Nat Hist, Div Mammals, Washington, DC 20013 USA. [Hailer, Frank] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Washington, DC 20008 USA. [Hailer, Frank] Senckenberg Gesell Nat Forsch, Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany. [Pauline de Guia, Anna] Univ Philippines Los Banos, Coll Arts & Sci, Inst Biol Sci, Anim Biol Div, Laguna 4031, Philippines. RP Saitoh, T (reprint author), Hokkaido Univ, Field Sci Ctr, Kita 11,Nishi 10, Sapporo, Hokkaido 0600811, Japan. EM tsaitoh@fsc.hokudai.ac.jp RI Hailer, Frank/C-9114-2012; Saitoh, Takashi/D-6021-2012 OI Hailer, Frank/0000-0002-2340-1726; Saitoh, Takashi/0000-0003-4085-5014 FU JSPS [22370006]; Smithsonian Restricted Endowment Funds; Smithsonian Center for Conservation and Evolutionary Genetics; "LOEWE - Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz" of Hesse's Ministry of Higher Education, Research, and the Arts FX We are indebted to Keisuke Nakata and the Forestry Agency of Japanese Government for providing the material analyzed in this paper. We thank members of Field Science Centre, Hokkaido University who helped to collect samples in the field. We are grateful to Dr. Kristofer M. Helgen and Dr. Koji Fujimura for valuable comments and supporting, and Dr. Takahiro Segawa for supporting to construct haplotype trees. This work was supported by a JSPS Grant-in-Aid for Scientific Research (22370006) to TS. FH was supported by the Smithsonian Restricted Endowment Funds, the Smithsonian Center for Conservation and Evolutionary Genetics, and "LOEWE - Landes-Offensive zur Entwicklung Wissenschaftlich-okonomischer Exzellenz" of Hesse's Ministry of Higher Education, Research, and the Arts. Specimens collected in Niseko are deposited in Hokkaido University Natural History Museum under the following ID number; HUNHM46316, HUNHM48103, HUNHM48257, HUNHM48282, HUNHM 48283, HUNHM48284, HUNHM 48445, HUNHM 48446, and HUNHM 48777. NR 46 TC 4 Z9 4 U1 0 U2 11 PU ZOOLOGICAL SOC JAPAN PI TOKYO PA TOSHIN-BUILDING, HONGO 2-27-2, BUNKYO-KU, TOKYO, 113-0033, JAPAN SN 0289-0003 J9 ZOOL SCI JI Zool. Sci. PD AUG PY 2013 VL 30 IS 8 BP 642 EP 650 DI 10.2108/zsj.30.642 PG 9 WC Zoology SC Zoology GA 190GT UT WOS:000322328100006 PM 23915157 ER PT J AU Bai, XN AF Bai, Xue-Ning TI WIND-DRIVEN ACCRETION IN PROTOPLANETARY DISKS. II. RADIAL DEPENDENCE AND GLOBAL PICTURE SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; instabilities; magnetohydrodynamics (MHD); methods: numerical; protoplanetary disks; turbulence ID HUBBLE-SPACE-TELESCOPE; YOUNG STELLAR OBJECTS; T-TAURI STARS; FORBIDDEN-LINE EMISSION; SURFACE-LAYER ACCRETION; MAGNETOROTATIONAL-INSTABILITY; NONLINEAR EVOLUTION; AMBIPOLAR DIFFUSION; DG-TAURI; IMAGING SPECTROGRAPH AB Non-ideal magnetohydrodynamical effects play a crucial role in determining the mechanism and efficiency of angular momentum transport as well as the level of turbulence in protoplanetary disks (PPDs), which are the key to understanding PPD evolution and planet formation. It was shown in our previous work that at 1 AU, the magnetorotational instability (MRI) is completely suppressed when both ohmic resistivity and ambipolar diffusion (AD) are taken into account, resulting in a laminar flow with accretion driven by magnetocentrifugal wind. In this work, we study the radial dependence of the laminar wind solution using local shearing-box simulations. The scaling relation on the angular momentum transport for the laminar wind is obtained, and we find that the wind-driven accretion rate can be approximated as (M) over dot approximate to 0.91 x 10(-8)R(AU)(1.21) (B-p/10 mG)M-0.93(circle dot) yr(-1), where B-p is the strength of the large-scale poloidal magnetic field threading the disk. The result is independent of disk surface density. Four criteria are outlined for the existence of the laminar wind solution: (1) ohmic resistivity dominated the midplane region, (2) the AD-dominated disk upper layer, (3) the presence of a (not too weak) net vertical magnetic flux, and (4) sufficiently well-ionized gas beyond the disk surface. All these criteria are likely to be met in the inner region of the disk from similar to 0.3 AU to about 5-10 AU for typical PPD accretion rates. Beyond this radius, the angular momentum transport is likely to proceed due to a combination of the MRI and disk wind, and eventually completely dominated by the MRI (in the presence of strong AD) in the outer disk. Our simulation results provide key ingredients for a new paradigm on the accretion processes in PPDs. C1 Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Bai, XN (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St,MS-51, Cambridge, MA 02138 USA. EM xbai@cfa.harvard.edu FU NASA through Space Telescope Science Institute [HST-HF-51301.01]; NASA [NAS5-26555] FX I thank the referee for useful comments and suggestions that improve the clarity of this paper. This work is supported by program number HST-HF-51301.01-A provided by NASA through a Hubble Fellowship grant from the Space Telescope Science Institute awarded to X.N.B., which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. NR 70 TC 36 Z9 37 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 96 DI 10.1088/0004-637X/772/2/96 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700018 ER PT J AU Barnard, R Garcia, M Murray, SS AF Barnard, R. Garcia, M. Murray, S. S. TI THE SECOND ULTRALUMINOUS X-RAY SOURCE TRANSIENT IN M31: CHANDRA, HUBBLE SPACE TELESCOPE, AND XMM OBSERVATIONS, AND EVIDENCE FOR AN EXTENDED CORONA SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: general ID BLACK-HOLE; LIGHT CURVES; BINARIES; ACCRETION; GALAXIES; STARS; COMPTONIZATION AB XMMU J004243.6+412519 is a transient X-ray source in M31, first discovered 2012 January 15. Different approaches to fitting the brightest follow-up observation gave luminosities 1.3-2.5 x 10(39) erg s(-1), making it the second ultraluminous X-ray source (ULX) in M31, with a probable black hole accretor. These different models represent different scenarios for the corona: optically thick and compact, or optically thin and extended. We obtained Chandra ACIS and Hubble Space Telescope Advanced Camera for Surveys observations of this object as part of our transient monitoring program, and also observed it serendipitously in a 120 ks XMM-Newton observation. We identify an optical counterpart at J2000 position 00:42:43.70 +41:25:18.54; its F435W (similar to B band) magnitude was 25.97 +/- 0.03 in the 2012 March 7 observation, and >28.4 at the 4 sigma level during the 2012 September 7 observation, indicating a low-mass donor. We created two alternative light curves, using the different corona scenarios, finding linear decay for the compact corona and exponential decay for the extended corona; linear decay implies a disk that is >5 mag brighter than we observed. We therefore favor the extended corona scenario, but caution that there is no statistical preference for this model in the X-ray spectra alone. Using two empirical relations between the X-ray to optical ratio and the orbital period, we estimate a period of similar to 9-30 hr; this period is consistent with that of the first ULX in M31 (18(-6)(+5) hr). C1 [Barnard, R.; Garcia, M.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MD USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU ESA member states; US (NASA); Chandra grants [GO2-13106X, GO1-12109X]; HST [GO-11833, GO-12014]; NASA [NAS8-03060] FX We thank the anonymous referee for his/her thoughtful comments that substantially improved this paper. We thank Z. Li for merging the Chandra data. This research has made use of data obtained from the Chandra data archive, and software provided by the Chandra X-Ray Center (CXC). We also include analysis of data from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the US (NASA). R. B. is funded by Chandra grants GO2-13106X and GO1-12109X, along with HST grants GO-11833 and GO-12014. M. R. G. and S. S. M are partially supported by NASA contract NAS8-03060. NR 34 TC 7 Z9 7 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 126 DI 10.1088/0004-637X/772/2/126 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700048 ER PT J AU Bogdan, A Forman, WR Kraft, RP Jones, C AF Bogdan, Akos Forman, William R. Kraft, Ralph P. Jones, Christine TI DETECTION OF A LUMINOUS HOT X-RAY CORONA AROUND THE MASSIVE SPIRAL GALAXY NGC 266 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 266); galaxies: ISM; galaxies: spiral; X-rays: galaxies; X-rays: general; X-rays: ISM ID DISK GALAXIES; GASEOUS HALO; EMISSION; SIMULATIONS; GAS AB The presence of luminous hot X-ray coronae in the dark matter halos of massive spiral galaxies is a basic prediction of galaxy formation models. However, observational evidence for such coronae is very scarce, with the first few examples having only been detected recently. In this paper, we study the large-scale diffuse X-ray emission associated with the massive spiral galaxy NGC 266. Using ROSAT and Chandra X-ray observations we argue that the diffuse emission extends at least similar to 70 kpc, whereas the bulk of the stellar light is confined to within similar to 25 kpc. Based on X-ray hardness ratios, we find that most of the diffuse emission is released at energies less than or similar to 1.2 keV, which indicates that this emission originates from hot X-ray gas. Adopting a realistic gas temperature and metallicity, we derive that in the (0.05-0.15)r(200) region (where r(200) is the virial radius) the bolometric X-ray luminosity of the hot gas is (4.3 +/- 0.8) x 10(40) erg s(-1) and the gas mass is (9.1 +/- 0.9) x 10(9) M-circle dot. These values are comparable to those observed for the two other well-studied X-ray coronae in spiral galaxies, suggesting that the physical properties of such coronae are similar. This detection offers an excellent opportunity for comparison of observations with detailed galaxy formation simulations. C1 [Bogdan, Akos; Forman, William R.; Kraft, Ralph P.; Jones, Christine] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Bogdan, A (reprint author), Smithsonian Astrophys Observ, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu OI Forman, William/0000-0002-9478-1682 FU NASA; NSF; NASA [PF1-120081, NAS8-03060]; CXC; Smithsonian Institution FX We thank the anonymous referee for helpful comments. A.B. thanks Alexey Vikhlinin for helpful discussions about the ROSAT PSF. This research has made use of Chandra data provided by the CXC. 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 NASA and NSF. The authors acknowledge the usage of the HyperLeda database. A.B. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant number PF1-120081 awarded by the CXC, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. W.F. and C.J. acknowledge support from the Smithsonian Institution. NR 25 TC 20 Z9 20 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 AUG 1 PY 2013 VL 772 IS 2 AR 98 DI 10.1088/0004-637X/772/2/98 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700020 ER PT J AU Bogdan, A Forman, WR Vogelsberger, M Bourdin, H Sijacki, D Mazzotta, P Kraft, RP Jones, C Gilfanov, M Churazov, E David, LP AF Bogdan, Akos Forman, William R. Vogelsberger, Mark Bourdin, Herve Sijacki, Debora Mazzotta, Pasquale Kraft, Ralph P. Jones, Christine Gilfanov, Marat Churazov, Eugene David, Laurence P. TI HOT X-RAY CORONAE AROUND MASSIVE SPIRAL GALAXIES: A UNIQUE PROBE OF STRUCTURE FORMATION MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (NGC 1961, NGC 6753); galaxies: ISM; galaxies: spiral; X-rays: galaxies; X-rays: general; X-rays: ISM ID MOVING-MESH COSMOLOGY; SMOOTHED PARTICLE HYDRODYNAMICS; GALACTIC NUCLEUS FEEDBACK; XMM-NEWTON; STAR-FORMATION; ELLIPTIC GALAXY; DISK GALAXIES; STELLAR MASS; INTERGALACTIC MEDIUM; CHANDRA OBSERVATION AB Luminous X-ray gas coronae in the dark matter halos of massive spiral galaxies are a fundamental prediction of structure formation models, yet only a few such coronae have been detected so far. In this paper, we study the hot X-ray coronae beyond the optical disks of two "normal" massive spirals, NGC 1961 and NGC 6753. Based on XMM-Newton X-ray observations, hot gaseous emission is detected to similar to 60 kpc-well beyond their optical radii. The hot gas has a best-fit temperature of kT similar to 0.6 keV and an abundance of similar to 0.1 Solar, and exhibits a fairly uniform distribution, suggesting that the quasi-static gas resides in hydrostatic equilibrium in the potential well of the galaxies. The bolometric luminosity of the gas in the (0.05-0.15)r(200) region (r(200) is the virial radius) is similar to 6 x 10(40) erg s(-1) for both galaxies. The baryon mass fractions of NGC 1961 and NGC 6753 are f(b,NGC 1961) similar to 0.11 and f(b,NGC 6753) similar to 0.09, which values fall short of the cosmic baryon fraction. The hot coronae around NGC 1961 and NGC 6753 offer an excellent basis to probe structure formation simulations. To this end, the observations are confronted with the moving mesh code arepo and the smoothed particle hydrodynamics code gadget. Although neither model gives a perfect description, the observed luminosities, gas masses, and abundances favor the arepo code. Moreover, the shape and the normalization of the observed density profiles are better reproduced by arepo within similar to 0.5r(200). However, neither model incorporates efficient feedback from supermassive black holes or supernovae, which could alter the simulated properties of the X-ray coronae. With the further advance of numerical models, the present observations will be essential in constraining the feedback effects in structure formation simulations. C1 [Bogdan, Akos; Forman, William R.; Vogelsberger, Mark; Sijacki, Debora; Mazzotta, Pasquale; Kraft, Ralph P.; Jones, Christine; David, Laurence P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bourdin, Herve; Mazzotta, Pasquale] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Gilfanov, Marat; Churazov, Eugene] Max Planck Inst Astrophys, D-85748 Garching, Germany. RP Bogdan, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM abogdan@cfa.harvard.edu RI Churazov, Eugene/A-7783-2013; Mazzotta, Pasquale/B-1225-2016; OI Mazzotta, Pasquale/0000-0002-5411-1748; Forman, William/0000-0002-9478-1682 FU National Aeronautics and Space Administration; National Science Foundation; NASA [PF1-120081, NAS8-03060]; Chandra X-ray Center; Smithsonian Institution; ESA Member States; NASA FX We thank the anonymous referee for useful comments. We thank Alexey Vikhlinin for helpful discussions about SMART-X, Volker Springel for careful reading, and Rob Crain for critical comments. This work uses observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. In this work the NASA/IPAC Extragalactic Database (NED) have been used. The authors acknowledge use of the HyperLeda database (http://leda.univ-lyon1.fr). A.B. acknowledges support provided by NASA through Einstein Postdoctoral Fellowship grant No. PF1-120081 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. W.F. and C.J. acknowledge support from the Smithsonian Institution. NR 89 TC 30 Z9 30 U1 1 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 97 DI 10.1088/0004-637X/772/2/97 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700019 ER PT J AU Brescia, M Cavuoti, S D'Abrusco, R Longo, G Mercurio, A AF Brescia, M. Cavuoti, S. D'Abrusco, R. Longo, G. Mercurio, A. TI PHOTOMETRIC REDSHIFTS FOR QUASARS IN MULTI-BAND SURVEYS SO ASTROPHYSICAL JOURNAL LA English DT Article DE catalogs; galaxies: distances and redshifts; methods: data analysis; quasars: general; surveys ID DIGITAL-SKY-SURVEY; 7TH DATA RELEASE; FUNCTION MINIMIZATION; CONJUGATE GRADIENTS; GALAXIES; SDSS; EVOLUTION; SELECTION; EXPLORER; MISSION AB The Multi Layer Perceptron with Quasi Newton Algorithm (MLPQNA) is a machine learning method that can be used to cope with regression and classification problems on complex and massive data sets. In this paper, we give a formal description of the method and present the results of its application to the evaluation of photometric redshifts for quasars. The data set used for the experiment was obtained by merging four different surveys (Sloan Digital Sky Survey, GALEX, UKIDSS, and WISE), thus covering a wide range of wavelengths from the UV to the mid-infrared. The method is able (1) to achieve a very high accuracy, (2) to drastically reduce the number of outliers and catastrophic objects, and (3) to discriminate among parameters (or features) on the basis of their significance, so that the number of features used for training and analysis can be optimized in order to reduce both the computational demands and the effects of degeneracy. The best experiment, which makes use of a selected combination of parameters drawn from the four surveys, leads, in terms of Delta z(norm) (i.e., (z(spec) - z(phot))/(1 + z(spec))), to an average of Delta z(norm) = 0.004, a standard deviation of sigma = 0.069, and a median absolute deviation, MAD = 0.02, over the whole redshift range (i.e., z(spec) <= 3.6), defined by the four-survey cross-matched spectroscopic sample. The fraction of catastrophic outliers, i.e., of objects with photo-z deviating more than 2 sigma from the spectroscopic value, is <3%, leading to sigma = 0.035 after their removal, over the same redshift range. The method is made available to the community through the DAMEWARE Web application. C1 [Brescia, M.; Mercurio, A.] INAF Astron Observ Capodimonte, I-80131 Naples, Italy. [Brescia, M.; Cavuoti, S.; Longo, G.] Univ Naples Federico II, Dept Phys, I-80126 Naples, Italy. [D'Abrusco, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Brescia, M (reprint author), INAF Astron Observ Capodimonte, Via Moiariello 16, I-80131 Naples, Italy. EM brescia@oacn.inaf.it RI D'Abrusco, Raffaele/L-2767-2016; Cavuoti, Stefano/B-4650-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Cavuoti, Stefano/0000-0002-3787-4196; Brescia, Massimo/0000-0001-9506-5680 FU Project F.A.R.O.; PRIN-INAF; US Virtual Astronomical Observatory; National Science Foundation; National Aeronautics and Space Administration; PRIN-MIUR FX The authors thank the anonymous referee for comments and suggestions that helped to improve the paper, and the whole DAMEWARE team6 for many useful discussions. The authors also thank the financial support of Project F.A.R.O., third call by the University Federico II of Naples, and of the PRIN-MIUR 2011 for Euclid Mission. G. L. thanks Professor G. S. Djorgovski and the whole Department of Astronomy at the California Institute of Technology in Pasadena for their hospitality. A. M. and M. B. acknowledge the financial support of PRIN-INAF 2010, Architecture and Tomography of Galaxy Clusters. R. D'A. acknowledges the financial support of the US Virtual Astronomical Observatory, which is sponsored by the National Science Foundation and the National Aeronautics and Space Administration. NR 59 TC 18 Z9 18 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 140 DI 10.1088/0004-637X/772/2/140 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700062 ER PT J AU Clarke, TE Randall, SW Sarazin, CL Blanton, EL Giacintucci, S AF Clarke, T. E. Randall, S. W. Sarazin, C. L. Blanton, E. L. Giacintucci, S. TI CHANDRA VIEW OF THE ULTRA-STEEP SPECTRUM RADIO SOURCE IN A2443: MERGER SHOCK-INDUCED COMPRESSION OF FOSSIL RADIO PLASMA? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual (A2443); radio continuum: galaxies; X-rays: galaxies: clusters ID GALAXY CLUSTER; X-RAY; COLD FRONTS; BOW SHOCK; RELICS; CORES; WAVES; REDSHIFTS; EMISSION; CATALOG AB We present a new Chandra X-ray observation of the intracluster medium in the galaxy cluster A2443, hosting an ultra-steep spectrum radio source. The data reveal that the intracluster medium is highly disturbed. The thermal gas in the core is elongated along a northwest to southeast axis and there is a cool tail to the north. We also detect two X-ray surface brightness edges near the cluster core. The edges appear to be consistent with an inner cold front to the northeast of the core and an outer shock front to the southeast of the core. The southeastern edge is coincident with the location of the radio relic as expected for shock (re) acceleration or adiabatic compression of fossil relativistic electrons. C1 [Clarke, T. E.] USN, Res Lab, Washington, DC 20375 USA. [Randall, S. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Sarazin, C. L.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Blanton, E. L.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Blanton, E. L.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Giacintucci, S.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Giacintucci, S.] Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA. RP Clarke, TE (reprint author), USN, Res Lab, Code 7213, Washington, DC 20375 USA. EM tracy.clarke.ca@nrl.navy.mil RI Blanton, Elizabeth/H-4501-2014; OI Randall, Scott/0000-0002-3984-4337 FU National Aeronautics and Space Administration, through Chandra Award Number [GO1-12007Z]; 6.1 Base funding; Chandra X-ray Center through NASA contract [NAS8-03060]; Smithsonian Institution; NASA Chandra Grants [GO9-0135X, GO9-0148X, GO1-12169X]; NASA ADAP grant [NNX11AD15G]; NASA through the Astrophysics Data Analysis Program [NNX10AC98G]; NASA award RSA [1440385]; NASA through Einstein Postdoctoral Fellowship [PF0-110071]; Chandra X-ray Center; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science FX T. E. C. was supported in part for this work by the National Aeronautics and Space Administration, through Chandra Award Number GO1-12007Z. Basic research in radio astronomy at the Naval Research Laboratory is supported by 6.1 Base funding. S. R. is supported by the Chandra X-ray Center through NASA contract NAS8-03060 and the Smithsonian Institution. C. L. S. was supported in part by NASA Chandra Grants GO9-0135X, GO9-0148X, and GO1-12169X, and NASA ADAP grant NNX11AD15G. E. L. B. was partially supported by NASA through the Astrophysics Data Analysis Program, grant number NNX10AC98G, and through NASA award RSA No. 1440385 issued by JPL/Caltech. S. G. acknowledges the support of NASA through Einstein Postdoctoral Fellowship PF0-110071 awarded by the Chandra X-ray Center. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. NR 58 TC 6 Z9 6 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 84 DI 10.1088/0004-637X/772/2/84 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700006 ER PT J AU Cranmer, SR Wilner, DJ MacGregor, MA AF Cranmer, Steven R. Wilner, David J. MacGregor, Meredith A. TI CONSTRAINING A MODEL OF TURBULENT CORONAL HEATING FOR AU MICROSCOPII WITH X-RAY, RADIO, AND MILLIMETER OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE radio continuum: stars; stars: coronae; stars: individual (AU Microscopii); submillimeter: stars; turbulence; X-rays: stars ID T TAURI STARS; MAIN-SEQUENCE STARS; LOW-MASS STARS; M-DWARFS; DEBRIS DISK; TRANSITION REGION; MAGNETIC CARPET; DUST DYNAMICS; BRIGHT POINTS; SOLAR CORONA AB Many low-mass pre-main-sequence stars exhibit strong magnetic activity and coronal X-ray emission. Even after the primordial accretion disk has been cleared out, the star's high-energy radiation continues to affect the formation and evolution of dust, planetesimals, and large planets. Young stars with debris disks are thus ideal environments for studying the earliest stages of non-accretion-driven coronae. In this paper we simulate the corona of AU Mic, a nearby active M dwarf with an edge-on debris disk. We apply a self-consistent model of coronal loop heating that was derived from numerical simulations of solar field-line tangling and magnetohydrodynamic turbulence. We also synthesize the modeled star's X-ray luminosity and thermal radio/millimeter continuum emission. A realistic set of parameter choices for AU Mic produces simulated observations that agree with all existing measurements and upper limits. This coronal model thus represents an alternative explanation for a recently discovered ALMA central emission peak that was suggested to be the result of an inner "asteroid belt" within 3 AU of the star. However, it is also possible that the central 1.3 mm peak is caused by a combination of active coronal emission and a bright inner source of dusty debris. Additional observations of this source's spatial extent and spectral energy distribution at millimeter and radio wavelengths will better constrain the relative contributions of the proposed mechanisms. C1 [Cranmer, Steven R.; Wilner, David J.; MacGregor, Meredith A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Cranmer, SR (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. OI MacGregor, Meredith/0000-0001-7891-8143 NR 72 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 149 DI 10.1088/0004-637X/772/2/149 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700071 ER PT J AU Ivison, RJ Swinbank, AM Smail, I Harris, AI Bussmann, RS Cooray, A Cox, P Fu, H Kovacs, A Krips, M Narayanan, D Negrello, M Neri, R Penarrubia, J Richard, J Riechers, DA Rowlands, K Staguhn, JG Targett, TA Amber, S Baker, AJ Bourne, N Bertoldi, F Bremer, M Calanog, JA Clements, DL Dannerbauer, H Dariush, A De Zotti, G Dunne, L Eales, SA Farrah, D Fleuren, S Franceschini, A Geach, JE George, RD Helly, JC Hopwood, R Ibar, E Jarvis, MJ Kneib, JP Maddox, S Omont, A Scott, D Serjeant, S Smith, MWL Thompson, MA Valiante, E Valtchanov, I Vieira, J van der Werf, P AF Ivison, R. J. Swinbank, A. M. Smail, Ian Harris, A. I. Bussmann, R. S. Cooray, A. Cox, P. Fu, H. Kovacs, A. Krips, M. Narayanan, D. Negrello, M. Neri, R. Penarrubia, J. Richard, J. Riechers, D. A. Rowlands, K. Staguhn, J. G. Targett, T. A. Amber, S. Baker, A. J. Bourne, N. Bertoldi, F. Bremer, M. Calanog, J. A. Clements, D. L. Dannerbauer, H. Dariush, A. De Zotti, G. Dunne, L. Eales, S. A. Farrah, D. Fleuren, S. Franceschini, A. Geach, J. E. George, R. D. Helly, J. C. Hopwood, R. Ibar, E. Jarvis, M. J. Kneib, J. -P. Maddox, S. Omont, A. Scott, D. Serjeant, S. Smith, M. W. L. Thompson, M. A. Valiante, E. Valtchanov, I. Vieira, J. van der Werf, P. TI HERSCHEL-ATLAS: A BINARY HyLIRG PINPOINTING A CLUSTER OF STARBURSTING PROTOELLIPTICALS SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: high-redshift; galaxies: starburst; infrared: galaxies; radio continuum: galaxies; radio lines: galaxies; submillimeter: galaxies ID STAR-FORMATION RATES; ULTRALUMINOUS INFRARED GALAXIES; LUMINOUS SUBMILLIMETER GALAXIES; SCIENCE DEMONSTRATION PHASE; SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; GREEN BANK TELESCOPE; HIGH-REDSHIFT; MOLECULAR GAS; MASS FUNCTION AB Panchromatic observations of the best candidate hyperluminous infrared galaxies from the widest Herschel extragalactic imaging survey have led to the discovery of at least four intrinsically luminous z = 2.41 galaxies across an approximate to 100 kpc region-a cluster of starbursting protoellipticals. Via subarcsecond interferometric imaging we have measured accurate gas and star formation surface densities. The two brightest galaxies span similar to 3 kpc FWHM in submillimeter/radio continuum and CO J = 4-3, and double that in CO J = 1-0. The broad CO line is due partly to the multitude of constituent galaxies and partly to large rotational velocities in two counter-rotating gas disks-a scenario predicted to lead to the most intense starbursts, which will therefore come in pairs. The disks have M-dyn of several x 10(11) M-circle dot, and gas fractions of similar to 40%. Velocity dispersions are modest so the disks are unstable, potentially on scales commensurate with their radii: these galaxies are undergoing extreme bursts of star formation, not confined to their nuclei, at close to the Eddington limit. Their specific star formation rates place them greater than or similar to 5x above the main sequence, which supposedly comprises large gas disks like these. Their high star formation efficiencies are difficult to reconcile with a simple volumetric star formation law. N-body and dark matter simulations suggest that this system is the progenitor of a B(inary)-type approximate to 10(14.6)-M-circle dot cluster. C1 [Ivison, R. J.; Ibar, E.] Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Ivison, R. J.; Penarrubia, J.; Targett, T. A.; George, R. D.] Univ Edinburgh, Inst Astron, Royal Observ, Edinburgh EH9 3HJ, Midlothian, Scotland. [Swinbank, A. M.; Smail, Ian; Helly, J. C.] Univ Durham, Inst Computat Cosmol, Durham DH1 3LE, England. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cooray, A.; Fu, H.; Calanog, J. A.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Cox, P.; Krips, M.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Kovacs, A.] Univ Minnesota, Dept Astron, Minneapolis, MN 55414 USA. [Narayanan, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Negrello, M.; De Zotti, G.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Richard, J.] Univ Lyon 1, Ctr Rech Astrophys Lyon, F-69561 St Genis Laval, France. [Riechers, D. A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Rowlands, K.; Bourne, N.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Staguhn, J. G.] Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. [Amber, S.; Hopwood, R.; Serjeant, S.] Open Univ, Dept Phys Sci, Milton Keynes MK7 6AA, Bucks, England. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bertoldi, F.] Univ Bonn, Argelander Inst Astron, D-53121 Bonn, Germany. [Bremer, M.] Univ Bristol, HH Wills Phys Lab, Bristol BS8 1TL, Avon, England. [Clements, D. L.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Dept Phys, London SW7 2AZ, England. [Dannerbauer, H.] Univ Vienna, Inst Astrophys, A-1180 Vienna, Austria. [Dariush, A.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [De Zotti, G.] SISSA, I-34136 Trieste, Italy. [Dunne, L.; Maddox, S.] Univ Canterbury, Dept Phys & Astron, Christchurch 1, New Zealand. [Eales, S. A.; Smith, M. W. L.; Valiante, E.] Cardiff Univ, Sch Phys & Astron, Cardiff CF24 3AA, S Glam, Wales. [Farrah, D.] Virginia Polytech Inst & State Univ, Dept Phys, Blacksburg, VA 24061 USA. [Fleuren, S.] Queen Mary Univ London, Sch Phys & Astron, London E1 4NS, England. [Franceschini, A.] Univ Padua, Dept Astron, I-35122 Padua, Italy. [Geach, J. E.; Thompson, M. A.] Univ Hertfordshire, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Ibar, E.] Catholic Univ Chile, Dept Astron & Astrofis, Casilla 306 22, Santiago, Chile. [Jarvis, M. J.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M. J.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. [Kneib, J. -P.] Observ Geneva, EPFL SB IPEP LASTRO, CH-1290 Sauverny, Switzerland. [Omont, A.] Univ Paris 06, UPMC, F-75014 Paris, France. [Omont, A.] CNRS, UMR7095, F-75014 Paris, France. [Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Valtchanov, I.] Herschel Sci Ctr, European Space Astron Ctr, ESA, E-28691 Villanueva De La Canada, Spain. [Vieira, J.] CALTECH, Pasadena, CA 91125 USA. [van der Werf, P.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Ivison, RJ (reprint author), Royal Observ, Sci & Technol Facil Council, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. RI Smail, Ian/M-5161-2013; Kneib, Jean-Paul/A-7919-2015; Kovacs, Attila/C-1171-2010; Ivison, R./G-4450-2011; OI Maddox, Stephen/0000-0001-5549-195X; Smail, Ian/0000-0003-3037-257X; Kneib, Jean-Paul/0000-0002-4616-4989; Kovacs, Attila/0000-0001-8991-9088; Ivison, R./0000-0001-5118-1313; De Zotti, Gianfranco/0000-0003-2868-2595; Scott, Douglas/0000-0002-6878-9840 FU European Research Council (ERC); NASA through JPL; STFC; ERC; ASI/INAF [I/072/09/0] FX R.J.I. acknowledges support from the European Research Council (ERC) in the form of Advanced Grant, COSMICISM. The Herschel-ATLAS is a project with Herschel, which is an ESA Space Observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. The H-ATLAS Web site is www.h-atlas.org. US participants in H-ATLAS acknowledge support from NASA through a contract from JPL. I. R. S. acknowledges support from STFC and ERC. M.N. and G.dZ. acknowledge financial support from ASI/INAF Agreement I/072/09/0. NR 106 TC 54 Z9 54 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 137 DI 10.1088/0004-637X/772/2/137 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700059 ER PT J AU Korzennik, SG Rabello-Soares, MC Schou, J Larson, TP AF Korzennik, S. G. Rabello-Soares, M. C. Schou, J. Larson, T. P. TI ACCURATE CHARACTERIZATION OF HIGH-DEGREE MODES USING MDI OBSERVATIONS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: activity; Sun: helioseismology; Sun: oscillations ID MICHELSON DOPPLER IMAGER; HIGH-DEGREE FREQUENCIES; SOLAR-CYCLE; DIFFERENTIAL ROTATION; SPLITTINGS; EIGENFUNCTIONS; INTERMEDIATE; SPECTRUM; SURFACE AB We present the first accurate characterization of high-degree modes, derived using the best Michelson Doppler Imager (MDI) full-disk full-resolution data set available. A 90 day long time series of full-disk 2 arcsec pixel(-1) resolution Dopplergrams was acquired in 2001, thanks to the high rate telemetry provided by the Deep Space Network. These Dopplergrams were spatially decomposed using our best estimate of the image scale and the known components of MDI's image distortion. A multi-taper power spectrum estimator was used to generate power spectra for all degrees and all azimuthal orders, up to l = 1000. We used a large number of tapers to reduce the realization noise, since at high degrees the individual modes blend into ridges and thus there is no reason to preserve a high spectral resolution. These power spectra were fitted for all degrees and all azimuthal orders, between l = 100 and l = 1000, and for all the orders with substantial amplitude. This fitting generated in excess of 5.2x10(6) individual estimates of ridge frequencies, line widths, amplitudes, and asymmetries (singlets), corresponding to some 5700 multiplets (l, n). Fitting at high degrees generates ridge characteristics, characteristics that do not correspond to the underlying mode characteristics. We used a sophisticated forward modeling to recover the best possible estimate of the underlying mode characteristics (mode frequencies, as well as line widths, amplitudes, and asymmetries). We describe in detail this modeling and its validation. The modeling has been extensively reviewed and refined, by including an iterative process to improve its input parameters to better match the observations. Also, the contribution of the leakage matrix on the accuracy of the procedure has been carefully assessed. We present the derived set of corrected mode characteristics, which includes not only frequencies, but line widths, asymmetries, and amplitudes. We present and discuss their uncertainties and the precision of the ridge-to-mode correction schemes, through a detailed assessment of the sensitivity of the model to its input set. The precision of the ridge-to-mode correction is indicative of any possible residual systematic biases in the inferred mode characteristics. In our conclusions, we address how to further improve these estimates, and the implications for other data sets, like GONG+ and HMI. C1 [Korzennik, S. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rabello-Soares, M. C.; Schou, J.; Larson, T. P.] Stanford Univ, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA. RP Korzennik, SG (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. RI Rabello Soares, Maria Cristina/C-3207-2013; OI Rabello Soares, Maria Cristina/0000-0003-0172-3713 FU NASA at Stanford University [NAG5-8878, NAG5-10483]; Stanford [PR-6333]; NASA [NAG5-9819, NNG05GD58G] FX The Solar Oscillations Investigation-Michelson Doppler Imager project on SOHO is supported by NASA grant NAG5-8878 and NAG5-10483 at Stanford University. SOHO is a project of international cooperation between ESA and NASA. S. G. K. was supported by Stanford contract PR-6333 and NASA grants NAG5-9819 and NNG05GD58G. NR 30 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 AUG 1 PY 2013 VL 772 IS 2 AR 87 DI 10.1088/0004-637X/772/2/87 PG 28 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700009 ER PT J AU Lohfink, AM Reynolds, CS Jorstad, SG Marscher, AP Miller, ED Aller, H Aller, MF Brenneman, LW Fabian, AC Miller, JM Mushotzky, RF Nowak, MA Tombesi, F AF Lohfink, Anne M. Reynolds, Christopher S. Jorstad, Svetlana G. Marscher, Alan P. Miller, Eric D. Aller, Hugh Aller, Margo F. Brenneman, Laura W. Fabian, Andrew C. Miller, Jon M. Mushotzky, Richard F. Nowak, Michael A. Tombesi, Francesco TI AN X-RAY VIEW OF THE JET CYCLE IN THE RADIO-LOUD AGN 3C120 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: individual (3C120); galaxies: jets; galaxies: nuclei; radio continuum: galaxies; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE SPIN; GALAXY 3C 120; ACCRETION-DISK; XMM-NEWTON; RELATIVISTIC JETS; MAGNETOHYDRODYNAMIC SIMULATIONS; EMISSION-LINES; IRON LINES; CONNECTION AB We present a study of the central engine in the broad-line radio galaxy 3C120 using a multi-epoch analysis of a deep XMM-Newton observation and two deep Suzaku pointings (in 2012). In order to place our spectral data into the context of the disk-disruption/jet-ejection cycles displayed by this object, we monitor the source in the UV/X-ray bands, and in the radio band. We find three statistically acceptable spectral models: a disk-reflection model, a jet model, and a jet+disk model. Despite being good descriptions of the data, the disk-reflection model violates the radio constraints on the inclination, and the jet model has a fine-tuning problem, requiring a jet contribution exceeding that expected. Thus, we argue for a composite jet+disk model. Within the context of this model, we verify the basic predictions of the jet-cycle paradigm, finding a truncated/refilling disk during the Suzaku observations and a complete disk extending down to the innermost stable circular orbit during the XMM-Newton observation. The idea of a refilling disk is further supported by the detection of the ejection of a new jet knot approximately one month after the Suzaku pointings. We also discover a step-like event in one of the Suzaku pointings in which the soft band lags the hard band. We suggest that we are witnessing the propagation of a disturbance from the disk into the jet on a timescale set by the magnetic field. C1 [Lohfink, Anne M.; Reynolds, Christopher S.; Mushotzky, Richard F.; Tombesi, Francesco] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Lohfink, Anne M.; Reynolds, Christopher S.; Mushotzky, Richard F.; Tombesi, Francesco] Univ Maryland, Joint Space Sci Inst JSI, College Pk, MD 20742 USA. [Jorstad, Svetlana G.; Marscher, Alan P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Miller, Eric D.; Nowak, Michael A.] MIT, Kavli Inst Astrophys, Cambridge, MA 02139 USA. [Aller, Hugh; Aller, Margo F.; Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Brenneman, Laura W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Lohfink, AM (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM alohfink@astro.umd.edu RI Jorstad, Svetlana/H-6913-2013; XRAY, SUZAKU/A-1808-2009 OI Jorstad, Svetlana/0000-0001-9522-5453; FU NASA [NNX12AE13G, NNX11AQ03G]; NSF grant [AST-907893]; Royal Society FX The authors thank the anonymous referee for comments that improved this manuscript. We thank Phil Cowperthwaite, Javier Garcia, and Abdu Zoghbi for useful discussions throughout the duration of this work. A.M.L. and C.S.R. gratefully acknowledge NASA for support under the Astrophysical Data Analysis Program (ADAP) grant NNX12AE13G. The research at Boston University was supported by NSF grant AST-907893 and NASA grant NNX11AQ03G. The VLBA is operated by the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.. A.C.F. thanks the Royal Society for support. NR 58 TC 29 Z9 29 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 83 DI 10.1088/0004-637X/772/2/83 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700005 ER PT J AU Luo, B Brandt, WN Alexander, DM Harrison, FA Stern, D Bauer, FE Boggs, SE Christensen, FE Comastri, A Craig, WW Fabian, AC Farrah, D Fiore, F Fuerst, F Grefenstette, BW Hailey, CJ Hickox, R Madsen, KK Matt, G Ogle, P Risaliti, G Saez, C Teng, SH Walton, DJ Zhang, WW AF Luo, B. Brandt, W. N. Alexander, D. M. Harrison, F. A. Stern, D. Bauer, F. E. Boggs, S. E. Christensen, F. E. Comastri, A. Craig, W. W. Fabian, A. C. Farrah, D. Fiore, F. Fuerst, F. Grefenstette, B. W. Hailey, C. J. Hickox, R. Madsen, K. K. Matt, G. Ogle, P. Risaliti, G. Saez, C. Teng, S. H. Walton, D. J. Zhang, W. W. TI WEAK HARD X-RAY EMISSION FROM TWO BROAD ABSORPTION LINE QUASARS OBSERVED WITH NuSTAR: COMPTON-THICK ABSORPTION OR INTRINSIC X-RAY WEAKNESS? SO ASTROPHYSICAL JOURNAL LA English DT Article DE accretion, accretion disks; galaxies: active; galaxies: nuclei; quasars: absorption lines; quasars: emission lines; X-rays: general ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; SPECTRAL ENERGY-DISTRIBUTIONS; OPTICALLY SELECTED QUASARS; XMM-NEWTON SPECTROSCOPY; HUBBLE-SPACE-TELESCOPE; ACCRETION DISK WINDS; RADIO-LOUD QUASARS; SEYFERT 1 GALAXIES; 7TH DATA RELEASE AB We present Nuclear Spectroscopic Telescope Array (NuSTAR) hard X-ray observations of two X-ray weak broad absorption line (BAL) quasars, PG 1004+130 (radio loud) and PG 1700+518 (radio quiet). Many BAL quasars appear X-ray weak, probably due to absorption by the shielding gas between the nucleus and the accretion-disk wind. The two targets are among the optically brightest BAL quasars, yet they are known to be significantly X-ray weak at rest-frame 2-10 keV (16-120 times fainter than typical quasars). We would expect to obtain approximate to 400-600 hard X-ray (greater than or similar to 10 keV) photons with NuSTAR, provided that these photons are not significantly absorbed (N-H less than or similar to 10(24) cm(-2)). However, both BAL quasars are only detected in the softer NuSTAR bands (e.g., 4-20 keV) but not in its harder bands (e.g., 20-30 keV), suggesting that either the shielding gas is highly Compton-thick or the two targets are intrinsically X-ray weak. We constrain the column densities for both to be N-H approximate to 7 x 10(24) cm(-2) if the weak hard X-ray emission is caused by obscuration from the shielding gas. We discuss a few possibilities for how PG 1004+130 could have Compton-thick shielding gas without strong Fe K alpha line emission; dilution from jet-linked X-ray emission is one likely explanation. We also discuss the intrinsic X-ray weakness scenario based on a coronal-quenching model relevant to the shielding gas and disk wind of BAL quasars. Motivated by our NuSTAR results, we perform a Chandra stacking analysis with the Large Bright Quasar Survey BAL quasar sample and place statistical constraints upon the fraction of intrinsically X-ray weak BAL quasars; this fraction is likely 17%-40%. C1 [Luo, B.; Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Luo, B.; Brandt, W. N.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Alexander, D. M.; Hickox, R.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Harrison, F. A.; Fuerst, F.; Grefenstette, B. W.; Madsen, K. K.; Walton, D. J.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Stern, D.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bauer, F. E.; Saez, C.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Bauer, F. E.] Space Sci Inst, Boulder, CO 80301 USA. [Boggs, S. E.; Craig, W. W.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, F. E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Comastri, A.] INAF, Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Craig, W. W.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Fiore, F.] Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. [Hailey, C. J.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Hickox, R.] Dartmouth Coll, Dept Phys & Astron, Hanover, NH 03755 USA. [Matt, G.] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Ogle, P.] CALTECH, IPAC, Pasadena, CA 91125 USA. [Risaliti, G.] INAF, Osservatorio Astrofis Arcetri, I-50125 Florence, Italy. [Risaliti, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Teng, S. H.] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Zhang, W. W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Luo, B (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. RI Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Risaliti, Guido/0000-0002-3556-977X; Alexander, David/0000-0002-5896-6313; Fiore, Fabrizio/0000-0002-4031-4157 FU California Institute of Technology (Caltech) NuSTAR [44A-1092750]; NASA ADP Grant [NNX10AC99G]; Leverhulme trust; Science Technology and Facilities Council; Basal-CATA [PFB-06/2007]; CONICYT-Chile [FONDECYT 1101024, Anillo ACT1101, FONDECYT 3120198]; NASA [NNG08FD60C]; National Aeronautics and Space Administration FX We acknowledge support from the California Institute of Technology (Caltech) NuSTAR subcontract 44A-1092750 (B.L. and W.N.B.), NASA ADP Grant NNX10AC99G (B.L. and W.N.B.), the Leverhulme trust and the Science Technology and Facilities Council (D.M.A.), Basal-CATA Grant PFB-06/2007 and CONICYT-Chile Grants FONDECYT 1101024 and Anillo ACT1101 (F.E.B.), and CONICYT-Chile Grant FONDECYT 3120198 (C.S.). We thank M. Young for help with the planning of this project and K. Forster for help with the NuSTAR data access, and we thank M. Balokovic, K. Boydstun, T. N. Lu, B. P. Miller, Jianfeng Wu, and T. Yaqoob for helpful discussions. We thank the referee, S. C. Gallagher, for carefully reviewing the manuscript and providing helpful comments.; This work was supported under NASA contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. We thank the NuSTAR Operations, Software and Calibration teams for support with the execution and analysis of these observations. This research has made use of NuSTAR-DAS jointly developed by the ASI Science Data Center (ASDC, Italy) and Caltech (USA). NR 146 TC 24 Z9 24 U1 0 U2 12 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 153 DI 10.1088/0004-637X/772/2/153 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700075 ER PT J AU Milisavljevic, D Fesen, RA AF Milisavljevic, Dan Fesen, Robert A. TI A DETAILED KINEMATIC MAP OF CASSIOPEIA A'S OPTICAL MAIN SHELL AND OUTER HIGH-VELOCITY EJECTA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (Cassiopeia A); ISM: supernova remnants; supernovae: general ID CORE-COLLAPSE SUPERNOVAE; LARGE-MAGELLANIC-CLOUD; X-RAY; REMNANT CASSIOPEIA; 3-DIMENSIONAL STRUCTURE; PROPER MOTIONS; LIGHT ECHOES; A SUPERNOVA; MAGNETOROTATIONAL INSTABILITY; STRIPPED-ENVELOPE AB We present three-dimensional (3D) kinematic reconstructions of optically emitting material in the young Galactic supernova remnant Cassiopeia A (Cas A). These Doppler maps have the highest spectral and spatial resolutions of any previous survey of Cas A and represent the most complete catalog of its optically emitting material to date. We confirm that the bulk of Cas A's optically bright ejecta populate a torus-like geometry tilted approximately 30 degrees with respect to the plane of the sky with a -4000 to +6000 km s(-1) radial velocity asymmetry. Near-tangent viewing angle effects and an inhomogeneous surrounding circumstellar material/interstellar medium environment suggest that this geometry and velocity asymmetry may not be faithfully representative of the remnant's true 3D structure or the kinematic properties of the original explosion. The majority of the optical ejecta are arranged in several well-defined and nearly circular ring-like structures with diameters between approximately 30 '' (0.5 pc) and 2' (2 pc). These ejecta rings appear to be a common phenomenon of young core-collapse remnants and may be associated with post-explosion input of energy from plumes of radioactive Ni-56-rich ejecta that rise, expand, and compress non-radioactive material. Our optical survey encompasses Cas A's faint outlying ejecta knots and exceptionally high-velocity NE and SW streams of S-rich debris often referred to as "jets." These outer knots, which exhibit a chemical make-up suggestive of an origin deep within the progenitor star, appear to be arranged in opposing and wide-angle outflows with opening half-angles of approximate to 40 degrees. C1 [Milisavljevic, Dan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Fesen, Robert A.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu FU National Science Foundation [AST-0908237]; NASA [NAS 5-26555] FX We thank an anonymous referee for comments that improved this paper's content and presentation. D. Patnaude, R. Chevalier, J. Thorstensen and G. Wegner provided helpful discussions and comments. T. DeLaney kindly provided infrared and X-ray data in advance of publication. David Adalsteinsson provided considerable support with the DataTank software (http://www.visualdatatools.com), which was used to prepare some figures and the animations. Surface reconstruction was aided with the use of MeshLab (http://meshlab.sourceforge.net), a tool developed with the support of the 3D-CoForm project. This material is based upon work supported by the National Science Foundation under grant No. AST-0908237.; This material is also based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. NR 85 TC 22 Z9 22 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD AUG 1 PY 2013 VL 772 IS 2 AR 134 DI 10.1088/0004-637X/772/2/134 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186EL UT WOS:000322024700056 ER PT J AU Socrates, A Sironi, L AF Socrates, Aristotle Sironi, Lorenzo TI PHOTON FEEDBACK: SCREENING AND THE EDDINGTON LIMIT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE dust, extinction; galaxies: general; galaxies: starburst; ISM: jets and outflows; radiative transfer ID RADIATION PRESSURE; NONLINEAR EVOLUTION; STELLAR FEEDBACK; STAR-FORMATION; COSMIC-RAYS; GALAXIES; MASS; WINDS; DISCS; DISKS AB Bright star-forming galaxies radiate well below their Eddington limits. The value of the flux-mean opacity that mediates the radiation force onto matter is orders of magnitude smaller than the UV or optical dust opacity. On empirical grounds, it is shown that high-redshift ULIRGs radiate at two orders of magnitude below their Eddington limits, while the local starbursters M82 and Arp 220 radiate at a few percent of their Eddington limits. A model for the radiative transfer of UV and optical light in dust-rich environments is considered. Radiation pressure on dust does not greatly affect the large-scale gas dynamics of star-forming galaxies. C1 [Socrates, Aristotle] Inst Adv Study, Princeton, NJ 08540 USA. [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Socrates, A (reprint author), Inst Adv Study, Einstein Dr, Princeton, NJ 08540 USA. EM socrates@ias.edu; lsironi@cfa.harvard.edu FU John N. Bahcall Fellowship at the Institute for Advanced Study, Princeton; NASA through Einstein Postdoctoral Fellowship [PF1-120090]; Chandra X-ray Center; NASA [NAS8-03060] FX A.S. is supported by a John N. Bahcall Fellowship at the Institute for Advanced Study, Princeton. L.S. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. We gratefully thank M. Michalowski for providing the SED templates of high-redshift ULIRGs, as well as Jenny Greene and Avi Loeb for comments. We thank the referee, Eliot Quataert, for providing constructive comments. NR 27 TC 4 Z9 4 U1 1 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD AUG 1 PY 2013 VL 772 IS 2 AR L21 DI 10.1088/2041-8205/772/2/L21 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 186CR UT WOS:000322020000008 ER PT J AU Bret, A Stockem, A Fiuza, F Ruyer, C Gremillet, L Narayan, R Silva, LO AF Bret, Antoine Stockem, A. Fiuza, F. Ruyer, C. Gremillet, L. Narayan, R. Silva, L. O. TI Relativistic collisionless shocks formation in pair plasmas SO JOURNAL OF PLASMA PHYSICS LA English DT Article ID PARTICLE-ACCELERATION; INSTABILITIES; ELECTRONS; BEAM AB Collisionless shocks are ubiquitous in astrophysics and in the laboratory. Recent numerical simulations and experiments have shown how these can arise from the encounter of two collisionless plasma shells. When the shells interpenetrate, the overlapping region turns unstable, triggering the shock formation. As a first step toward a microscopic understanding of the process, we here analyze in detail the initial instability phase. On the one hand, 2D relativistic PIC simulations are performed where two unmagnetized, symmetric, and initially cold pair plasmas collide. On the other hand, the instabilities at work are analyzed, as well as the field at saturation and the seed field which gets amplified. For mildly relativistic motions and onward, Weibel modes with omega = 0 + i delta govern the linear phase. We derive an expression for the duration of the linear phase in reasonable agreement with the simulations. C1 [Bret, Antoine] Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. [Stockem, A.; Fiuza, F.; Silva, L. O.] Inst Super Tecn, GoLP Inst Plasmas & Fusao Nucl, Lab Assoc, Lisbon, Portugal. [Ruyer, C.; Gremillet, L.] CEA, DAM, DIF, F-91297 Arpajon, France. [Narayan, R.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Bret, A (reprint author), Univ Castilla La Mancha, ETSI Ind, E-13071 Ciudad Real, Spain. EM antoineclaude.bret@uclm.es RI Silva, Luis/C-3169-2009; Bret, Antoine/C-9112-2009; OI Silva, Luis/0000-0003-2906-924X; Bret, Antoine/0000-0003-2030-0046; Fiuza, Frederico/0000-0002-8502-5535; Stockem, Anne Gabriele/0000-0003-4614-8118; Narayan, Ramesh/0000-0002-1919-2730 FU Spanish Ministerio de Educacion y Ciencia [ENE2009-09276]; European Research Council [267841]; FCT (Portugal) [PTDC/FIS/111720/2009, SFRH/BD/38952/2007] FX This work was supported by projects ENE2009-09276 of the Spanish Ministerio de Educacion y Ciencia, the European Research Council (ERC-2010-AdG Grant 267841), and FCT (Portugal) grants PTDC/FIS/111720/2009 and SFRH/BD/38952/2007. Thanks are due to Lorenzo Sironi for useful discussions. NR 20 TC 1 Z9 1 U1 0 U2 13 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3778 EI 1469-7807 J9 J PLASMA PHYS JI J. Plasma Phys. PD AUG PY 2013 VL 79 BP 367 EP 370 DI 10.1017/S0022377813000354 PN 4 PG 4 WC Physics, Fluids & Plasmas SC Physics GA 189ER UT WOS:000322250600003 ER PT J AU van der Sande, MT Poorter, L Schnitzer, SA Markesteijn, L AF van der Sande, Masha T. Poorter, Lourens Schnitzer, Stefan A. Markesteijn, Lars TI Are lianas more drought-tolerant than trees? A test for the role of hydraulic architecture and other stem and leaf traits SO OECOLOGIA LA English DT Article DE Panama; Drought tolerance; Functional traits; Cavitation resistance; Hydraulic conductivity; Lianas; Saplings ID DRY FOREST CANOPY; TROPICAL FOREST; XYLEM CAVITATION; FUNCTIONAL TRAITS; LOWLAND FOREST; WOODY-PLANTS; TRADE-OFFS; GROWTH; VULNERABILITY; STRATEGIES AB Lianas are an important component of Neotropical forests, where evidence suggests that they are increasing in abundance and biomass. Lianas are especially abundant in seasonally dry tropical forests, and as such it has been hypothesized that they are better adapted to drought, or that they are at an advantage under the higher light conditions in these forests. However, the physiological and morphological characteristics that allow lianas to capitalize more on seasonal forest conditions compared to trees are poorly understood. Here, we evaluate how saplings of 21 tree and liana species from a seasonal tropical forest in Panama differ in cavitation resistance (P (50)) and maximum hydraulic conductivity (K (h)), and how saplings of 24 tree and liana species differ in four photosynthetic leaf traits (e.g., maximum assimilation and stomatal conductance) and six morphological leaf and stem traits (e.g., wood density, maximum vessel length, and specific leaf area). At the sapling stage, lianas had a lower cavitation resistance than trees, implying lower drought tolerance, and they tended to have a higher potential hydraulic conductivity. In contrast to studies focusing on adult trees and lianas, we found no clear differences in morphological and photosynthetic traits between the life forms. Possibly, lianas and trees are functionally different at later ontogenetic stages, with lianas having deeper root systems than trees, or experience their main growth advantage during wet periods, when they are less vulnerable to cavitation and can achieve high conductivity. This study shows, however, that the hydraulic characteristics and functional traits that we examined do not explain differences in liana and tree distributions in seasonal forests. C1 [van der Sande, Masha T.; Poorter, Lourens] Univ Wageningen & Res Ctr, Forest Ecol & Forest Management Grp, NL-6700 AA Wageningen, Netherlands. [Schnitzer, Stefan A.; Markesteijn, Lars] Univ Wisconsin, Dept Biol Sci, Milwaukee, WI 53201 USA. [Schnitzer, Stefan A.; Markesteijn, Lars] Smithsonian Trop Res Inst, Balboa, Panama. RP van der Sande, MT (reprint author), Univ Wageningen & Res Ctr, Forest Ecol & Forest Management Grp, POB 47, NL-6700 AA Wageningen, Netherlands. EM masha.vandersande@wur.nl OI Schnitzer, Stefan/0000-0002-2715-9455; van der Sande, Masha/0000-0002-6845-2308 FU Netherlands Organisation for Scientific Research (NWO); US National Science Foundation [NSF DEB-0613666, NSF DEB-0845071, NSF DEB-1019436]; Stichting Fonds Dr. Christine Buisman FX This research was financially supported by a Rubicon grant by the Netherlands Organisation for Scientific Research (NWO) to L. M., and by US National Science Foundation grants (NSF DEB-0613666, NSF DEB-0845071, NSF DEB-1019436) to S. A. S. M.v.d.S. was supported by a travel grant by Stichting Fonds Dr. Christine Buisman. We thank the Smitsonian Tropical Research Institute for the use of facilities, David Brassfield and Oldemar Valdez for field assistance and initial species identification, and two anonymous reviewers for valuable comments on an earlier manuscript. NR 48 TC 17 Z9 19 U1 7 U2 116 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD AUG PY 2013 VL 172 IS 4 BP 961 EP 972 DI 10.1007/s00442-012-2563-x PG 12 WC Ecology SC Environmental Sciences & Ecology GA 188GF UT WOS:000322180000005 PM 23277211 ER PT J AU Patrick, CJ Fernandez, DH AF Patrick, Christopher J. Fernandez, Dylan H. TI The beta-richness of two detritivore caddisflies affects fine organic matter export SO OECOLOGIA LA English DT Article DE Meta-ecosystem; Decomposition; Spatial distribution; Network; Subsidy ID ECOSYSTEM FUNCTION; FOREST STREAM; BIOTIC HOMOGENIZATION; POPULATION-DYNAMICS; SPECIES-DIVERSITY; PATCH DYNAMICS; BIODIVERSITY; ECOLOGY; METACOMMUNITY; DECOMPOSITION AB We used stream networks as a model system to test whether the ecosystem function, upstream production, and export of fine organic particles, an important subsidy to downstream habitats, would vary between two stream networks with identical detritivore species but different spatial distributions (i.e. high or low beta-richness). Our experiment employed artificial stream networks with two simulated tributaries. We used two species of detritivorous caddisflies, Lepidostoma sp. and Pycnopsyche guttifer, in either sympatry (low beta-richness) or allopatry (high beta-richness) in the tributaries of each network. The tributaries were given either senesced or green speckled alder (Alnus incana rugosa). In the networks with senesced leaves, particle export was more than twice as great when the detritivores were in allopatry whereas interference competition in sympatry reduced particle export. In the networks with green leaves, particle export did not significantly vary between the allopatric and sympatric distributions because the interference competition was reduced and the two species had similar feeding rates on green leaves. Humans are altering beta-richness by homogenizing or differentiating flora and fauna across habitats; however, little is known about how altering this type of biodiversity will affect ecosystem functions. Our experimental manipulation is a simple version of a change in the beta-richness of the detritivores in a more complex stream network in nature. These results may indicate that shifts in species distributions across sites may significantly affect ecosystem functions, even when no species are lost from a watershed. C1 [Patrick, Christopher J.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Patrick, Christopher J.; Fernandez, Dylan H.] Univ Notre Dame, Dept Biol Sci, Notre Dame, IN 46656 USA. [Fernandez, Dylan H.] Univ Wisconsin, Coll Nat Resources, Stevens Point, WI 54481 USA. RP Patrick, CJ (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd,POB 28, Edgewater, MD 21037 USA. EM patrickc@si.edu; Fernandez@uwsp.edu FU University of Notre Dame Environmental Research Center; Notre Dame Center for Environmental Science and Technology; NSF IGERT [0504495] FX Many thanks go to Gary Belovsky for helpful comments and critique that significantly improved the quality of this manuscript. We also thank Todd Crowl, Jennifer Tank, and Jason McLachlan for advice and guidance during the design of this experiment. This work was funded by the University of Notre Dame Environmental Research Center, Notre Dame Center for Environmental Science and Technology, and NSF IGERT grant award # 0504495. NR 65 TC 1 Z9 1 U1 2 U2 36 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD AUG PY 2013 VL 172 IS 4 BP 1105 EP 1115 DI 10.1007/s00442-012-2550-2 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 188GF UT WOS:000322180000018 PM 23247687 ER PT J AU Klimesova, J Dolezal, J St'astna, P AF Klimesova, Jitka Dolezal, Jiri St'astna, Petra TI Growth of the alpine herb Rumex alpinus over two decades: effect of climate fluctuations and local conditions SO PLANT ECOLOGY LA English DT Article DE Herb-chronology; Low Tatra Mts.; Rumex alpinus ID CASSIOPE-TETRAGONA; ALTITUDINAL CHANGES; PERENNIAL FORBS; DWARF SHRUBS; VEGETATION; TEMPERATURE; PRECIPITATION; DIVERGENCE; PHENOLOGY; SNOWBANK AB Plants in arctic and alpine habitats could potentially escape the effects of climatic fluctuations by surviving in suitable microsites. We tested this hypothesis by conducting a herb-chronological analysis of the morphological growth markers retained on the rhizomes of the clonal herb Rumex alpinus-a common plant with a broad ecological amplitude found in the alpine zone of the Low Tatra Mts., Western Carpathians, Slovakia. We asked whether aspects of plant growth were related to the climatic conditions measured at a local weather station over two approximately decade-long study periods (1977-1988 and 2001-2010) on both snowbed and non-snowbed sites. Although the latter period had average summer temperatures that were about 2 A degrees C warmer than the first, both had the same average growing season length and average total monthly precipitation. Snow accumulation and other climatic events shortened the growing seasons for the plants in the first period, thus reducing vegetative growth. On the other hand, climatic events prolonging the growing seasons supported plant growth and flowering in the snowbed site. In the second, warmer period, growing season lengths were not related to plant performance but August temperatures had a positive effect on plant growth in both the snowbed and non-snowbed sites. Our results imply that mesoclimatic factors substantially affect plant growth, although their relative importance might change with climate fluctuations altering their influence in sites of differing snow accumulation. C1 [Klimesova, Jitka; Dolezal, Jiri] Acad Sci Czech Republic, Inst Bot, Sect Plant Ecol, CS-37982 Trebon, Czech Republic. [Dolezal, Jiri] Univ South Bohemia, Fac Sci, Ceske Budejovice 37005, Czech Republic. [St'astna, Petra] Krkonose Mts Natl Pk Adm, Vrchlabi 54301, Czech Republic. RP Klimesova, J (reprint author), Smithsonian Environm Res Ctr, 647 Contees Wharf Rd, Edgewater, MD 21037 USA. EM klimesova@butbn.cas.cz; dolezal@butbn.cas.cz; pstastna@krnap.cz RI Klimesova, Jitka/A-1525-2009; Dolezal, Jiri/H-1583-2014 FU Grant agency of the Czech Republic [GA526/09/0963]; long-term research development project of Institute of Botany ASCR [RVO 67985939]; GACR [13-13368S]; University of South Bohemia [GAJU 138/2010/P] FX We dedicate the work to memory of our late colleague Leos Klimes who participated on the first sampling of Rumex alpinus. English corrections were kindly provided by Brian McMillan, invaluable comments were provided by Dennis Whigham. Study was partly supported by Grant agency of the Czech Republic GA526/09/0963 and by a long-term research development project of Institute of Botany ASCR No. RVO 67985939. JD was supported during the elaboration of this paper by GACR 13-13368S, and the University of South Bohemia (GAJU 138/2010/P). NR 48 TC 0 Z9 0 U1 1 U2 40 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1385-0237 J9 PLANT ECOL JI Plant Ecol. PD AUG PY 2013 VL 214 IS 8 BP 1071 EP 1084 DI 10.1007/s11258-013-0232-8 PG 14 WC Plant Sciences; Ecology; Forestry SC Plant Sciences; Environmental Sciences & Ecology; Forestry GA 186HA UT WOS:000322031500009 ER PT J AU Mozdzer, TJ Megonigal, JP AF Mozdzer, Thomas J. Megonigal, J. Patrick TI Increased Methane Emissions by an Introduced Phragmites australis Lineage under Global Change SO WETLANDS LA English DT Article DE Invasive; Conspecific; Congener; Phragmites; Methane; Greenhouse Gas; Elevated carbon dioxide; Nitrogen; Wetland ID ELEVATED CARBON-DIOXIDE; SPARTINA-ALTERNIFLORA; GREENHOUSE GASES; ATMOSPHERIC CO2; TIDAL WETLANDS; NORTH-AMERICA; COMMON REED; PLANT; SOIL; INVASION AB North American wetlands have been invaded by an introduced lineage of the common reed, Phragmites australis. Native lineages occur in North America, but many populations have been extirpated by the introduced conspecific lineage. Little is known about how subtle changes in plant lineage may affect methane (CH4) emissions. Native and introduced Phragmites were grown under current and predicted future levels of atmospheric CO2 and nitrogen(N) pollution in order to understand how CH4 emissions may vary between conspecific lineages. We found introduced Phragmites emitted more CH4 than native Phragmites, and that CH4 emissions increased significantly in both with CO2+N treatment. There was no significant difference in CH4 production potentials, but CH4 oxidation potentials were higher in soils from the introduced lineage. Intraspecific plant responses to resource availability changed CH4 emissions, with plant density, root mass, and leaf area being significantly positively correlated with higher emissions. The absence of CO2-only or N-only effects highlights a limitation on the generalization that CH4 emissions are proportional to plant productivity. Our data suggest that intraspecific changes in plant community composition have important implications for greenhouse emissions. Furthermore, global change-enhanced invasion by introduced Phragmites may increase CH4 emissions unless these factors cause a compensatory increase in carbon sequestration. C1 [Mozdzer, Thomas J.; Megonigal, J. Patrick] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Mozdzer, Thomas J.] Bryn Mawr Coll, Dept Biol, Bryn Mawr, PA 19010 USA. RP Mozdzer, TJ (reprint author), Bryn Mawr Coll, Dept Biol, 101 N Merion Ave, Bryn Mawr, PA 19010 USA. EM tmozdzer@brynmawr.edu RI Mozdzer, Thomas/A-3599-2014 OI Mozdzer, Thomas/0000-0002-1053-0967 FU Smithsonian Institution fellowship FX We thank D. Gonzalez, N. Mudd, J. Duls, and P. Shands for their assistance in executing the experiment, and L.A. Meyerson for providing the propagule material. Funding was provided from a Smithsonian Institution fellowship to T.J. Mozdzer NR 37 TC 17 Z9 19 U1 1 U2 74 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0277-5212 J9 WETLANDS JI Wetlands PD AUG PY 2013 VL 33 IS 4 BP 609 EP 615 DI 10.1007/s13157-013-0417-x PG 7 WC Ecology; Environmental Sciences SC Environmental Sciences & Ecology GA 186DT UT WOS:000322022900004 ER PT J AU Thompson, AR Adam, TC Hultgren, KM Thacker, CE AF Thompson, Andrew R. Adam, Thomas C. Hultgren, Kristin M. Thacker, Christine E. TI Ecology and Evolution Affect Network Structure in an Intimate Marine Mutualism SO AMERICAN NATURALIST LA English DT Article DE mutualism; network topology; specialization; shrimp goby; forbidden link ID CRYPTOCENTRUS-STEINITZI PISCES; ALPHEUS-PURPURILENTICULARIS CRUSTACEA; SHRIMP PARTNER SPECIFICITY; COEVOLUTIONARY NETWORKS; TACTILE COMMUNICATION; DEMOGRAPHICALLY OPEN; COMMUNITY STRUCTURE; NESTED STRUCTURE; FOOD WEBS; RED-SEA AB Elucidating patterns and causes of interaction among mutualistic species is a major focus of ecology, and recent meta-analyses of terrestrial networks show that network-level reciprocal specialization tends to be higher in intimate mutualisms than in nonintimate mutualisms. It is largely unknown, however, whether this pattern holds for and what factors affect specialization in marine mutualisms. Here we present the first analysis of network specialization (H-2') for marine mutualistic networks. Specialization among eight Indo-Pacific networks of obligate mutualistic gobies and shrimps was indistinguishable from that among comparably intimate terrestrial mutualisms (ants-myrmecophytes) and higher than that among nonintimate ones (seed dispersers). Specialization was affected by variability in habitat use for both gobies and shrimps and by phylogenetic history for shrimps. Habitat use was phylogenetically conserved among shrimp, and thus effects of shrimp phylogeny on partner choice were mediated in part by habitat. By contrast, habitat use and pairing patterns in gobies were not related to phylogenetic history. This asymmetry appears to result from evolutionary constraints on partner use in shrimps and convergence among distantly related gobies to utilize burrows provided by multiple shrimp species. Results indicate that the evolution of mutualism is affected by life-history characteristics that transcend environments and that different factors constrain interactions in disparate ecosystems. C1 [Thompson, Andrew R.] Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Fisheries Resources Div, Southwest Fisheries Sci Ctr, La Jolla, CA 92037 USA. [Thompson, Andrew R.; Thacker, Christine E.] Nat Hist Museum Angeles Cty, Los Angeles, CA 90007 USA. [Adam, Thomas C.] Univ Calif Santa Barbara, Coastal Res Ctr, Inst Marine Sci, Santa Barbara, CA 93106 USA. [Hultgren, Kristin M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. [Hultgren, Kristin M.] Seattle Univ, Dept Biol, Seattle, WA 98122 USA. RP Thompson, AR (reprint author), Natl Ocean & Atmospher Adm, Natl Marine Fisheries Serv, Fisheries Resources Div, Southwest Fisheries Sci Ctr, La Jolla, CA 92037 USA. EM andrew.thompson@noaa.gov FU W. M. Keck foundation; R. M. Parsons foundation; National Science Foundation Moorea Coral Reef Long Term Ecological Research project [OCE 04-17412] FX We are grateful to J. P. Chen, D. Geiger, M. Jeng, I. Karplus, J. S. White, and B. Wolcott and to the staffs of the Mahonia Na Dari Research Institute of Kimbe Bay, Papua New Guinea, and the UCB (University of California, Berkeley) Gump Research Station in Moorea, French Polynesia, for their support and assistance with fieldwork, collections, and/or analysis. Comments by N. Bowlin, R. Nisbet, A. Rossberg, S. Sandin, W. Watson, and two anonymous reviewers improved the manuscript. This work was supported by grants from the W. M. Keck and R. M. Parsons foundations in support of the program in Molecular Systematics and Evolution at the Natural History Museum of Los Angeles County and the National Science Foundation Moorea Coral Reef Long Term Ecological Research project (OCE 04-17412). This is contribution 197 of the UCB Richard B. Gump South Pacific Research Station. NR 84 TC 8 Z9 8 U1 6 U2 55 PU UNIV CHICAGO PRESS PI CHICAGO PA 1427 E 60TH ST, CHICAGO, IL 60637-2954 USA SN 0003-0147 EI 1537-5323 J9 AM NAT JI Am. Nat. PD AUG PY 2013 VL 182 IS 2 BP E58 EP E72 DI 10.1086/670803 PG 15 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 181XI UT WOS:000321703400003 PM 23852363 ER PT J AU Regan, TJ Taylor, BL Thompson, GG Cochrane, JF Ralls, K Runge, MC Merrick, R AF Regan, Tracey J. Taylor, Barbara L. Thompson, Grant G. Cochrane, Jean Fitts Ralls, Katherine Runge, Michael C. Merrick, Richard TI Testing Decision Rules for Categorizing Species' Extinction Risk to Help Develop Quantitative Listing Criteria for the US Endangered Species Act SO CONSERVATION BIOLOGY LA English DT Article DE Bayesian analysis; loss functions; performance testing; population viability analysis ID UNCERTAINTY; ADVICE; MODELS AB Lack of guidance for interpreting the definitions of endangered and threatened in the U.S. Endangered Species Act (ESA) has resulted in case-by-case decision making leaving the process vulnerable to being considered arbitrary or capricious. Adopting quantitative decision rules would remedy this but requires the agency to specify the relative urgency concerning extinction events over time, cutoff risk values corresponding to different levels of protection, and the importance given to different types of listing errors. We tested the performance of 3 sets of decision rules that use alternative functions for weighting the relative urgency of future extinction events: a threshold rule set, which uses a decision rule of x% probability of extinction over y years; a concave rule set, where the relative importance of future extinction events declines exponentially over time; and a shoulder rule set that uses a sigmoid shape function, where relative importance declines slowly at first and then more rapidly. We obtained decision cutoffs by interviewing several biologists and then emulated the listing process with simulations that covered a range of extinction risks typical of ESA listing decisions. We evaluated performance of the decision rules under different data quantities and qualities on the basis of the relative importance of misclassification errors. Although there was little difference between the performance of alternative decision rules for correct listings, the distribution of misclassifications differed depending on the function used. Misclassifications for the threshold and concave listing criteria resulted in more overprotection errors, particularly as uncertainty increased, whereas errors for the shoulder listing criteria were more symmetrical. We developed and tested the framework for quantitative decision rules for listing species under the U.S. ESA. If policy values can be agreed on, use of this framework would improve the implementation of the ESA by increasing transparency and consistency. C1 [Regan, Tracey J.] Univ Melbourne, Sch Bot, Parkville, Vic 3010, Australia. [Regan, Tracey J.; Taylor, Barbara L.] Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, La Jolla, CA 92037 USA. [Thompson, Grant G.] NOAA, Resource Ecol & Fisheries Management Div, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Cochrane, Jean Fitts] US Fish & Wildlife Serv, Endangered Species Program, Arlington, VA 22203 USA. [Ralls, Katherine] Smithsonian Inst, Natl Zool Pk, Smithsonian Conservat Biol Inst, Washington, DC 20008 USA. [Runge, Michael C.] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Merrick, Richard] Natl Marine Fisheries Serv, Off Assistant Administrator, Silver Spring, MD 20910 USA. RP Regan, TJ (reprint author), Univ Melbourne, Sch Bot, Parkville, Vic 3010, Australia. EM tregan@unimelb.edu.au RI Runge, Michael/E-7331-2011 OI Runge, Michael/0000-0002-8081-536X FU National Marine Fisheries Service; U.S. Fish and Wildlife Service; National Research Council; Australian Research Council Centre of Excellence for Environmental Decisions FX T.J.R. was jointly funded by the National Marine Fisheries Service and the U.S. Fish and Wildlife Service through a fellowship with the National Research Council and the Australian Research Council Centre of Excellence for Environmental Decisions. We thank L. Maguire, M. Nammack, T. Ragen, and S. Rumsey for expert advice; and A. Read, P. Boveng, P. Wade, and M. Burgman for their useful comments. We honour the passing of Dr. Dan Goodman who provided software and intellectual stimulation for this project. Dan devoted much of his career to integrating decision theory into conservation biology and his mentoring was very important to several authors of this work. NR 34 TC 8 Z9 8 U1 0 U2 46 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0888-8892 J9 CONSERV BIOL JI Conserv. Biol. PD AUG PY 2013 VL 27 IS 4 BP 821 EP 831 DI 10.1111/cobi.12055 PG 11 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 185PB UT WOS:000321980800019 PM 23646933 ER PT J AU Sanchez, AG Kazin, EA Beutler, F Chuang, CH Cuesta, AJ Eisenstein, DJ Manera, M Montesano, F Nichol, RC Padmanabhan, N Percival, W Prada, F Ross, AJ Schlegel, DJ Tinker, J Tojeiro, R Weinberg, DH Xu, XY Brinkmann, J Brownstein, JR Schneider, DP Thomas, D AF Sanchez, Ariel G. Kazin, Eyal A. Beutler, Florian Chuang, Chia-Hsun Cuesta, Antonio J. Eisenstein, Daniel J. Manera, Marc Montesano, Francesco Nichol, Robert C. Padmanabhan, Nikhil Percival, Will Prada, Francisco Ross, Ashley J. Schlegel, David J. Tinker, Jeremy Tojeiro, Rita Weinberg, David H. Xu, Xiaoying Brinkmann, J. Brownstein, Joel R. Schneider, Donald P. Thomas, Daniel TI The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological constraints from the full shape of the clustering wedges SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE cosmological parameters; large-scale structure of Universe ID DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; REDSHIFT-SPACE DISTORTIONS; PROBE WMAP OBSERVATIONS; MICROWAVE BACKGROUND ANISOTROPIES; HALO OCCUPATION DISTRIBUTION; 2-POINT CORRELATION-FUNCTION; SCALE POWER SPECTRUM; ACOUSTIC-OSCILLATIONS; DARK ENERGY AB We explore the cosmological implications of the clustering wedges, xi(perpendicular to)(s) and xi()(s), of the CMASS Data Release 9 sample of the Sloan Digital Sky Survey III (SDSS-III) Baryon Oscillation Spectroscopic Survey. These clustering wedges are defined by averaging the full two-dimensional correlation function, xi(mu, s), over the ranges 0 < mu < 0.5 and 0.5 < mu < 1, respectively. These measurements allow us to constrain the parameter combinations D-A(z)/r(s)(z(d)) = 9.03 +/- 0.21 and cz/(r(s)(z(d))H(z)) = 12.14 +/- 0.43 at the mean redshift of the sample, z = 0.57. We combine the information from the clustering wedges with recent measurements of cosmic microwave background (CMB), baryon acoustic oscillations and Type Ia supernovae to obtain constraints on the cosmological parameters of the standard Lambda cold dark matter (Lambda CDM) model and a number of potential extensions. The information encoded in the clustering wedges is most useful when the dark energy equation of state is allowed to deviate from its standard Lambda CDM value. The combination of all data sets shows no evidence of a deviation from a constant dark energy equation of state, in which case we find w(DE) = -1.013 +/- 0.064, in complete agreement with a cosmological constant. We explore potential deviations from general relativity (GR) by constraining the growth rate f(z) = d ln D(a)/d ln a, in which case the combination of the CMASS clustering wedges with CMB data implies f(z = 0.57) = 0.719(-0.096)(+0.092), in accordance with the predictions of GR. Our results clearly illustrate the additional constraining power of anisotropic clustering measurements with respect to that of angle-averaged quantities. C1 [Sanchez, Ariel G.; Montesano, Francesco] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Kazin, Eyal A.] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Kazin, Eyal A.] ARC Ctr Excellence All Sky Astrophys CAASTRO, Hawthorn, Vic 3122, Australia. [Beutler, Florian; Schlegel, David J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Chuang, Chia-Hsun; Prada, Francisco] Univ Autonoma Madrid, UAM CSIC, Inst Fis Teor, E-28049 Madrid, Spain. [Cuesta, Antonio J.; Padmanabhan, Nikhil] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Eisenstein, Daniel J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Manera, Marc; Nichol, Robert C.; Percival, Will; Ross, Ashley J.; Tojeiro, Rita; Thomas, Daniel] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Prada, Francisco] Campus Int Excellence UAM CSIC, E-28049 Madrid, Spain. [Prada, Francisco] Inst Astrofis Andalucia CSIC, E-18080 Granada, Spain. [Tinker, Jeremy] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Weinberg, David H.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Weinberg, David H.] Ohio State Univ, CCAPP, Columbus, OH 43210 USA. [Xu, Xiaoying] Carnegie Mellon Univ, Dept Phys, Pittsburgh, PA 15213 USA. [Brinkmann, J.] Apache Point Observ, Sunspot, NM 88349 USA. [Brownstein, Joel R.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Schneider, Donald P.] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. RP Sanchez, AG (reprint author), Max Planck Inst Extraterr Phys, Postfach 1312,Giessenbachstr, D-85741 Garching, Germany. EM arielsan@mpe.mpg.de OI Beutler, Florian/0000-0003-0467-5438; Cuesta Vazquez, Antonio Jose/0000-0002-4153-9470 FU Transregional Collaborative Research Centre TR33 'The Dark Universe' of the German Research Foundation (DFG); Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO) [CE110001020]; ICG; SEPNet; University of Portsmouth; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; University of Arizona; Brazilian Participation Group; Brookhaven National Laboratory; University of Cambridge; Carnegie Mellon University; University of Florida; French Participation Group; German Participation Group; Harvard University; Instituto de Astrofisica de Canarias; Michigan State/Notre Dame/JINA Participation Group; Johns Hopkins University; Lawrence Berkeley National Laboratory; Max Planck Institute for Astrophysics; Max Planck Institute for Extraterrestrial Physics; New Mexico State University; New York University; Ohio State University; Pennsylvania State University; Princeton University; Spanish Participation Group; University of Tokyo; University of Utah; Vanderbilt University; University of Virginia; University of Washington; Yale University; NASA Office of Space Science FX AGS acknowledges support by the Transregional Collaborative Research Centre TR33 'The Dark Universe' of the German Research Foundation (DFG). EK is supported by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAAS-TRO), through project number CE110001020.; Numerical computations for the PTHALOS mocks were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet and the University of Portsmouth.; Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation and the U.S. Department of Energy.; SDSS-III is managed by the Astrophysical Research Consortium for the Participating Institutions of the SDSS-III Collaboration including the University of Arizona, the Brazilian Participation Group, Brookhaven National Laboratory, University of Cambridge, Carnegie Mellon University, University of Florida, the French Participation Group, the German Participation Group, Harvard University, the Instituto de Astrofisica de Canarias, the Michigan State/Notre Dame/JINA Participation Group, Johns Hopkins University, Lawrence Berkeley National Laboratory, Max Planck Institute for Astrophysics, Max Planck Institute for Extraterrestrial Physics, New Mexico State University, New York University, Ohio State University, Pennsylvania State University, University of Portsmouth, Princeton University, the Spanish Participation Group, University of Tokyo, University of Utah, Vanderbilt University, University of Virginia, University of Washington and Yale University.; We acknowledge the use of the Legacy Archive for Microwave Background Data Analysis (LAMBDA). Support for LAMBDA is provided by the NASA Office of Space Science. NR 123 TC 48 Z9 48 U1 0 U2 5 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 EI 1365-2966 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD AUG PY 2013 VL 433 IS 2 BP 1202 EP 1222 DI 10.1093/mnras/stt799 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178QK UT WOS:000321462300023 ER PT J AU Otto, E Tarasov, M Grimes, PK Chekushkin, A Kuzmin, LS Yassin, G AF Otto, Ernst Tarasov, Mikhail Grimes, Paul K. Chekushkin, Artem Kuzmin, Leonid S. Yassin, Ghassan TI Optical response of a titanium-based cold-electron bolometer SO SUPERCONDUCTOR SCIENCE & TECHNOLOGY LA English DT Article ID TUNNEL-JUNCTIONS AB We present experimental results on the testing of cold-electron bolometer (CEB) detectors comprised of a thin Ti film absorber and two SIN junctions integrated with a planar antenna. The CEB performance was tested in a He-3 sorption cryostat HELIOX-AC-V at bath temperatures of 280-305 mK. The optical response was measured using the hot/cold load method by flipping a Cu reflector opposite a blackbody surface inside a 3 K shield and using a thermal source with variable temperature. In the first experiment, the detector chip was mounted in an optical sample-holder whose aperture was switched towards or away from a blackbody source changing the incident radiation temperature from 3 K to 270 mK. As a result, we measured the optical response to a 3 K/270 mK radiation temperature change. The measured voltage response value for the detector integrated in a double-dipole antenna was Delta V-out = 120 mu V. This corresponds to a noise equivalent power of NEP = V-n/(dV/dP) = 3.5 x 10(-17) W Hz(-1/2), where dV/dP is the voltage to power response obtained from the incoming power estimation based on the Planck formula. C1 [Otto, Ernst; Grimes, Paul K.; Yassin, Ghassan] Univ Oxford, Dept Phys, Oxford, England. [Otto, Ernst; Tarasov, Mikhail; Chekushkin, Artem; Kuzmin, Leonid S.] Chalmers, S-41296 Gothenburg, Sweden. [Tarasov, Mikhail; Chekushkin, Artem] Russian Acad Sci, Kotelnikov Inst Radio Engn & Elect, Moscow, Russia. [Grimes, Paul K.] Smithsonian Astrophys Observ, Cambridge, MA USA. RP Otto, E (reprint author), Univ Oxford, Dept Phys, Oxford, England. EM otto.mc2@gmail.com RI Tarasov, Mikhail/B-2221-2014; Kuzmin, Leonid/M-5153-2016 OI Tarasov, Mikhail/0000-0002-8330-9163; FU New College, Oxford; Physics Department of Oxford University; Swedish Institute; Swedish Vetenskapsradet; Russian Ministry of Sciences and Education [11.G34.31.0029] FX This work was supported in part by a Wykeham Scholarship from New College, Oxford, the Physics Department of Oxford University, the Swedish Institute, the Swedish Vetenskapsradet and the Russian Ministry of Sciences and Education under grant No. 11.G34.31.0029. NR 12 TC 3 Z9 3 U1 0 U2 15 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0953-2048 J9 SUPERCOND SCI TECH JI Supercond. Sci. Technol. PD AUG PY 2013 VL 26 IS 8 AR 085020 DI 10.1088/0953-2048/26/8/085020 PG 5 WC Physics, Applied; Physics, Condensed Matter SC Physics GA 181ZL UT WOS:000321709400026 ER PT J AU Liu, HP Hershler, R Lang, B Davies, J AF Liu, Hsiu-Ping Hershler, Robert Lang, Brian Davies, Justin TI Molecular evidence for cryptic species in a narrowly endemic western North American springsnail (Pyrgulopsis gilae) SO CONSERVATION GENETICS LA English DT Article DE Phylogeography; Gastropoda; Springs; Conservation; Cryptic species ID NYMPHOPHILINE GASTROPODS; HYDROBIIDAE; BASIN AB Pyrgulopsis gilae is a small springsnail that is narrowly distributed along the forks of the upper Gila River and currently being managed as a threatened and sensitive species by the State of New Mexico and United States Forest Service, respectively. A previous phylogeographic study of this species based on mitochondrial COI sequences delineated substantial divergence between several populations along the lower and upper reaches of the East Fork Gila River. The present study surveyed COI variation among a larger number of populations across the entire geographic range of P. gilae. Three haplotype groupings were delineated that were congruently resolved as clades by a Bayesian analysis. One of the clades was composed of populations along the lower East Fork and mainstem Gila River and corresponds to P. gilae as originally circumscribed. The other two clades were composed of populations along the Middle Fork and upper East Fork Gila River that were recently referred to P. gilae. These three geographically isolated clades do not share any haplotypes, have significant F-ST values, and are differentiated from each other by 3.9-6.3 % sequence divergence. Based on this evidence we suggest that the clades represent distinct species and should be managed as separate conservation units pending taxonomic revision of P. gilae. This study provides additional evidence that geographically disjunct subunits of Pyrgulopsis species often represent distinct monophyletic lineages that may warrant formal taxonomic recognition, and thus underscores the importance of fine-scale conservation genetics studies of these imperiled organisms. C1 [Liu, Hsiu-Ping; Davies, Justin] Metropolitan State Univ Denver, Dept Biol, Denver, CO 80217 USA. [Hershler, Robert] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. [Lang, Brian] New Mexico Dept Game & Fish, Santa Fe, NM 87507 USA. RP Hershler, R (reprint author), Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20013 USA. EM hershlerr@si.edu FU New Mexico Department of Game and Fish [10-516-0000-00010]; United States Fish and Wildlife Service [E-54] FX We thank Marilyn Myers (USFWS) for providing specimens. This project was supported, in part, by an award (to RH) from the New Mexico Department of Game and Fish (Contract #10-516-0000-00010) and Section funding (Grant E-54) from the United States Fish and Wildlife Service. NR 32 TC 3 Z9 3 U1 1 U2 10 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 1566-0621 J9 CONSERV GENET JI Conserv. Genet. PD AUG PY 2013 VL 14 IS 4 BP 917 EP 923 DI 10.1007/s10592-013-0483-x PG 7 WC Biodiversity Conservation; Genetics & Heredity SC Biodiversity & Conservation; Genetics & Heredity GA 176CD UT WOS:000321279900015 ER PT J AU Young, CM Emson, RH Rice, ME Tyler, PA AF Young, Craig M. Emson, Roland H. Rice, Mary E. Tyler, Paul A. TI A paradoxical mismatch of fecundity and recruitment in deep-sea opportunists: Cocculinid and pseudococculinid limpets colonizing vascular plant remains on the Bahamian Slope SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Deep sea; Reproduction; Gastropoda; Limpets; Recruitment; Bathyal ID WOOD-BORING BIVALVES; HYDROTHERMAL VENTS; NORTHEAST PACIFIC; RAPID GROWTH; LARVAL LIFE; DEVELOPMENTAL ARREST; XYLOPHAGA-ATLANTICA; REPRODUCTION; GASTROPODA; OCEAN AB Between 1992 and 1994, palm fronds and bundles of fibrous material (rolled door mats of Chinese dragon grass) were deployed by submersible every 3 months at 520 m depth in the Tongue of the Ocean, Bahamas. Substrata were recovered after 3-month and 6-month exposure periods and searched intensively for invertebrate colonists. Recruitment surfaces were colonized during every exposure period by three species of cocculiniform limpets, Cocculina rathbuni, Cocculina emsoni, and Notocrater youngi. At least two species appeared in each season, but the relative numbers varied in a way that may indicate seasonal differences in reproduction. Gonad development could be observed through the transparent shell of C. rathbuni, which attained sexual maturity in less than 3 months and had a maximum instantaneous fecundity of 40 eggs. Growth rates (0.025-0.044 mm/day) were high when scaled to adult body size. We used current-meter data from the deployment site to calculate the fluxes of larvae that would be required to produce the measured levels of recruitment. Observed recruitment would require larval densities of hundreds of thousands to millions of larvae per km(3). Nevertheless, it is remarkable that these snails are able to succeed with an opportunistic strategy given their low fecundity and lecithotrophic development. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Young, Craig M.] Univ Oregon, Oregon Inst Marine Biol, Charleston, OR 97420 USA. [Emson, Roland H.] Kings Coll London, Dept Biosci, London WC2R 2LS, England. [Rice, Mary E.] Smithsonian Marine Stn Ft Pierce, Ft Pierce, FL USA. [Tyler, Paul A.] Univ Southampton, Natl Oceanog Ctr, Southampton, Hants, England. RP Young, CM (reprint author), Univ Oregon, Oregon Inst Marine Biol, POB 5389, Charleston, OR 97420 USA. EM cmyoung@uoregon.edu FU NSF [OCE-9116560, OCE-0527139, OCE-9633784] FX This work was supported by NSF grants OCE-9116560, OCE-0527139, and OCE-9633784. We thank the submersible pilots of the Johnson-Sea-Link submersibles and the ship captains of R.V. Seward Johnson and R.V. Edwin Link for years of outstanding logistical support, and an army of students, postdocs and colleagues who helped sort tiny animals from recruitment collectors. Jerry Harasewych kindly provided the scanning electron micrographs in Fig. 1 as well as useful comments on the manuscript. This is contribution Number 904 from the Smithsonian Marine Laboratory at Ft. Pierce. NR 56 TC 5 Z9 5 U1 0 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD AUG PY 2013 VL 92 SI SI BP 36 EP 45 DI 10.1016/j.dsr2.2013.01.027 PG 10 WC Oceanography SC Oceanography GA 174SZ UT WOS:000321177000005 ER PT J AU Pawson, DL Pawson, DJ AF Pawson, David L. Pawson, Doris J. TI Bathyal sea urchins of the Bahamas, with notes on covering behavior in deep sea echinoids (Echinodermata: Echinoidea) SO DEEP-SEA RESEARCH PART II-TOPICAL STUDIES IN OCEANOGRAPHY LA English DT Article DE Echinodermata; Echinoidea; Bathyal; Covering; Bahamas; Caribbean ID STRONGYLOCENTROTUS-DROEBACHIENSIS; PARACENTROTUS-LIVIDUS; LIGHT; ADHESION; SUNLIGHT; LAMARCK AB In a survey of the bathyal echinoderms of the Bahama Islands region using manned submersibles, approximately 200 species of echinoderms were encountered and documented; 33 species were echinoids, most of them widespread in the general Caribbean area. Three species were found to exhibit covering behavior, the piling of debris on the upper surface of the body. Active covering is common in at least 20 species of shallow-water echinoids, but it has been reliably documented previously only once in deep-sea habitats. Images of covered deep-sea species, and other species of related interest, are provided. Some of the reasons adduced in the past for covering in shallow-water species, such as reduction of incident light intensity, physical camouflage, ballast in turbulent water, protection from desiccation, presumably do not apply in bathyal species. The main reasons for covering in deep, dark, environments are as yet unknown. Some covering behavior in the deep sea may be related to protection of the genital pores, ocular plates, or madreporite. Covering in some deep-sea species may also be merely a tactile reflex action, as some authors have suggested for shallow-water species. Published by Elsevier Ltd. C1 [Pawson, David L.; Pawson, Doris J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Pawson, DL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. EM pawsond@si.edu FU National Museum of Natural History's Small Grant Program; Smithsonian Regents' Fellowship; Smithsonian Marine Station at Fort Pierce; NMNH's Small Grants program; Harbor Branch Oceanographic Institution, Inc. FX DLP is most grateful to John E. Miller, Gordon Hendler, and Porter M. Kier, treasured colleagues and lifelong friends, for the wonderful experience of field work in many parts of Florida and the Caribbean, especially the many dives in the Johnson-Sea-Link submersibles. Partial support for this research was provided by a Smithsonian Regents' Fellowship, the Smithsonian Marine Station at Fort Pierce, the NMNH's Small Grants program, and by Harbor Branch Oceanographic Institution, Inc.; In June 2011, and again in August 2012, we made a total of six dives at Curacao, in the Curasub, based at Substation Curacao, to depths of approximately 305 m. These dives were part of the Smithsonian Institution's Deep Reef Observation Project, organized and led by Dr. Carole Baldwin (NMNH). We thank Dr. Baldwin, and Mr. Adriaan "Dutch" Shrier, owner of Substation Curacao, for enabling our participation in this project. We also thank the National Museum of Natural History's Small Grant Program for financial support, and Cristina Castillo for valuable assistance. NR 58 TC 17 Z9 17 U1 2 U2 18 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0967-0645 J9 DEEP-SEA RES PT II JI Deep-Sea Res. Part II-Top. Stud. Oceanogr. PD AUG PY 2013 VL 92 SI SI BP 207 EP 213 DI 10.1016/j.dsr2.2013.01.023 PG 7 WC Oceanography SC Oceanography GA 174SZ UT WOS:000321177000024 ER PT J AU Renfrew, RB Kim, D Perlut, N Smith, J Fox, J Marra, PP AF Renfrew, Rosalind B. Kim, Daniel Perlut, Noah Smith, Joseph Fox, James Marra, Peter P. TI Phenological matching across hemispheres in a long-distance migratory bird SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Bobolink; Dolichonyx oryzivorus; geolocators; migration phenology; migratory connectivity; Normalized Difference Vegetation Index ID WARBLER WILSONIA-PUSILLA; SWALLOW HIRUNDO-RUSTICA; GOOSE BRANTA-LEUCOPSIS; WEST-AFRICAN RAINFALL; EAGLE AQUILA-POMARINA; SPRING ARRIVAL DATE; NEOTROPICAL MIGRANT; DOLICHONYX-ORYZIVORUS; ECOLOGICAL CONDITIONS; SOUTH-AMERICA AB Aim In the Northern Hemisphere, bird migration from the tropic to the temperate zone in spring is thought to proceed at a rate determined in large part by local phenology. In contrast, little is understood about where birds go or the factors that determine why they move or where they stop during the post-breeding period. Location Study sites were in Oregon, Nebraska and Vermont, and location data we collected extend south to Argentina. Methods We deployed light-level geolocators on individual Bobolinks from three populations across the breeding range and compare their southbound movement phenology to austral greening as indicated by the Normalized Difference Vegetation Index. Results Bobolinks from all breeding populations synchronously arrived and remained for up to several weeks in two sequential, small non-breeding areas that were separated by thousands of kilometres, before staging for pre-alternate moult. Similar to the migration patterns of birds to northern breeding areas, movements into the Southern Hemisphere corresponded to increasing primary productivity. Main conclusions Our findings suggest that the Bobolink's southbound migration is broadly constrained by resource availability, and its non-breeding distribution has been shaped by the seasonal phenology of grasslands in both time and space. This is the first documentation of individual birds from across a continental breeding range exhibiting phenological matching during their post-breeding southward migration. Known conservation threats overlap temporally and spatially with large concentrations of Bobolinks, and should be closely examined. We emphasize the need to consider how individuals move and interact with their environment throughout their annual cycle and over hemispheric scales. C1 [Renfrew, Rosalind B.] Vermont Ctr Ecostudies, Norwich, VT 05055 USA. [Kim, Daniel] Platte River Whooping Crane Trust, Wood River, NE 68883 USA. [Perlut, Noah] Univ New England, Dept Environm Studies, Biddeford, ME 04005 USA. [Smith, Joseph] Nature Conservancy, New Jersey Chapter, Delmont, NJ 08314 USA. [Fox, James] British Antarctic Survey, Nat Environm Res Council, Cambridge CB3 0ET, England. [Marra, Peter P.] Smithsonian Conservat Biol Inst, Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. RP Renfrew, RB (reprint author), Vermont Ctr Ecostudies, POB 420, Norwich, VT 05055 USA. EM rrenfrew@vtecostudies.org FU Charles Blake Fund of the Nuttall Ornithological Club FX This project was made possible by the generous friends of the Vermont Center for Ecostudies. We gratefully acknowledge the Charles Blake Fund of the Nuttall Ornithological Club and Terry Precision Cycling for additional, critical support. In-kind support was provided by the Platte River Whooping Crane Maintenance Trust, Portland State University, the Smithsonian Migratory Bird Center, the University of New England, the University of Vermont and the Galipeau family. Thanks to Joseph Smith, who generously contributed time and expertise to compile NDVI data. Thanks to Jim Dastyck and Tim Bodeen of the Malheur National Wildlife Refuge for access and logistical support. We thank Shelburne Farms for access to their land. We thank the many dedicated field biologists who assisted with data collection: Nathan Banet, Lindsay Bauman, Dominique Bondi, Kristin Cattrano, Tina Centofante, Chris Chutter, Julie Coffey, Hannah Davies, Katie Dunbar, Lindsay Ferrotte, Ryan Fox, Becca Gordon, Tom Lawrence, Chris Mulvey, Michael Murphy, Louis Ramirez, Luke Redmond, Jessica Rempel, Barb Roscoe, Travis Rusch, Joel Thielen, Dacia Wiitala and Heather Wills. NR 81 TC 20 Z9 20 U1 6 U2 94 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 EI 1472-4642 J9 DIVERS DISTRIB JI Divers. Distrib. PD AUG PY 2013 VL 19 IS 8 BP 1008 EP 1019 DI 10.1111/ddi.12080 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 178JV UT WOS:000321444900013 ER PT J AU Prado-Oviedo, NA Malloy, EJ Deng, XY Brown, JL AF Prado-Oviedo, Natalia A. Malloy, Elizabeth J. Deng, Xinyi Brown, Janine L. TI Hyperprolactinemia is not associated with hyperestrogenism in noncycling African elephants (Loxodonta africana) SO GENERAL AND COMPARATIVE ENDOCRINOLOGY LA English DT Article DE Hyperestrogenism; Ovarian cyclicity; Estrogen; Prolactin; Pituitary; Progestagens ID RAT PITUITARY TISSUES; ASIAN ELEPHANT; PROLACTIN SECRETION; LUTEINIZING-HORMONE; CYCLICITY STATUS; SERUM PROLACTIN; MESSENGER-RNA; NORTH-AMERICA; ESTROUS-CYCLE; TUMOR CELLS AB African elephants in US zoos are not reproducing at replacement levels. This is in part due to physiological problems, one of which is abnormal ovarian cyclicity that has been linked to increased prolactin secretion (hyperprolactinemia). A relationship between increased estrogen production (hyperestrogenism) and hyperprolactinemia has been found in other species. Therefore, the objective of this study was to determine if elevated prolactin was associated with increased estrogen concentrations in non-cycling African elephants. In cycling elephants (n = 12), prolactin secretion followed a normal cyclic pattern, with higher concentrations observed during the follicular phase; overall mean concentration was similar to 18 ng/ml and baseline prolactin was similar to 6 ng/ml. Non-cycling females (n = 18) were categorized into three groups: (1) low prolactin (<15 ng/ml; n = 3); (2) moderate hyperprolactinemia (16-30 ng/ml; n = 7); and marked hyperprolactinemia (>31 ng/ml; n = 8). Mean urinary estrogen conjugate concentrations ranged from 5.4 to 41.4 ng/mg Crt, and were similar between normal cycling (15.4 +/- 1.5 ng/mg Crt) and non-cycling, low prolactin elephants (18.4 +/- 7.3 ng/mg Crt), but were lower in moderate (9.4 +/- 1.3 ng/mg Crt) and marked hyperprolactinemic (9.8 +/- 1.1 ng/mg Crt) groups (P < 0.05). In conclusion, African elephants appear to be sensitive to alterations in prolactin production, with both low (e.g., a non-cycling pattern) and high prolactin secretion being associated with abnormal ovarian activity. However, hyperestrogenism was not related to hyperprolactinemia in the non-cycling females. (C) 2013 Elsevier Inc. All rights reserved. C1 [Prado-Oviedo, Natalia A.] George Mason Univ, Dept Environm Sci & Publ Policy, Fairfax, VA 22030 USA. [Prado-Oviedo, Natalia A.; Brown, Janine L.] Smithsonian Conservat Biol Inst, Ctr Species Survival, Front Royal, VA 22630 USA. [Malloy, Elizabeth J.] American Univ, Dept Math & Stat, Washington, DC 20016 USA. [Deng, Xinyi] Boston Univ, Dept Math & Stat, Boston, MA 02215 USA. RP Prado-Oviedo, NA (reprint author), George Mason Univ, Dept Environm Sci & Publ Policy, 4400 Univ Dr, Fairfax, VA 22030 USA. EM npradoov@gmu.edu FU Morris Animal Foundation [D08ZO-069]; Ella F. Helmlinge Biology Fellowship at American University FX We gratefully acknowledge all the participating institutions for diligently providing urine and serum samples for this study: Caldwell Zoo, Hogle Zoo, Indianapolis Zoo, Jacksonville Zoo, Lee Richardson Zoo, Lion Country Safari, Miami Metro. Zoo, Nashville Zoo, Riverbanks Zoos, Seneca Park Zoo, and Virginia Zoo. Special thanks to Nicole Parker, Nicole Presley and Sarah Putman of the SCBI Endocrine Laboratory for technical assistance; and to Coralie Munro at UC Davis for providing antibody (EC) and technical assistance. We thank Dr. Al Parlow and the National Hormone and Pituitary Program (Rockville, MD) for providing prolactin standard and antiserum; along with Siemens Medical Solutions Diagnostics (Los Angeles, CA) for in-kind support of serum progesterone kits. We thank the anonymous reviewers for their constrictive criticism of this manuscript. This project was supported by grants from the Morris Animal Foundation (Grant ID#: D08ZO-069), and the Ella F. Helmlinge Biology Fellowship at American University. NR 74 TC 4 Z9 4 U1 2 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0016-6480 J9 GEN COMP ENDOCR JI Gen. Comp. Endocrinol. PD AUG 1 PY 2013 VL 189 BP 7 EP 14 DI 10.1016/j.ygcen.2013.03.035 PG 8 WC Endocrinology & Metabolism SC Endocrinology & Metabolism GA 175LF UT WOS:000321231500002 PM 23623777 ER PT J AU Tirelli, T Gamba, M Pessani, D Tudge, CC AF Tirelli, Tina Gamba, Marco Pessani, Daniela Tudge, Christopher C. TI Spermatophore and spermatozoal ultrastructure of the Mediterranean hermit crab Pagurus excavatus (Paguridae: Anomura: Decapoda) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article DE morphology; description; reproductive products; Crustacea; Decapoda ID MALE REPRODUCTIVE-SYSTEM; SOUTHWESTERN-ATLANTIC; SPERM TRANSFER; CRUSTACEA; PAGUROIDEA; MORPHOLOGY; DIOGENIDAE; FAMILIES; PHYLOGENY; GONOPORE AB The ultrastructure of the spermatophores and spermatozoa of the Mediterranean hermit crab Pagurus excavatus are described, using transmission electron microscopy. The size of the different parts of the spermatophore and spermatozoa are given and their ultrastructure described and compared to similar data already present in the literature for other hermit crabs. The morphology and ultrastructure of the spermatophore and spermatozoa of P. excavatus are species-specific, clearly distinguishing the species from the others already described. The spermatophore and spermatozoa show some similarities with those produced by other representatives of the genus. In particular, the tripartite spermatophore is divided into two halves by the lateral ridge and, as with the spermatophores produced by other species belonging to the genus Pagurus, it is morphologically very different from any other Paguroidea. The spermatozoa are composed of an ovoidal acrosomal vesicle capped by the operculum; the acrosome has a length: width ratio of approximately 1.75, therefore larger than 1 as reported for all anomurans studied to date. At the base of the acrosomal vesicle, there is the thin cytoplasm, the large nucleus and three arms positioned to form a 120 degrees angle between each other. The present description is an important additional step allowing for better understanding of the relationships among the different hermit crab taxa. C1 [Tirelli, Tina; Gamba, Marco; Pessani, Daniela] Univ Turin, Life Sci & Syst Biol Dept, I-10123 Turin, Italy. [Tudge, Christopher C.] American Univ, Dept Biol, Washington, DC 20016 USA. [Tudge, Christopher C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20013 USA. RP Tirelli, T (reprint author), Univ Turin, Life Sci & Syst Biol Dept, Via Accademia Albertina 13, I-10123 Turin, Italy. EM santina.tirelli@unito.it RI Gamba, Marco/I-1184-2012 OI Gamba, Marco/0000-0001-9545-2242 NR 62 TC 0 Z9 0 U1 0 U2 6 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD AUG PY 2013 VL 93 IS 5 BP 1363 EP 1371 DI 10.1017/S0025315412001877 PG 9 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 179HI UT WOS:000321510200018 ER PT J AU Fronhofer, EA Sperr, EB Kreis, A Ayasse, M Poethke, HJ Tschapka, M AF Fronhofer, Emanuel A. Sperr, Ellen B. Kreis, Anna Ayasse, Manfred Poethke, Hans Joachim Tschapka, Marco TI Picky hitch-hikers: vector choice leads to directed dispersal and fat-tailed kernels in a passively dispersing mite SO OIKOS LA English DT Article ID CALYPTROGYNE-GHIESBREGHTIANA ARECACEAE; LONG-DISTANCE DISPERSAL; FOREST UNDERSTORY PALM; SEED DISPERSAL; HABITAT PERSISTENCE; REDUCED DISPERSAL; POLLINATING BATS; FRUIT INITIATION; COSTA-RICA; EVOLUTION AB Dispersal is a central life-history trait for most animals and plants: it allows to colonize new habitats, escape from competition or avoid inbreeding. Yet, not all species are mobile enough to perform sufficient dispersal. Such passive dispersers may use more mobile animals as dispersal vectors. If multiple potential vectors are available, an active choice can allow to optimize the dispersal process and to determine the distribution of dispersal distances, i.e. an optimal dispersal kernel. We explore dispersal and vector choice in the neotropical flower mite Spadiseius calyptrogynae using a dual approach which combines experiments with an individual-based simulation model. Spadiseius calyptrogynae is found in lowland rainforests in Costa Rica. It inhabits inflorescences of the understorey palm Calyptrogyne ghiesbreghtiana and is phoretic on a number of flower visitors including bats, beetles and stingless bees. We hypothesised that the mites should optimise their dispersal kernel by actively choosing a specific mix of potential phoretic vectors. In a simple olfactometer setup we showed that the flower mites do indeed discriminate between potential vectors. Subsequently we used an individual-based model to analyse the evolutionary forces responsible for the observed patterns of vector choice. The mites combine vectors exhibiting long-distance dispersal with those allowing for more localized dispersal. This results in a fat-tailed dispersal kernel that guarantees the occasional colonization of new host plant patches (long distance) while optimizing the exploitation of clumped resources (local dispersal). Additionally, kin competition results in a preference for small vectors that transport only few individuals at a time. At the same time, these vectors lead to directed dispersal towards suitable habitat, which increases the stability of this very specialized interaction. Our findings can be applied to other phoretic systems but also to vector-based seed dispersal, for example. C1 [Fronhofer, Emanuel A.; Kreis, Anna; Poethke, Hans Joachim] Univ Wurzburg, Field Stn Fabrikschleichach, DE-96181 Rauhenebrach, Germany. [Sperr, Ellen B.; Ayasse, Manfred; Tschapka, Marco] Univ Ulm, Inst Expt Ecol, DE-89069 Ulm, Germany. [Tschapka, Marco] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Fronhofer, EA (reprint author), Univ Wurzburg, Field Stn Fabrikschleichach, Glashuttenstr 5, DE-96181 Rauhenebrach, Germany. EM fronhofer@biozentrum.uni-wuerzburg.de RI Fronhofer, Emanuel/J-9784-2013 OI Fronhofer, Emanuel/0000-0002-2219-784X FU German Excellence Initiative; German Academic Exchange Service (DAAD); German Science Foundation [DFG: TS 81/2-1] FX The authors would like to thank Dries Bonte for very helpful comments. Furthermore, we thank Daniel Lewanzik for help with handling the bats, Javier Guevara for kindly issuing the research permits (064-2012-SINAC), OTS and the whole La Selva team for invaluable help and support. EAF was supported by a grant of the German Excellence Initiative to the Graduate School of Life Sciences, University of Wurzburg. AK thanks the German Academic Exchange Service (DAAD) for funding. EBS and MT were supported by the German Science Foundation (DFG: TS 81/2-1). NR 61 TC 9 Z9 9 U1 5 U2 52 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0030-1299 EI 1600-0706 J9 OIKOS JI Oikos PD AUG PY 2013 VL 122 IS 8 BP 1254 EP 1264 DI 10.1111/j.1600-0706.2013.00503.x PG 11 WC Ecology SC Environmental Sciences & Ecology GA 183NP UT WOS:000321823300015 ER PT J AU Legates, DR Soon, W Briggs, WM AF Legates, David R. Soon, Willie Briggs, William M. TI Learning and Teaching Climate Science: The Perils of Consensus Knowledge Using Agnotology SO SCIENCE & EDUCATION LA English DT Article ID GREENHOUSE AB Agnotology has been defined in a variety of ways including "the study of ignorance and its cultural production" and "the study of how and why ignorance or misunderstanding exists." More recently, however, it has been posited that agnotology should be used in the teaching of climate change science. But rather than use agnotology to enhance an understanding of the complicated nature of the complex Earth's climate, the particular aim is to dispel alternative viewpoints to the so-called consensus science. One-sided presentations of controversial topics have little place in the classroom as they serve only to stifle debate and do not further knowledge and enhance critical thinking. Students must understand not just what is known and why it is known to be true but also what remains unknown and where the limitations on scientific understanding lie. Fact recitation coupled with demonizing any position or person who disagrees with a singularly-derived conclusion has no place in education. Instead, all sides must be covered in highly debatable and important topics such as climate change, because authoritarian science never will have all the answers to such complex problems. C1 [Legates, David R.] Univ Delaware, Dept Geog, Newark, DE 19716 USA. [Soon, Willie] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Legates, DR (reprint author), Univ Delaware, Dept Geog, Newark, DE 19716 USA. EM legates@udel.edu NR 20 TC 3 Z9 3 U1 3 U2 38 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0926-7220 J9 SCI EDUC-NETHERLANDS JI Sci. Educ. PD AUG PY 2013 VL 22 IS 8 BP 2007 EP 2017 DI 10.1007/s11191-013-9588-3 PG 11 WC Education & Educational Research; History & Philosophy Of Science SC Education & Educational Research; History & Philosophy of Science GA 180DD UT WOS:000321572300006 ER PT J AU Allendorf, TD Allendorf, K AF Allendorf, Teri D. Allendorf, Keera TI Gender and Attitudes toward Protected Areas in Myanmar SO SOCIETY & NATURAL RESOURCES LA English DT Article DE attitudes; gender; Myanmar; park-people relationships; perceptions; protected areas ID CHATTHIN WILDLIFE SANCTUARY; NATIONAL-PARK; LOCAL PEOPLE; CONSERVATION ATTITUDES; COMMUNITY ATTITUDES; BIOSPHERE-RESERVE; FOREST RESOURCES; PERCEPTIONS; INDIA; MANAGEMENT AB From grassroots conservation projects to international committees on the environment, women's representation is an important component of a fair, inclusive, and effective conservation process. In this article, we focus on gender differences in local residents' attitudes toward protected areas in Myanmar. We found women are less likely to have a positive attitude toward the protected areas and are less likely to express perceptions of problems and benefits associated with the areas than men. Using decomposition analysis, we find that the majority of the difference between men's and women's attitudes is explained by these differences in perceptions. Further, much of the difference is explained by men being more likely to perceive conservation and ecosystem service benefits than women, which is the most influential determinant of attitude. C1 [Allendorf, Teri D.] Univ Wisconsin, Dept Forest & Wildlife Ecol, Madison, WI USA. [Allendorf, Teri D.] Natl Zool Pk, Conservat Ecol Ctr, Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Allendorf, Keera] Univ Illinois, Dept Sociol, Champaign, IL USA. RP Allendorf, TD (reprint author), 110 Elm St, Mazomanie, WI 53560 USA. EM teriallendorf@yahoo.com OI Allendorf, Keera/0000-0002-4346-6121 NR 45 TC 8 Z9 8 U1 2 U2 17 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0894-1920 J9 SOC NATUR RESOUR JI Soc. Nat. Resour. PD AUG 1 PY 2013 VL 26 IS 8 BP 962 EP 976 DI 10.1080/08941920.2012.729295 PG 15 WC Environmental Studies; Planning & Development; Sociology SC Environmental Sciences & Ecology; Public Administration; Sociology GA 176RH UT WOS:000321321300007 ER PT J AU Stenning, DC Lee, TCM van Dyk, DA Kashyap, V Sandell, J Young, CA AF Stenning, David C. Lee, Thomas C. M. van Dyk, David A. Kashyap, Vinay Sandell, Julia Young, C. Alex TI Morphological Feature Extraction for Statistical Learning With Applications To Solar Image Data SO STATISTICAL ANALYSIS AND DATA MINING LA English DT Article DE mathematical morphology; image analysis; classification; sunspots; coronal loops; skeletonization AB Many areas of science are generating large volumes of digital image data. In order to take full advantage of the high-resolution and high-cadence images modern technology is producing, methods to automatically process and analyze large batches of such images are needed. This involves reducing complex images to simple representations such as binary sketches or numerical summaries that capture embedded scientific information. Using techniques derived from mathematical morphology, we demonstrate how to reduce solar images into simple 'sketch' representations and numerical summaries that can be used for statistical learning. We demonstrate our general techniques on two specific examples: classifying sunspot groups and recognizing coronal loop structures. Our methodology reproduces manual classifications at an overall rate of 90% on a set of 119 magnetogram and white light images of sunspot groups. We also show that our methodology is competitive with other automated algorithms at producing coronal loop tracings and demonstrate robustness through noise simulations. (C) 2013 Wiley Periodicals, Inc. C1 [Stenning, David C.] Univ Calif Irvine, Dept Stat, Irvine, CA 92617 USA. [Lee, Thomas C. M.] Univ Calif Davis, Dept Stat, Davis, CA 95616 USA. [van Dyk, David A.] Univ London Imperial Coll Sci Technol & Med, Dept Math, Stat Sect, London SW7 2AZ, England. [Kashyap, Vinay] Smithsonian Astrophys Observ, Div High Energy Astrophys, Cambridge, MA 02138 USA. [Sandell, Julia] Univ Penn, Dept Phys, Philadelphia, PA 19104 USA. [Young, C. Alex] NASA GSFC, Heliophys Sci Div, Greenbelt, MD 20771 USA. RP van Dyk, DA (reprint author), Univ London Imperial Coll Sci Technol & Med, Dept Math, Stat Sect, Huxley Bldg, London SW7 2AZ, England. EM dvandyk@imperial.ac.uk NR 15 TC 5 Z9 5 U1 0 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1932-1864 EI 1932-1872 J9 STAT ANAL DATA MIN JI Stat. Anal. Data Min. PD AUG PY 2013 VL 6 IS 4 SI SI BP 329 EP 345 DI 10.1002/sam.11200 PG 17 WC Computer Science, Artificial Intelligence; Computer Science, Interdisciplinary Applications; Statistics & Probability SC Computer Science; Mathematics GA V41CX UT WOS:000209525400006 ER PT J AU Shapira, I Shanas, U Raubenheimer, D Knapp, C Alberts, S Brunton, D AF Shapira, Idan Shanas, Uri Raubenheimer, David Knapp, Craig Alberts, Susan Brunton, Dianne TI Laboratory rats as conspecific biocontrol agents for invasive Norway rats R-norvegicus SO BIOLOGICAL CONTROL LA English DT Article DE Conspecific attraction; Invasive species; Rattus norvegicus; Biocontrol; Pest; Management ID PUBLIC-HEALTH; NEW-ZEALAND; BEHAVIOR; ISLAND; CONSERVATION; WILD; ERADICATION; SONGBIRDS; DISEASES; RODENTS AB We tested whether conspecific attraction can be more efficient than food bait for the detection and capture of an invasive, social species, the Norway rat Rattus norvegicus. We compared trapping rates between male and female laboratory rats and food baited controls at four mainland sites with low rat population densities, three recreational sites (Zoos) with an abundance of food in the environment, and in manipulated island rat incursions. Live lures were more efficient than food baits at both the mainland and recreational sites. There were no differences between the attractiveness of lure animals based on gender either of the lure or of the captured animals. In the manipulated rat incursions, where radio collared male rats were released on a rat free island, two animals were caught with female lures, and the third lost its collar and evaded detection. In the current study we advocate that animal behavior can help inform and guide innovative tools for the control and management of invasive species. We show that laboratory rats might be efficient as lures for their wild counterparts. Furthermore, our results emphasize the need for a flexible and varied rat control toolbox. We suggest that the use of laboratory rats should be considered in future control management plans for invasive Norway rats. (c) 2013 Elsevier Inc. All rights reserved. C1 [Shapira, Idan; Brunton, Dianne] Massey Univ, Ecol & Conservat Grp, Inst Nat Sci, North Shore City 0745, Auckland, New Zealand. [Shanas, Uri] Univ Haifa, Dept Biol, Fac Nat Sci, Tivon, Israel. [Raubenheimer, David] Massey Univ, Nutrit Ecol Grp, Inst Nat Sci, North Shore City 0745, Auckland, New Zealand. [Knapp, Craig] Auckland Zoo, Auckland, New Zealand. [Alberts, Susan] Smithsonian Natl Zool Pk, Integrated Pest Management Dept, Washington, DC USA. RP Shapira, I (reprint author), Massey Univ, Ecol & Conservat Grp, Inst Nat Sci, Private Bag 102 904, North Shore City 0745, Auckland, New Zealand. EM shapiraidan@gmail.com; shanas@research.haifa.a-c.il; d.raubenheimer@massey.ac.nz; Craig.Knap-p@aucklandcouncil.govt.nz; AlbertsS@si.edu; d.h.brunton@massey.ac.nz FU Massey University Research Fund (MURF); AC Research Grant FX We thank the Department of Conservation (DOC), Auckland Zoo (AZ), Hamilton Zoo (HZ), Smithsonian National Zoological Park (SNZP), Shakespeare Open Sanctuary Society (SOSSI), Auckland Council (AC), Forest and Bird (F&B), P. Stevenson and T. Lawson for permission to conduct these experiments. Special thanks should go to P. Brown & F. Buchanan (DOC), S. Burgess & M. Maitland (AC), J. Staniland & A. Warneford (F&B), I. Fraser & T. Joustra (AZ), S. Kudewe and A. Peterson (HZ), A. Hiza, G. Ose & B. King (SNZP) and J. Thoresen for significant administration and field assistance, to A. Petzer from the University of Auckland for kindly supplying laboratory rats and to Honda Marine (NZ) for supplying a motorboat for transport to Browns Island. This study was partly funded by the Massey University Research Fund (MURF) and AC Research Grant. NR 65 TC 2 Z9 2 U1 0 U2 29 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 1049-9644 J9 BIOL CONTROL JI Biol. Control PD AUG PY 2013 VL 66 IS 2 BP 83 EP 91 DI 10.1016/j.biocontrol.2013.04.003 PG 9 WC Biotechnology & Applied Microbiology; Entomology SC Biotechnology & Applied Microbiology; Entomology GA 167WR UT WOS:000320666600002 ER PT J AU Akbari, A Akbari, M Hill, RJ AF Akbari, Amir Akbari, Mohsen Hill, Reghan J. TI Effective thermal conductivity of two-dimensional anisotropic two-phase media SO INTERNATIONAL JOURNAL OF HEAT AND MASS TRANSFER LA English DT Article DE Effective thermal conductivity; Porous media; Anisotropy; Analytical model ID SPHEROIDAL INCLUSIONS; TRANSPORT-PROPERTIES; ELLIPTIC CYLINDERS; COMPOSITES; SPHERES; RESISTANCE; ARRAYS; LATTICES AB The effective thermal conductivity of anisotropic two-phase media is studied. Using Chang's unit cell, a new analytical solution is developed for anisotropic materials based on the self-consistent field concept. The structure comprises randomly distributed aligned elliptical inclusions embedded in a continuous medium. Inclusions have arbitrary aspect ratio and arbitrary orientation relative to the coordinate system of interest. The temperature distribution is solved and averaged in the unit cell to obtain all the components. The model shows correct limiting properties in all its independent variables. In particular, it yields Maxwell's theory in the limit where the inclusion aspect ratio approaches unity. Compact expressions for the components of the effective thermal conductivity are presented. The present model is compared with available expressions for anisotropic systems based on an equivalent inclusion model. To assess the accuracy of these, the closure problem associated with the volume averaging method with periodic boundary condition is numerically solved. The present model agrees well with the result of the periodic unit cell compared with equivalent inclusion based methods, particularly for low aspect ratios and moderate particle volume fractions. This is consistent with Ochoa-Tapia's analysis for isotropic systems that Chang's unit cell can accurately approximate spatially periodic models in a wider range of porosities compared to Maxwell's theory. The present solution can serve as a general 2D model for anisotropic structures with dilute to moderate inclusion concentrations. (c) 2013 Elsevier Ltd. All rights reserved. C1 [Akbari, Amir; Hill, Reghan J.] McGill Univ, Dept Chem Engn, Montreal, PQ H3A 0C5, Canada. [Akbari, Mohsen] McGill Univ, Dept Biomed Engn, Montreal, PQ H3A 1A4, Canada. [Akbari, Mohsen] Harvard Smithsonian Ctr Astrophys, Brigham & Womens Hosp, Sch Med, Ctr Biomed Engn,Dept Med, Cambridge, MA 02139 USA. [Akbari, Mohsen] MIT, Harvard Mit Div Hlth Sci & Technol, Cambridge, MA 02139 USA. RP Akbari, A (reprint author), McGill Univ, Dept Chem Engn, Montreal, PQ H3A 0C5, Canada. EM amir.akbari2@mail.mcgill.ca; mohsen.akbari2@mail.mcgill.ca; reghan.hill@mcgill.ca FU Natural Science and Engineering Research Council (NSERC) of Canada; NSERC FX A.A. acknowledges financial support of Natural Science and Engineering Research Council (NSERC) of Canada. M.A. acknowledges an NSERC postdoctoral fellowship. NR 38 TC 3 Z9 3 U1 3 U2 31 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0017-9310 J9 INT J HEAT MASS TRAN JI Int. J. Heat Mass Transf. PD AUG PY 2013 VL 63 BP 41 EP 50 DI 10.1016/j.ijheatmasstransfer.2013.03.008 PG 10 WC Thermodynamics; Engineering, Mechanical; Mechanics SC Thermodynamics; Engineering; Mechanics GA 162TW UT WOS:000320289900006 ER PT J AU Martinez, A Di Domenico, M Jorger, K Norenburg, J Worsaae, K AF Martinez, Alejandro Di Domenico, Maikon Joerger, Katharina Norenburg, Jon Worsaae, Katrine TI Description of three new species of Protodrilus (Annelida, Protodrilidae) from Central America SO MARINE BIOLOGY RESEARCH LA English DT Article DE Meiofauna; interstitial; scanning electron microscopy; barcoding; Caribbean ID INTERSTITIAL POLYCHAETE; SYSTEMATICS; PHYLOGENY; RECONSTRUCTION; ULTRASTRUCTURE; ARCHIANNELIDA; SEQUENCES; EVOLUTION; PATTERNS; ORGANS AB Three new species of Protodrilus are described from the shallow Western Atlantic waters of Belize and Panama: P. smithsoni sp. nov., P. draco sp. nov. and P. hochbergi sp. nov. Protodrilus smithsoni sp. nov. resembles P. jagersteni and P. submersus from New Zealand, differing by (i) the presence of a dorsal ciliated area on segments 56 of males, (ii) lateral organs extending only to segment 15 (versus 16) and (iii) the smaller size of body and palps. Protodrilus draco sp. nov. is similar to the European P. hypoleucus and P. helgolandicus, but differs in (i) each pygidial lobe possessing a short cirrus and (ii) the posterior-most lateral organ extending dorsally. Protodrilus hochbergi sp. nov. resembles P. purpureus and P. schneideri from the Eastern Atlantic, but differs in (i) the extension of the salivary glands to segment 15 (versus 6) and (ii) the presence of paired lateral ciliary bands on the prostomium. This first exploration of Protodrilus along the Caribbean coast of Central America revealed five new species (three described here), but not P. corderoi, a species described from Brazil and recorded at Dominica. The findings indicate a putative high diversity of Protodrilus species in the Western Atlantic, comparable to the well-sampled Eastern Atlantic (18 reported species). The close resemblance to described species stresses the importance of detailed morphological studies, preferably including scanning electron microscopy, as well as DNA data, in order to describe and identify species of Protodrilus. C1 [Martinez, Alejandro; Worsaae, Katrine] Univ Copenhagen, Marine Biol Sect, DK-3000 Helsingor, Denmark. [Di Domenico, Maikon] Univ Fed Parana, Benth Lab, Ctr Marine Studies, BR-80060000 Curitiba, Parana, Brazil. [Joerger, Katharina] Bavarian State Collect Zool, Mollusca Dept, Munich, Germany. [Norenburg, Jon] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Martinez, A (reprint author), Univ Copenhagen, Marine Biol Sect, Strandpromenaden 5, DK-3000 Helsingor, Denmark. EM amartinez@bio.ku.dk RI Norenburg, Jon/K-3481-2015; Worsaae, Katrine/L-8739-2014 OI Norenburg, Jon/0000-0001-7776-1527; Worsaae, Katrine/0000-0003-0443-4298 FU Encyclopedia of Life Biodiversity Synthesis Group; Encyclopedia of Life fellowship; Carlsberg Foundation; Freja fellowship (University of Copenhagen); Volkswagen Foundation FX Field efforts were in part supported by a grant from Encyclopedia of Life Biodiversity Synthesis Group to JLN and Rachel Collin. We are greatly indebted to Rachel Collin and the rest of the competent staff at the Bocas Marine Laboratory of the Smithsonian Tropical Research Institute. We thank all the students and professors who participated at the surveys at Bocas del Toro, especially Ashleigh Smythe, Rick Hochberg, Marco Curini-Galletti, Fernando Pardos, Christopher Laumer, Barbara Eder, Tiago Jose Pereira, Sofia Pyataeva and Kevin Kocot, who sorted out a lot of material from our samples. We thank Peter Rask Moller and Daniel I. Gouge for assisting with collecting (often by SCUBA diving) at Belize and Bocas del Toro. We also thank Prof. Angelika Brandt, curator of the NT II collection at the Zoologisches Museum of Hamburg, as well as Kathrin Philipps-Bussau and Petra Wagner, for facilitating us access to the type material of three species of Protodrilus. The travelling costs of AM and MDD were partially financed by an Encyclopedia of Life fellowship. The travel costs of KW and laboratory work was financed by grants for K. Worsaae from the Carlsberg Foundation and a Freja fellowship (University of Copenhagen). K. Jorger received funding by a PhD scholarship from the Volkswagen Foundation. NR 32 TC 11 Z9 11 U1 0 U2 22 PU TAYLOR & FRANCIS AS PI OSLO PA KARL JOHANS GATE 5, NO-0154 OSLO, NORWAY SN 1745-1000 J9 MAR BIOL RES JI Mar. Biol. Res. PD AUG 1 PY 2013 VL 9 IS 7 BP 676 EP 691 DI 10.1080/17451000.2013.765574 PG 16 WC Ecology; Marine & Freshwater Biology SC Environmental Sciences & Ecology; Marine & Freshwater Biology GA 130JC UT WOS:000317909700004 ER PT J AU Ticay-Rivas, JR del Pozo-Banos, M Eberhard, WG Alonso, JB Travieso, CM AF Ticay-Rivas, Jaime R. del Pozo-Banos, Marcos Eberhard, William G. Alonso, Jesus B. Travieso, Carlos M. TI Spider specie identification and verification based on pattern recognition of it cobweb SO EXPERT SYSTEMS WITH APPLICATIONS LA English DT Article DE Spider specie recognition; Biometrics on animals; Cobwebs; Identification/Verification approaches; Pattern recognition; Expert systems; Artificial intelligence ID PRINCIPAL COMPONENT ANALYSIS; FEATURE-EXTRACTION; ALGORITHMS; DIVERSITY AB Biodiversity conservation is a global priority where the study of every type of living form is a fundamental task. Inside the huge number of the planet species, spiders play an important role in almost every habitat: This paper presents a comprehensive study on the reliability of the most used features extractors to face the problem of spider specie recognition by using their cobwebs, both in identification and verification modes. We have applied a preprocessing to the cobwebs images in order to obtain only the valid information and compute the optimal size to reach the highest performance. We have used the principal component analysis (PCA), independent component analysis (ICA), Discrete Cosine Transform (DCT), Wavelet Transform (DWT) and discriminative common vectors as features extractors, and proposed the fusion of several of them to improve the system's performance. Finally, we have used the Least Square Vector Support Machine with radial basis function as a classifier. We have implemented K-Fold and Hold-Out cross-validation techniques in order to obtain reliable results. PCA provided the best performance, reaching a 99.65% +/- 0.21 of success rate in identification mode and 99.98% +/- 0.04 of the area under de Reveicer Operating Characteristic (ROC) curve in verification mode. The best combination of features extractors was PCA, DCT, DWT and ICA, which achieved a 99.96% +/- 0.16 of success rate in identification mode and perfect verification. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ticay-Rivas, Jaime R.; del Pozo-Banos, Marcos; Alonso, Jesus B.; Travieso, Carlos M.] Univ Las Palmas Gran Canaria, Inst Technol Dev & Innovat Commun, Signals & Commun Dept, Las Palmas Gran Canaria 35017, Las Palmas, Spain. [Eberhard, William G.] Univ Costa Rica, Smithsonian Trop Res Inst, San Jose, Costa Rica. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Jose, Costa Rica. RP Travieso, CM (reprint author), Univ Las Palmas Gran Canaria, Inst Technol Dev & Innovat Commun, Signals & Commun Dept, Campus Univ Tafira, Las Palmas Gran Canaria 35017, Las Palmas, Spain. EM jrticay@idetic.eu; mpozo@idetic.eu; william.eberhard@gmail.com; jalonso@dsc.ulpgc.es; ctravieso@dsc.ulpgc.es RI Alonso, Jesus/N-5977-2014; Travieso-Gonzalez, Carlos M./N-5967-2014; del Pozo Banos, Marcos/R-8617-2016 OI Alonso, Jesus/0000-0002-7866-585X; Travieso-Gonzalez, Carlos M./0000-0002-4621-2768; del Pozo Banos, Marcos/0000-0003-1502-389X FU Spanish Government; Agencia Espanola de Cooperacion Internacional para el Desarrollo [D/027406/09, D/033858/10, A1/039089/11] FX This work has been supported by Spanish Government, in particular by "Agencia Espanola de Cooperacion Internacional para el Desarrollo" under funds from D/027406/09 for 2010, D/033858/10 for 2011 and A1/039089/11 for 2012. NR 27 TC 3 Z9 3 U1 0 U2 69 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0957-4174 EI 1873-6793 J9 EXPERT SYST APPL JI Expert Syst. Appl. PD AUG PY 2013 VL 40 IS 10 BP 4213 EP 4225 DI 10.1016/j.eswa.2013.01.024 PG 13 WC Computer Science, Artificial Intelligence; Engineering, Electrical & Electronic; Operations Research & Management Science SC Computer Science; Engineering; Operations Research & Management Science GA 120IB UT WOS:000317162900039 ER PT J AU Marriner, N Flaux, C Morhange, C Stanley, JD AF Marriner, Nick Flaux, Clement Morhange, Christophe Stanley, Jean-Daniel TI Tracking Nile Delta Vulnerability to Holocene Change SO PLOS ONE LA English DT Article ID SEA-LEVEL CHANGES; CLIMATE-CHANGE; MISSISSIPPI DELTA; SEDIMENT; CHINA; FLUCTUATIONS; SETTLEMENTS; SUBSIDENCE; EVOLUTION; RESPONSES AB Understanding deltaic resilience in the face of Holocene climate change and human impacts is an important challenge for the earth sciences in characterizing the full range of present and future wetland responses to global warming. Here, we report an 8000-year mass balance record from the Nile Delta to reconstruct when and how this sedimentary basin has responded to past hydrological shifts. In a global Holocene context, the long-term decrease in Nile Delta accretion rates is consistent with insolation-driven changes in the 'monsoon pacemaker', attested throughout the mid-latitude tropics. Following the early to mid-Holocene growth of the Nile's deltaic plain, sediment losses and pronounced erosion are first recorded after similar to 4000 years ago, the corollaries of falling sediment supply and an intensification of anthropogenic impacts from the Pharaonic period onwards. Against the backcloth of the Saharan 'depeopling', reduced river flow underpinned by a weakening of monsoonal precipitation appears to have been particularly conducive to the expansion of human activities on the delta by exposing productive floodplain lands for occupation and irrigation agriculture. The reconstruction suggests that the Nile Delta has a particularly long history of vulnerability to extreme events (e. g. floods and storms) and sea-level rise, although the present sediment-starved system does not have a direct Holocene analogue. This study highlights the importance of the world's deltas as sensitive archives to investigate Holocene geosystem responses to climate change, risks and hazards, and societal interaction. C1 [Marriner, Nick] Univ Franche Comte, CNRS, Lab Chronoenvironm, F-25030 Besancon, France. [Marriner, Nick] CNRS, Ctr Rech & Enseignement Geosci Environm, Aix En Provence, France. [Flaux, Clement; Morhange, Christophe] Univ Aix Marseille, Ctr Rech & Enseignement Geosci Environm, Aix En Provence, France. [Stanley, Jean-Daniel] Smithsonian Inst, Natl Museum Nat Hist, Geoarchaeol Program, Washington, DC 20560 USA. RP Marriner, N (reprint author), Univ Franche Comte, CNRS, Lab Chronoenvironm, F-25030 Besancon, France. EM marriner@cerege.fr OI Marriner, Nick/0000-0002-7916-6059 FU Agence Nationale de la Recherche [Paleomed: 09-BLAN-0323-01, Geomar: ANR-12-SENV-0008-03]; Artemis Institut National des Sciences de l'Univers FX This research was funded by the Agence Nationale de la Recherche (Paleomed: 09-BLAN-0323-01 and Geomar: ANR-12-SENV-0008-03) and Artemis Institut National des Sciences de l'Univers. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 64 TC 7 Z9 7 U1 2 U2 31 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 29 PY 2013 VL 8 IS 7 AR e69195 DI 10.1371/journal.pone.0069195 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 204MP UT WOS:000323369700022 PM 23922692 ER PT J AU Naoz, S Narayan, R AF Naoz, Smadar Narayan, Ramesh TI Generation of Primordial Magnetic Fields on Linear Overdensity Scales SO PHYSICAL REVIEW LETTERS LA English DT Article ID BARYONIC STRUCTURE FORMATION; 21-CM FLUCTUATIONS; THERMAL GENERATION; EARLY UNIVERSE; STAR-FORMATION; HIGH-REDSHIFT; 1ST GALAXIES; TEV BLAZARS; SIMULATIONS; PERTURBATIONS AB Magnetic fields appear to be present in all galaxies and galaxy clusters. Recent measurements indicate that a weak magnetic field may be present even in the smooth low density intergalactic medium. One explanation for these observations is that a seed magnetic field was generated by some unknown mechanism early in the life of the Universe, and was later amplified by various dynamos in nonlinear objects like galaxies and clusters. We show that a primordial magnetic field is expected to be generated in the early Universe on purely linear scales through vorticity induced by scale-dependent temperature fluctuations, or equivalently, a spatially varying speed of sound of the gas. Residual free electrons left over after recombination tap into this vorticity to generate magnetic field via the Biermann battery process. Although the battery operates even in the absence of any relative velocity between dark matter and gas at the time of recombination, the presence of such a relative velocity modifies the predicted spatial power spectrum of the magnetic field. At redshifts of order a few tens, we estimate a root mean square field strength of order 10(-25)-10(-24) G on comoving scales similar to 10 kpc. This field, which is generated purely from linear perturbations, is expected to be amplified significantly after reionization, and to be further boosted by dynamo processes during nonlinear structure formation. C1 [Naoz, Smadar; Narayan, Ramesh] Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, Cambridge, MA 02138 USA. RP Naoz, S (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theory & Computat, 60 Garden St, Cambridge, MA 02138 USA. EM snaoz@cfa.harvard.edu OI Narayan, Ramesh/0000-0002-1919-2730; Naoz, Smadar/0000-0002-9802-9279 FU NASA through an Einstein Postdoctoral Fellowship; Chandra X-ray Center; NASA [PF2-130096]; NASA Grant [NNX11AE16G] FX We thank Antoine Bret, Avi Loeb, and Lorenzo Sironi for useful discussions. We also thank Francesco Miniati and the anonymous referees for useful comments on the manuscript. S. N. was supported by NASA through an Einstein Postdoctoral Fellowship awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. PF2-130096. R. N. acknowledges partial support from NASA Grant No. NNX11AE16G. NR 48 TC 14 Z9 14 U1 0 U2 3 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 29 PY 2013 VL 111 IS 5 AR 051303 DI 10.1103/PhysRevLett.111.051303 PG 5 WC Physics, Multidisciplinary SC Physics GA 193RL UT WOS:000322579100004 PM 23952384 ER PT J AU Cooper, MJ Martin, RV Livesey, NJ Degenstein, DA Walker, KA AF Cooper, Matthew J. Martin, Randall V. Livesey, Nathaniel J. Degenstein, Doug A. Walker, Kaley A. TI Analysis of satellite remote sensing observations of low ozone events in the tropical upper troposphere and links with convection SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article DE ozone; convection; ENSO; upper troposphere ID DEEP CONVECTION; OSCILLATION; CHEMISTRY; SPECTROMETER; CLIMATOLOGY; VARIABILITY; RETRIEVALS; OSIRIS AB Satellite observations from three instruments (Microwave Limb Sounder, Optical Spectrograph and Infrared Imaging System, and Atmospheric Chemistry Experiment Fourier Transform Spectrometer) reveal coherent patterns of low ozone events (<20 ppb) in the tropical upper troposphere. Using a chemical transport model (GEOS-Chem), we find that these events result from deep convective processes that rapidly transport air with low ozone concentrations from the marine boundary layer. These events occur with greater frequency over the tropical South Pacific warm pool, which is consistent with ozonesonde observations. The satellite observations indicate spatial shifts in the frequency of low ozone events that we attribute to changes in convection. As the location of the warm pool shifts eastward during El Nino events, the location of the most frequent low ozone events in the satellite record follows. Mapping of low ozone events over time reveals eastward propagating systems resembling the Madden-Julian Oscillation. These observations and analyses strengthen the link between deep convection and ozone concentrations in the tropical upper troposphere. C1 [Cooper, Matthew J.; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Livesey, Nathaniel J.] CALTECH, Jet Prop Lab, Pasadena, CA USA. [Degenstein, Doug A.] Univ Saskatchewan, Inst Space & Atmospher Sci, Dept Phys & Engn Phys, Saskatoon, SK, Canada. [Walker, Kaley A.] Univ Toronto, Dept Phys, Toronto, ON, Canada. [Walker, Kaley A.] Univ Waterloo, Dept Chem, Waterloo, ON N2L 3G1, Canada. RP Cooper, MJ (reprint author), Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. EM cooperm2@dal.ca RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014 OI Martin, Randall/0000-0003-2632-8402; FU NSERC; Canadian Space Agency FX We thank Ian Folkins for helpful comments that improved the manuscript. This research was supported by funding from the Canadian Space Agency. MC was partially supported by an NSERC Fellowship. NR 29 TC 7 Z9 7 U1 1 U2 16 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 JUL 28 PY 2013 VL 40 IS 14 BP 3761 EP 3765 DI 10.1002/grl.50717 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 204TP UT WOS:000323392700049 ER PT J AU Munoz-Jaramillo, A Balmaceda, LA DeLuca, EE AF Munoz-Jaramillo, Andres Balmaceda, Laura A. DeLuca, Edward E. TI Using the Dipolar and Quadrupolar Moments to Improve Solar-Cycle Predictions Based on the Polar Magnetic Fields SO PHYSICAL REVIEW LETTERS LA English DT Article ID DYNAMO MODELS; FACULAE; EVOLUTION AB The solar cycle and its associated magnetic activity are the main drivers behind changes in the interplanetary environment and Earth's upper atmosphere (commonly referred to as space weather and climate). In recent years there has been an effort to develop accurate solar cycle predictions, leading to nearly a hundred widely spread predictions for the amplitude of solar cycle 24. Here we show that cycle predictions can be made more accurate if performed separately for each hemisphere, taking advantage of information about both the dipolar and quadrupolar moments of the solar magnetic field during minimum. C1 [Munoz-Jaramillo, Andres; DeLuca, Edward E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Munoz-Jaramillo, Andres] Univ Corp Atmospher Res, Boulder, CO 80307 USA. [Munoz-Jaramillo, Andres] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Balmaceda, Laura A.] ICATE CONICET, Inst Astron Terr & Space Sci, San Juan, Argentina. RP Munoz-Jaramillo, A (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM amunoz@cfa.harvard.edu RI DeLuca, Edward/L-7534-2013; OI Balmaceda, Laura/0000-0003-1162-5498; DeLuca, Edward/0000-0001-7416-2895; Munoz-Jaramillo, Andres/0000-0002-4716-0840 FU NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program; University of Utah; [SP02H1701R] FX We are thankful to Sami Solanki, Mari a Dasi-Espuig,and Maria Navas-Moreno, and two anonymous referees for useful discussions and suggestions. This research is supported by the NASA Living With a Star Jack Eddy Postdoctoral Fellowship Program, administered by the UCAR Visiting Scientist Programs. Andres Munoz-Jaramillo is grateful to David Kieda for his support and sponsorship at the University of Utah. E. DeLuca was supported by Contract No. SP02H1701R from Lockheed Martin to SAO. NR 30 TC 10 Z9 10 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 26 PY 2013 VL 111 IS 4 AR 041106 DI 10.1103/PhysRevLett.111.041106 PG 5 WC Physics, Multidisciplinary SC Physics GA 259OT UT WOS:000327536900002 PM 23931351 ER PT J AU Holt, BG Lessard, JP Borregaard, MK Fritz, SA Araujo, MB Dimitrov, D Fabre, PH Graham, CH Graves, GR Jonsson, KA Nogues-Bravo, D Wang, ZH Whittaker, RJ Fjeldsa, J Rahbek, C AF Holt, Ben G. Lessard, Jean-Philippe Borregaard, Michael K. Fritz, Susanne A. Araujo, Miguel B. Dimitrov, Dimitar Fabre, Pierre-Henri Graham, Catherine H. Graves, Gary R. Jonsson, Knud A. Nogues-Bravo, David Wang, Zhiheng Whittaker, Robert J. Fjeldsa, Jon Rahbek, Carsten TI Response to Comment on "An Update of Wallace's Zoogeographic Regions of the World" SO SCIENCE LA English DT Editorial Material ID BIRDS; DIVERSITY; PATTERNS C1 [Holt, Ben G.; Lessard, Jean-Philippe; Borregaard, Michael K.; Fritz, Susanne A.; Araujo, Miguel B.; Graves, Gary R.; Nogues-Bravo, David; Wang, Zhiheng; Whittaker, Robert J.; Rahbek, Carsten] Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. [Holt, Ben G.] Univ E Anglia, Sch Biol Sci, Norwich NR4 7TJ, Norfolk, England. [Lessard, Jean-Philippe] McGill Univ, Dept Biol, Quebec Ctr Biodivers Sci, Montreal, PQ H3A 1B1, Canada. [Fritz, Susanne A.] Biodivers & Climate Res Ctr BiK F, D-60325 Frankfurt, Germany. [Fritz, Susanne A.] Senckenberg Gesell Nat Forsch, D-60325 Frankfurt, Germany. [Araujo, Miguel B.] CSIC, Natl Museum Nat Sci, Dept Biogeog & Global Change, E-28006 Madrid, Spain. [Araujo, Miguel B.] Univ Evora, Ctr Invest Biodiversidade & Recursos Genet, P-7000 Evora, Portugal. [Araujo, Miguel B.; Dimitrov, Dimitar; Fabre, Pierre-Henri; Graves, Gary R.; Jonsson, Knud A.; Nogues-Bravo, David; Wang, Zhiheng; Fjeldsa, Jon; Rahbek, Carsten] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. [Dimitrov, Dimitar] Univ Oslo, Nat Hist Museum, NO-0318 Oslo, Norway. [Graham, Catherine H.] SUNY Stony Brook, Dept Ecol & Evolut, Stony Brook, NY 11794 USA. [Graves, Gary R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Whittaker, Robert J.] Univ Oxford, Sch Geog & Environm, Biodivers Res Grp, Ctr Environm, Oxford OX1 3QY, England. RP Lessard, JP (reprint author), Univ Copenhagen, Dept Biol, Ctr Macroecol Evolut & Climate, DK-2100 Copenhagen O, Denmark. EM jplessard@bio.ku.dk RI publist, CMEC/C-3010-2012; publicationpage, cmec/B-4405-2017; Rahbek, Carsten/L-1129-2013; Dimitrov, Dimitar/A-9563-2009; Borregaard, Michael/B-8442-2008; Graham, Catherine/A-9560-2011; Fjeldsa, Jon/A-9699-2013; Whittaker, Robert/H-1548-2015; Araujo, Miguel/B-6117-2008; Fritz, Susanne/M-9872-2014; Wang, Zhiheng/G-1750-2010 OI Jonsson, Knud/0000-0002-1875-9504; Holt, Ben G./0000-0003-0831-9684; Dimitrov, Dimitar/0000-0001-5830-5702; Borregaard, Michael/0000-0002-8146-8435; Fjeldsa, Jon/0000-0003-0790-3600; Whittaker, Robert/0000-0001-7775-3383; Araujo, Miguel/0000-0002-5107-7265; Fritz, Susanne/0000-0002-4085-636X; NR 14 TC 2 Z9 2 U1 7 U2 70 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 JUL 26 PY 2013 VL 341 IS 6144 DI 10.1126/science.1237541 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 189HX UT WOS:000322259200023 PM 23888024 ER PT J AU Crassard, R Petraglia, MD Drake, NA Breeze, P Gratuze, B Alsharekh, A Arbach, M Groucutt, HS Khalidi, L Michelsen, N Robin, CJ Schiettecatte, J AF Crassard, Remy Petraglia, Michael D. Drake, Nick A. Breeze, Paul Gratuze, Bernard Alsharekh, Abdullah Arbach, Mounir Groucutt, Huw S. Khalidi, Lamya Michelsen, Nils Robin, Christian J. Schiettecatte, Jeremie TI Middle Palaeolithic and Neolithic Occupations around Mundafan Palaeolake, Saudi Arabia: Implications for Climate Change and Human Dispersals SO PLOS ONE LA English DT Article ID SULTANATE-OF-OMAN; WAHIBA SAND SEA; SOUTHERN ARABIA; INDIAN MONSOON; LATE PLEISTOCENE; HOLOCENE LAKES; YEMEN; AFRICA; INTERIOR; DESERT AB Arabian Peninsula is a key region for understanding climate change and human occupation history in a marginal environment. The Mundafan palaeolake is situated in southern Saudi Arabia, in the Rub' al-Khali (the 'Empty Quarter'), the world's largest sand desert. Here we report the first discoveries of Middle Palaeolithic and Neolithic archaeological sites in association with the palaeolake. We associate the human occupations with new geochronological data, and suggest the archaeological sites date to the wet periods of Marine Isotope Stage 5 and the Early Holocene. The archaeological sites indicate that humans repeatedly penetrated the ameliorated environments of the Rub' al-Khali. The sites probably represent short-term occupations, with the Neolithic sites focused on hunting, as indicated by points and weaponry. Middle Palaeolithic assemblages at Mundafan support a lacustrine adaptive focus in Arabia. Provenancing of obsidian artifacts indicates that Neolithic groups at Mundafan had a wide wandering range, with transport of artifacts from distant sources. C1 [Crassard, Remy; Khalidi, Lamya] Maison Orient & Mediterranee, CNRS, UMR Archeorient 5133, Lyon, France. [Petraglia, Michael D.; Groucutt, Huw S.] Univ Oxford, Sch Archaeol, Res Lab Archaeol & Hist Art, Oxford, England. [Petraglia, Michael D.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. [Drake, Nick A.; Breeze, Paul] Kings Coll London, Dept Geog, London WC2R 2LS, England. [Gratuze, Bernard] Ctr Ernest Babelon, CNRS, UMR Iramat 5060, Orleans, France. [Alsharekh, Abdullah] King Saud Univ, Coll Tourism & Archaeol, Dept Archaeol, Riyadh, Saudi Arabia. [Alsharekh, Abdullah] Minist Higher Educ, Riyadh, Saudi Arabia. [Arbach, Mounir; Robin, Christian J.; Schiettecatte, Jeremie] CNRS, UMR Orient & Mediterranee Mondes Semit 8167, Ivry, France. [Michelsen, Nils] Tech Univ Darmstadt, Inst Angew Geowissensch, Darmstadt, Germany. RP Crassard, R (reprint author), Maison Orient & Mediterranee, CNRS, UMR Archeorient 5133, Lyon, France. EM remy.crassard@mom.fr OI GRATUZE, Bernard/0000-0001-6136-8085; Crassard, Remy/0000-0002-2403-1894 FU French Embassy in Saudi Arabia; French Ministry of Foreign Affairs; Fondation Fyssen grant 'Subvention de Recherche; Natural Environment Research Council [NE/J500306/1]; European Research Council [295719]; IRAMAT- Universite d'Orleans - UTBM; CEPAM - Universite de Nice Sophia-Antipolis; CRAHM - Universite de Caen; CAA - Universite de Rennes FX This research was funded by the French Embassy in Saudi Arabia (to CJR), the French Ministry of Foreign Affairs (to CJR), the Fondation Fyssen grant 'Subvention de Recherche 2013' (to RC), the Natural Environment Research Council grant no. NE/J500306/1 (to PB) and the European Research Council grant no. 295719 (to MDP). Obsidian analyses were funded by a Plan Pluri-Formation entitled "CODAI Archeomateriaux inorganiques'' (IRAMAT- Universite d'Orleans - UTBM, CEPAM - Universite de Nice Sophia-Antipolis, CRAHM - Universite de Caen, CAA - Universite de Rennes). The funders had no role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 81 TC 3 Z9 3 U1 1 U2 21 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 24 PY 2013 VL 8 IS 7 AR e69665 DI 10.1371/journal.pone.0069665 PG 22 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 188BY UT WOS:000322167900088 PM 23894519 ER PT J AU de Santana, CD Vari, RP Wosiacki, WB AF de Santana, Carlos David Vari, Richard P. Wosiacki, Wolmar B. TI The Untold Story of the Caudal Skeleton in the Electric Eel (Ostariophysi: Gymnotiformes: Electrophorus) SO PLOS ONE LA English DT Article ID FISHES; APTERONOTIDAE; TELEOSTEI; INTERRELATIONSHIPS; SILURIFORMES; GYMNOTOIDEI; MORPHOLOGY; DIVERSITY; ECOLOGY; BOLIVIA AB Alternative hypotheses had been advanced as to the components forming the elongate fin coursing along the ventral margin of much of the body and tail from behind the abdominal region to the posterior margin of the tail in the Electric Eel, Electrophorus electricus. Although the original species description indicated that this fin was a composite of the caudal fin plus the elongate anal fin characteristic of other genera of the Gymnotiformes, subsequent researchers proposed that the posterior region of the fin was formed by the extension of the anal fin posteriorly to the tip of the tail, thereby forming a "false caudal fin." Examination of ontogenetic series of the genus reveal that Electrophorus possesses a true caudal fin formed of a terminal centrum, hypural plate and a low number of caudal-fin rays. The confluence of the two fins is proposed as an additional autapomorphy for the genus. Under all alternative proposed hypotheses of relationships within the order Gymnotiformes, the presence of a caudal fin in Electrophorus optimized as being independent of the occurence of the morphologically equivalent structure in the Apteronotidae. Possible functional advantages to the presence of a caudal fin in the genus are discussed. C1 [de Santana, Carlos David; Vari, Richard P.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20560 USA. [de Santana, Carlos David; Wosiacki, Wolmar B.] Museu Paraense Emilio Goeldi, Setor Ictiol, Belem, Para, Brazil. RP de Santana, CD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20560 USA. EM apteronotidae@ig.com.br RI Wosiacki, Wolmar/I-1724-2012 OI Wosiacki, Wolmar/0000-0002-4013-8501 FU Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology of the National Museum of Natural History; Smithsonian Institution; Conselho Nacional de Pesquisa (CNPq); CNPq/Ciencia sem Fronteiras [245622/2012-8] FX Funding for the research was provided to RPV and CDS by the Herbert R. and Evelyn Axelrod Chair in Systematic Ichthyology of the National Museum of Natural History, Smithsonian Institution, and to WBW by Conselho Nacional de Pesquisa (CNPq). CDS was supported by a Posdoctoral Fellowship from the CNPq/Ciencia sem Fronteiras (245622/2012-8). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 48 TC 3 Z9 3 U1 1 U2 26 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 24 PY 2013 VL 8 IS 7 AR e68719 DI 10.1371/journal.pone.0068719 PG 8 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 188BY UT WOS:000322167900023 PM 23894337 ER PT J AU Lemeshko, M Yao, NY Gorshkov, AV Weimer, H Bennett, SD Momose, T Gopalakrishnan, S AF Lemeshko, Mikhail Yao, Norman Y. Gorshkov, Alexey V. Weimer, Hendrik Bennett, Steven D. Momose, Takamasa Gopalakrishnan, Sarang TI Controllable quantum spin glasses with magnetic impurities embedded in quantum solids SO PHYSICAL REVIEW B LA English DT Article ID HIGH-RESOLUTION SPECTROSCOPY; POSITION MEASUREMENT; POLAR-MOLECULES; OPTICAL-FIELDS; CS ATOMS; HE-4; PARAHYDROGEN; CRYSTALS; DYNAMICS; RELAXATION AB Magnetic impurities embedded in inert solids can exhibit long coherence times and interact with one another via their intrinsic anisotropic dipolar interaction. We argue that, as a consequence of these properties, disordered ensembles of magnetic impurities provide an effective platform for realizing a controllable, tunable version of the dipolar quantum spin glass seen in LiHoxY1-xF4. Specifically, we propose and analyze a system composed of dysprosium atoms embedded in solid helium. We describe the phase diagram of the system and discuss the realizability and detectability of the quantum spin glass and antiglass phases. C1 [Lemeshko, Mikhail] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lemeshko, Mikhail] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Lemeshko, Mikhail; Gorshkov, Alexey V.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Gorshkov, Alexey V.] CALTECH, Inst Quantum Informat & Matter, Pasadena, CA 91125 USA. [Weimer, Hendrik] Leibniz Univ Hannover, Inst Theoret Physik, D-30167 Hannover, Germany. [Momose, Takamasa] Univ British Columbia, Dept Chem, Vancouver, BC V6T IZ1, Canada. RP Lemeshko, M (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM mlemeshko@cfa.harvard.edu RI Gorshkov, Alexey/A-9848-2008 OI Gorshkov, Alexey/0000-0003-0509-3421 FU NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory; DOE [FG02-97ER25308]; Lee A. DuBridge foundation; IQIM; NSF Physics FrontierCenter; Moore foundation; Harvard Quantum Optics Center FX We are indebted to Mikhail Lukin, Ariel Amir, and Benjamin Lev for insightful discussions. M.L. acknowledges support from NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. N.Y.Y. acknowledges support from the DOE (FG02-97ER25308). A.V.G. acknowledges funding from the Lee A. DuBridge foundation and from the IQIM, an NSF Physics FrontierCenter with support of the Moore foundation. S.G. acknowledges support from the Harvard Quantum Optics Center. M.L. and A.V.G. thank KITP for hospitality. NR 106 TC 3 Z9 3 U1 1 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1098-0121 J9 PHYS REV B JI Phys. Rev. B PD JUL 24 PY 2013 VL 88 IS 1 AR 014426 DI 10.1103/PhysRevB.88.014426 PG 7 WC Physics, Condensed Matter SC Physics GA 188TC UT WOS:000322215500003 ER PT J AU Gharashi, SE Blume, D AF Gharashi, Seyed Ebrahim Blume, D. TI Correlations of the Upper Branch of 1D Harmonically Trapped Two-Component Fermi Gases SO PHYSICAL REVIEW LETTERS LA English DT Article ID IMPENETRABLE BOSONS; FERROMAGNETISM; DUALITY; SYSTEMS; ATOMS AB We present highly accurate energy spectra and eigenfunctions of small 1D harmonically trapped two-component Fermi gases with interspecies delta-function interactions, and analyze the correlations of the so-called upper branch (i.e., the branch that describes a repulsive Fermi gas consisting of atoms but no molecules) for positive and negative coupling constants. Changes of the two-body correlations as a function of the interspecies coupling strength reflect the competition of the interspecies interaction and the effective repulsion due to the Pauli exclusion principle, and are interpreted as a few-body analog of a transition from a nonmagnetic to a magnetic phase. Moreover, we show that the eigenstate psi(adia) of the infinitely strongly interacting system with vertical bar n(1) + n(2)vertical bar > 2 and vertical bar n(1) - n(2)vertical bar < n (n(1) and n(2) denote the number of fermions of components 1 and 2, respectively), which is reached experimentally by adiabatically changing the system parameters, does not, as previously proposed, coincide with the wave function psi(G) obtained by applying a generalized Fermi-Fermi mapping function to the eigenfunction of the non-interacting single-component Fermi gas. C1 [Gharashi, Seyed Ebrahim; Blume, D.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. [Blume, D.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. RP Gharashi, SE (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. RI Gharashi, Seyed Ebrahim/E-5378-2016 OI Gharashi, Seyed Ebrahim/0000-0002-8798-7615 FU ARO; National Science Foundation FX We acknowledge stimulating discussions and correspondence with Selim Jochim and his group members. We also acknowledge fruitful discussions with Chris H. Greene on how to connect results obtained within the Schrodinger equation and mean-field equation frameworks. We thank Jason Ho and Liming Guan for pointing out Ref. [16] to us. Support by the ARO is gratefully acknowledged. This work was additionally supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and the Smithsonian Astrophysical Observatory. NR 36 TC 54 Z9 54 U1 0 U2 12 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUL 24 PY 2013 VL 111 IS 4 AR 045302 DI 10.1103/PhysRevLett.111.045302 PG 5 WC Physics, Multidisciplinary SC Physics GA 188TV UT WOS:000322218000008 PM 23931379 ER PT J AU Li, JF Abuduresule, I Hueber, FM Li, WY Hu, XJ Li, YZ Li, CS AF Li, Jin-Feng Abuduresule, Idelisi Hueber, Francis M. Li, Wen-Ying Hu, Xin-Jun Li, Yue-Zhuo Li, Cheng-Sen TI Buried in Sands: Environmental Analysis at the Archaeological Site of Xiaohe Cemetery, Xinjiang, China SO PLOS ONE LA English DT Article ID YANGHAI TOMBS; POLLEN GRAINS; BRONZE-AGE; BP; POACEAE AB Palynomorphs extracted from the mud coffins and plant remains preserved at the archaeological site of Xiaohe Cemetery (Cal. 3980 to 3540 years BP) in Lop Nur Desert of Xinjiang, China were investigated for the reconstruction of the ancient environments at the site. The results demonstrate that the Xiaohe People lived at a well-developed oasis, which was surrounded by extensive desert. The vegetation in the oasis consisted of Populus, Phragmites, Typha and probably of Gramineae, while the desert surrounding the oasis had some common drought-resistant plants dominated by Ephedra, Tamarix, Artemisia and Chenopodiaceae. This present work provides the first data of the environmental background at this site for further archaeological investigation. C1 [Li, Jin-Feng; Li, Cheng-Sen] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing, Peoples R China. [Abuduresule, Idelisi; Li, Wen-Ying; Hu, Xin-Jun] Xinjiang Cultural Rel & Archaeol Inst, Urumqi, Peoples R China. [Hueber, Francis M.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Li, Yue-Zhuo] Sanya Museum Nat Hist, Sanya, Peoples R China. RP Li, CS (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing, Peoples R China. EM lics@ibcas.ac.cn FU National Social Science Fund [12AZD085] FX This investigation was supported by a National Social Science Fund grant (No. 12AZD085). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 36 TC 3 Z9 3 U1 3 U2 13 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 22 PY 2013 VL 8 IS 7 AR e68957 DI 10.1371/journal.pone.0068957 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 187PW UT WOS:000322132100033 PM 23894382 ER PT J AU Lee, TE Cross, MC AF Lee, Tony E. Cross, M. C. TI Quantum-classical transition of correlations of two coupled cavities SO PHYSICAL REVIEW A LA English DT Article ID 2ND-HARMONIC GENERATION; OSCILLATORS; SYNCHRONIZATION; LATTICES AB We study the difference between quantum and classical behavior in a pair of nonidentical cavities with second-harmonic generation. In the classical limit, each cavity has a limit-cycle solution, in which the photon number oscillates periodically in time. Coupling between the cavities leads to synchronization of the oscillations and classical correlations between the cavities. In the quantum limit, there are quantum correlations due to entanglement. The quantum correlations persist even when the cavities are far off resonance with each other, in stark contrast with the classical case. We also find that the quantum and classical limits are connected by an intermediate regime of almost no correlations. Our results can be extended to a wide variety of quantum models. C1 [Lee, Tony E.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lee, Tony E.; Cross, M. C.] CALTECH, Dept Phys, Pasadena, CA 91125 USA. RP Lee, TE (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [DMR-1003337] FX We thank Mark Rudner and Sarang Gopalakrishnan for useful discussions. This work was supported by NSF through Grant No. DMR-1003337 and through a grant to ITAMP. NR 46 TC 13 Z9 13 U1 1 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL 22 PY 2013 VL 88 IS 1 AR 013834 DI 10.1103/PhysRevA.88.013834 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 187IW UT WOS:000322111800015 ER PT J AU Blanchard, PK Bayliss, MB McDonald, M Dahle, H Gladders, MD Sharon, K Mushotzky, R AF Blanchard, Peter K. Bayliss, Matthew B. McDonald, Michael Dahle, Hakon Gladders, Michael D. Sharon, Keren Mushotzky, Richard TI SEARCHING FOR COOLING SIGNATURES IN STRONG LENSING GALAXY CLUSTERS: EVIDENCE AGAINST BARYONS SHAPING THE MATTER DISTRIBUTION IN CLUSTER CORES SO ASTROPHYSICAL JOURNAL LA English DT Article DE dark matter; galaxies: clusters: general; galaxies: clusters: intracluster medium; galaxies: elliptical and lenticular, cD; galaxies: star formation; gravitational lensing: strong ID ACTIVE GALACTIC NUCLEI; GIANT ARC STATISTICS; EMISSION-LINE NEBULAE; H-ALPHA FILAMENTS; STAR-FORMATION; LENSED GALAXIES; CROSS-SECTIONS; FLOW CLUSTERS; OF-SIGHT; UNIVERSE AB The process by which the mass density profile of certain galaxy clusters becomes centrally concentrated enough to produce high strong lensing (SL) cross-sections is not well understood. It has been suggested that the baryonic condensation of the intracluster medium (ICM) due to cooling may drag dark matter to the cores and thus steepen the profile. In this work, we search for evidence of ongoing ICM cooling in the first large, well-defined sample of SL selected galaxy clusters in the range 0.1 < z < 0.6. Based on known correlations between the ICM cooling rate and both optical emission line luminosity and star formation, we measure, for a sample of 89 SL clusters, the fraction of clusters that have [O II]lambda lambda 3727 emission in their brightest cluster galaxy (BCG). We find that the fraction of line-emitting BCGs is constant as a function of redshift for z > 0.2 and shows no statistically significant deviation from the total cluster population. Specific star formation rates, as traced by the strength of the 4000 angstrom break, D-4000, are also consistent with the general cluster population. Finally, we use optical imaging of the SL clusters to measure the angular separation, R-arc, between the arc and the center of mass of each lensing cluster in our sample and test for evidence of changing [O II] emission and D-4000 as a function of R-arc, a proxy observable for SL cross-sections. D-4000 is constant with all values of Rarc, and the [O II] emission fractions show no dependence on R-arc for R-arc > 10 '' and only very marginal evidence of increased weak [O II] emission for systems with R-arc < 10 ''. These results argue against the ability of baryonic cooling associated with cool core activity in the cores of galaxy clusters to strongly modify the underlying dark matter potential, leading to an increase in SL cross-sections. C1 [Blanchard, Peter K.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Blanchard, Peter K.; Bayliss, Matthew B.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bayliss, Matthew B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [McDonald, Michael] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Dahle, Hakon] Univ Oslo, Inst Theoret Astrophys, NO-0315 Oslo, Norway. [Gladders, Michael D.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Gladders, Michael D.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Sharon, Keren] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Mushotzky, Richard] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Blanchard, PK (reprint author), Univ Calif Berkeley, Dept Astron, B-20 Hearst Field Annex 3411, Berkeley, CA 94720 USA. EM pblanchard@fas.harvard.edu FU National Science Foundation Research Experiences for Undergraduates (REU); Department of Defense [0754568]; Smithsonian Institution; NSF Astronomy Division [AST-1009012]; Research Corporation FX This work is supported in part by the National Science Foundation Research Experiences for Undergraduates (REU) and Department of Defense Awards to Stimulate and Support Undergraduate Research Experiences (ASSURE) programs under grant number 0754568 and by the Smithsonian Institution. Part of this work was based on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. M. B. B. acknowledges support from the NSF Astronomy Division under grant number AST-1009012. M. M. acknowledges support provided by NASA through a Hubble Fellowship grant from STScI. M. D. G. thanks the Research Corporation for support of this work through a Cottrell Scholars award. We would like to thank Jonathan McDowell and Marie Machacek for helpful feedback on early drafts of this paper. NR 73 TC 4 Z9 4 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2013 VL 772 IS 1 AR 24 DI 10.1088/0004-637X/772/1/24 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700024 ER PT J AU Girart, JM Frau, P Zhang, Q Koch, PM Qiu, K Tang, YW Lai, SP Ho, PTP AF Girart, J. M. Frau, P. Zhang, Q. Koch, P. M. Qiu, K. Tang, Y. -W. Lai, S. -P. Ho, P. T. P. TI DR 21(OH): A HIGHLY FRAGMENTED, MAGNETIZED, TURBULENT DENSE CORE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (DR 21(OH)); ISM: magnetic fields; polarization; stars: formation; submillimeter: ISM; techniques: polarimetric ID MASS STAR-FORMATION; CYGNUS X REGION; H-II REGIONS; 1333 IRAS 4A; MOLECULAR CLOUDS; METHANOL MASERS; FORMING REGIONS; INTERFEROMETRIC OBSERVATIONS; SUBMILLIMETER ARRAY; AMBIPOLAR DIFFUSION AB We present high angular resolution observations of the massive star-forming core DR21(OH) at 880 mu m using the Submillimeter Array (SMA). The dense core exhibits an overall velocity gradient in a Keplerian-like pattern, which breaks at the center of the core where SMA 6 and SMA 7 are located. The dust polarization shows a complex magnetic field, compatible with a toroidal configuration. This is in contrast with the large, parsec-scale filament that surrounds the core, where there is a smooth magnetic field. The total magnetic field strengths in the filament and in the core are 0.9 and 2.1 mG, respectively. We found evidence of magnetic field diffusion at the core scales, far beyond the expected value for ambipolar diffusion. It is possible that the diffusion arises from fast magnetic reconnection in the presence of turbulence. The dynamics of the DR 21(OH) core appear to be controlled energetically in equal parts by the magnetic field, magnetohydrodynamic turbulence, and the angular momentum. The effect of the angular momentum (this is a fast rotating core) is probably causing the observed toroidal field configuration. Yet, gravitation overwhelms all the forces, making this a clear supercritical core with a mass-to-flux ratio of similar or equal to 6 times the critical value. However, simulations show that this is not enough for the high level of fragmentation observed at 1000 AU scales. Thus, rotation and outflow feedback are probably the main causes of the observed fragmentation. C1 [Girart, J. M.; Frau, P.] CSIC, IEEC, Fac Ciencies, Inst Ciencies Espai, E-08193 Bellaterra, Catalonia, Spain. [Frau, P.] Observ Astron Nacl, E-28014 Madrid, Spain. [Zhang, Q.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koch, P. M.; Tang, Y. -W.; Lai, S. -P.; Ho, P. T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Qiu, K.] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Lai, S. -P.] Natl Tsing Hua Univ, Inst Astron, Hsinchu 30013, Taiwan. [Lai, S. -P.] Natl Tsing Hua Univ, Dept Phys, Hsinchu 30013, Taiwan. RP Girart, JM (reprint author), CSIC, IEEC, Fac Ciencies, Inst Ciencies Espai, Campus UAB,C5P 2, E-08193 Bellaterra, Catalonia, Spain. EM girart@ice.cat RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica; ASIAA; SAO; Spanish MINECO [AYA2011-30228-C03-02, AYA2008-04451-E]; Catalan AGAUR [2009SGR1172]; National Science Council of Taiwan [NSC 98-2112-M-007-007-MY3, NSC 101-2119-M-007-004] FX The SMA data were taken as part of the Legacy SMA project "Filaments, Star Formation and Magnetic Fields" (PI: Qizhou Zhang). 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. We thank all members of the SMA staff that made these observations possible, as well as the ASIAA and the SAO for the support on the Legacy project. We also thank M. Padovani for providing the polarization data from simulations. J.M.G. and P.F. are supported by the Spanish MINECO AYA2011-30228-C03-02, AYA2008-04451-E, and Catalan AGAUR 2009SGR1172 grants. S.P. L. acknowledges support from the National Science Council of Taiwan with grants NSC 98-2112-M-007-007-MY3 and NSC 101-2119-M-007-004. NR 85 TC 30 Z9 30 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2013 VL 772 IS 1 AR 69 DI 10.1088/0004-637X/772/1/69 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700069 ER PT J AU Guillot, S Servillat, M Webb, NA Rutledge, RE AF Guillot, Sebastien Servillat, Mathieu Webb, Natalie A. Rutledge, Robert E. TI MEASUREMENT OF THE RADIUS OF NEUTRON STARS WITH HIGH SIGNAL-TO-NOISE QUIESCENT LOW-MASS X-RAY BINARIES IN GLOBULAR CLUSTERS SO ASTROPHYSICAL JOURNAL LA English DT Article DE globular clusters: individual (M28, M13, NGC 5139, NGC 6304, NGC 6397); stars: neutron; X-rays: binaries ID EQUATION-OF-STATE; XMM-NEWTON OBSERVATIONS; RR LYRAE STARS; OMEGA-CENTAURI; DENSE MATTER; MILKY-WAY; NGC 6397; CEN X-4; ROSAT OBSERVATIONS; MODEL ATMOSPHERES AB This paper presents the measurement of the neutron star (NS) radius using the thermal spectra from quiescent low-mass X-ray binaries (qLMXBs) inside globular clusters (GCs). Recent observations of NSs have presented evidence that cold ultra dense matter-present in the core of NSs-is best described by "normal matter" equations of state (EoSs). Such EoSs predict that the radii of NSs, R-NS, are quasi-constant (within measurement errors, of similar to 10%) for astrophysically relevant masses (M-NS > 0.5 M-circle dot). The present work adopts this theoretical prediction as an assumption, and uses it to constrain a single R-NS value from five qLMXB targets with available high signal-to-noise X-ray spectroscopic data. Employing a Markov chain Monte-Carlo approach, we produce the marginalized posterior distribution for R-NS, constrained to be the same value for all five NSs in the sample. An effort was made to include all quantifiable sources of uncertainty into the uncertainty of the quoted radius measurement. These include the uncertainties in the distances to the GCs, the uncertainties due to the Galactic absorption in the direction of the GCs, and the possibility of a hard power-law spectral component for count excesses at high photon energy, which are observed in some qLMXBs in the Galactic plane. Using conservative assumptions, we found that the radius, common to the five qLMXBs and constant for a wide range of masses, lies in the low range of possible NS radii, R-NS = 9.1(-1.5)(+1.3) km (90%-confidence). Such a value is consistent with low-R-NS equations of state. We compare this result with previous radius measurements of NSs from various analyses of different types of systems. In addition, we compare the spectral analyses of individual qLMXBs to previous works. C1 [Guillot, Sebastien; Rutledge, Robert E.] McGill Univ, Dept Phys, Montreal, PQ H2X 3R4, Canada. [Servillat, Mathieu] Univ Paris Diderot, CEA Saclay, CNRS, Lab AIM CEA DSM IRFU SAp, F-91191 Gif Sur Yvette, France. [Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Webb, Natalie A.] Univ Toulouse, UPS OMP, IRAP, Toulouse, France. [Webb, Natalie A.] CNRS, IRAP, F-31028 Toulouse 4, France. RP Guillot, S (reprint author), McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H2X 3R4, Canada. EM guillots@physics.mcgill.ca; rutledge@physics.mcgill.ca FU NSERC via the Vanier CGS program; NSERC; NASA/Chandra grant [GO0-11063X]; Centre National d'Etudes Spatiales (CNES) FX The authors would like to thank the referee for useful remarks that improved the clarity of this article. S. G. is a Vanier Canada Graduate Scholar and acknowledges the support of NSERC via the Vanier CGS program. R. E. R. is supported by an NSERC Discovery grant. M. S. acknowledges supports from NASA/Chandra grant GO0-11063X and the Centre National d'Etudes Spatiales (CNES). The authors would like to thank Keith A. Arnaud and Craig Gordon for their precious help with the use of XSPEC and PyXSPEC. The authors are also very grateful toward Rene Breton for sharing his python implementation of the "Stretch-Move" algorithm. Finally, the authors also acknowledge the use of archived XMM and Chandra data from the High Energy Astrophysics Archive Research Center Online Service, provided by the NASA GSFC. NR 120 TC 107 Z9 109 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2013 VL 772 IS 1 AR 7 DI 10.1088/0004-637X/772/1/7 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700007 ER PT J AU Gupta, A Mathur, S Krongold, Y Nicastro, F AF Gupta, A. Mathur, S. Krongold, Y. Nicastro, F. TI DISCOVERY OF RELATIVISTIC OUTFLOW IN THE SEYFERT GALAXY Ark 564 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: Seyfert; quasars: absorption lines; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; VELOCITY IONIZED OUTFLOW; HOT INTERGALACTIC MEDIUM; ACCRETION DISC OUTFLOWS; X-RAY-SPECTRA; QUASAR FEEDBACK; CHANDRA HETGS; ARAKELIAN-564; MODEL; WINDS AB We present Chandra High Energy Transmission Grating Spectra of the narrow-line Seyfert-1 galaxy Ark 564. The spectrum shows numerous absorption lines which are well modeled with low-velocity outflow components usually observed in Seyfert galaxies. There are, however, some residual absorption lines which are not accounted for by low-velocity outflows. Here, we present identifications of the strongest lines as K alpha transitions of O VII (two lines) and O VI at outflow velocities of similar to 0.1c. These lines are detected at 6.9 sigma, 6.2 sigma, and 4.7 sigma, respectively, and cannot be due to chance statistical fluctuations. Photoionization models with ultra-high velocity components improve the spectral fit significantly, providing further support for the presence of relativistic outflow in this source. Without knowing the location of the absorber, its mass and energy outflow rates cannot be well constrained; we find (E) over dot (outflow)/L-bol lower limit of >= 0.006% assuming a bi-conical wind geometry. This is the first time that absorption lines with ultra-high velocities are unambiguously detected in the soft X-ray band. The presence of outflows with relativistic velocities in active galactic nuclei (AGNs) with Seyfert-type luminosities is hard to understand and provides valuable constraints to models of AGN outflows. Radiation pressure is unlikely to be the driving mechanism for such outflows and magnetohydrodynamic may be involved. C1 [Gupta, A.; Mathur, S.] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Krongold, Y.] Univ Nacl Autonoma Mexico, Inst Astron, Mexico City 04510, DF, Mexico. [Nicastro, F.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nicastro, F.] Osservatorio Astron Roma INAF, I-00040 Monte Porzio Catone, RM, Italy. [Mathur, S.] Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA. RP Gupta, A (reprint author), Ohio State Univ, Dept Astron, 174 W 18th Ave, Columbus, OH 43210 USA. EM agupta@astronomy.ohio-state.edu OI Nicastro, Fabrizio/0000-0002-6896-1364 FU National Aeronautics and Space Administration through Chandra Award issued by the Chandra X-ray Observatory Center [TM9-0010X]; National Aeronautics Space Administration [NAS8-03060]; CONACyT [168519]; UNAM-DGAPA [PAPIIT IN103712] FX Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number TM9-0010X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. YK acknowledges support from CONACyT 168519 grant and UNAM-DGAPA PAPIIT IN103712 grant. NR 36 TC 11 Z9 11 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2013 VL 772 IS 1 AR 66 DI 10.1088/0004-637X/772/1/66 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700066 ER PT J AU Lu, RS Fish, VL Akiyama, K Doeleman, SS Algaba, JC Bower, GC Brinkerink, C Chamberlin, R Crew, G Cappallo, RJ Dexter, M Freund, R Friberg, P Gurwell, MA Ho, PTP Honma, M Inoue, M Jorstad, SG Krichbaum, TP Loinard, L MacMahon, D Marrone, DP Marscher, AP Moran, JM Plambeck, R Pradel, N Primiani, R Tilanus, RPJ Titus, M Weintroub, J Wright, M Young, KH Ziurys, LM AF Lu, Ru-Sen Fish, Vincent L. Akiyama, Kazunori Doeleman, Sheperd S. Algaba, Juan C. Bower, Geoffrey C. Brinkerink, Christiaan Chamberlin, Richard Crew, Geoffrey Cappallo, Roger J. Dexter, Matt Freund, Robert Friberg, Per Gurwell, Mark A. Ho, Paul T. P. Honma, Mareki Inoue, Makoto Jorstad, Svetlana G. Krichbaum, Thomas P. Loinard, Laurent MacMahon, David Marrone, Daniel P. Marscher, Alan P. Moran, James M. Plambeck, Richard Pradel, Nicolas Primiani, Rurik Tilanus, Remo P. J. Titus, Michael Weintroub, Jonathan Wright, Melvyn Young, Ken H. Ziurys, Lucy M. TI FINE-SCALE STRUCTURE OF THE QUASAR 3C 279 MEASURED WITH 1.3 mm VERY LONG BASELINE INTERFEROMETRY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets; quasars: individual (3C 279); radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; SAGITTARIUS-A-ASTERISK; SUPERMASSIVE BLACK-HOLE; COMPACT RADIO-SOURCES; GHZ VLBI OBSERVATIONS; SUPERLUMINAL MOTION; RELATIVISTIC JET; HIGH-FREQUENCIES; 3C-279; KINEMATICS AB We report results from five day very long baseline interferometry observations of the well-known quasar 3C 279 at 1.3 mm (230 GHz) in 2011. The measured nonzero closure phases on triangles including stations in Arizona, California, and Hawaii indicate that the source structure is spatially resolved. We find an unusual inner jet direction at scales of similar to 1 pc extending along the northwest-southeast direction (P.A. = 127 degrees +/- 3 degrees), as opposed to other (previously) reported measurements on scales of a few parsecs showing inner jet direction extending to the southwest. The 1.3 mm structure corresponds closely with that observed in the central region of quasi-simultaneous super-resolution Very Long Baseline Array images at 7 mm. The closure phase changed significantly on the last day when compared with the rest of observations, indicating that the inner jet structure may be variable on daily timescales. The observed new direction of the inner jet shows inconsistency with the prediction of a class of jet precession models. Our observations indicate a brightness temperature of similar to 8 x 10(10) K in the 1.3 mm core, much lower than that at centimeter wavelengths. Observations with better uv coverage and sensitivity in the coming years will allow the discrimination between different structure models and will provide direct images of the inner regions of the jet with 20-30 mu as (5-7 light months) resolution. C1 [Lu, Ru-Sen; Fish, Vincent L.; Doeleman, Sheperd S.; Crew, Geoffrey; Cappallo, Roger J.; Titus, Michael] MIT, Haystack Observ, Westford, MA 01886 USA. [Akiyama, Kazunori; Honma, Mareki] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Akiyama, Kazunori] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. [Doeleman, Sheperd S.; Gurwell, Mark A.; Moran, James M.; Primiani, Rurik; Weintroub, Jonathan; Young, Ken H.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Algaba, Juan C.; Ho, Paul T. P.; Inoue, Makoto; Pradel, Nicolas] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Bower, Geoffrey C.; Dexter, Matt; MacMahon, David; Plambeck, Richard; Wright, Melvyn] Univ Calif Berkeley, Radio Astron Lab, Dept Astron, Berkeley, CA 94720 USA. [Brinkerink, Christiaan] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands. [Chamberlin, Richard] CALTECH, Submillimeter Observ, Hilo, HI 96720 USA. [Freund, Robert; Marrone, Daniel P.; Ziurys, Lucy M.] Univ Arizona, Steward Observ, Arizona Radio Observ, Tucson, AZ 85721 USA. [Friberg, Per; Tilanus, Remo P. J.] Joint Astron Ctr, James Clerk Maxwell Telescope, Hilo, HI 96720 USA. [Honma, Mareki] Grad Univ Adv Studies, Mitaka, Tokyo 1818588, Japan. [Jorstad, Svetlana G.; Marscher, Alan P.] Boston Univ, Inst Astrophys Res, Boston, MA 02215 USA. [Jorstad, Svetlana G.] St Petersburg State Univ, Astron Inst, St Petersburg 198504, Russia. [Krichbaum, Thomas P.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. [Loinard, Laurent] Univ Nacl Autonoma Mexico, Ctr Radiostron & Astrofis, Morelia 58089, Michoacan, Mexico. [Tilanus, Remo P. J.] Netherlands Org Sci Res, NL-2509 AC The Hague, Netherlands. RP Lu, RS (reprint author), MIT, Haystack Observ, Route 40, Westford, MA 01886 USA. EM rslu@haystack.mit.edu RI Jorstad, Svetlana/H-6913-2013; OI Jorstad, Svetlana/0000-0001-9522-5453; Marrone, Daniel/0000-0002-2367-1080; Akiyama, Kazunori/0000-0002-9475-4254; Moran, James/0000-0002-3882-4414 FU National Science Foundation (NSF); Smithsonian Institution; Academia Sinica; NSF ATI program [AST-0905844]; NSF URO program [AST-1140030]; NASA through the Fermi Guest Investigator Program; CONACyT, Mexico [104497]; DGAPA, UNAM [IN118110]; John Simon Guggenheim Memorial Foundation FX High-frequency VLBI work at MIT Haystack Observatory is supported by grants from the National Science Foundation (NSF). 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. High-frequency VLBI work at the Arizona Radio Observatory is partially supported through the NSF ATI (AST-0905844) and URO (AST-1140030) programs. This study makes use of 43 GHz VLBA data from the Boston University gamma-ray blazar monitoring program (http://www.bu.edu/blazars/VLBAproject.html), funded by NASA through the Fermi Guest Investigator Program. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. L. L. acknowledges the financial support of CONACyT, Mexico (project 104497) DGAPA, UNAM (project IN118110), and the John Simon Guggenheim Memorial Foundation (Fellowship 2010-2011). NR 42 TC 11 Z9 11 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2013 VL 772 IS 1 AR 13 DI 10.1088/0004-637X/772/1/13 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700013 ER PT J AU Martin, NF Slater, CT Schlafly, EF Morganson, E Rix, HW Bell, EF Laevens, BPM Bernard, EJ Ferguson, AMN Finkbeiner, DP Burgett, WS Chambers, KC Hodapp, KW Kaiser, N Kudritzki, RP Magnier, EA Morgan, JS Price, PA Tonry, JL Wainscoat, RJ AF Martin, Nicolas F. Slater, Colin T. Schlafly, Edward F. Morganson, Eric Rix, Hans-Walter Bell, Eric F. Laevens, Benjamin P. M. Bernard, Edouard J. Ferguson, Annette M. N. Finkbeiner, Douglas P. Burgett, William S. Chambers, Kenneth C. Hodapp, Klaus W. Kaiser, Nicholas Kudritzki, Rolf-Peter Magnier, Eugene A. Morgan, Jeffrey S. Price, Paul A. Tonry, John L. Wainscoat, Richard J. TI LACERTA I AND CASSIOPEIA III. TWO LUMINOUS AND DISTANT ANDROMEDA SATELLITE DWARF GALAXIES FOUND IN THE 3 pi PAN-STARRS1 SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (Andromeda XXXI, Andromeda XXXII, Cassiopeia III, Lacerta I); Local Group ID MILKY-WAY SATELLITES; SPHEROIDAL SATELLITE; BAYESIAN-APPROACH; LOCAL GROUP; M31; CALIBRATION; TRIANGULUM; EVOLUTION; DISCOVERY; SYSTEM AB We report the discovery of two new dwarf galaxies, Lacerta I/Andromeda XXXI (Lac I/And XXXI) and Cassiopeia III/Andromeda XXXII (Cas III/And XXXII), in stacked Pan-STARRS1 r(P1)- and i(P1)-band imaging data. Both are luminous systems (M-V similar to -12) located at projected distances of 20 degrees.3 and 10 degrees.5 from M31. Lac I and Cas III are likely satellites of the Andromeda galaxy with heliocentric distances of 756(-28)(+44) kpc and 772(-56)(+61) kpc, respectively, and corresponding M31-centric distances of 275 +/- 7 kpc and 144(-4)(+6) kpc. The brightest of recent Local Group member discoveries, these two new dwarf galaxies owe their late discovery to their large sizes (r(h) = 4.2(-0.5)(+0.4) arcminor 912(-93)(+124) pc for Lac I; r(h) = 6.5(-1.0)(+1.2) arcmin or 1456 +/- 267 pc for Cas III) and consequently low surface brightness (mu(0) similar to 26.0 mag arcsec(-2)), as well as to the lack of a systematic survey of regions at large radii from M31, close to the Galactic plane. This latter limitation is now alleviated by the 3 pi Pan-STARRS1 survey, which could lead to the discovery of other distant Andromeda satellite dwarf galaxies. C1 [Martin, Nicolas F.; Laevens, Benjamin P. M.] Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, F-67000 Strasbourg, France. [Martin, Nicolas F.; Schlafly, Edward F.; Morganson, Eric; Rix, Hans-Walter; Laevens, Benjamin P. M.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Slater, Colin T.; Bell, Eric F.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bernard, Edouard J.; Ferguson, Annette M. N.] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Finkbeiner, Douglas P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Burgett, William S.; Chambers, Kenneth C.; Hodapp, Klaus W.; Kaiser, Nicholas; Kudritzki, Rolf-Peter; Magnier, Eugene A.; Morgan, Jeffrey S.; Tonry, John L.; Wainscoat, Richard J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Price, Paul A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Martin, NF (reprint author), Univ Strasbourg, CNRS, Observ Astron Strasbourg, UMR 7550, 11 Rue Univ, F-67000 Strasbourg, France. EM nicolas.martin@astro.unistra.fr OI Bernard, Edouard/0000-0002-8722-225X FU CNRS through PICS project [PICS06183]; DFG [SFB 881]; NSF [AST 1008342]; National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; National Science Foundation [AST-1238877] FX N.F.M. gratefully acknowledges the CNRS for support through PICS project PICS06183. N.F.M. and H.-W.R. acknowledge support by the DFG through the SFB 881. C. T. S. and E. F. B. acknowledge support from NSF grant AST 1008342.; The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg, and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, Queen's University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation under grant No. AST-1238877, and the University of Maryland. NR 34 TC 42 Z9 43 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 20 PY 2013 VL 772 IS 1 AR 15 DI 10.1088/0004-637X/772/1/15 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700015 ER PT J AU Yen, HW Takakuwa, S Ohashi, N Ho, PTP AF Yen, Hsi-Wei Takakuwa, Shigehisa Ohashi, Nagayoshi Ho, Paul T. P. TI UNVEILING THE EVOLUTIONARY SEQUENCE FROM INFALLING ENVELOPES TO KEPLERIAN DISKS AROUND LOW-MASS PROTOSTARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; ISM: individual objects (B335, NGC 1333 IRAS 4B, L1448-mm, L1527 IRS, TMC-1A, L1489 IRS); ISM: kinematics and dynamics; ISM: molecules; stars: formation ID YOUNG STELLAR OBJECTS; CLASS-I PROTOSTARS; STAR-FORMATION EFFICIENCY; L1551 IRS 5; SUBMILLIMETER ARRAY; PROTOSTELLAR SYSTEM; CIRCUMSTELLAR DISKS; MAGNETIC BRAKING; DENSE CORES; CLOUD CORES AB We performed Submillimeter Array observations in the (CO)-O-18 (2-1) emission line toward six Class 0 and I protostars to study rotational motions of their surrounding envelopes and circumstellar material on 100-1000 AU scales. (CO)-O-18 (2-1) emission with intensity peaks located at the protostellar positions is detected toward all six sources. The rotational velocities of the protostellar envelopes as a function of radius were measured from the position-velocity diagrams perpendicular to the outflow directions passing through the protostellar positions. Two Class 0 sources, B335 and NGC 1333 IRAS 4B, show no detectable rotational motion, while L1527 IRS (Class 0/I) and L1448-mm (Class 0) exhibit rotational motions with radial profiles of V-rot proportional to r(-1.0 +/- 0.2) and proportional to r(-1.0 +/- 0.1), respectively. The other Class I sources, TMC-1A and L1489 IRS, exhibit the fastest rotational motions among the sample, and their rotational motions have flatter radial profiles of V-rot proportional to r(-0.6 +/- 0.1) and proportional to r(-0.5 +/- 0.1), respectively. The rotational motions with the radial dependence of similar to r(-1) can be interpreted as rotation with a conserved angular momentum in a dynamically infalling envelope, while those with the radial dependence of similar to r(-0.5) can be interpreted as Keplerian rotation. These observational results demonstrate categorization of rotational motions from infalling envelopes to Keplerian-disk formation. Models of the inside-out collapse where the angular momentum is conserved are discussed and compared with our observational results. C1 [Yen, Hsi-Wei] Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan. [Yen, Hsi-Wei; Takakuwa, Shigehisa; Ohashi, Nagayoshi; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Ohashi, Nagayoshi] Natl Inst Nat Sci, Natl Astron Observ Japan, Subaru Telescope, Hilo, HI 96720 USA. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Yen, HW (reprint author), Natl Taiwan Univ, Inst Astrophys, Taipei 10617, Taiwan. EM hwyen@asiaa.sinica.edu.tw FU Smithsonian Institute; Academia Sinica; National Science Council of Taiwan [NSC 99-2112-M-001-013-MY3]; NSC [99-2112-M-001-008-MY3] FX The Submillimeter Array (SMA) is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institute and the Academia Sinica.; We thank the anonymous referee for insightful comments and suggestions, and all the SMA staffs supporting this work. S. T. acknowledges a grant from the National Science Council of Taiwan (NSC 99-2112-M-001-013-MY3) in support of this work. The research of N.O. was partially supported by NSC 99-2112-M-001-008-MY3. NR 106 TC 29 Z9 29 U1 0 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 20 PY 2013 VL 772 IS 1 AR 22 DI 10.1088/0004-637X/772/1/22 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181NG UT WOS:000321673700022 ER PT J AU Dragomir, D Matthews, JM Eastman, JD Cameron, C Howard, AW Guenther, DB Kuschnig, R Moffat, AFJ Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Dragomir, Diana Matthews, Jaymie M. Eastman, Jason D. Cameron, Chris Howard, Andrew W. Guenther, David B. Kuschnig, Rainer Moffat, Anthony F. J. Rowe, Jason F. Rucinski, Slavek M. Sasselov, Dimitar Weiss, Werner W. TI MOST* DETECTS TRANSITS OF HD 97658b, A WARM, LIKELY VOLATILE-RICH SUPER-EARTH SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE planets and satellites: formation; planets and satellites: interiors; stars: individual (HD 97658); techniques: photometric ID Y-2 ISOCHRONES; EXOPLANETS; PHOTOMETRY; SPACE AB Through photometric monitoring of the extended transit window of HD 97658b with the MOST space telescope, we have found that this exoplanet transits with an ephemeris consistent with that predicted from radial velocity measurements. The mid-transit times are 5.6 sigma earlier than those of the unverified transit-like signals reported in 2011, and we find no connection between the two sets of events. The transit depth together with our determined stellar radius (R-star = 0.703(-0.034)(+0.039) R-circle dot) indicates a 2.34(-0.15)(+0.18) R-circle plus super-Earth. When combined with the radial velocity determined mass of 7.86 +/- 0.73 M-circle plus, our radius measure allows us to derive a planet density of 3.44(-0.82)(+0.91) g cm(-3). Models suggest that a planet with our measured density has a rocky core that is enveloped in an atmosphere composed of lighter elements. The star of the HD 97658 system is the second brightest known to host a transiting super-Earth, facilitating follow-up studies of this not easily daunted, warm and likely volatile-rich exoplanet. C1 [Dragomir, Diana; Eastman, Jason D.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Dragomir, Diana; Eastman, Jason D.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA USA. [Matthews, Jaymie M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Cameron, Chris] Cape Breton Univ, Dept Math Phys & Geol, Sydney, NS B1P 6L2, Canada. [Howard, Andrew W.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Guenther, David B.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Kuschnig, Rainer; Weiss, Werner W.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Moffat, Anthony F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Moffat, Anthony F. J.] Obs Mont Megant, Notre Dame Des Bois, PQ J0B 2E0, Canada. [Rowe, Jason F.] SETI Inst, Mountain View, CA 94043 USA. [Rowe, Jason F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, Slavek M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Dragomir, D (reprint author), Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr Suite 102, Goleta, CA 93117 USA. EM diana@lcogt.net RI Howard, Andrew/D-4148-2015; OI Howard, Andrew/0000-0001-8638-0320; Eastman, Jason/0000-0003-3773-5142; Dragomir, Diana/0000-0003-2313-467X FU Natural Sciences and Engineering Research Council of Canada; FQRNT (Quebec); Austrian Science Fund [P22691-N16]; Austrian Research Promotion Agency-ALR FX The Natural Sciences and Engineering Research Council of Canada supports the research of D.B.G., J.M.M., A.F.J.M., and S.M.R. Additional support for A.F.J.M. comes from FQRNT (Quebec). R.K. and W.W.W. were supported by the Austrian Science Fund (P22691-N16) and by the Austrian Research Promotion Agency-ALR. NR 21 TC 31 Z9 31 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 JUL 20 PY 2013 VL 772 IS 1 AR L2 DI 10.1088/2041-8205/772/1/L2 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181VC UT WOS:000321696500002 ER PT J AU Kunert-Bajraszewska, M Siemiginowska, A Labiano, A AF Kunert-Bajraszewska, M. Siemiginowska, A. Labiano, A. TI AN X-RAY COOLING-CORE CLUSTER SURROUNDING A LOW-POWER COMPACT STEEP SPECTRUM RADIO SOURCE 1321+045 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: clusters: general; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; DIGITAL SKY SURVEY; STAR-FORMATION; EMITTING GAS; GALAXIES; EMISSION; FEEDBACK; STATISTICS; ACCRETION; EVOLUTION AB We discovered an X-ray cluster in a Chandra observation of the compact steep spectrum (CSS) radio source 1321+045 (z = 0.263). CSS sources are thought to be young radio objects at the beginning of their evolution and can potentially test the cluster heating process. 1321+045 is a relatively low-luminosity source and its morphology consists of two radio lobes on the opposite sides of a radio core with no evidence for jets or hotspots. The optical emission line ratios are consistent with an interstellar medium dominated by active galactic nucleus photoionization with a small contribution from star formation, and no contributions from shocks. Based on these ratios, we classify 1321+045 as a low excitation galaxy (LEG) and suggest that its radioactivity is in a coasting phase. The X-ray emission associated with the radio source is detected with 36.1 +/- 8.3 counts, but the origin of this emission is highly uncertain. The current X-ray image of the cluster does not show any signatures of a radio source impact on the cluster medium. Chandra detects the cluster emission at >3 sigma level out to similar to 60 '' (240 kpc). We obtain the best-fit beta model parameters of the surface brightness profile of beta = 0.58 +/- 0.2 and a core radius of 9.4(-0.9)(+1.1) arcsec. The average temperature of the cluster is equal to kT = 4.4(-0.3)(+0.5) keV, with a temperature and cooling profile indicative of a cooling core. We measure the cluster luminosity L(0.5-2 keV) = 3 x 10(44) erg s(-1) and mass 1.5 x 10(14) M-circle dot. C1 [Kunert-Bajraszewska, M.] Nicholas Copernicus Univ, Fac Phys Astron & Informat, Torun Ctr Astron, PL-87100 Torun, Poland. [Siemiginowska, A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Labiano, A.] Ctr Astrobiol CSIC INTA, E-28850 Madrid, Spain. RP Kunert-Bajraszewska, M (reprint author), Nicholas Copernicus Univ, Fac Phys Astron & Informat, Torun Ctr Astron, Grudziacka 5, PL-87100 Torun, Poland. EM magda@astro.uni.torun.pl RI Kunert-Bajraszewska, Magdalena/F-9060-2014 FU NASA [NAS8-03060]; Chandra grants [GO1-12124X] FX This research has made use of data obtained by the Chandra X-ray Observatory, and Chandra X-ray Center (CXC) in the application packages CIAO, ChIPS, and Sherpa. This research is funded in part by NASA contract NAS8-03060. Partial support for this work was provided by the Chandra grants GO1-12124X. NR 38 TC 3 Z9 3 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 20 PY 2013 VL 772 IS 1 AR L7 DI 10.1088/2041-8205/772/1/L7 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181VC UT WOS:000321696500007 ER PT J AU Crassard, R Petraglia, MD Parker, AG Parton, A Roberts, RG Jacobs, Z Alsharekh, A Al-Omari, A Breeze, P Drake, NA Groucutt, HS Jennings, R Regagnon, E Shipton, C AF Crassard, Remy Petraglia, Michael D. Parker, Adrian G. Parton, Ash Roberts, Richard G. Jacobs, Zenobia Alsharekh, Abdullah Al-Omari, Abdulaziz Breeze, Paul Drake, Nick A. Groucutt, Huw S. Jennings, Richard Regagnon, Emmanuelle Shipton, Ceri TI Beyond the Levant: First Evidence of a Pre-Pottery Neolithic Incursion into the Nefud Desert, Saudi Arabia SO PLOS ONE LA English DT Article ID HOLOCENE HUMID PERIOD; RUB AL-KHALI; NEAR-EAST; AGRICULTURAL ORIGINS; SOUTHERN ARABIA; CAL BC; SEDIMENTS; DOMESTICATION; PLEISTOCENE; PREHISTORY AB Pre-Pottery Neolithic assemblages are best known from the fertile areas of the Mediterranean Levant. The archaeological site of Jebel Qattar 101 (JQ-101), at Jubbah in the southern part of the Nefud Desert of northern Saudi Arabia, contains a large collection of stone tools, adjacent to an Early Holocene palaeolake. The stone tool assemblage contains lithic types, including El-Khiam and Helwan projectile points, which are similar to those recorded in Pre-Pottery Neolithic A and Pre-Pottery Neolithic B assemblages in the Fertile Crescent. Jebel Qattar lies similar to 500 kilometres outside the previously identified geographic range of Pre-Pottery Neolithic cultures. Technological analysis of the typologically diagnostic Jebel Qattar 101 projectile points indicates a unique strategy to manufacture the final forms, thereby raising the possibility of either direct migration of Levantine groups or the acculturation of mobile communities in Arabia. The discovery of the Early Holocene site of Jebel Qattar suggests that our view of the geographic distribution and character of Pre-Pottery Neolithic cultures may be in need of revision. C1 [Crassard, Remy; Regagnon, Emmanuelle] CNRS, UMR Archeorient 5133, Lyon, France. [Petraglia, Michael D.; Parton, Ash; Groucutt, Huw S.; Jennings, Richard] Univ Oxford, Sch Archaeol, Res Lab Archaeol & Hist Art, Oxford, England. [Petraglia, Michael D.] Smithsonian Inst, Human Origins Program, Washington, DC 20560 USA. [Parker, Adrian G.] Oxford Brookes Univ, Human Origins & Palaeoenvironm Res Grp, Oxford OX3 0BP, England. [Roberts, Richard G.; Jacobs, Zenobia] Univ Wollongong, Ctr Archaeol Sci, Sch Earth & Environm Sci, Wollongong, NSW, Australia. [Alsharekh, Abdullah] King Saud Univ, Coll Tourism & Archaeol, Dept Archaeol, Riyadh, Saudi Arabia. [Alsharekh, Abdullah] Minist Higher Educ, Riyadh, Saudi Arabia. [Al-Omari, Abdulaziz] Saudi Commiss Tourism & Antiqu, Taif Antiqu Off, At Taif, Saudi Arabia. [Breeze, Paul; Drake, Nick A.] Kings Coll London, Dept Geog, London, England. [Shipton, Ceri] Univ Queensland, Sch Social Sci, Brisbane, Qld 4072, Australia. RP Crassard, R (reprint author), CNRS, UMR Archeorient 5133, Lyon, France. EM remy.crassard@mom.fr OI Jennings, Richard/0000-0001-9996-7518; Crassard, Remy/0000-0002-2403-1894 FU National Geographic Society; Leakey Foundation; European Research Council [295719]; Australian Research Council; Fondation Fyssen ('Subvention de Recherche') FX This research was funded by the National Geographic Society (to MDP), the Leakey Foundation (to MDP), the European Research Council (number 295719, to MDP), the Australian Research Council (to RGR and ZJ) and the Fondation Fyssen ('Subvention de Recherche 2013', to RC). The authors acknowledge the Australian Research Council for OSL sample collection and dating through laboratory analysis. The funders had no role in the study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 127 TC 31 Z9 31 U1 0 U2 19 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 19 PY 2013 VL 8 IS 7 AR e68061 DI 10.1371/journal.pone.0068061 PG 20 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 191CY UT WOS:000322391400004 PM 23894294 ER PT J AU Reale, F Orlando, S Testa, P Peres, G Landi, E Schrijver, CJ AF Reale, Fabio Orlando, Salvatore Testa, Paola Peres, Giovanni Landi, Enrico Schrijver, Carolus J. TI Bright Hot Impacts by Erupted Fragments Falling Back on the Sun: A Template for Stellar Accretion SO SCIENCE LA English DT Article ID T-TAURI STARS; X-RAY SPECTROSCOPY; DISK ACCRETION; HYDRAE; EMISSION; SHOCKS; DIAGNOSTICS; PLASMA AB Impacts of falling fragments observed after the eruption of a filament in a solar flare on 7 June 2011 are similar to those inferred for accretion flows on young stellar objects. As imaged in the ultraviolet (UV)-extreme UV range by the Atmospheric Imaging Assembly onboard the Solar Dynamics Observatory, many impacts of dark, dense matter display uncommonly intense, compact brightenings. High-resolution hydrodynamic simulations show that such bright spots, with plasma temperatures increasing from similar to 10(4) to similar to 10(6) kelvin, occur when high-density plasma (>>10(10) particles per cubic centimeter) hits the solar surface at several hundred kilometers per second, producing high-energy emission as in stellar accretion. The high-energy emission comes from the original fragment material and is heavily absorbed by optically thick plasma, possibly explaining the lower mass accretion rates inferred from x-rays relative to UV-optical-near infrared observations of young stars. C1 [Reale, Fabio; Peres, Giovanni] Univ Palermo, Dipartimento Fis & Chim, I-90134 Palermo, Italy. [Reale, Fabio; Orlando, Salvatore; Peres, Giovanni] Osserv Astron Palermo, Ist Nazl Astrofis INAF, I-90134 Palermo, Italy. [Testa, Paola] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Landi, Enrico] Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. [Schrijver, Carolus J.] Lockheed Martin Adv Technol Ctr, Palo Alto, CA 94304 USA. RP Reale, F (reprint author), Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy. EM reale@astropa.unipa.it RI Landi, Enrico/H-4493-2011; OI PERES, Giovanni/0000-0002-6033-8180; Orlando, Salvatore/0000-0003-2836-540X; Reale, Fabio/0000-0002-1820-4824 FU Italian Ministero dell'Universita e Ricerca; Agenzia Spaziale Italiana [I/023/09/0]; Lockheed-Martin [SP02H1701R]; NASA [NNG04EA00C, NNX11AC20G, NNX10AQ58G]; NSF [AGS-1154443]; INAF; U.S. Department of Energy; CINECA [HP10CEG9MW]; INAF/Osservatorio Astronomico di Palermo FX We thank B. De Pontieu for help and suggestions. F. R., G. P., and S.O. acknowledge support from Italian Ministero dell'Universita e Ricerca and Agenzia Spaziale Italiana, contract I/023/09/0. P. T. was supported by contract SP02H1701R from Lockheed-Martin to the Smithsonian Astrophysical Observatory. P. T. and C.J.S. are supported by NASA contract NNG04EA00C for the SDO AIA. E. L. is supported by NASA grants NNX11AC20G and NNX10AQ58G and NSF grant AGS-1154443. S.O. acknowledges partial support from the INAF. The software used in this work was, in part, developed by the U.S. Department of Energy-supported Advanced Simulation and Computing/Alliance Center for Astrophysical Thermonuclear Flashes at the University of Chicago. We acknowledge the CINECA Award HP10CEG9MW and INAF/Osservatorio Astronomico di Palermo for high-performance computing resources and support. SDO data were supplied courtesy of the SDO/HMI and SDO/AIA consortia. SDO is the first mission to be launched for NASA's Living With a Star Program. See the supplementary materials for details on the data, data analysis, and modeling. NR 26 TC 26 Z9 26 U1 0 U2 7 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JUL 19 PY 2013 VL 341 IS 6143 BP 251 EP 253 DI 10.1126/science.1235692 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 185HV UT WOS:000321959300035 PM 23788734 ER PT J AU Taylor, RC Ryan, MJ AF Taylor, R. C. Ryan, M. J. TI Interactions of Multisensory Components Perceptually Rescue Tungara Frog Mating Signals SO SCIENCE LA English DT Article ID BEHAVIOR; COMMUNICATION; INFERENCE; SELECTION; CHOICE AB Sexual signals are often complex and perceived by multiple senses. How animals integrate signal components across sensory modalities can influence signal evolution. Here we show that two relatively unattractive signals that are perceived acoustically and visually can be combined in a pattern to form a signal that is attractive to female tungara frogs. Such unanticipated perceptual effects suggest that the evolution of complex signals can occur by alteration of the relationships among already-existing traits. C1 [Taylor, R. C.] Salisbury Univ, Dept Biol, Salisbury, MD 21801 USA. [Ryan, M. J.] Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. [Ryan, M. J.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Ryan, MJ (reprint author), Univ Texas Austin, Sect Integrat Biol, Austin, TX 78712 USA. EM mryan@utexas.edu FU NSF [IBN 0517328, IBN 0078150, IOS 1120031]; Clark Hubbs Regents Professorship FX We are grateful to the NSF (grants IBN 0517328, IBN 0078150, and IOS 1120031) and the Clark Hubbs Regents Professorship (M.J.R.) for funding and the Smithsonian Tropical Research Institute for logistical support. We thank E. Balaban for helpful discussion and H. Farris, S. Partan, S. Pika, G. Rosenthal, and three anonymous reviewers for their comments on the manuscript. We thank B. Klein and Moey, Incorporated for design and fabrication of the robotic frogs. We are especially grateful to the interns who assisted in data collection. All research reported here complied with IACUC protocols from Salisbury University, the University of Texas, and the Smithsonian Tropical Research Institute. We obtained all required permits from the Government of Panama. Data will be archived in the Dryad Data Repository at dx.doi.org/10.5061/dryad.pk85. NR 24 TC 26 Z9 26 U1 2 U2 51 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 JUL 19 PY 2013 VL 341 IS 6143 BP 273 EP 274 DI 10.1126/science.1237113 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 185HV UT WOS:000321959300042 PM 23744778 ER PT J AU Cairns, SD Zibrowius, H AF Cairns, Stephen D. Zibrowius, Helmut TI Stylasteridae (Cnidaria, Hydrozoa, Filifera) from South Africa SO ZOOTAXA LA English DT Article DE Cnidaria; Stylasteridae; South Africa; new species; zoogeography; Pedicularia ID GENERIC REVISION; COELENTERATA; WATER AB We describe and figure the 20 species of stylasterid hydrozoans known from South Africa. These consist of seven new species, six range extensions, and seven species previously known from South African. Most of the specimens reported resulted from expeditions of the Pieter Faure (1898-1903) and Meiring Naude (1975-1987), and are deposited primarily in the South African Museum (Cape Town). A replacement name (Errina australis) is proposed for the junior homonym Errina hicksoni Cairns, 1991. A brief history of species discovery of the South African stylasterids is presented. The new morphological term dactyloglossa is introduced to define a baffle-like structure found in dactylopores of some species. Of the 20 South African species, 12 (60%) are not yet known outside that area. Three patterns of distribution were noted: species confined to the tropical region of South Africa, those found in both the tropical and warm temperate regions of S. Africa, and those found only in the warm temperate regions, three in the latter group sharing their distribution with cold temperate southern South America and two with warm temperate New Zealand, representing a circum-southern temperate distribution. C1 [Cairns, Stephen D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. [Zibrowius, Helmut] Ctr Oceanol Marseille, Marine Endoume Stn, F-13007 Marseille, France. RP Cairns, SD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. EM cairnss@si.edu; helmut.zibrowius@orange.fr NR 78 TC 3 Z9 3 U1 2 U2 10 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1175-5326 EI 1175-5334 J9 ZOOTAXA JI Zootaxa PD JUL 18 PY 2013 VL 3691 IS 1 BP 1 EP 57 PG 57 WC Zoology SC Zoology GA 184LF UT WOS:000321890400001 PM 26167568 ER PT J AU Zhang, JB Li, RQ Xiang, XG Manchester, SR Lin, L Wang, W Wen, J Chen, ZD AF Zhang, Jing-Bo Li, Rui-Qi Xiang, Xiao-Guo Manchester, Steven R. Lin, Li Wang, Wei Wen, Jun Chen, Zhi-Duan TI Integrated Fossil and Molecular Data Reveal the Biogeographic Diversification of the Eastern Asian-Eastern North American Disjunct Hickory Genus (Carya Nutt.) SO PLOS ONE LA English DT Article ID ATLANTIC LAND-BRIDGE; DIVERGENCE TIMES; TIBETAN PLATEAU; HISTORICAL BIOGEOGRAPHY; PHYLOGENETIC INFERENCE; POSTGLACIAL EXPANSION; GEOGRAPHIC RANGE; PLANT DIVERSITY; MASS EXTINCTION; MIXED MODELS AB The hickory genus (Carya) contains ca. 17 species distributed in subtropical and tropical regions of eastern Asia and subtropical to temperate regions of eastern North America. Previously, the phylogenetic relationships between eastern Asian and eastern North American species of Carya were not fully confirmed even with an extensive sampling, biogeographic and diversification patterns had thus never been investigated in a phylogenetic context. We sampled 17 species of Carya and 15 species representing all other genera of the Juglandaceae as outgroups, with eight nuclear and plastid loci to reconstruct the phylogeny of Carya. The phylogenetic positions of seven extinct genera of the Juglandaceae were inferred using morphological characters and the molecular phylogeny as a backbone constraint. Divergence times within Carya were estimated with relaxed Bayesian dating. Biogeographic analyses were performed in DIVA and LAGRANGE. Diversification rates were inferred by LASER and APE packages. Our results support two major clades within Carya, corresponding to the lineages of eastern Asia and eastern North America. The split between the two disjunct clades is estimated to be 21.58 (95% HPD 11.07-35.51) Ma. Genus-level DIVA and LAGRANGE analyses incorporating both extant and extinct genera of the Juglandaceae suggested that Carya originated in North America, and migrated to Eurasia during the early Tertiary via the North Atlantic land bridge. Fragmentation of the distribution caused by global cooling in the late Tertiary resulted in the current disjunction. The diversification rate of hickories in eastern North America appeared to be higher than that in eastern Asia, which is ascribed to greater ecological opportunities, key morphological innovations, and polyploidy. C1 [Zhang, Jing-Bo; Li, Rui-Qi; Xiang, Xiao-Guo; Lin, Li; Wang, Wei; Chen, Zhi-Duan] Chinese Acad Sci, Inst Bot, State Key Lab Systemat & Evolutionary Bot, Beijing, Peoples R China. [Manchester, Steven R.] Univ Florida, Florida Museum Nat Hist, Gainesville, FL 32611 USA. [Wen, Jun] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Wen, J (reprint author), Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20560 USA. EM wenj@si.edu; zhiduan@ibcas.ac.cn FU National Natural Science Foundation of China [NNSF 31270268, NNSF 31061160184]; Chinese Academy of Sciences [2011T1S24] FX This work was supported by the National Natural Science Foundation of China (NNSF 31270268 and NNSF 31061160184) and Chinese Academy of Sciences Visiting Professorship for Senior International Scientists (2011T1S24). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 124 TC 17 Z9 18 U1 5 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 JUL 16 PY 2013 VL 8 IS 7 AR e70449 DI 10.1371/journal.pone.0070449 PG 13 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 186SF UT WOS:000322064300130 PM 23875028 ER PT J AU Bai, F Chisholm, R Sang, WG Dong, M AF Bai, Fan Chisholm, Ryan Sang, Weiguo Dong, Ming TI Spatial Risk Assessment of Alien Invasive Plants in China SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID CLIMATE-CHANGE; BIOLOGICAL INVASIONS; INTERNATIONAL-TRADE; GEOGRAPHICAL ORIGIN; PROPAGULE PRESSURE; NORTHERN CHINA; INVASIBILITY; DIVERSITY; DISTURBANCE; VEGETATION AB The large-scale distribution patterns of alien invasive plants (AIP) can provide key information and a theoretical basis for management strategies, including the prevention of invasions, the control and eradication of established AIPs, and the identification of areas at high risk of invasion. This study aims to quantify distribution patterns of AIP in China, to develop approaches that measure the social, economic, and ecological impacts, and to identify areas that are at higher risk of plant invasion. Based on published literature, there were 384 AIPs in China, representing 233 genera from 66 families. Climatic factors were among the primary factors determining AIPs overall distribution patterns. The majority of AIPs were tropically distributed in China, meaning that they were mainly restricted to southern China. Temperate-distributed AIPs, those distributed only or predominantly in northern China, were fewer but had higher average rates of spread than tropically distributed AIPs. Average ecological and economic impact per AIP was negatively correlated with AIP richness, meaning that areas with relatively few AIPs nevertheless have some of the most detrimental ones. Our comparative evaluation showed that the risk of invasion differed among regions of China, with high-risk areas in southern China (Yunnan, Guangxi, and Guangdong) and central coastal areas of eastern China (Shandong, Hebei, and Jiangsu). In the context of climate change, areas around latitudes of 33 degrees N, including Hebei, Shandong, Henan, and Jiangsu, should be given more attention for the control and prevention of plant invasions. Predictions of high-risk areas for future invasions differed depending on the scale of aggregation and the evaluation index, indicating that invasive risk assessments should be based on multiple factors. C1 [Bai, Fan; Sang, Weiguo; Dong, Ming] Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. [Chisholm, Ryan] Natl Univ Singapore, Fac Sci, Dept Biol Sci, Singapore 117543, Singapore. [Chisholm, Ryan] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Sang, WG (reprint author), Chinese Acad Sci, Inst Bot, State Key Lab Vegetat & Environm Change, Beijing 100093, Peoples R China. EM swg@ibcas.ac.cn; dongming@ibcas.ac.cn RI Chisholm, Ryan/H-8033-2012 FU Public Environment Benefits Programme of Ministry of Environment Protection [201209027-2]; 111 Program of the Bureau of China Foreign Experts and Ministry of Education [2008-B08044]; National Basic Research Program of China (973 Program) [2009CB119200]; Chinese Academy of Science [2011T2S18]; U.S. NSF [DEB-1046113] FX This study was supported by the grants the "Public Environment Benefits Programme" of Ministry of Environment Protection (201209027-2), the "111 Program" of the Bureau of China Foreign Experts and Ministry of Education (2008-B08044), National Basic Research Program of China (973 Program 2009CB119200), and the Chinese Academy of Science and their Fellowship for International Scientists Programme (2011T2S18). Many critical comments on the manuscript were received in the 2012 Smithsonian CTFS/SIGEO and CForBio Workshop in Seattle (U.S. NSF grant DEB-1046113). We greatly appreciate the many useful criticisms and comments that the reviewers have provided. NR 64 TC 8 Z9 11 U1 4 U2 63 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD JUL 16 PY 2013 VL 47 IS 14 BP 7624 EP 7632 DI 10.1021/es400382c PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 186QS UT WOS:000322059800009 PM 23738912 ER PT J AU Lamsal, LN Martin, RV Parrish, DD Krotkov, NA AF Lamsal, L. N. Martin, R. V. Parrish, D. D. Krotkov, N. A. TI Scaling Relationship for NO2 Pollution and Urban Population Size: A Satellite Perspective SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID OZONE MONITORING INSTRUMENT; FINE PARTICULATE MATTER; UNITED-STATES; NITROGEN-DIOXIDE; AIR-POLLUTION; NORTH-AMERICA; GLOBAL BURDEN; POWER-PLANTS; EMISSIONS; MORTALITY AB Concern is growing about the effects of urbanization on air pollution and health. Nitrogen dioxide (NO2) released primarily from combustion processes, such as traffic, is a short-lived atmospheric pollutant that serves as an air-quality indicator and is itself a health concern. We derive a global distribution of ground-level NO2 concentrations from tropospheric NO2 columns retrieved from the Ozone Monitoring Instrument (OMI). Local scaling factors from a three-dimensional chemistry-transport model (GEOS-Chem) are used to relate the OMI NO2 columns to ground-level concentrations. The OMI-derived surface NO2 data are significantly correlated (r = 0.69) with in situ surface measurements. We examine how the OMI-derived ground-level NO2 concentrations, OMI NO2 columns, and bottom-up NOx emission inventories relate to urban population. Emission hot spots, such as power plants, are excluded to focus on urban relationships. The correlation of surface NO2 with population is significant for the three countries and one continent examined here: United States (r = 0.71), Europe (r = 0.67), China (r = 0.69), and India (r = 0.59). Urban NO2 pollution, like other urban properties, is a power law scaling function of the population size: NO2 concentration increases proportional to population raised to an exponent. The value of the exponent varies by region from 0.36 for India to 0.66 for China, reflecting regional differences in industrial development and per capita emissions. It has been generally established that energy efficiency increases and, therefore, per capita NO emissions decrease with urban population; here, we show how outdoor ambient NO2 concentrations depend upon urban population in different global regions. C1 [Lamsal, L. N.] Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA. [Lamsal, L. N.; Krotkov, N. A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Martin, R. V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Martin, R. V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Parrish, D. D.] NOAA, Earth Syst Res Lab, Div Chem Sci, Boulder, CO 80305 USA. RP Lamsal, LN (reprint author), Univ Space Res Assoc, Goddard Earth Sci Technol & Res, Columbia, MD 21044 USA. EM lok.lamsal@nasa.gov RI Martin, Randall/C-1205-2014; Chem, GEOS/C-5595-2014; Parrish, David/E-8957-2010; Krotkov, Nickolay/E-1541-2012; Manager, CSD Publications/B-2789-2015 OI Martin, Randall/0000-0003-2632-8402; Parrish, David/0000-0001-6312-2724; Krotkov, Nickolay/0000-0001-6170-6750; FU NASA's Earth Science Directorate Atmospheric Composition Program; Natural Sciences and Engineering Research Council of Canada FX We thank Aaron van Donkelaar for performing the GEOS-Chem nested simulation. The work was supported by NASA's Earth Science Directorate Atmospheric Composition Program and the Natural Sciences and Engineering Research Council of Canada. NR 53 TC 36 Z9 39 U1 5 U2 87 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD JUL 16 PY 2013 VL 47 IS 14 BP 7855 EP 7861 DI 10.1021/es400744g PG 7 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 186QS UT WOS:000322059800036 PM 23763377 ER PT J AU Nadel, D Danin, A Power, RC Rosen, AM Bocquentin, F Tsatskin, A Rosenberg, D Yeshurun, R Weissbrod, L Rebollo, NR Barzilai, O Boaretto, E AF Nadel, Dani Danin, Avinoam Power, Robert C. Rosen, Arlene M. Bocquentin, Fanny Tsatskin, Alexander Rosenberg, Danny Yeshurun, Reuven Weissbrod, Lior Rebollo, Noemi R. Barzilai, Omry Boaretto, Elisabetta TI Earliest floral grave lining from 13,700-11,700-y-old Natufian burials at Raqefet Cave, Mt. Carmel, Israel SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE burial customs; preburial preparation; radiocarbon dates ID NEANDERTHAL BURIAL; LEVANT; ORIGINS AB Flowering plants possess mechanisms that stimulate positive emotional and social responses in humans. It is difficult to establish when people started to use flowers in public and ceremonial events because of the scarcity of relevant evidence in the archaeological record. We report on uniquely preserved 13,700-11,700-y-old grave linings made of flowers, suggesting that such use began much earlier than previously thought. The only potentially older instance is the questionable use of flowers in the Shanidar IV Neanderthal grave. The earliest cemeteries (ca. 15,000-11,500 y ago) in the Levant are known from Natufian sites in northern Israel, where dozens of burials reflect a wide range of inhumation practices. The newly discovered flower linings were found in four Natufian graves at the burial site of Raqefet Cave, Mt. Carmel, Israel. Large identified plant impressions in the graves include stems of sage and other Lamiaceae (Labiatae; mint family) or Scrophulariaceae (figwort family) species; accompanied by a plethora of phytoliths, they provide the earliest direct evidence now known for such preparation and decoration of graves. Some of the plant species attest to spring burials with a strong emphasis on colorful and aromatic flowers. Cave floor chiseling to accommodate the desired grave location and depth is also evident at the site. Thus, grave preparation was a sophisticated planned process, embedded with social and spiritual meanings reflecting a complex preagricultural society undergoing profound changes at the end of the Pleistocene. C1 [Nadel, Dani; Tsatskin, Alexander; Rosenberg, Danny; Yeshurun, Reuven; Weissbrod, Lior] Univ Haifa, Zinman Inst Archaeol, IL-91905 Jerusalem, Israel. [Danin, Avinoam] Hebrew Univ Jerusalem, IL-91904 Jerusalem, Israel. [Power, Robert C.] Max Planck Inst Evolutionare Anthropol, Plant Foods & Hominin Dietary Ecol Res Grp, D-04103 Leipzig, Germany. [Rosen, Arlene M.] Univ Texas Austin, Dept Anthropol, Austin, TX 78712 USA. [Bocquentin, Fanny] CNRS, USR 3132, Ctr Rech Francais Jerusalem, F-75794 Paris, France. [Yeshurun, Reuven] Smithsonian Inst, Natl Museum Nat Hist, Program Human Ecol & Archaeobiol, Washington, DC 20560 USA. [Rebollo, Noemi R.; Barzilai, Omry; Boaretto, Elisabetta] Weizmann Inst Sci, Weizmann Inst, Max Planck Ctr Integrat Archaeol, Dangoor Res Accelerator Mass Spectrometer Radioca, IL-76100 Rehovot, Israel. RP Nadel, D (reprint author), Univ Haifa, Zinman Inst Archaeol, IL-91905 Jerusalem, Israel. EM dnadel@research.haifa.ac.il RI Yeshurun, Reuven/A-3182-2013; OI Weissbrod, Lior/0000-0003-3401-8180 FU National Geographic Society [8915-11]; Wenner-Gren Foundation [7481]; Irene Levi-Sala CARE Foundation; Israel Science Foundation [475/10] FX We thank G. Bar-Oz, A. Belfer-Cohen, L. Conyers, S. Filin, I. Hershkovitz, D. Kaufman, G. Lengyel, M. Weinstein-Evron, A. Weisskopf, and D. Bruggeman for their support, comments and advice; R. Shafir and T.R. Sevi for laboratory and field assistance; E. Mintz for help in sample preparation; and A. Lambert and G. Bosset, who also assisted in field work. Digital figures were prepared by A. Regev. Photographs were taken by E. Bartov (Fig. S4B), A. Danin (Fig. 4B), R. Power (Fig. 4 C and D), M. Eisenberg (Fig. S2 C and D), and E. Gerstein (Figs. 2A, 3AB. 4A, S1 A, B, C, and D, S2 A and B, S3 A and C). Field work was conducted under permits from the Israel Antiquities Authority and the Israel Nature and Parks Authority. This project was supported by Grant 8915-11 from the National Geographic Society, Grant 7481 from the Wenner-Gren Foundation, and the Irene Levi-Sala CARE Foundation. Radiocarbon dating was funded by Grant 475/10 from the Israel Science Foundation (to E. B.). NR 37 TC 16 Z9 16 U1 1 U2 44 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 16 PY 2013 VL 110 IS 29 BP 11774 EP 11778 DI 10.1073/pnas.1302277110 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 187AB UT WOS:000322086100037 PM 23818584 ER PT J AU Zhou, Q Herd, CDK Yin, QZ Li, XH Wu, FY Li, QL Liu, Y Tang, GQ McCoy, TJ AF Zhou, Qin Herd, Christopher D. K. Yin, Qing-Zhu Li, Xian-Hua Wu, Fu-Yuan Li, Qiu-Li Liu, Yu Tang, Guo-Qiang McCoy, Timothy J. TI Geochronology of the Martian meteorite Zagami revealed by U-Pb ion probe dating of accessory minerals SO EARTH AND PLANETARY SCIENCE LETTERS LA English DT Article DE Mars; geochronology; shergottite; uranium-lead; baddeleyite ID ISOTOPIC SYSTEMATICS; SNC METEORITES; RB-SR; DIFFERENTIATION HISTORY; MARS; SHERGOTTY; SHOCK; AGES; CRYSTALLIZATION; PETROGENESIS AB The precise chronology of geological events on Mars is hampered by the lack of absolute ages for the Martian timescale, and the significant uncertainties that result from the extrapolation of the lunar timescale to Mars (Hartmann and Neukum, 2001). Martian meteorites represent the only samples of Mars currently available. Attempts to identify source craters for the meteorites have thus far proven inconclusive (Hamilton et al., 2003; Lang et al., 2009; Mouginis-Mark and Boyce, 2012), precluding their use in constraining the absolute Martian timescale. The majority of the known Martian meteorites are basalts ("shergottites"); all dated shergottites have mineral separate (Rb-Sr or Sm-Nd) ages of <600 Ma (Borg et al., 2005). Here we report a U-238/Pb-206 age of 182.7 +/- 6.9 Ma by ion microprobe analysis of baddeleyite (ZrO2) grains in the Zagami shergottite. There is no correlation between discordancy and baddeleyite grain location relative to shock metamorphism. Mineral petrography demonstrates that baddeleyite is the result of late-stage igneous crystallization, and Raman spectroscopy shows that baddeleyite has not been transformed by shock into preservable high-pressure polymorphs. Supported by an age of 153 +/- 81 Ma for phosphate grains, obtained using the same method, we conclude that Zagami crystallized at similar to 180 Ma, in agreement with previous results from mineral separate geochronology. Therefore, the shergottites represent igneous rocks preferentially ejected from young terrains on Mars in a small number of ejection events. (C) 2013 Elsevier B.V. All rights reserved. C1 [Zhou, Qin; Li, Xian-Hua; Wu, Fu-Yuan; Li, Qiu-Li; Liu, Yu; Tang, Guo-Qiang] Chinese Acad Sci, Inst Geol & Geophys, State Key Lab Lithospher Evolut, Beijing 100029, Peoples R China. [Zhou, Qin] Univ Chinese Acad Sci, Beijing 100029, Peoples R China. [Herd, Christopher D. K.] Univ Alberta, Dept Earth & Atmospher Sci, Edmonton, AB T6G 2E3, Canada. [Yin, Qing-Zhu] Univ Calif Davis, Dept Geol, Davis, CA 95616 USA. [McCoy, Timothy J.] Smithsonian Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20560 USA. RP Herd, CDK (reprint author), Univ Alberta, Dept Earth & Atmospher Sci, 1-26 Earth Sci Bldg, Edmonton, AB T6G 2E3, Canada. EM herd@ualberta.ca RI Yin, Qing-Zhu/B-8198-2009; WU, Fu-Yuan/K-5354-2015; OI Yin, Qing-Zhu/0000-0002-4445-5096; Li, Qiuli/0000-0002-7280-5508 FU Natural Sciences and Engineering Research Council of Canada [261740-08]; Smithsonian Senior Research Fellowship; State Key Laboratory of Lithospheric Evolution, IGG-CAS [Z201003]; NSFC [41221002] FX C.H. and Q.Z.Y. initiated the project. C.H. and Q.Z. carried out location and characterization of baddeleyite grains. Ion microprobe analysis was carried out by Q.Z., X.H.L., Q.L.L., Y.L., G.Q.T. and Q.Z.Y., QZ., F.Y.W., and Q.L.L. were involved in the development of apatite standard NW-1. T.M. provided hosting for C.H. during the Smithsonian Fellowship, and contributed to manuscript revision. All authors discussed the results and contributed to the manuscript. Funding was provided by the Natural Sciences and Engineering Research Council of Canada Discovery Grant 261740-08 and a Smithsonian Senior Research Fellowship to C.H. for locating and characterizing baddeleyite grains. The work was supported in part by State Key Laboratory of Lithospheric Evolution, IGG-CAS Grants Z201003 and NSFC grants of 41221002 for ion probe analysis. We thank Linda Welzenbach of the Smithsonian National Museum of Natural History for assistance with the loan of USNM 6545, and Ed Scott and Lydia Hallis of the University of Hawaii for the UH 218 and UH 233 sections used in the study. We are grateful to Sergei Matveev for assistance with application of the EPMA Particle Search method. We are indebted to Qian Mao at IGG, CAS for his technical assistance with the BSE imaging, to Junfang Zhao at TIPC, CAS for her help with the Raman spectra. We thank two anonymous reviewers for suggestions that improved the manuscript, and the Editor Mark Harrison for his efficient editorial handling. NR 54 TC 15 Z9 15 U1 2 U2 14 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0012-821X J9 EARTH PLANET SC LETT JI Earth Planet. Sci. Lett. PD JUL 15 PY 2013 VL 374 BP 156 EP 163 DI 10.1016/j.epsl.2013.05.035 PG 8 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 221MT UT WOS:000324663700015 ER PT J AU Swanson, BO George, MN Anderson, SP Christy, JH AF Swanson, Brook O. George, Matthew N. Anderson, Stuart P. Christy, John H. TI Evolutionary variation in the mechanics of fiddler crab claws SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Closing force; Cuticle damage; Structural damage; Signal efficiency; Trade-off ID FEMALE CHOICE; MALE COMPETITION; WAVING DISPLAY; UCA-MJOEBERGI; CLOSING FORCE; TRADE-OFF; BODY-SIZE; GENUS UCA; PREFERENCE; OCYPODIDAE AB Background: Fiddler crabs, genus Uca, are classic examples of how intense sexual selection can produce exaggerated male traits. Throughout the genus the enlarged "major" cheliped (claw) of the male fiddler crab is used both as a signal for attracting females and as a weapon for combat with other males. However, the morphology of the major claw is highly variable across the approximately 100 species within the genus. Here we address variation, scaling, and correlated evolution in the mechanics of the major claw by analyzing the morphology and mechanical properties of the claws of 21 species of fiddler crabs from the Pacific, Gulf and Atlantic coasts of the Americas. Results: We find that the mechanics that produce claw closing forces, the sizes of claws and the mechanical strength of the cuticle of claws are all highly variable across the genus. Most variables scale isometrically with body size across species but claw force production scales allometrically with body size. Using phylogenetically independent contrasts, we find that the force that a claw can potentially produce is positively correlated with the strength of the cuticle on the claw where forces are delivered in a fight. There is also a negative correlation between the force that a claw can potentially produce and the size of the claw corrected for the mass of the claw. Conclusions: These relationships suggest that there has been correlated evolution between force production and armoring, and that there is a tradeoff between claw mechanics for signaling and claw mechanics for fighting. C1 [Swanson, Brook O.; George, Matthew N.; Anderson, Stuart P.] Gonzaga Univ, Dept Biol, Spokane, WA 99258 USA. [Christy, John H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Swanson, BO (reprint author), Gonzaga Univ, Dept Biol, 502 E Boone Ave, Spokane, WA 99258 USA. EM swansonb@gonzaga.edu FU Gonzaga University office of sponsored research; M.J. Murdock charitable trust; HHMI; AFOSR [FA9550-10-1-0209] FX This work was supported by the Gonzaga University office of sponsored research, the M.J. Murdock charitable trust, HHMI and the AFOSR (grant FA9550-10-1-0209 to BOS). Alexei Maklakov and two anonymous reviewers provided comments on earlier versions of the manuscript. We also thank the staff of the STRI for logistical support. NR 47 TC 5 Z9 5 U1 4 U2 57 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 JUL 15 PY 2013 VL 13 AR 137 DI 10.1186/1471-2148-13-137 PG 11 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 184RF UT WOS:000321910300001 PM 23855770 ER PT J AU Connolly, CB Au, YS Chae, E Tscherbul, TV Buchachenko, AA Ketterle, W Doyle, JM AF Connolly, Colin B. Au, Yat Shan Chae, Eunmi Tscherbul, Timur V. Buchachenko, Alexei A. Ketterle, Wolfgang Doyle, John M. TI Zeeman relaxation induced by spin-orbit coupling in cold antimony-helium collisions SO PHYSICAL REVIEW A LA English DT Article ID HARTREE-FOCK; BASIS-SETS; CLUSTER; PSEUDOPOTENTIALS; ENERGIES; ATOMS AB We investigate Zeeman relaxation in cold Sb(S-4(3/2)degrees)-He collisions in a magnetic field. Ensembles of > 10(13) laser-ablated Sb atoms are cooled in cryogenic He-4 buffer gas to 800 mK and inelastic collisions are observed to equilibrate the m(J)-state distribution to the translational temperature. The ratio gamma of momentum transfer to inelastic collision rates is measured to be <= 9.1 x 10(2). We also perform quantum scattering calculations of Sb-He-4 collisions, based on ab initio interaction potentials, that demonstrate significant anisotropy of the ground state induced by the spin-orbit interaction. Agreement is obtained between theory and experiment with a approximate to 10% increase in the ab initio potential depth. This work suggests that buffer-gas-cooled pnictogen atoms lighter than Sb can be loaded into a magnetic trap. C1 [Connolly, Colin B.; Au, Yat Shan; Chae, Eunmi; Doyle, John M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Ketterle, Wolfgang] MIT, Dept Phys, Cambridge, MA 02139 USA. [Connolly, Colin B.; Au, Yat Shan; Chae, Eunmi; Tscherbul, Timur V.; Ketterle, Wolfgang; Doyle, John M.] Harvard Univ, MIT, Ctr Ultracold Atoms, Cambridge, MA 02139 USA. [Tscherbul, Timur V.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Tscherbul, Timur V.] Univ Toronto, Dept Chem, Chem Phys Theory Grp, Toronto, ON M5S 3H6, Canada. [Buchachenko, Alexei A.] Moscow MV Lomonosov State Univ, Dept Chem, Moscow 119991, Russia. [Buchachenko, Alexei A.] Russian Acad Sci, Inst Problems Chem Phys, Chernogolovka 142432, Russia. RP Connolly, CB (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RI Buchachenko, Alexei/C-8452-2012; Tscherbul, Timur/K-3286-2014 OI Buchachenko, Alexei/0000-0003-0701-5531; Tscherbul, Timur/0000-0001-5689-040X FU NSF [PHY-1067990]; NSF through the Harvard-MIT Center for Ultracold Atoms; RFBR [11-03-00081] FX We are grateful to Roman Krems for use of his scattering code and for many helpful discussions. This work was supported by the NSF under Grant No. PHY-1067990 and through the Harvard-MIT Center for Ultracold Atoms, and by RFBR under Project No. 11-03-00081. NR 32 TC 1 Z9 1 U1 0 U2 11 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1050-2947 J9 PHYS REV A JI Phys. Rev. A PD JUL 15 PY 2013 VL 88 IS 1 AR 012707 DI 10.1103/PhysRevA.88.012707 PG 8 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 183SH UT WOS:000321837000012 ER PT J AU Burns, JO Kring, DA Hopkins, JB Norris, S Lazio, TJW Kasper, J AF Burns, Jack O. Kring, David A. Hopkins, Joshua B. Norris, Scott Lazio, T. Joseph W. Kasper, Justin TI A lunar L2-Farside exploration and science mission concept with the Orion Multi-Purpose Crew Vehicle and a teleoperated lander/rover SO ADVANCES IN SPACE RESEARCH LA English DT Article DE Human cis-lunar missions; Moon; Planets and satellites: formation, Surfaces; Radio astronomy; Space vehicles: instruments; Telerobotics ID POLE-AITKEN BASIN; SCHRODINGER-BASIN; ATMOSPHERE; UNIVERSE; SURFACE; SCALE AB A novel concept is presented in this paper for a human mission to the lunar L2 (Lagrange) point that would be a proving ground for future exploration missions to deep space while also overseeing scientifically important investigations. In an L2 halo orbit above the lunar farside, the astronauts aboard the Orion Crew Vehicle would travel 15% farther from Earth than did the Apollo astronauts and spend almost three times longer in deep space. Such a mission would serve as a first step beyond low Earth orbit and prove out operational spaceflight capabilities such as life support, communication, high speed re-entry, and radiation protection prior to more difficult human exploration missions. On this proposed mission, the crew would teleoperate landers/rovers on the unexplored lunar farside, which would obtain samples from the geologically interesting farside and deploy a low radio frequency telescope. Sampling the South Pole-Aitken basin, one of the oldest impact basins in the solar system, is a key science objective of the 2011 Planetary Science Decadal Survey. Observations at low radio frequencies to track the effects of the Universe's first stars/galaxies on the intergalactic medium are a priority of the 2010 Astronomy and Astrophysics Decadal Survey. Such telerobotic oversight would also demonstrate capability for human and robotic cooperation on future, more complex deep space missions such as exploring Mars. (C) 2012 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 [Burns, Jack O.] Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Burns, Jack O.; Kring, David A.; Lazio, T. Joseph W.; Kasper, Justin] NASA, Ames Res Ctr, Lunar Sci Inst, Moffett Field, CA 94089 USA. [Kring, David A.] USRA Lunar & Planetary Inst, Ctr Lunar Sci & Explorat, Houston, TX 77058 USA. [Hopkins, Joshua B.; Norris, Scott] CO TSB, Lockheed Martin Space Syst, Denver, CO 80127 USA. [Lazio, T. Joseph W.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Kasper, Justin] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Burns, JO (reprint author), Univ Colorado, Dept Astrophys & Planetary Sci, Ctr Astrophys & Space Astron, 593 UCB, Boulder, CO 80309 USA. EM jack.burns@colorado.edu RI Kasper, Justin/D-1152-2010 OI Kasper, Justin/0000-0002-7077-930X FU Lunar University Network for Astrophysics Research; NASA Lunar Science Institute [NNA09DB30A, NNA09DB33A]; NASA FX The development of this mission concept was supported by the Lunar University Network for Astrophysics Research (http://lunar.colorado.edu), headquartered at the University of Colorado Boulder, and the LPI-JSC Center for Lunar Science and Exploration in Houston (http://www.lpi.usra.edu/nlsi/), both funded by the NASA Lunar Science Institute (NASA Cooperative Agreements NNA09DB30A and NNA09DB33A, respectively). Part of this research was conducted at the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. We thank Y. Takahashi for the use of his electromagnetic propagation code to study diffraction effects at locations on the lunar farside and A. Datta for porting/running the code at U. Colorado. We also thank Mattie Toll for her editorial assistance and Terry Fong for insightful discussions on telerobotics In addition, we are grateful to Dan Lester for helpful comments on an earlier draft of this paper. NR 46 TC 17 Z9 18 U1 0 U2 24 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0273-1177 J9 ADV SPACE RES JI Adv. Space Res. PD JUL 15 PY 2013 VL 52 IS 2 BP 306 EP 320 DI 10.1016/j.asr.2012.11.016 PG 15 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA 174LQ UT WOS:000321157400007 ER PT J AU Hao, GX Boyle, M Zhou, LJ Duan, YP AF Hao, Guixia Boyle, Michael Zhou, Lijuan Duan, Yongping TI The Intracellular Citrus Huanglongbing Bacterium, 'Candidatus Liberibacter asiaticus' Encodes Two Novel Autotransporters SO PLOS ONE LA English DT Article ID LEUCINE-RICH REPEAT; DOUBLE-STRANDED-RNA; TRANSLOCATOR DOMAIN; PLANT PATHOGEN; ADHESIN YADA; PROTEIN; EXPRESSION; RECEPTOR; LOCALIZATION; DIVERSITY AB Proteins secreted by the type V secretion system (T5SS), known as autotransporters, are large extracellular virulence proteins localized to the bacterial poles. In this study, we characterized two novel autotransporter proteins of 'Candidatus Liberibacter asiaticus' (Las), and redesignated them as LasA(I) and LasA(II) in lieu of the previous names Hyv(I) and Hyv(II). As a phloem-limited, intracellular bacterial pathogen, Las has a significantly reduced genome and causes huanglongbing (HLB), a devastating disease of citrus worldwide. Bioinformatic analyses revealed that LasA(I) and LasA(II) share the structural features of an autotransporter family containing large repeats of a passenger domain and a unique C-terminal translocator domain. When fused to the GFP gene and expressed in E. coli, the LasA(I) C-terminus and the full length LasA(II) were localized to the bacterial poles, similar to other members of autotransporter family. Despite the absence of a typical signal peptide, LasA(I) was found to localize at the cell surface by immuno-dot blot using a monoclonal antibody against the partial LasA(I) protein. Its surface localization was also confirmed by the removal of the LasA(I) antigen using a proteinase K treatment of the intact bacterial cells. When co-inoculated with a P19 gene silencing suppressor and transiently expressed in tobacco leaves, the GFP-LasA(I) translocator targeted to the mitochondria. This is the first report that Las encodes novel autotransporters that target to mitochondria when expressed in the plants. These findings may lead to a better understanding of the pathogenesis of this intracellular bacterium. C1 [Hao, Guixia; Zhou, Lijuan; Duan, Yongping] USDA ARS, United States Hort Res Lab, Ft Pierce, FL USA. [Boyle, Michael] Smithsonian Marine Stn, Ft Pierce, FL USA. RP Duan, YP (reprint author), USDA ARS, United States Hort Res Lab, Ft Pierce, FL USA. EM yongping.duan@ars.usda.gov FU Florida Citrus Advanced Technology Program [162, 310] FX Funding for this work was provided by the Florida Citrus Advanced Technology Program award 162 and 310. Mention of trade names or commercial products in this article is solely for the purpose of providing specific information and does not imply recommendation or endorsement by the U.S. Department of Agriculture. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 44 TC 5 Z9 6 U1 0 U2 13 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 11 PY 2013 VL 8 IS 7 AR UNSP e68921 DI 10.1371/journal.pone.0068921 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 188UA UT WOS:000322218800052 PM 23874813 ER PT J AU Harrison, GF Kim, K Collins, AG AF Harrison, Genelle F. Kim, Kiho Collins, Allen G. TI Low genetic diversity of the putatively introduced, brackish water hydrozoan, Blackfordia virginica (Leptothecata: Blackfordiidae), throughout the United States, with a new record for Lake Pontchartrain, Louisiana SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE founder effect; genetic variation; Hydrozoa; invasive species; medusa ID CNIDARIA; ESTUARY; MITOCHONDRIAL; PHYLOGENY AB Despite first being described from Virginia, the widely distributed brackish water hydrozoan Blackfordia virginica is often hypothesized to have been introduced from the Black Sea to the United States. However, the alternative view that B. virginica was introduced to the Black Sea also persists in the literature. This study investigates the population structure of B. virginica in the United States to assess the directionality and/or the number of introduction events. During 2009 and 2010, estuaries were sampled from Delaware to Louisiana for brackish water hydromedusae. Nineteen samples of Blackfordia virginica were collected from four localities, including a channel running between St. Catherines Island and Lake Pontchartrain, Louisiana, a region for which it had not been reported prior to this study. We PCR amplified and sequenced two mitochondrial markers (COI & 16S), and one nuclear marker (ITS 1). We compared data from individuals collected on the east coast of the United States with individuals collected in California. This revealed low diversity (two haplotypes with a maximal p-difference of 0.03% for COI and just a single haplotype for 16S) and no unique haplotypes at any locality. Low genetic variability, shared haplotypes in disparate localities, and a lack of unique haplotypes in any population are consistent with a founder effect, suggesting a single introduction and subsequent spread throughout the United States. C1 [Harrison, Genelle F.] Smithsonian Inst, Museum Support Ctr, Dept Entomol, Suitland, MD 20746 USA. [Kim, Kiho] American Univ, Dept Environm Sci, Washington, DC 20016 USA. [Collins, Allen G.] NOAA, Natl Systemat Lab, Fisheries Serv, Washington, DC 20560 USA. [Collins, Allen G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Washington, DC 20560 USA. RP Harrison, GF (reprint author), Smithsonian Inst, Museum Support Ctr, Dept Entomol, 4210 Silver Hill Rd, Suitland, MD 20746 USA. EM HarrisonG@si.edu FU Smithsonian Institution; National Systematics Lab of NOAA's Fisheries Service; American University FX We thank Dr. Mariah Meek for providing specimens of B. virginica from California. We also thank Dr. David Carlini for his review of an earlier version of this work. Funding for this project was provided by the Smithsonian Institution, the National Systematics Lab of NOAA's Fisheries Service, and American University. NR 27 TC 1 Z9 2 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 10 PY 2013 VL 126 IS 2 BP 91 EP 102 PG 12 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186NC UT WOS:000322050300001 ER PT J AU Flint, OS AF Flint, Oliver S., Jr. TI Notes on some Panorpa from northeastern North America with the redescription of Panorpa insolens (Mecoptera: Panorpidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE differentiation; distribution; mid-Atlantic states; scorpionfly; variation AB Three closely related species of the Panorpa banksiana species group, P. dissimilis Carpenter, P. gracilis Carpenter, and P. palustris Byers are distinguishable by differences in the male genitalia and distribution. Panorpa debilis Westwood is shown to consist of five forms, differing in characteristics of the aedeagal hamulus, ventral parameres, and distributions. The exact identity of P. debilis and P. canadensis Banks is determined from the study of the type or recently collected examples from near the type locality. Because the ventral parameres of P. nebulosa Westwood and P. flexa Carpenter are often curved and crossed apically in both species, leading to misidentifications, a characteristic of the dististyles is shown to distinguish the two. The presence of P. confusa Westwood is confirmed in Virginia, and the appearance of its ventral parameres is discussed. Panorpa longicornis Carpenter, P. subfurcata Westwood, and P. subulifera Byers are transferred to the P. virginica group, and differences between them are discussed and figured, and their ranges in the state are outlined. The identity of P. insolens Carpenter is established, and it is redescribed and distinguished from its close relatives P. helena Byers and an unnamed species in Kentucky. The species is recorded from Arkansas, Illinois, Indiana, Iowa, Kansas, Michigan, Minnesota, Missouri, North Carolina, Ohio, Tennessee, Virginia, West Virginia, and Wisconsin. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol MRC 169, Washington, DC 20013 USA. RP Flint, OS (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Entomol MRC 169, Washington, DC 20013 USA. EM flinto@si.edu NR 21 TC 3 Z9 3 U1 0 U2 2 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 10 PY 2013 VL 126 IS 2 BP 120 EP 136 PG 17 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186NC UT WOS:000322050300003 ER PT J AU de Sant'Anna, VB Collette, BB Godfrey, SJ AF de Sant'Anna, Vivianne B. Collette, Bruce B. Godfrey, Stephen J. TI Belone countermani, a new Miocene needlefish (Belonidae) from the St. Marys Formation of Calvert Cliffs, Maryland SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Belone; Belonidae; Calvert Cliffs; Maryland; Miocene; needlefish; St. Marys Formation ID BELONIFORM FISHES; CHESAPEAKE GROUP; SYSTEMATICS; TELEOSTEI; REMAINS; USA AB Belone is distinguished from other genera of Belonidae mostly because of its complete cephalic sensory system, presence of gill rakers, vomerine teeth, and the pattern of its dentition. This eastern North Atlantic genus contains two extant species and at least three described fossil species from Lower Oligocene and Upper Miocene formations in Europe. dagger Belone countermani, sp. nov., a new species of needlefish from the Tortonian Upper Miocene St. Marys Formation of Calvert Cliffs (Maryland, U.S.A.), is described herein based on a well-preserved three-dimensional associated pair of upper and lower jaws. This rostrum represents the only record of this genus in the western North Atlantic Ocean. dagger Belone countermani is characterized by a unique dental pattern on the dentary. The dentary commissural region is filled with several rows of small accessory teeth (five to seven) that gradually decrease in number of rows; along the symphysial region there is one inner row of conical teeth and one external row of accessory teeth. Discovery of dagger Belone countermani indicates that extant Be lone species are a relict diversity of an old group that had a wider distribution that included the western North Atlantic. C1 [de Sant'Anna, Vivianne B.] Pontificia Univ Catolica Rio Grande do Sul, Lab Vertebrate Systemat, BR-90619900 Porto Alegre, RS, Brazil. [Collette, Bruce B.] Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, Natl Museum Nat Hist, Washington, DC 20013 USA. [Godfrey, Stephen J.] Calvert Marine Museum, Dept Paleontol, Solomons, MD 20688 USA. [Godfrey, Stephen J.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Collette, BB (reprint author), Smithsonian Inst, Natl Marine Fisheries Serv Systemat Lab, Natl Museum Nat Hist, POB 3701,MRC 0153, Washington, DC 20013 USA. EM zapteryx@yahoo.com; collettb@si.edu; Godfresj@co.cal.md.us FU CNPq; Board of Calvert County Commissioners; citizens of Calvert County, Maryland; Clarissa and Lincoln Dryden Endowment for Paleontology at the Calvert Marine Museum FX This publication was made possible with funding from the CNPq Post-doctoral fellowship (VBS), the Board of Calvert County Commissioners, the citizens of Calvert County, Maryland, and the Clarissa and Lincoln Dryden Endowment for Paleontology at the Calvert Marine Museum. R. Hulbert (FLMNH) provided information on fossil needlefish from Florida. For helping with the X-rays, we thank S. Raredon (USNM). J. Tyler and E. Hilton reviewed the manuscript and provided comments that improved it. We thank the following for making comparative material available: R. Arrindell and B. Brown (AMNH), J. Lundberg and M. Sabaj (ANSP), J. Maclaine and O. Crimmen (BMNH), J. Demouthe, S. Mainsfield, and S. Willard (CAS), K. Swagel, M. Rogers, and P. Willink (FMNH), V. Rheu and S. Macleod (LACM), S. Iglesias, G. Clement, G, Duhamel, and C. Sagne (MNHN), M. Gasparik and J. Palfy (NHMUS), P. Buckup and M. Britto (MNRJ), O. Oyakawa (MZUSP), S. Kullander and B. Kajrup (NRM), A. Bannikov (PIN), H. Fernandez and E. Holm (ROM), R. Robins (FLMNH), D. Nelson (UMMZ), R. Van, L. Parenti, J. Finan, and J. Williams (USNM). NR 58 TC 0 Z9 0 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 10 PY 2013 VL 126 IS 2 BP 137 EP 150 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186NC UT WOS:000322050300004 ER PT J AU Olson, SL AF Olson, Storrs L. TI Hawaii's first fossil bird: history, geological age, and taxonomic status of the extinct goose Geochen rhuax Wetmore (Ayes: Anatidae) SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Anseriformes; Branta rhuax; evolution; Holocene; waterfowl ID KAUAI; ANSERIFORMES; DREPANIDINI; ISLANDS; GEESE AB The history of discovery of the fossil goose Geochen rhuax. Wetmore on the island of Hawaii is reviewed through archival records and the literature. Although the age of the fossil was previously undetermined, recent radiocarbon dates establish that the age of the lava flow immediately overlying the bones was 9170 +/- 100 yrs b.p. A very large extinct, flightless goose that is abundant in latest Holocene lava tubes on the western versant of the island of Hawaii was previously determined by mtDNA to be part of the Hawaiian radiation of Branta. This goose is now also known from the southeastern versant of the island. Although the holotype of Geochen rhuax is somewhat smaller in size, it is considered to belong to the same species lineage as the more recent fossils, and all giant goose fossils from Hawaiian Island are here referred to as Branta rhuax, new combination. C1 Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM olsons@si.edu NR 25 TC 1 Z9 1 U1 3 U2 11 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X EI 1943-6327 J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 10 PY 2013 VL 126 IS 2 BP 161 EP 168 PG 8 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186NC UT WOS:000322050300006 ER PT J AU Olson, SL Hearty, PJ AF Olson, Storrs L. Hearty, Paul J. TI Fossilized egg indicates probable breeding of Brown Pelican (Pelecanus occidentalis) on Bermuda in the Middle Pleistocene SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE extinction; fossil birds; interglacials; Marine Isotope Stage 11; Pelecanidae; sea levels ID SEA-LEVEL HIGHSTAND; QUATERNARY DEPOSITS; AVES PROCELLARIIDAE; GEOCHRONOLOGY; STRATIGRAPHY; POECILOZONITES; CALIFORNIA; GENUS; KA AB A large, relatively intact fossil bird's egg collected on Bermuda over a century ago is identified here as that of a Brown Pelican Pelecanus occidentalis, a species known historically only as an occasional vagrant in Bermuda. Although the exact provenance and age were originally unknown, contemporary descriptions of the stratigraphy and subsequent amino acid ratios of the attached limestone matrix establish the age as a Middle Pleistocene interglacial, probably Marine Isotope Stage (MIS) 11 or perhaps slightly older. The presence of an egg is a very likely indication of at least a small former breeding colony of Brown Pelicans on Bermuda. Ecological conditions during interglacial periods and presence of potential fish prey would have made such a colonization feasible. C1 [Olson, Storrs L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Hearty, Paul J.] Univ N Carolina, Dept Environm Studies, Wilmington, NC 28403 USA. RP Olson, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. EM olsons@si.edu NR 43 TC 1 Z9 1 U1 0 U2 4 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 10 PY 2013 VL 126 IS 2 BP 169 EP 177 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186NC UT WOS:000322050300007 ER PT J AU Emry, RJ Korth, WW AF Emry, Robert J. Korth, William W. TI The eomyid rodent Paradjidaumo Burke from the late Eocene White River Formation, Flagstaff Rim area, Wyoming SO PROCEEDINGS OF THE BIOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Chadronian; Eocene; Eomyidae; Paradjidaumo hansonorum; Paradjidaumo nanus; Rodentia AB Two species of the eomyid rodent Paradjidaumo are recognized from the Chadronian (latest Eocene) White River Formation in the Flagstaff Rim area of Wyoming: P. hansonorum from early Chadronian levels and P. nanus, new species, from higher levels representing the middle Chadronian. C1 [Emry, Robert J.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Korth, William W.] Rochester Inst Vertebrate Paleontol, Rochester, NY 14610 USA. RP Emry, RJ (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM emryr@si.edu NR 19 TC 0 Z9 0 U1 0 U2 3 PU BIOL SOC WASHINGTON PI WASHINGTON PA NAT MUSEUM NAT HIST SMITHSONIAN INST, WASHINGTON, DC 20560 USA SN 0006-324X J9 P BIOL SOC WASH JI Proc. Biol. Soc. Wash. PD JUL 10 PY 2013 VL 126 IS 2 BP 178 EP 186 PG 9 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 186NC UT WOS:000322050300008 ER PT J AU Andrews, SM Rosenfeld, KA Kraus, AL Wilner, DJ AF Andrews, Sean M. Rosenfeld, Katherine A. Kraus, Adam L. Wilner, David J. TI THE MASS DEPENDENCE BETWEEN PROTOPLANETARY DISKS AND THEIR STELLAR HOSTS SO ASTROPHYSICAL JOURNAL LA English DT Article DE protoplanetary disks; submillimeter: planetary systems ID T-TAURI STARS; MAIN-SEQUENCE STARS; HERBIG AE/BE STARS; BROWN DWARF DISKS; SUBMILLIMETER CONTINUUM FLUX; TERM PHOTOMETRIC VARIABILITY; CIRCUMSTELLAR DUST DISKS; AURIGA MOLECULAR CLOUD; HUBBLE-SPACE-TELESCOPE; GIANT PLANET FORMATION AB We present a substantial extension of the millimeter (mm) wave continuum photometry catalog for circumstellar dust disks in the Taurus star-forming region, based on a new "snapshot" lambda = 1.3 mm survey with the Submillimeter Array. Combining these new data with measurements in the literature, we construct a mm-wave luminosity distribution, f(L-mm), for Class II disks that is statistically complete for stellar hosts with spectral types earlier than M8.5 and has a 3 sigma depth of roughly 3 mJy. The resulting census eliminates a longstanding selection bias against disks with late-type hosts, and thereby demonstrates that there is a strong correlation between L-mm and the host spectral type. By translating the locations of individual stars in the Hertzsprung-Russell diagram into masses and ages, and adopting a simple conversion between L-mm and the disk mass, M-d, we confirm that this correlation corresponds to a statistically robust relationship between the masses of dust disks and the stars that host them. A Bayesian regression technique is used to characterize these relationships in the presence of measurement errors, data censoring, and significant intrinsic scatter: the best-fit results indicate a typical 1.3 mm flux density of similar to 25 mJy for 1 M-circle dot hosts and a power-law scaling L-mm proportional to M-*(1.5-2.0). We suggest that a reasonable treatment of dust temperature in the conversion from L-mm to M-d favors an inherently linear M-d proportional to M-* scaling, with a typical disk-to-star mass ratio of similar to 0.2%-0.6%. The measured rms dispersion around this regression curve is +/- 0.7 dex, suggesting that the combined effects of diverse evolutionary states, dust opacities, and temperatures in these disks imprint a full width at half-maximum range of a factor of similar to 40 on the inferred M-d (or L-mm) at any given host mass. We argue that this relationship between M-d and M-* likely represents the origin of the inferred correlation between giant planet frequency and host star mass in the exoplanet population, and provides some basic support for the core accretion model for planet formation. Moreover, we caution that the effects of incompleteness and selection bias must be considered in comparative studies of disk evolution, and illustrate that fact with statistical comparisons of f (L-mm) between the Taurus catalog presented here and incomplete subsamples in the Ophiuchus, IC 348, and Upper Sco young clusters. C1 [Andrews, Sean M.; Rosenfeld, Katherine A.; Kraus, Adam L.; Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Andrews, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM sandrews@cfa.harvard.edu FU Harvard-Smithsonian Center for Astrophysics; Smithsonian Institution; Academia Sinica FX We are very grateful to Rahul Shetty and Brandon Kelly for their invaluable advice on a Bayesian approach to linear regression analysis, to Jonathan Williams for providing the full set of mm-wave measurements for IC 348 members, and to Til Birnstiel and Anaelle Maury for helpful comments and critiques. We also thank the referee for a prompt and constructive review that helped fortify the presentation of our key conclusions. A.L.K. was supported by a Clay Fellowship from the Harvard-Smithsonian Center for Astrophysics. The SMA is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The research involved in this article has made extensive use of the SIMBAD database, operated at CDS, Strasbourg, France and the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. NR 249 TC 126 Z9 126 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 129 DI 10.1088/0004-637X/771/2/129 PG 40 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700054 ER PT J AU Bean, JL Desert, JM Seifahrt, A Madhusudhan, N Chilingarian, I Homeier, D Szentgyorgyi, A AF Bean, Jacob L. Desert, Jean-Michel Seifahrt, Andreas Madhusudhan, Nikku Chilingarian, Igor Homeier, Derek Szentgyorgyi, Andrew TI GROUND-BASED TRANSIT SPECTROSCOPY OF THE HOT-JUPITER WASP-19b IN THE NEAR-INFRARED SO ASTROPHYSICAL JOURNAL LA English DT Article DE planets and satellites: atmospheres; planets and satellites: individual (WASP-19b); techniques: photometric ID EARTH GJ 1214B; BAND THERMAL EMISSION; EXOPLANET HD 189733B; SECONDARY ECLIPSE; TRANSMISSION SPECTRUM; C/O RATIO; MU-M; TEMPERATURE INVERSION; MODEL ATMOSPHERES; GIANT PLANETS AB We present ground-based measurements of the transmission and emission spectra of the hot-Jupiter WASP-19b in nine spectroscopic channels from 1.25 to 2.35 mu m. The measurements are based on the combined analysis of time-series spectroscopy obtained during two complete transits and two complete secondary eclipses of the planet. The observations were performed with the MMIRS instrument on the Magellan II telescope using the technique of multi-object spectroscopy with wide slits. We compare the transmission and emission data to theoretical models to constrain the composition and thermal structure of the planet's atmosphere. Our measured transmission spectrum exhibits a scatter that corresponds to 1.3 scale heights of the planet's atmosphere, which is consistent with the size of spectral features predicted by theoretical models for a clear atmosphere. We detect the secondary eclipses of the planet at significances ranging from 2.2 sigma to 14.4 sigma. The secondary eclipse depths, and the significances of the detections increase toward longer wavelengths. Our measured emission spectrum is consistent with a 2250 K effectively isothermal one-dimensional model for the planet's dayside atmosphere. This model also matches previously published photometric measurements from the Spitzer Space Telescope and ground-based telescopes. These results demonstrate the important role that ground-based observations using multi-object spectroscopy can play in constraining the properties of exoplanet atmospheres, and they also emphasize the need for high-precision measurements based on observations of multiple transits and eclipses. C1 [Bean, Jacob L.; Seifahrt, Andreas] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Desert, Jean-Michel] CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. [Madhusudhan, Nikku] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Madhusudhan, Nikku] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Chilingarian, Igor; Szentgyorgyi, Andrew] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Chilingarian, Igor] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Homeier, Derek] Univ Lyon, Ecole Normale Super Lyon, CNRS, Ctr Rech Astrophys Lyon,UMR 5574, F-69364 Lyon 07, France. RP Bean, JL (reprint author), Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA. EM jbean@oddjob.uchicago.edu RI Chilingarian, Igor/N-5117-2016; OI Chilingarian, Igor/0000-0002-7924-3253; Homeier, Derek/0000-0002-8546-9128 FU Alfred P. Sloan Foundation; NASA through the Sagan Exoplanet Fellowship program FX J.L.B. acknowledges support from the Alfred P. Sloan Foundation. J.-M.D. acknowledges funding from NASA through the Sagan Exoplanet Fellowship program administered by the NASA Exoplanet Science Institute (NExScI). The results presented are based on observations made with the 6.5 m Magellan telescopes located at Las Campanas Observatory. NR 70 TC 31 Z9 32 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 108 DI 10.1088/0004-637X/771/2/108 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700033 ER PT J AU Bernardi, G Greenhill, LJ Mitchell, DA Ord, SM Hazelton, BJ Gaensler, BM De Oliveira-Costa, A Morales, MF Shankar, NU Subrahmanyan, R Wayth, RB Lenc, E Williams, CL Arcus, W Arora, BS Barnes, DG Bowman, JD Briggs, FH Bunton, JD Cappallo, RJ Corey, BE Deshpande, A DeSouza, L Emrich, D Goeke, R Herne, D Hewitt, JN Johnston-Hollitt, M Kaplan, D Kasper, JC Kincaid, BB Koenig, R Kratzenberg, E Lonsdale, CJ Lynch, MJ McWhirter, SR Morgan, E Oberoi, D Pathikulangara, J Prabu, T Remillard, RA Rogers, AEE Roshi, A Salah, JE Sault, RJ Srivani, KS Stevens, J Tingay, SJ Waterson, M Webster, RL Whitney, AR Williams, A Wyithe, JSB AF Bernardi, G. Greenhill, L. J. Mitchell, D. A. Ord, S. M. Hazelton, B. J. Gaensler, B. M. de Oliveira-Costa, A. Morales, M. F. Shankar, N. Udaya Subrahmanyan, R. Wayth, R. B. Lenc, E. Williams, C. L. Arcus, W. Arora, B. S. Barnes, D. G. Bowman, J. D. Briggs, F. H. Bunton, J. D. Cappallo, R. J. Corey, B. E. Deshpande, A. deSouza, L. Emrich, D. Goeke, R. Herne, D. Hewitt, J. N. Johnston-Hollitt, M. Kaplan, D. Kasper, J. C. Kincaid, B. B. Koenig, R. Kratzenberg, E. Lonsdale, C. J. Lynch, M. J. McWhirter, S. R. Morgan, E. Oberoi, D. Pathikulangara, J. Prabu, T. Remillard, R. A. Rogers, A. E. E. Roshi, A. Salah, J. E. Sault, R. J. Srivani, K. S. Stevens, J. Tingay, S. J. Waterson, M. Webster, R. L. Whitney, A. R. Williams, A. Wyithe, J. S. B. TI A 189 MHz, 2400 deg(2) POLARIZATION SURVEY WITH THE MURCHISON WIDEFIELD ARRAY 32-ELEMENT PROTOTYPE SO ASTROPHYSICAL JOURNAL LA English DT Article DE diffuse radiation; ISM: magnetic fields; polarization; radio continuum: general; surveys; techniques: interferometric ID UNDERSTANDING RADIO POLARIMETRY; PULSAR ROTATION MEASURES; 21 CM EPOCH; POWER SPECTRUM; MULTIFREQUENCY POLARIMETRY; FOREGROUND REMOVAL; GALACTIC EMISSION; POINT SOURCES; SOUTHERN SKY; FORNAX-A AB We present a Stokes I, Q and U survey at 189 MHz with the Murchison Widefield Array 32 element prototype covering 2400 deg(2). The survey has a 15.6 arcmin angular resolution and achieves a noise level of 15 mJy beam(-1). We demonstrate a novel interferometric data analysis that involves calibration of drift scan data, integration through the co-addition of warped snapshot images, and deconvolution of the point-spread function through forward modeling. We present a point source catalog down to a flux limit of 4 Jy. We detect polarization from only one of the sources, PMN J0351-2744, at a level of 1.8% +/- 0.4%, whereas the remaining sources have a polarization fraction below 2%. Compared to a reported average value of 7% at 1.4 GHz, the polarization fraction of compact sources significantly decreases at low frequencies. We find a wealth of diffuse polarized emission across a large area of the survey with a maximum peak of similar to 13 K, primarily with positive rotation measure values smaller than +10 rad m(-2). The small values observed indicate that the emission is likely to have a local origin (closer than a few hundred parsecs). There is a large sky area at alpha >= 2(h)30(m) where the diffuse polarized emission rms is fainter than 1 K. Within this area of low Galactic polarization we characterize the foreground properties in a cold sky patch at (alpha, delta) = (4(h), -27 degrees.6) in terms of three-dimensional power spectra. C1 [Bernardi, G.; Greenhill, L. J.; de Oliveira-Costa, A.; Kasper, J. C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mitchell, D. A.; Sault, R. J.; Webster, R. L.; Wyithe, J. S. B.] Univ Melbourne, Melbourne, Vic, Australia. [Mitchell, D. A.; Gaensler, B. M.; Subrahmanyan, R.; Wayth, R. B.; Lenc, E.; Briggs, F. H.; Tingay, S. J.; Webster, R. L.; Wyithe, J. S. B.] CAASTRO, Redfern, NSW 20169, Australia. [Ord, S. M.; Wayth, R. B.; Arcus, W.; Arora, B. S.; Emrich, D.; Herne, D.; Lynch, M. J.; Tingay, S. J.; Waterson, M.] Curtin Univ, Int Ctr Radio Astron Res, Perth, WA 6845, Australia. [Hazelton, B. J.; Morales, M. F.] Univ Washington, Seattle, WA 98195 USA. [Gaensler, B. M.; Lenc, E.; deSouza, L.] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Shankar, N. Udaya; Subrahmanyan, R.; Deshpande, A.; Prabu, T.; Roshi, A.; Srivani, K. S.] Raman Res Inst, Bangalore 560080, Karnataka, India. [Williams, C. L.; Goeke, R.; Hewitt, J. N.; Morgan, E.; Remillard, R. A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA USA. [Barnes, D. G.] Swinburne Univ Technol, Melbourne, Vic, Australia. [Bowman, J. D.] Arizona State Univ, Tempe, AZ USA. [Briggs, F. H.; Waterson, M.] Australian Natl Univ, Canberra, ACT, Australia. [Bunton, J. D.; deSouza, L.; Koenig, R.; Pathikulangara, J.] CSIRO Astron & Space Sci, Sydney, NSW, Australia. [Cappallo, R. J.; Corey, B. E.; Kincaid, B. B.; Kratzenberg, E.; Lonsdale, C. J.; McWhirter, S. R.; Rogers, A. E. E.; Salah, J. E.; Whitney, A. R.] MIT, Haystack Observ, Westford, MA 01886 USA. [Johnston-Hollitt, M.] Victoria Univ Wellington, Wellington, New Zealand. [Kaplan, D.] Univ Wisconsin, Milwaukee, WI 53201 USA. [Oberoi, D.] Tata Inst Fundamental Res, Natl Ctr Radio Astrophys, Pune, Maharashtra, India. [Stevens, J.] Univ Tasmania, Hobart, Tas, Australia. [Williams, A.] Univ Western Australia, Nedlands, WA 6009, Australia. RP Bernardi, G (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM gbernardi@cfa.harvard.edu RI Bunton, John/A-4944-2008; Kasper, Justin/D-1152-2010; Wayth, Randall/B-2444-2013; Williams, Andrew/K-2931-2013; Emrich, David/B-7002-2013; Udayashankar , N/D-4901-2012; M, Manjunath/N-4000-2014; Deshpande, Avinash/D-4868-2012; Subrahmanyan, Ravi/D-4889-2012 OI Gaensler, Bryan/0000-0002-3382-9558; Kasper, Justin/0000-0002-7077-930X; Wayth, Randall/0000-0002-6995-4131; Williams, Andrew/0000-0001-9080-0105; Emrich, David/0000-0002-4058-1837; M, Manjunath/0000-0001-8710-0730; FU Australian Research Council [LE0775621, LE0882938]; National Science Foundation [AST-0457585, AST-0821321, AST-0908884, AST-1008353, PHY-0835713]; U.S. Air Force Office of Scientific Research [FA9550-0510247]; Australian National Collaborative Research Infrastructure Strategy; Australia India Strategic Research Fund; Smithsonian Astrophysical Observatory; MIT School of Science; MIT Marble Astrophysics Fund; Raman Research Institute; Australian National University; iVEC Petabyte Data Store; NVIDIA; International Centre for Radio Astronomy Research; Western Australian State government; [CE110001020] FX We thank an anonymous referee for helpful suggestions which improved the manuscript. This scientific work uses data obtained from the Murchison Radio-astronomy Observatory. G. B. thanks Matt McQuinn, Roberto Pizzo and Mario Santos for useful discussions about several topics of the present work. We acknowledge the Wajarri Yamatji people as the traditional owners of the Observatory site. Support for this work comes from the Australian Research Council (grant numbers LE0775621 and LE0882938), the National Science Foundation (grant numbers AST-0457585, AST-0821321, AST-0908884, AST-1008353 and PHY-0835713), the U.S. Air Force Office of Scientific Research (grant number FA9550-0510247), the Australian National Collaborative Research Infrastructure Strategy, the Australia India Strategic Research Fund, the Smithsonian Astrophysical Observatory, the MIT School of Science, MIT Marble Astrophysics Fund, the Raman Research Institute, the Australian National University, the iVEC Petabyte Data Store, the NVIDIA sponsored CUDA Center for Excellence at Harvard University, and the International Centre for Radio Astronomy Research, a Joint Venture of Curtin University of Technology and The University of Western Australia, funded by the Western Australian State government. The Centre for Allsky Astrophysics is an Australian Research Council Centre of Excellence, funded by grant CE110001020. The MRO is managed by the CSIRO, who also provide operational support to the MWA. NR 97 TC 31 Z9 31 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 105 DI 10.1088/0004-637X/771/2/105 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700030 ER PT J AU Di Stefano, R Matthews, J Lepine, S AF Di Stefano, Rosanne Matthews, James Lepine, Sebastien TI NEARBY PLANETARY SYSTEMS AS LENSES DURING PREDICTED CLOSE PASSAGES TO BACKGROUND STARS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: low-mass ID EVENTS; CATALOG; CHANNEL AB The Einstein rings and proper motions of nearby stars tend to be large. Thus, every year some foreground stars within a few hundred parsecs of Earth induce gravitational lensing events in background stars. In some of these cases, the events may exhibit evidence of planets orbiting the nearby star. In fact, planets can even be discovered during relatively distant passages. Here, we study the lensing signatures associated with planets orbiting nearby high-proper-motion stars. We find the following. (1) Wide-orbit planets can be detected for all distances of closest approach between the foreground and background stars, potentially producing independent events long before and/or after the closest approach. (2) Close-orbit planets can be detected for intermediate distances of closest approach, producing quasiperiodic signatures that may occur days or weeks before and after the stellar-lens event. (3) Planets in the so-called zone for resonant lensing can significantly increase the magnification when the distance of closest approach is small, making the stellar-lens event easier to detect, while simultaneously providing evidence for planets. Because approaches close enough to allow planets to be detected can be predicted, we can plan observing strategies to take advantage of the theoretical framework built in this paper, which describes the sequence of expected effects in terms of a sequence of detection regimes. C1 [Di Stefano, Rosanne; Matthews, James] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Matthews, James] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Lepine, Sebastien] Amer Museum Nat Hist, Dept Astrophys, Div Phys Sci, New York, NY 10024 USA. [Lepine, Sebastien] CUNY, Grad Ctr, Dept Phys, New York, NY 10016 USA. RP Di Stefano, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST-0908878, AST-0908406] FX We thank Christopher Stubbs, Christopher Crockett, Fred Walters, David Charbonneau, Zachory Berta, and the MEarth project; Jochen Greiner at GROND; and Matthew Templeton and the AAVSO for their help and advice. This work was supported in part by NSF under AST-0908878 and under AST-0908406. NR 22 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 JUL 10 PY 2013 VL 771 IS 2 AR 79 DI 10.1088/0004-637X/771/2/79 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700004 ER PT J AU Hara, C Shimajiri, Y Tsukagoshi, T Kurono, Y Saigo, K Nakamura, F Saito, M Wilner, D Kawabe, R AF Hara, C. Shimajiri, Y. Tsukagoshi, T. Kurono, Y. Saigo, K. Nakamura, F. Saito, M. Wilner, David Kawabe, R. TI THE ROTATING OUTFLOW, ENVELOPE, AND DISK OF THE CLASS-0/I PROTOSTAR [BHB2007]#11 IN THE PIPE NEBULA SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: clouds; ISM: individual objects ([BHB2007]#11); ISM: molecules; radio continuum: ISM; stars: formation ID STAR-FORMATION ACTIVITY; T TAURI STAR; DENSE CORE; MOLECULAR OUTFLOWS; BARNARD 59; EMISSION; SYSTEM; EXTINCTION; CLOUD; B59 AB We present the results of observations toward a low-mass Class-0/I protostar [ BHB2007]#11 (B59#11) in the nearby (d = 130 pc) star-forming region Barnard 59 (B59), in the Pipe Nebula. We utilize the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope (similar to 22 '' resolution), focusing on the CO(3-2), HCO+, (HCO+)-C-13(4-3), and 1.1 mm dust-continuum emission transitions. We also show Submillimeter Array (SMA) data with similar to 5 '' resolution in (CO)-C-12, (CO)-C-13, (CO)-O-18(2-1), and 1.3 mm dust-continuum emission. From ASTE CO(3-2) observations, we found that B59#11 is blowing a collimated outflow whose axis lies almost on the plane of the sky. The outflow traces well a cavity-like structure seen in the 1.1 mm dust-continuum emission. The results of SMA (CO)-C-13 and (CO)-O-18(2-1) observations have revealed that a compact and elongated structure of dense gas is associated with B59#11; the structure is oriented perpendicular to the outflow axis. There is a compact dust condensation with a size of 350 x 180 AU seen in the SMA 1.3 mm continuum map, and the direction of its major axis is almost the same as that of the dense gas elongation. The distributions of (CO)-C-13 and (CO)-O-18 emission also show velocity gradients along their major axes, which are thought to arise from the envelope/disk rotation. From detailed analysis of the SMA data, we infer that B59#11 is surrounded by a Keplerian disk with a radius of less than 350 AU. In addition, the SMA CO(2-1) image shows a velocity gradient in the outflow in the same direction as that of the dense gas rotation. We suggest that this velocity gradient indicates rotation in the outflow. C1 [Hara, C.] Univ Tokyo, Tokyo 1130033, Japan. [Hara, C.; Shimajiri, Y.; Kurono, Y.; Saigo, K.; Nakamura, F.; Saito, M.; Kawabe, R.] Natl Astron Observ Japan, Tokyo 1810015, Japan. [Shimajiri, Y.] Nobeyama Radio Observ, Minamimaki, Nagano 3841305, Japan. [Tsukagoshi, T.] Ibaraki Univ, Mito, Ibaraki 3108512, Japan. [Saito, M.; Kawabe, R.] Joint ALMA Observ, Santiago 7630355, Chile. [Wilner, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Hara, C (reprint author), Univ Tokyo, 7-3-1 Hongo Bunkyo, Tokyo 1130033, Japan. EM c.hara@nao.ac.jp NR 52 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 128 DI 10.1088/0004-637X/771/2/128 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700053 ER PT J AU Lunnan, R Chornock, R Berger, E Milisavljevic, D Drout, M Sanders, NE Challis, PM Czekala, I Foley, RJ Fong, W Huber, ME Kirshner, RP Leibler, C Marion, GH McCrum, M Narayan, G Rest, A Roth, KC Scolnic, D Smartt, SJ Smith, K Soderberg, AM Stubbs, CW Tonry, JL Burgett, WS Chambers, KC Kudritzki, RP Magnier, EA Price, PA AF Lunnan, R. Chornock, R. Berger, E. Milisavljevic, D. Drout, M. Sanders, N. E. Challis, P. M. Czekala, I. Foley, R. J. Fong, W. Huber, M. E. Kirshner, R. P. Leibler, C. Marion, G. H. McCrum, M. Narayan, G. Rest, A. Roth, K. C. Scolnic, D. Smartt, S. J. Smith, K. Soderberg, A. M. Stubbs, C. W. Tonry, J. L. Burgett, W. S. Chambers, K. C. Kudritzki, R-P Magnier, E. A. Price, P. A. TI PS1-10bzj: A FAST, HYDROGEN-POOR SUPERLUMINOUS SUPERNOVA IN A METAL-POOR HOST GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae: general; supernovae: individual (PS1-10bzj) ID MASS-METALLICITY RELATION; STAR-FORMING GALAXIES; DIGITAL SKY SURVEY; CORE-COLLAPSE SUPERNOVAE; YALE-CHILE MUSYC; RAY BURST HOSTS; LIGHT CURVES; SHOCK BREAKOUT; IC SUPERNOVAE; ULTRALUMINOUS SUPERNOVAE AB We present observations and analysis of PS1-10bzj, a superluminous supernova (SLSN) discovered in the Pan-STARRS Medium Deep Survey at a redshift z = 0.650. Spectroscopically, PS1-10bzj is similar to the hydrogenpoor SLSNe 2005ap and SCP 06F6, though with a steeper rise and lower peak luminosity (M-bol similar or equal to -21.4 mag) than previous events. We construct a bolometric light curve, and show that while PS1-10bzj's energetics were less extreme than previous events, its luminosity still cannot be explained by radioactive nickel decay alone. We explore both a magnetar spin-down and circumstellar interaction scenario and find that either can fit the data. PS1-10bzj is located in the Extended Chandra Deep Field South and the host galaxy is imaged in a number of surveys, including with the Hubble Space Telescope. The host is a compact dwarf galaxy (MB approximate to -18 mag, diameter less than or similar to 800 pc), with a low stellar mass (M-* approximate to 2.4 x 10(7) M-circle dot), young stellar population (tau(*) approximate to 5 Myr), and a star formation rate of similar to 2-3 M-circle dot yr(-1). The specific star formation rate is the highest seen in an SLSN host so far (similar to 100 Gyr(-1)). We detect the [OIII] lambda 4363 line, and find a low metallicity: 12 + (O/H) = 7.8 +/- 0.2 (similar or equal to 0.1 Z(circle dot)). Together, this indicates that at least some of the progenitors of SLSNe come from young, low-metallicity populations. C1 [Lunnan, R.; Chornock, R.; Berger, E.; Milisavljevic, D.; Drout, M.; Sanders, N. E.; Challis, P. M.; Czekala, I.; Foley, R. J.; Fong, W.; Kirshner, R. P.; Leibler, C.; Marion, G. H.; Narayan, G.; Soderberg, A. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Huber, M. E.; Tonry, J. L.; Burgett, W. S.; Chambers, K. C.; Kudritzki, R-P; Magnier, E. A.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Leibler, C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [McCrum, M.; Smartt, S. J.; Smith, K.] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland. [Rest, A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Roth, K. C.] Gemini Observ, Hilo, HI 96720 USA. [Scolnic, D.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Stubbs, C. W.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Price, P. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Lunnan, R (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM rlunnan@cfa.harvard.edu RI Stubbs, Christopher/C-2829-2012; OI Stubbs, Christopher/0000-0003-0347-1724; Lunnan, Ragnhild/0000-0001-9454-4639; Narayan, Gautham/0000-0001-6022-0484; Czekala, Ian/0000-0002-1483-8811; Chambers, Kenneth /0000-0001-6965-7789 FU National Aeronautics and Space Administration through the Planetary Science Division of the NASA Science Mission Directorate [NNX08AR22G]; FAS Science Division Research Computing Group at Harvard University; European Research Council under the European Union's Seventh Framework Programme/ERC [291222]; National Science Foundation [AST-1009749, AST-1211196]; [GS-2010B-Q-4]; [GS-2011A-Q-29]; [GS-2011B-Q-44] FX We thank the staff members at PS1, Gemini, and Magellan for their assistance with performing these observations. The Pan-STARRS1 Surveys (PS1) have been made possible through contributions of the Institute for Astronomy, the University of Hawaii; the Pan-STARRS Project Office; the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching; The Johns Hopkins University; Durham University; the University of Edinburgh; Queen's University Belfast; the Harvard-Smithsonian Center for Astrophysics; the Las Cumbres Observatory Global Telescope Network Incorporated; the National Central University of Taiwan; the Space Telescope Science Institute; and the National Aeronautics and Space Administration under grant No. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate. This work is based in part on observations obtained at the Gemini Observatory (under Programs GS-2010B-Q-4 and GS-2011A-Q-29 (PI: Berger) and GS-2011B-Q-44 (PI: Chornock)), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia, Tecnologia e Inovacao (Brazil), and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This paper includes data based on observations made with the NASA/ESA Hubble Space Telescope and obtained from the Hubble Legacy Archive, which is a collaboration between the Space Telescope Science Institute (STScI/NASA), the Space Telescope European Coordinating Facility (ST-ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA). Some of the computations in this paper were run on the Odyssey cluster supported by the FAS Science Division Research Computing Group at Harvard University. The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. [291222] (PI: S.J. Smartt). Partial support for this work was provided by National Science Foundation grants AST-1009749 and AST-1211196. NR 83 TC 34 Z9 34 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 97 DI 10.1088/0004-637X/771/2/97 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700022 ER PT J AU Mineo, S Rappaport, S Steinhorn, B Levine, A Gilfanov, M Pooley, D AF Mineo, S. Rappaport, S. Steinhorn, B. Levine, A. Gilfanov, M. Pooley, D. TI SPATIALLY RESOLVED STAR FORMATION IMAGE AND THE ULTRALUMINOUS X-RAY SOURCE POPULATION IN NGC 2207/IC 2163 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; galaxies: individual (NGC 2207/IC 2163); galaxies: interactions; galaxies: nuclei; galaxies: starburst; galaxies: structure; stars: formation; stars: luminosity function, mass function; stars: neutron ID SPACE-TELESCOPE OBSERVATIONS; CARTWHEEL RING GALAXY; BLACK-HOLES; INTERACTING GALAXIES; LUMINOSITY FUNCTION; GRAZING ENCOUNTER; ANTENNAE GALAXIES; FORMING GALAXIES; NUMBER COUNTS; XMM-NEWTON AB The colliding galaxy pair NGC 2207/IC 2163, at a distance of similar to 39 Mpc, was observed with Chandra, and an analysis reveals 28 well resolved X-ray sources, including 21 ultraluminous X-ray sources (ULXs) with L-X greater than or similar to 10(39) erg s(-1), as well as the nucleus of NGC 2207. The number of ULXs is comparable with the largest numbers of ULXs per unit mass in any galaxy yet reported. In this paper we report on these sources, and quantify how their locations correlate with the local star formation rates seen in spatially resolved star formation rate density images that we have constructed using combinations of GALEX FUV and Spitzer 24 mu m images. We show that the numbers of ULXs are strongly correlated with the local star formation rate densities surrounding the sources, but that the luminosities of these sources are not strongly correlated with star formation rate density. C1 [Mineo, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rappaport, S.] MIT Dept Phys, Cambridge, MA 02139 USA. [Rappaport, S.] Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Rappaport, S.; Pooley, D.] Eureka Sci, El Sobrante, CA 94803 USA. [Steinhorn, B.] Harvard Univ, Sch Med, Harvard MIT Div Hlth Sci & Technol, Boston, MA 02115 USA. [Levine, A.] MIT Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Gilfanov, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Gilfanov, M.] Russian Acad Sci, Space Res Inst, Moscow 117997, Russia. RP Mineo, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smineo@head.cfa.harvard.edu; sar@mit.edu; bsteinho@mit.edu; aml@space.mit.edu; gilfanov@mpa-garching.mpg.de; pooley@gmail.com FU Chandra Grants [GO1-12111X, GO2-13105A]; NASA; National Science Foundation FX The authors are grateful to Michele Kaufman, Mark Krumholz, Adam Leroy, and Pepi Fabbiano for helpful discussions. The authors thank the anonymous referee for helpful comments that improved this paper. S.R., D.P., and A.L. acknowledge support from Chandra Grants GO1-12111X and GO2-13105A. We made use of Chandra archival data and software provided by the Chandra X-ray Center (CXC) in the application package CIAO. We also utilized the software tool SAOImage DS9, developed by Smithsonian Astrophysical Observatory. The FUV, 3.6 mu m, and 24 mu m images were taken from GALEX and Spitzer archives, respectively. The Spitzer Space Telescope is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the NASA. GALEX is a NASA Small Explorer, launched in 2003 April. We also made use 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 National Science Foundation. Helpful information was found in 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 55 TC 7 Z9 7 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 133 DI 10.1088/0004-637X/771/2/133 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700058 ER PT J AU Oberg, KI Boamah, MD Fayolle, EC Garrod, RT Cyganowski, CJ van der Tak, F AF Oeberg, Karin I. Boamah, Mavis D. Fayolle, Edith C. Garrod, Robin T. Cyganowski, Claudia J. van der Tak, Floris TI THE SPATIAL DISTRIBUTION OF ORGANICS TOWARD THE HIGH-MASS YSO NGC 7538 IRS9 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; circumstellar matter; ISM: individual objects (NGC 7538 IRS9); molecular processes; stars: formation; stars: massive ID STAR-FORMING REGIONS; BIPOLAR MOLECULAR OUTFLOWS; YOUNG STARS; HOT CORES; COMPLEX CHEMISTRY; METHANOL MASERS; CHEMICAL-MODEL; NGC-7538 IRS-9; LINE SURVEY; PROTOSTARS AB Complex molecules have been broadly classified into three generations dependent on the mode of formation and the required formation temperature (<25, 25-100 K, and >100 K). Around massive young stellar objects (MYSOs), icy grain mantles and gas are exposed to increasingly higher temperatures as material accretes from the outer envelope in toward the central hot region. The combination of this temperature profile and the generational chemistry should result in a changing complex molecular composition with radius around MYSOs. We combine IRAM 30 m and Submillimeter Array observations to explore the spatial distribution of organic molecules around the high-mass young stellar object NGC 7538 IRS9, whose weak complex molecule emission previously escaped detection. We find that emission from N-bearing organics and CH3OH present substantial increases in emission around 8000 AU and R <3000 AU, while unsaturated O-bearing molecules and hydrocarbons do not. The increase in line flux for some complex molecules in the envelope, around 8000 AU or 25 K, is consistent with recent model predictions of an onset of complex ice chemistry at 20-30 K. The emission increase for many of the same molecules at R <3000 AU suggests the presence of a weak hot core, where thermal ice evaporation and hot gas-phase reactions drive the chemistry. Complex organics thus form at all radii and temperatures around this protostar, but the composition changes dramatically as the temperature increases, which is used together with an adapted gas-grain astrochemical model to constrain the chemical generation(s) to which different classes of molecules belong. C1 [Oeberg, Karin I.] Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. [Oeberg, Karin I.] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Boamah, Mavis D.] Wellesley Coll, Wellesley, MA 02481 USA. [Fayolle, Edith C.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Garrod, Robin T.] Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. [Cyganowski, Claudia J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [van der Tak, Floris] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [van der Tak, Floris] SRON Netherlands Inst Space Res, NL-9747 AD Groningen, Netherlands. RP Oberg, KI (reprint author), Univ Virginia, Dept Chem, Charlottesville, VA 22904 USA. EM oberg@virginia.edu OI Fayolle, Edith/0000-0001-8109-5256 FU Smithsonian Institution; Academia Sinica; NASA Astrophysics Theory Program [NNX11AC38G]; NSF [AST-1003134] FX The manuscript has benefited from discussions with Ewine van Dishoeck and comments and suggestions from an anonymous referee. 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. R.T.G. acknowledges support from the NASA Astrophysics Theory Program through grant NNX11AC38G. C.J.C. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1003134. NR 40 TC 10 Z9 10 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 JUL 10 PY 2013 VL 771 IS 2 AR 95 DI 10.1088/0004-637X/771/2/95 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700020 ER PT J AU Sohn, J Hwang, HS Lee, MG Lee, GH Lee, JC AF Sohn, Jubee Hwang, Ho Seong Lee, Myung Gyoon Lee, Gwang-Ho Lee, Jong Chul TI ACTIVITY IN GALACTIC NUCLEI OF COMPACT GROUP GALAXIES IN THE LOCAL UNIVERSE SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: groups: general; galaxies: interactions; galaxies: nuclei ID DIGITAL SKY SURVEY; HOST GALAXIES; X-RAY; BLACK-HOLES; INFRARED GALAXIES; ELLIPTIC GALAXIES; SCALING RELATIONS; FORMING GALAXIES; STAR-FORMATION; RICH CLUSTERS AB We study the nuclear activity of galaxies in local compact groups. We use a spectroscopic sample of 238 galaxies in 58 compact groups from the Sloan Digital Sky Survey data release 7 to estimate the fraction of active galactic nucleus (AGN) host galaxies in compact groups, and to compare it with those in cluster and field regions. We use emission-line ratio diagrams to identify AGN host galaxies and find that the AGN fraction of compact group galaxies is 17%-42% depending on the AGN classification method. The AGN fraction in compact groups is not the highest among the galaxy environments. This trend remains even if we use several subsamples segregated by galaxy morphology and optical luminosity. The AGN fraction for early-type galaxies decreases with increasing galaxy number density, but the fraction for late-type galaxies changes little. We find no mid-infrared detected AGN host galaxies in our sample of compact groups using Wide-field Infrared Survey Explorer data. These results suggest that the nuclear activity of compact group galaxies (mostly early types) is not strong because of lack of gas supply even though they may experience frequent galaxy-galaxy interactions and mergers that could trigger nuclear activity. C1 [Sohn, Jubee; Lee, Myung Gyoon; Lee, Gwang-Ho] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. [Hwang, Ho Seong] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Lee, Jong Chul] Korea Astron & Space Sci Inst, Taejon 305348, South Korea. RP Sohn, J (reprint author), Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151742, South Korea. EM jbsohn@astro.snu.ac.kr; hhwang@cfa.harvard.edu; mglee@astro.snu.ac.kr; ghlee@astro.snu.ac.kr; jclee@kasi.re.kr FU Mid-career Researcher Program through an NRF; MEST [2010-0013875, 2011-0007215]; Global Ph.D. Fellowship Program through an NRF; NRF; Korean Government; National Aeronautics and Space Administration; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX We thank the anonymous referee for useful comments that improved the manuscript. This work is supported in part by a Mid-career Researcher Program through an NRF grant funded by the MEST (No. 2010-0013875). J.S. is supported by Global Ph.D. Fellowship Program through an NRF funded by the MEST (No. 2011-0007215). H.S.H. acknowledges the Smithsonian Institution for supporting his post-doctoral fellowship. G.H.L. acknowledges support by the NRF grant funded by the Korean Government (NRF-2012-Fostering Core Leaders of the Future Basic Science Program). J.C.L. is a member of Dedicated Researchers for Extragalactic AstronoMy (DREAM) in Korea Astronomy and Space Science Institute (KASI). This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. 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, 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 76 TC 9 Z9 9 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 10 PY 2013 VL 771 IS 2 AR 106 DI 10.1088/0004-637X/771/2/106 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176XS UT WOS:000321340700031 ER PT J AU Zahid, HJ Geller, MJ Kewley, LJ Hwang, HS Fabricant, DG Kurtz, MJ AF Zahid, H. Jabran Geller, Margaret J. Kewley, Lisa J. Hwang, Ho Seong Fabricant, Daniel G. Kurtz, Michael J. TI THE CHEMICAL EVOLUTION OF STAR-FORMING GALAXIES OVER THE LAST 11 BILLION YEARS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: abundances; galaxies: evolution; galaxies: high-redshift; galaxies: ISM ID MASS-METALLICITY RELATION; ACTIVE GALACTIC NUCLEI; REDSHIFT SURVEY; HOST GALAXIES; STELLAR MASS; OXYGEN; GAS; LUMINOSITY; ABUNDANCES; OUTFLOWS AB We calculate the stellar mass-metallicity relation at five epochs ranging to z similar to 2.3. We quantify evolution in the shape of the mass-metallicity relation as a function of redshift; the mass-metallicity relation flattens at late times. There is an empirical upper limit to the gas-phase oxygen abundance in star-forming galaxies that is independent of redshift. From examination of the mass-metallicity relation and its observed scatter, we show that the flattening at late times is a consequence of evolution in the stellar mass where galaxies enrich to this empirical upper metallicity limit; there is also evolution in the fraction of galaxies at a fixed stellar mass that enrich to this limit. The stellar mass where metallicities begin to saturate is similar to 0.7 dex smaller in the local universe than it is at z similar to 0.8. C1 [Zahid, H. Jabran; Kewley, Lisa J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Zahid, H. Jabran; Geller, Margaret J.; Hwang, Ho Seong; Fabricant, Daniel G.; Kurtz, Michael J.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Kewley, Lisa J.] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. RP Zahid, HJ (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Kurtz, Michael/0000-0002-6949-0090 FU NSF EARLY CAREER AWARD [AST07-48559] FX We thank the referee for useful comments that improved the content of this Letter, John Moustakas, Vivienne Wilde, and Nelson Caldwell for providing useful advice and routines, and Kiyoto Yabe and Dawn Erb for sharing their data. We thank Susan Tokarz, Sean Moran, and Warren Brown for the careful reduction of the SHELS data, and Mike Calkins and Perry Berlind for operating Hectospec. H. J. Z. is grateful to Freeha Riaz and Ananda Wickramsekera for their warm and generous hospitality. H. J. Z. and L. J. K. acknowledge support by NSF EARLY CAREER AWARD AST07-48559. NR 44 TC 62 Z9 61 U1 1 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 10 PY 2013 VL 771 IS 2 AR L19 DI 10.1088/2041-8205/771/2/L19 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 172WI UT WOS:000321036000001 ER PT J AU Blaimer, BB Fisher, BL AF Blaimer, Bonnie B. Fisher, Brian L. TI How Much Variation Can One Ant Species Hold? Species Delimitation in the Crematogaster kelleri-Group in Madagascar SO PLOS ONE LA English DT Article ID HYMENOPTERA-FORMICIDAE; EVOLUTION; BIOGEOGRAPHY; PHYLOGENY; DNA; INFERENCE; REVISION; TAXONOMY; HISTORY; MODELS AB We investigated the species-level taxonomy of the Malagasy Crematogaster (Crematogaster) kelleri-group and an additional more distantly related species of the same subgenus. Morphological data from worker, queen and male ants, as well as genetic data from three nuclear genes (long wavelength rhodopsin, arginine kinase and carbomoylphosphate synthase) and one mitochondrial marker (cytochrome oxidase I) led to the recognition of six species. Within the C. kelleri-group, three new species are described: C. hazolava Blaimer sp. n., C. hafahafa Blaimer sp. n. and C. tavaratra Blaimer sp. n. The previously described taxa C. kelleri Forel and C. madagascariensis Andre are validated by our analysis. Conversely, our data suggests synonymy of C. adrepens Forel (with C. kelleri) and C. gibba Emery (with C. madagascariensis). A more distantly related and phylogenetically isolated species, C. tsisitsilo Blaimer sp. n., is further described. We report high levels of morphological and molecular variation in C. kelleri and illustrate that this variation can be explained partly by geography. Species descriptions, images, distribution maps and identification keys based on worker ants, as well as on queen and male ants where available, are presented for all six species. Our work highlights the elevated species richness of Crematogaster ants throughout Madagascar's humid forests, especially in the far northern tip of the island, and the need to use multiple data sources to ensure clear demarcation of this diversity. C1 [Blaimer, Bonnie B.] Smithsonian Inst, Dept Entomol, Washington, DC 20560 USA. [Blaimer, Bonnie B.; Fisher, Brian L.] Calif Acad Sci, Dept Entomol, San Francisco, CA 94118 USA. [Blaimer, Bonnie B.] Univ Calif Davis, Dept Entomol, Davis, CA 95616 USA. RP Blaimer, BB (reprint author), Smithsonian Inst, Dept Entomol, NHB 169, Washington, DC 20560 USA. EM bonnieblaimer@gmail.com OI Fisher, Brian/0000-0002-4653-3270 FU National Science Foundation [DEB-0072713, DEB-0344731, DEB-0842395, DEB-0842204, DEB-1107515]; Entomology Department at UC Davis; National Geographic Society [W173-11]; American Philosophical Society FX This research was funded by the National Science Foundation (www.nsf.gov; grants DEB-0072713, DEB-0344731, DEB-0842395 to B.L.F., DEB-0842204 to P.S. Ward and DEB-1107515 to B.B.B. and P.S. Ward), the Entomology Department at UC Davis (entomology.ucdavis.edu; B.B.B.), the National Geographic Society (www.nationalgeographic.com; W173-11 to B.B.B.) and the American Philosophical Society (www.amphilsoc.org; Lewis & Clark grant to B.B.B.). The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 44 TC 7 Z9 7 U1 0 U2 25 PU PUBLIC LIBRARY SCIENCE PI SAN FRANCISCO PA 1160 BATTERY STREET, STE 100, SAN FRANCISCO, CA 94111 USA SN 1932-6203 J9 PLOS ONE JI PLoS One PD JUL 9 PY 2013 VL 8 IS 7 AR e68082 DI 10.1371/journal.pone.0068082 PG 31 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 182JD UT WOS:000321736900053 PM 23874503 ER PT J AU Nguyen, DD Wu, CH Moree, WJ Lamsa, A Medema, MH Zhao, XL Gavilan, RG Aparicio, M Atencio, L Jackson, C Ballesteros, J Sanchez, J Watrous, JD Phelan, VV van de Wiel, C Kersten, RD Mehnaz, S De Mot, R Shank, EA Charusanti, P Nagarajan, H Duggan, BM Moore, BS Bandeira, N Palsson, BO Pogliano, K Gutierrez, M Dorrestein, PC AF Don Duy Nguyen Wu, Cheng-Hsuan Moree, Wilna J. Lamsa, Anne Medema, Marnix H. Zhao, Xiling Gavilan, Ronnie G. Aparicio, Marystella Atencio, Librada Jackson, Chanaye Ballesteros, Javier Sanchez, Joel Watrous, Jeramie D. Phelan, Vanessa V. van de Wiel, Corine Kersten, Roland D. Mehnaz, Samina De Mot, Rene Shank, Elizabeth A. Charusanti, Pep Nagarajan, Harish Duggan, Brendan M. Moore, Bradley S. Bandeira, Nuno Palsson, Bernhard O. Pogliano, Kit Gutierrez, Marcelino Dorrestein, Pieter C. TI MS/MS networking guided analysis of molecule and gene cluster families SO PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA LA English DT Article DE MS/MS molecular networking; mass spectrometry; microbial ecology ID DESORPTION ELECTROSPRAY-IONIZATION; NONRIBOSOMAL PEPTIDE SYNTHETASES; AMBIENT MASS-SPECTROMETRY; GENOME-MINING APPROACH; RAPID IDENTIFICATION; ADENYLATION DOMAINS; BACTERIAL GENOMICS; BIOSYNTHESIS; POLYKETIDE; INTACT AB The ability to correlate the production of specialized metabolites to the genetic capacity of the organism that produces such molecules has become an invaluable tool in aiding the discovery of biotechnologically applicable molecules. Here, we accomplish this task by matching molecular families with gene cluster families, making these correlations to 60 microbes at one time instead of connecting one molecule to one organism at a time, such as how it is traditionally done. We can correlate these families through the use of nanospray desorption electrospray ionization MS/MS, an ambient pressure MS technique, in conjunction with MS/MS networking and peptidogenomics. We matched the molecular families of peptide natural products produced by 42 bacilli and 18 pseudomonads through the generation of amino acid sequence tags from MS/MS data of specific clusters found in the MS/MS network. These sequence tags were then linked to biosynthetic gene clusters in publicly accessible genomes, providing us with the ability to link particular molecules with the genes that produced them. As an example of its use, this approach was applied to two unsequenced Pseudoalteromonas species, leading to the discovery of the gene cluster for a molecular family, the bromoalterochromides, in the previously sequenced strain P. piscicida JCM 20779(T). The approach itself is not limited to 60 related strains, because spectral networking can be readily adopted to look at molecular family-gene cluster families of hundreds or more diverse organisms in one single MS/MS network. C1 [Don Duy Nguyen; Wu, Cheng-Hsuan; Zhao, Xiling; Watrous, Jeramie D.; van de Wiel, Corine; Dorrestein, Pieter C.] Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA. [Moree, Wilna J.; Phelan, Vanessa V.; van de Wiel, Corine; Duggan, Brendan M.; Moore, Bradley S.; Bandeira, Nuno; Dorrestein, Pieter C.] Univ Calif San Diego, Skaggs Sch Pharm & Pharmaceut Sci, La Jolla, CA 92093 USA. [Lamsa, Anne; Pogliano, Kit] Univ Calif San Diego, Div Biol Sci, La Jolla, CA 92093 USA. [Kersten, Roland D.; Moore, Bradley S.; Dorrestein, Pieter C.] Univ Calif San Diego, Scripps Inst Oceanog, Ctr Marine Biotechnol & Biomed, La Jolla, CA 92093 USA. [Charusanti, Pep; Nagarajan, Harish; Palsson, Bernhard O.] Univ Calif San Diego, Dept Bioengn, La Jolla, CA 92093 USA. [Bandeira, Nuno] Univ Calif San Diego, Dept Comp Sci & Engn, La Jolla, CA 92093 USA. [Bandeira, Nuno] Univ Calif San Diego, Natl Inst Hlth Ctr Computat Mass Spectrometry, La Jolla, CA 92093 USA. [Dorrestein, Pieter C.] Univ Calif San Diego, Dept Pharmacol, La Jolla, CA 92093 USA. [Medema, Marnix H.] Univ Groningen, Groningen Bioinformat Ctr, Dept Microbial Physiol, NL-9747 AG Groningen, Netherlands. [Gavilan, Ronnie G.; Aparicio, Marystella; Atencio, Librada; Jackson, Chanaye; Ballesteros, Javier; Sanchez, Joel; Gutierrez, Marcelino] Inst Sci Res & Technol Serv INDICASAT, Ctr Drug Discovery & Biodivers, City Of Knowledge 084301103, Panama. [Gavilan, Ronnie G.] Smithsonian Trop Res Inst, Ancon 084303092, Panama. [Mehnaz, Samina] Forman Christian Coll Univ, Dept Biol Sci, Lahore 54600, Pakistan. [De Mot, Rene] Katholieke Univ Leuven, Fac Biosci Engn, Ctr Microbial & Plant Genet, B-3001 Louvain, Belgium. [Shank, Elizabeth A.] Univ N Carolina, Dept Biol, Chapel Hill, NC 27599 USA. RP Dorrestein, PC (reprint author), Univ Calif San Diego, Dept Chem & Biochem, La Jolla, CA 92093 USA. EM pdorrestein@ucsd.edu RI Mehnaz, Samina/I-1533-2015; OI Charusanti, Pep/0000-0003-0009-6615; Shank, Elizabeth/0000-0002-4804-1966; Phelan, Vanessa/0000-0001-7156-9294; Medema, Marnix/0000-0002-2191-2821 FU Netherlands Technology Foundation (STW); Technology Programme of the Ministry of Economic Affairs (Grant STW) [10463]; Katholieke Universiteit Leuven Research Council Grant [GOA/011/2008]; National Institute of Health (NIH) [GM103809, GM097509, GM098105, AI095125, GM094802]; Fogarty International Center's International Cooperative Biodiversity Groups Program [TW006634]; Bruker Therapeutic Discovery Mass Spectrometry Center; NIH Grant [GMS10RR029121]; NIH/National Institute of General Medical Sciences Grant [8 P41 GM103485-05] FX We thank the Government of Panama (Autoridad Nacional del Ambiente and Aquatic Resources Authority of Panama) for granting permission to make the collections of the corals for the isolation of strains OT59 and 04M1A. M.H.M. was supported by The Netherlands Technology Foundation (STW), which is the applied science division of The Netherlands Organization for Scientific Research (NWO) and the Technology Programme of the Ministry of Economic Affairs (Grant STW 10463). R.D.M. acknowledges support from Katholieke Universiteit Leuven Research Council Grant GOA/011/2008. Financial support was provided by National Institute of Health (NIH) Grants GM103809 (to V.V.P.), GM097509 (to B.S.M., N.B., and P.C.D.), GM098105 (to B.O.P.) AI095125 (to K.P. and P.C.D.), and GM094802 (to P.C.D.) and the Fogarty International Center's International Cooperative Biodiversity Groups Program TW006634 (to M.G.). Instrumentation used in this study is supported by Bruker Therapeutic Discovery Mass Spectrometry Center and NIH Grant GMS10RR029121 (to P.C.D.). N.B. was partially supported by the NIH/National Institute of General Medical Sciences Grant 8 P41 GM103485-05. NR 60 TC 80 Z9 80 U1 9 U2 87 PU NATL ACAD SCIENCES PI WASHINGTON PA 2101 CONSTITUTION AVE NW, WASHINGTON, DC 20418 USA SN 0027-8424 J9 P NATL ACAD SCI USA JI Proc. Natl. Acad. Sci. U. S. A. PD JUL 9 PY 2013 VL 110 IS 28 BP E2611 EP E2620 DI 10.1073/pnas.1303471110 PG 10 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 183OT UT WOS:000321827000012 PM 23798442 ER PT J AU Cooke, R Ranere, A Pearson, G Dickau, R AF Cooke, Richard Ranere, Anthony Pearson, Georges Dickau, Ruth TI Radiocarbon chronology of early human settlement on the Isthmus of Panama (13,000-7000 BP) with comments on cultural affinities, environments, subsistence, and technological change SO QUATERNARY INTERNATIONAL LA English DT Article ID SOUTH-AMERICA; LATE PLEISTOCENE; HUMAN OCCUPATION; YOUNGER DRYAS; COSTA-RICA; STARCH GRAINS; NEW-WORLD; CLOVIS; SITE; HOLOCENE AB The first human migrants entering South America must have used the Isthmian route. Convincing archaeological evidence for pre-Clovis groups is lacking. Paleoindian artifacts including Clovis and Fishtail fluted projectile points have been found at several localities, but at only one site (Vampiros-1) in buried and radiocarbon-dated deposits (similar to 11,500-similar to 9000 BP). Close similarities between Clovis point reduction sequences at two Panamanian quarry-workshops to those of early US Clovis sites vouch for temporal proximity and suggest rapid movement of Clovis bands through Central America, 11,050-10,800 BP. Vampiros-1 and other rock-shelters were occupied during the early Holocene (10,000-7000 BP) when climate became warmer and wetter. Un-fluted bifacial projectile points were made until similar to 7000 BP. Widespread grinding stones and carbonized tree fruits announce a mixed economy at the beginning of the Holocene. Cultivated leren, arrowroot, squash and bottle gourd appeared by 8000 BP. There are no indicators of human activities at Lake La Yeguada (650 m asl), 14,000-11,150 BP, nor at Vampiros-1, 16,000-11,500 BP. Pre-Clovis populations were probably bound to the now-drowned Pacific coast. Intense burning and deforestation commenced at La Yeguada similar to 11,050 BP coevally with Clovis. Human impacts were thenceforth continuous. Swidden farming had largely removed forest cover by 7000 BP across seasonally arid Central Pacific Panama. Lake sediment data from forested areas with less seasonal climates on the Caribbean and Pacific watersheds indicate moderate human interference before 7000 BP. The mtDNA history of modern Panamanians confirms Native American continuity from before 10,000 BP and provides support for the Pacific route of initial dispersal into South America. (C) 2013 Elsevier Ltd and INQUA. All rights reserved. C1 [Cooke, Richard; Pearson, Georges] STRI Smithsonian Trop Res Inst, Ancon, Panama. [Ranere, Anthony] Temple Univ, Dept Anthropol, Philadelphia, PA 19122 USA. [Dickau, Ruth] Univ Exeter, Dept Archaeol, Exeter EX4 4QJ, Devon, England. RP Cooke, R (reprint author), Smithsonian Trop Res Inst, Apdo 0843-03092, Ancon, Panama. EM cooker@si.edu; ranere@temple.edu; georges_pearson@hotmail.com; rdickau@gmail.com FU Social Sciences and Humanities Research Council of Canada (SSHRC); Smithsonian Tropical Research Institute, Panama FX The authors would like to thank Dolores R. Piperno, Sebastien Perrot-Minot, Alessandro Achilli and Ugo Perego for making suggestions on various drafts or parts of them. Two anonymous reviewers reviewed the initial draft; their comments were most useful, and are greatly appreciated. John Griggs and Alvaro Brizuela provided information about a recent find of a re-sharpened fishtail projectile point near Lake Alajuela. Griggs also assisted with the preparation of the map. Alejandra Paton showed much patience and skill drawing the stone tools from Vampiros-1. We are grateful to Ben Turner for permitting analyses of Vampiros-1 soils in his laboratory at the Smithsonian Tropical Research Institute in Panama, and to Dayana Argudo for running the tests. Unpublished data have been included for Vampiros-1 (2004-2006 seasons). Fieldwork at Casita de Piedra was conducted by Ruth Dickau in 2007 with funding provided by the Social Sciences and Humanities Research Council of Canada (SSHRC). Pearson's excavations at Vampiros-1 in 2004-06 benefitted from a research grant from the Smithsonian Tropical Research Institute, Panama. Special thanks are due to Norm Catto and Gustavo Politis for their patience and understanding during the overly protracted preparation of this paper. NR 144 TC 8 Z9 8 U1 1 U2 22 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1040-6182 J9 QUATERN INT JI Quat. Int. PD JUL 8 PY 2013 VL 301 BP 3 EP 22 DI 10.1016/j.quaint.2013.02.032 PG 20 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 180NY UT WOS:000321603100002 ER PT J AU Meibom, S Torres, G Fressin, F Latham, DW Rowe, JF Ciardi, DR Bryson, ST Rogers, LA Henze, CE Janes, K Barnes, SA Marcy, GW Isaacson, H Fischer, DA Howell, SB Horch, EP Jenkins, JM Schuler, SC Crepp, J AF Meibom, Soren Torres, Guillermo Fressin, Francois Latham, David W. Rowe, Jason F. Ciardi, David R. Bryson, Steven T. Rogers, Leslie A. Henze, Christopher E. Janes, Kenneth Barnes, Sydney A. Marcy, Geoffrey W. Isaacson, Howard Fischer, Debra A. Howell, Steve B. Horch, Elliott P. Jenkins, Jon M. Schuler, Simon C. Crepp, Justin TI The same frequency of planets inside and outside open clusters of stars SO NATURE LA English DT Article ID INTERMEDIATE-MASS STARS; STELLAR CLUSTERS; NGC 6811; KEPLER; SYSTEMS; ISOCHRONES; DYNAMICS; FIELD AB Most stars and their planets form in open clusters. Over 95 per cent of such clusters have stellar densities too low (less than a hundred stars per cubic parsec) to withstand internal and external dynamical stresses and fall apart within a few hundred million years(1). Older open clusters have survived by virtue of being richer and denser in stars (1,000 to 10,000 per cubic parsec) when they formed. Such clusters represent a stellar environment very different from the birthplace of the Sun and other planet-hosting field stars. So far more than 800 planets have been found around Sun-like stars in the field(2). The field planets are usually the size of Neptune or smaller(3-5). In contrast, only four planets have been found orbiting stars in open clusters(6-8), all with masses similar to or greater than that of Jupiter. Here we report observations of the transits of two Sun-like stars by planets smaller than Neptune in the billion-year-old open cluster NGC6811. This demonstrates that small planets can form and survive in a dense cluster environment, and implies that the frequency and properties of planets in open clusters are consistent with those of planets around field stars in the Galaxy. C1 [Meibom, Soren; Torres, Guillermo; Fressin, Francois; Latham, David W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rowe, Jason F.; Bryson, Steven T.; Henze, Christopher E.; Howell, Steve B.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Ciardi, David R.] CALTECH, NASA, Exoplanet Sci Inst, Pasadena, CA 91125 USA. [Rogers, Leslie A.] CALTECH, Pasadena, CA 91125 USA. [Janes, Kenneth] Boston Univ, Boston, MA 02215 USA. [Barnes, Sydney A.] Leibniz Inst Astrophys, D-14467 Potsdam, Germany. [Barnes, Sydney A.] Space Sci Inst, Boulder, CO 80301 USA. [Marcy, Geoffrey W.; Isaacson, Howard] Univ Calif Berkeley, Berkeley, CA 94720 USA. [Fischer, Debra A.] Yale Univ, New Haven, CT 06520 USA. [Horch, Elliott P.] So Connecticut State Univ, New Haven, CT 06515 USA. [Jenkins, Jon M.] NASA, SETI Inst, Ames Res Ctr, Moffett Field, CA 94035 USA. [Schuler, Simon C.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Crepp, Justin] Univ Notre Dame, Notre Dame, IN 46556 USA. RP Meibom, S (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM smeibom@cfa.harvard.edu OI Ciardi, David/0000-0002-5741-3047; Schuler, Simon/0000-0001-7203-8014; Fischer, Debra/0000-0003-2221-0861 FU NASA's Science Mission Directorate; NASA [NNX09AH18A, HF-51313.01-A, NAS 5-26555]; Kepler mission via NASA Cooperative Agreement [NCC2-1390]; NASA's Kepler Participating Scientist Program [NNX12AC75G]; Space Telescope Science Institute FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. S. M. acknowledges support through NASA grant NNX09AH18A (The Kepler Cluster Study) and from the Kepler mission via NASA Cooperative Agreement NCC2-1390. G. T. acknowledges support through NASA's Kepler Participating Scientist Program grant NNX12AC75G. L. A. R. acknowledges NASA support through Hubble Fellowship grant HF-51313.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. NR 27 TC 37 Z9 37 U1 0 U2 9 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD JUL 4 PY 2013 VL 499 IS 7456 BP 55 EP 58 DI 10.1038/nature12279 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 176ED UT WOS:000321285600031 PM 23803764 ER PT J AU Ortega-Jimenez, VM Dudley, R AF Ortega-Jimenez, Victor Manuel Dudley, Robert TI Spiderweb deformation induced by electrostatically charged insects SO SCIENTIFIC REPORTS LA English DT Article ID ORB-WEAVING SPIDER; CAPTURE THREADS; SILK; WEBS; FORCES; ULOBORIDAE; STICKINESS AB Capture success of spider webs has been associated with their microstructure, ornamentation, and wind-induced vibrations. Indirect evidence suggests that statically charged objects can attract silk thread, but web deformations induced by charged insects have not yet been described. Here, we show under laboratory conditions that electrostatically charged honeybees, green bottle flies, fruit flies, aphids, and also water drops falling near webs of cross-spiders (Araneus diadematus) induce rapid thread deformation that enhances the likelihood of physical contact, and thus of prey capture. C1 [Ortega-Jimenez, Victor Manuel; Dudley, Robert] Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. [Dudley, Robert] Smithsonian Trop Res Inst, Balboa, Panama. RP Ortega-Jimenez, VM (reprint author), Univ Calif Berkeley, Dept Integrat Biol, Berkeley, CA 94720 USA. EM vortega@unc.edu OI Ortega-Jimenez, Victor Manuel/0000-0003-0024-5086 FU University of California MEXUS-CONACYT program FX We thank members of the Dudley flight mechanics lab and Daniel Hernandez-Cruz for their valuable comments and suggestions, and also Sarahi Arriaga-Ramirez for helping us with the apparatus used to measure charge. Victor Ortega was supported a grant from the University of California MEXUS-CONACYT program. NR 25 TC 9 Z9 9 U1 0 U2 35 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2045-2322 J9 SCI REP-UK JI Sci Rep PD JUL 4 PY 2013 VL 3 AR 2108 DI 10.1038/srep02108 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 176EP UT WOS:000321286800001 PM 23828093 ER PT J AU Mitchell, JC Smith, DG AF Mitchell, Joseph C. Smith, David G. TI Copeia 1913, Number 1: Origin and Authors SO COPEIA LA English DT Editorial Material C1 [Mitchell, Joseph C.] Mitchell Ecol Res Serv LLC, High Springs, FL 32655 USA. [Smith, David G.] Smithsonian Inst, Museum Support Ctr, Suitland, MD 20746 USA. RP Mitchell, JC (reprint author), Mitchell Ecol Res Serv LLC, POB 2520, High Springs, FL 32655 USA. EM dr.joe.mitchell@gmail.com; smithd@si.edu NR 10 TC 3 Z9 3 U1 2 U2 3 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD JUL 3 PY 2013 IS 2 BP 189 EP 193 DI 10.1643/OT-13-029 PG 5 WC Zoology SC Zoology GA AG2WL UT WOS:000335277700001 ER PT J AU Peixoto, LAW Dutra, GM de Santana, CD Wosiacki, WB AF Wanderley Peixoto, Luiz Antonio Dutra, Guilherme Moreira de Santana, Carlos David Wosiacki, Wolmar Benjamin TI A New Species of the Electric Fish Genus Hypopygus (Gymnotiformes: Hypopomidae) from the Lower Amazon Basin, Brazil SO COPEIA LA English DT Article ID OSTARIOPHYSI; TELEOSTEI AB Hypopygus benoneae, new species, is described from streams in the lower Rio Anapu, in the eastern portion of the Amazon basin, Brazil. The new species is diagnosed from all congeners by a unique set of characters, including the absence of the sixth infraorbital bone and 115-134 total anal-fin rays. Hypopygus benoneae, new species, is a member of a clade also comprising H. hoedemani, H. lepturus, and H. minissimus. The description of H. benoneae, new species, brings the number of species in Hypopygus to nine. A dichotomous key to the species of Hypopygus is provided. C1 [Wanderley Peixoto, Luiz Antonio; Dutra, Guilherme Moreira; de Santana, Carlos David; Wosiacki, Wolmar Benjamin] Museu Paraense Emilio Goeldi, BR-66040170 Belem, Para, Brazil. [de Santana, Carlos David] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Fishes, Washington, DC 20013 USA. RP Wosiacki, WB (reprint author), Museu Paraense Emilio Goeldi, Caixa Postal 399, BR-66040170 Belem, Para, Brazil. EM luizwp@yahoo.com.br; guilhermedutr@yahoo.com.br; csantana@museu-goeldi.br; wolmar@museu-goeldi.br RI Wosiacki, Wolmar/I-1724-2012 OI Wosiacki, Wolmar/0000-0002-4013-8501 NR 10 TC 1 Z9 2 U1 1 U2 4 PU AMER SOC ICHTHYOLOGISTS & HERPETOLOGISTS PI MIAMI PA MAUREEN DONNELLY, SECRETARY FLORIDA INT UNIV BIOLOGICAL SCIENCES, 11200 SW 8TH STREET, MIAMI, FL 33199 USA SN 0045-8511 EI 1938-5110 J9 COPEIA JI Copeia PD JUL 3 PY 2013 IS 2 BP 232 EP 237 DI 10.1643/CI-12-087 PG 6 WC Zoology SC Zoology GA AG2WL UT WOS:000335277700007 ER PT J AU Neale, P AF Neale, Patrick TI Species-Specific Responses to Combined Thermal-irradiance Stress in Microalgae - "Each is to its Own" SO PHOTOCHEMISTRY AND PHOTOBIOLOGY LA English DT Article ID PHOTOSYNTHESIS; PHOTOPROTECTION; PHOTOPHYSIOLOGY; PHYTOPLANKTON; ADAPTATION AB This article is a highlight of the study by Stamenkovic and Hanelt in this issue of Photochemistry and Photobiology describing the high-irradiance photophysiology of several strains of freshwater chlorophyte microalgal genus, Cosmarium. These strains exhibit distinct differences in how combined thermal- high irradiance stress is managed which can be related to the temperature and irradiance conditions of their native habitat. C1 Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. RP Neale, P (reprint author), Smithsonian Environm Res Ctr, POB 28, Edgewater, MD 21037 USA. EM nealep@si.edu NR 14 TC 1 Z9 1 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0031-8655 EI 1751-1097 J9 PHOTOCHEM PHOTOBIOL JI Photochem. Photobiol. PD JUL PY 2013 VL 89 IS 4 SI SI BP 822 EP 823 DI 10.1111/php.12081 PG 2 WC Biochemistry & Molecular Biology; Biophysics SC Biochemistry & Molecular Biology; Biophysics GA 284GN UT WOS:000329304200011 PM 23581710 ER PT J AU Baldwin, CC AF Baldwin, Carole C. TI The phylogenetic significance of colour patterns in marine teleost larvae SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE chromatophore; erythrophore; fish larvae; iridophore; western Caribbean; xanthophore ID EARLY-LIFE-HISTORY; WESTERN ATLANTIC; POPULATION CONNECTIVITY; EVOLUTIONARY HISTORY; MOLECULAR PHYLOGENY; LUTJANUS-SYNAGRIS; FISHES TELEOSTEI; CHEMICAL DEFENSE; FAMILY LABRIDAE; GOBIOID FISHES AB Ichthyologists, natural-history artists, and tropical-fish aquarists have described, illustrated, or photographed colour patterns in adult marine fishes for centuries, but colour patterns in marine fish larvae have largely been neglected. Yet the pelagic larval stages of many marine fishes exhibit subtle to striking, ephemeral patterns of chromatophores that warrant investigation into their potential taxonomic and phylogenetic significance. Colour patterns in larvae of over 200 species of marine teleosts, primarily from the western Caribbean, were examined from digital colour photographs, and their potential utility in elucidating evolutionary relationships at various taxonomic levels was assessed. Larvae of relatively few basal marine teleosts exhibit erythrophores, xanthophores, or iridophores (i.e. nonmelanistic chromatophores), but one or more of those types of chromatophores are visible in larvae of many basal marine neoteleosts and nearly all marine percomorphs. Whether or not the presence of nonmelanistic chromatophores in pelagic marine larvae diagnoses any major teleost taxonomic group cannot be determined based on the preliminary survey conducted, but there is a trend toward increased colour from elopomorphs to percomorphs. Within percomorphs, patterns of nonmelanistic chromatophores may help resolve or contribute evidence to existing hypotheses of relationships at multiple levels of classification. Mugilid and some beloniform larvae share a unique ontogenetic transformation of colour pattern that lends support to the hypothesis of a close relationship between them. Larvae of some tetraodontiforms and lophiiforms are strikingly similar in having the trunk enclosed in an inflated sac covered with xanthophores, a character that may help resolve the relationships of these enigmatic taxa. Colour patterns in percomorph larvae also appear to diagnose certain groups at the interfamilial, familial, intergeneric, and generic levels. Slight differences in generic colour patterns, including whether the pattern comprises xanthophores or erythrophores, often distinguish species. The homology, ontogeny, and possible functional significance of colour patterns in larvae are discussed. Considerably more investigation of larval colour patterns in marine teleosts is needed to assess fully their value in phylogenetic reconstruction.(c) 2013 The Linnean Society of London C1 Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. RP Baldwin, CC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Fishes, Washington, DC 20560 USA. EM baldwinc@si.edu FU Hunterdon Oceanographic Research Fund; Herbert R. and Evelyn Axelrod Endowment Fund for systematic ichthyology FX David Smith and Lee Weigt contributed to the field work that resulted in the Belize larval-fish images in numerous ways. The molecular data that enabled identifications of larvae analysed in this paper were published by Weigt etal. (2012), and a complete list of acknowledgements for the Belize field work is provided in that paper. Julie Mounts contributed greatly to photographic efforts in Belize. David Smith provided identifications of several larvae not identified through DNA analysis. David Johnson identified or corrected my misidentifications of species represented in several images by Joshua Lambus and Cedric Guigand, and he provided contact information for those photographers and Donald Hughes. I thank Allan Connell, Cedric Guigand, Joshua Lambus, Matthew D'Avella, Michael Miller, Donald Hughes, Chris Papero, Todd Gardner, Matthew Wittenrich, Robert Cowen, Daniel Benetti, and Dallas Alston for allowing me to use their images of fish larvae or assisting me in locating images. The addition of numerous fish species not represented in the Belize material greatly increased the taxonomic scope of the paper, and many of the additional images are so stunning that it was a privilege to study and incorporate them into this work. Ross Robertson provided a portable Wacom tablet and provided instructions on how to remove images from their original backgrounds. Without this editorial procedure, many of the Belize larval-fish images would not have been publishable. Sandra Raredon and Jeff Williams provided initial guidance on the best photographic equipment and equipment set-up for photography in the field. Wen-Hsiung Li, Chief Editor of Zoological Studies, and Aoi Sasaki of TERRAPUB (publisher of Aqua-BioScience Monographs), allowed the images in Figure 4B and Figure 5, respectively, to be reproduced. Katsumi Aida, Editor in Chief of Aqua-BioScience Monographs, facilitated communication with Sasaki. Fabio Di Dario, this journal's editorial staff, and anonymous reviewers provided suggestions that greatly improved the manuscript. This is contribution number 937 of the Caribbean Coral Reef Ecosystems Program, Smithsonian Institution, supported in part by the Hunterdon Oceanographic Research Fund. Publication of the colour figures was made possible in part through the generous support of the Herbert R. and Evelyn Axelrod Endowment Fund for systematic ichthyology and Mrs. Alexandra S. Baldwin. NR 109 TC 8 Z9 8 U1 0 U2 14 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 2013 VL 168 IS 3 BP 496 EP 563 DI 10.1111/zoj.12033 PG 68 WC Zoology SC Zoology GA 279KU UT WOS:000328959700004 ER PT J AU Santana, CD Vari, RP AF de Santana, Carlos David Vari, Richard P. TI Brown ghost electric fishes of the Apteronotus leptorhynchus species-group (Ostariophysi, Gymnotiformes); monophyly, major clades, and revision SO ZOOLOGICAL JOURNAL OF THE LINNEAN SOCIETY LA English DT Article DE cladistics; Guyana Shield; historical biogeography; morphological stasis; phylogenetics; sexual dimorphism ID FRESH-WATER FISHES; COLOMBIA GYMNOTIFORMES; EVOLUTIONARY STASIS; KNIFEFISH; MIOCENE; GENUS; TELEOSTEI; REDESCRIPTION; MORPHOLOGY; VENEZUELA AB Neotropical brown ghost electric knifefishes of the Apteronotus leptorhynchus species-group are reviewed. A series of synapomorphies delimit the species-group and the two major subunits that comprise that clade. The phylogeny is concordant with the hypothesis of a primary division within the clade resultant from Andean uplift events 8Mya and with the existence of ancestral components of the species-group 12Mya. Species of the species-group are characterized by morphological stasis across that time frame. Apteronotus leptorhynchus, previously considered to be a widely distributed and morphologically variable species, was found to encompass five species. The description of the four new species is supplemented by the redescription of the five previously recognized forms within the species-group. Members of this clade are broadly distributed through the Essequibo River and Rio Orinoco of the Atlantic slope of South America, the Rios Aroa, Atrato, Cauca, Magdalena, and Yaracuy, and the rivers of the Lago Maracaibo basin of the Caribbean slope and drainages in northern Colombia and Panama along the Pacific versant.(c) 2013 The Linnean Society of London C1 [de Santana, Carlos David; Vari, Richard P.] Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Vari, RP (reprint author), Smithsonian Inst, Div Fishes, Dept Vertebrate Zool, Natl Museum Nat Hist, MRC-159,Box 37012, Washington, DC 20013 USA. EM varir@si.edu FU Herbert R. and Evelyn Axelrod Chair; Postdoctoral Fellowship in the Division of Fishes, National Museum of Natural History, Smithsonian Institution FX Research associated with the project was supported by the Herbert R. and Evelyn Axelrod Chair and a Postdoctoral Fellowship in the Division of Fishes, National Museum of Natural History, Smithsonian Institution. We thank D. Taphorn for early discussions and insights on the Apteronotus species from Venezuela. We thank Jonathan Armbruster and David Werneke (AUM); Oliver Crimmen and James Maclain (BMNH); David Catania (CAS); Leo Smith and Mary Anne Rogers (FMNH); Javier Maldonado-Ocampo (IAvHP); Michael Retzer and Christopher Taylor (INHS); Lucia Rapp Py-Daniel (INPA); Francisco Provenzano (MBUCV); Donald Taphorn (MCNG); Karsten Hartel and Andrew Williston (MCZ); Paulo Buckup (MNRJ); Wolmar Wosiacki (MPEG); Mario de Pinna and Osvaldo Oyakawa (MZUSP); and Ronald Vonk (ZMA) for the loan of specimens and assistance during visits to their institutions. Sandra Raredon, Lisa Palmer, and Jeffrey Clayton provided assistance at USNM. Illustrations of specimens were prepared by T. Britt Griswold and the maps by Sandra Raredon (USNM). Figures 1 and 2 were prepared by Ai Nonaka and David Johnson. The manuscript benefitted from comments by Carl J. Ferraris, Jr. NR 78 TC 0 Z9 2 U1 2 U2 6 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 2013 VL 168 IS 3 BP 564 EP 596 DI 10.1111/zoj.12022 PG 33 WC Zoology SC Zoology GA 279KU UT WOS:000328959700005 ER PT J AU Lucas, RW Salguero-Gomez, R Cobb, DB Waring, BG Anderson, F McShea, WJ Casper, BB AF Lucas, Richard W. Salguero-Gomez, Roberto Cobb, David B. Waring, Bonnie G. Anderson, Frank McShea, William J. Casper, Brenda B. TI White-tailed deer (Odocoileus virginianus) positively affect the growth of mature northern red oak (Quercus rubra) trees SO ECOSPHERE LA English DT Article DE competition release; deer waste mechanism; dendroecology; forest; herbivory; Shenandoah National Park; Smithsonian Conservation Biology Institute; tree cores ID BELOW-GROUND COMPETITION; TERRESTRIAL ECOSYSTEMS; NITROGEN AVAILABILITY; FOREST ECOSYSTEMS; CARBON ALLOCATION; TEMPERATE FOREST; ANTICOSTI ISLAND; BOREAL FORESTS; CLIMATE-CHANGE; PLANT AB Understanding and predicting the effects of deer (Cervidae) on forest ecosystems present significant challenges in ecosystem ecology. Deer herbivory can cause large changes in the biomass and species composition of forest understory plant communities, including early life-cycle trees (i. e., seedlings and saplings). Such changes can impact juvenile to adult transitions and the future age structure and species composition of mature forests. Changes to understory vegetation also impact flow of energy and nutrients in forest ecosystems. Studies examining the influence of deer on mature trees, however, are rare and rely on extrapolating effects from early life cycle stages of trees. We tested the hypothesis that the absence of deer would result in an increase in the growth rate of mature trees by examining the impact of white-tailed deer (Odocoileus virginianus) on mature canopy trees. We examined incremental growth in individuals of Quercus rubra, an important component of temperate deciduous forests in North America, inside and outside 16-year deer exclosures in eastern U.S. deciduous forests. We found that adult trees inside exclosures grew less than those directly exposed to deer. Our findings highlight the indirect effects of white-tailed deer on the growth of adult individuals of Q. rubra in a way opposite of what would be expected from previous studies based on immature or understory tree populations. We suggest the increased growth of adult trees in the presence of deer may be explained by increased nutrient inputs through deer fecal and urine deposits and the alteration of the competitive environment belowground through the reduction of understory vegetation by browsing. Underscoring the ecological and demographic importance of adult trees in forest ecosystems, results from this study suggest the direct and indirect effects of deer on mature trees should not be overlooked. C1 [Lucas, Richard W.] SLU Swedish Univ Agr Sci, Dept Forest Ecol & Management, S-90183 Umea, Sweden. [Salguero-Gomez, Roberto] Max Planck Inst Demog Res, Evolutionary Biodemog Lab, D-18057 Rostock, Germany. [Salguero-Gomez, Roberto] Univ Queensland, Sch Biol Sci, Brisbane, Qld 4072, Australia. [Cobb, David B.] Univ Penn, Dept Cell & Dev Biol, Philadelphia, PA 19104 USA. [Waring, Bonnie G.] Univ Texas Austin, Dept Ecol Evolut & Behav, Austin, TX 78712 USA. [Anderson, Frank; Casper, Brenda B.] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [McShea, William J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Front Royal, VA 22630 USA. RP Lucas, RW (reprint author), SLU Swedish Univ Agr Sci, Dept Forest Ecol & Management, S-90183 Umea, Sweden. EM rlucas49@gmail.com RI Salguero-Gomez, Roberto/N-6016-2016 OI Salguero-Gomez, Roberto/0000-0002-6085-4433 FU Forests, a multi-disciplinary research program; MISTRA; Swedish Forestry Industry, SLU, Umea University, and Skogforsk FX We would like to express our thanks to M. Baker, R.S.G. Lucas, and other members of the BIOL 465 course of the University of Pennsylvania for help collecting field samples, the staff at the SCBI and SNP for facilitating sample collection, and to M. R. Lesser, N.J. Hasselquist, and R.A. Sponseller for comments on earlier versions of the manuscript. R. W. L. acknowledges funding from Future Forests, a multi-disciplinary research program supported by MISTRA, the Swedish Forestry Industry, SLU, Umea University, and Skogforsk. NR 66 TC 5 Z9 5 U1 10 U2 79 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 2150-8925 J9 ECOSPHERE JI Ecosphere PD JUL PY 2013 VL 4 IS 7 AR UNSP 84 DI 10.1890/ES13-00036.1 PG 15 WC Ecology SC Environmental Sciences & Ecology GA 256TC UT WOS:000327335800007 ER PT J AU Brearley, AJ Fagan, TJ Washio, M MacPherson, GJ AF Brearley, A. J. Fagan, T. J. Washio, M. MacPherson, G. J. TI ALTERATION VEINS IN ALLENDE CAIS: PRELIMINARY FIB/TEM OBSERVATIONS. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc ID RICH INCLUSIONS C1 [Brearley, A. J.] Univ New Mexico, Albuquerque, NM 87131 USA. [Fagan, T. J.; Washio, M.] Waseda Univ, Tokyo, Japan. [MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. NR 6 TC 0 Z9 0 U1 0 U2 1 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 2013 VL 48 SU 1 SI SI BP A68 EP A68 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800038 ER PT J AU Bullock, ES Corrigan, CM McCoy, TJ Hill, K AF Bullock, E. S. Corrigan, C. M. McCoy, T. J. Hill, K. TI UNRAVELING THE METAMORPHIC, IMPACT AND COOLING HISTORY OF EH3 CHONDRITES. SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Bullock, E. S.; Corrigan, C. M.; McCoy, T. J.; Hill, K.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM BullockE@si.edu NR 7 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A72 EP A72 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800042 ER PT J AU Corrigan, CM Lunning, NG AF Corrigan, C. M. Lunning, N. G. TI THE DIFFICULTY OF FINDING ANCIENT MELT CLASTS IN ORDINARY CHONDRITE IMPACT BRECCIAS SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Corrigan, C. M.] Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20560 USA. [Lunning, N. G.] Univ Tennessee, Knoxville, TN 37996 USA. EM corriganc@si.edu NR 15 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A95 EP A95 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800065 ER PT J AU Corrigan, CM Velbel, MA Vicenzi, EP Konicek, A AF Corrigan, C. M. Velbel, M. A. Vicenzi, E. P. Konicek, A. TI NAKHLITE NWA 5790: MODAL MINERALOGY AND COMPARISON WITH THE REST OF THE NAKHLITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Corrigan, C. M.] Smithsonian Inst, Washington, DC 20560 USA. [Velbel, M. A.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD USA. [Konicek, A.] NIST, Surface & Microanal Sci Div, Gaithersburg, MD 20899 USA. EM corriganc@si.edu NR 6 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A96 EP A96 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800066 ER PT J AU Lunning, NG McSween, HY Beck, AW AF Lunning, N. G. McSween, H. Y., Jr. Beck, A. W. TI HETEROGENEITY IN THE VESTAN REGOLITH: EVIDENCE FROM THE GRO 95 HED PAIRING GROUP SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Lunning, N. G.; McSween, H. Y., Jr.] Univ Tennessee, Knoxville, TN 37996 USA. [Beck, A. W.] NMNH, Smithsonian Inst, Washington, DC 20560 USA. EM nlunning@utk.edu RI Beck, Andrew/J-7215-2015 OI Beck, Andrew/0000-0003-4455-2299 NR 4 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A227 EP A227 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800197 ER PT J AU McCoy, TJ McKeown, DA Buechele, AC Tappero, R Gardner-Vandy, KG AF McCoy, T. J. McKeown, D. A. Buechele, A. C. Tappero, R. Gardner-Vandy, K. G. TI DO ENSTATITE CHONDRITES RECORD MULTIPLE OXIDATION STATES? SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc ID ACHONDRITE C1 [McCoy, T. J.; Gardner-Vandy, K. G.] Smithsonian Inst, Washington, DC 20560 USA. [McKeown, D. A.; Buechele, A. C.] Catholic Univ, Washington, DC 20064 USA. [Tappero, R.] Brookhaven Natl Lab, Upton, NY 11791 USA. EM mccoyt@si.edu NR 6 TC 0 Z9 0 U1 1 U2 1 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 2013 VL 48 SU 1 SI SI BP A237 EP A237 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800207 ER PT J AU Righter, K Fries, MD Gibson, EK Harrington, R Keller, LP McCoy, TJ Morris, RV Nagao, K Nakamura-Messenger, K Niles, P Nyquist, L Park, J Peng, ZX Shih, CY Simon, JI Zeigler, RA AF Righter, K. Fries, M. D. Gibson, E. K. Harrington, R. Keller, L. P. McCoy, T. J. Morris, R. V. Nagao, K. Nakamura-Messenger, K. Niles, P. Nyquist, L. Park, J. Peng, Z. X. Shih, C-Y Simon, J. I. Zeigler, R. A. TI CONSORTIUM STUDY OF THE CHELYABINSK METEORITE SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Righter, K.; Fries, M. D.; Gibson, E. K.; Keller, L. P.; Morris, R. V.; Niles, P.; Nyquist, L.; Simon, J. I.; Zeigler, R. A.] NASA, JSC, Houston, TX 77058 USA. [Harrington, R.; Nakamura-Messenger, K.; Peng, Z. X.; Shih, C-Y] NASA, JSC, JETS, Houston, TX 77058 USA. [McCoy, T. J.] Smithsonian Inst, Washington, DC 20560 USA. [Nagao, K.] Univ Tokyo, Earthquake Chem Lab, Bunkyo Ku, Tokyo 1130033, Japan. [Park, J.] Rutgers State Univ, Dept Chem, Wright Labs, Piscataway, NJ USA. NR 2 TC 0 Z9 0 U1 0 U2 2 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 2013 VL 48 SU 1 SI SI BP A296 EP A296 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800266 ER PT J AU Takigawa, A Vicenzi, EP Wight, S Alexander, CMO Nittler, LR Stroud, RM Huss, GR AF Takigawa, A. Vicenzi, E. P. Wight, S. Alexander, C. M. O'D. Nittler, L. R. Stroud, R. M. Huss, G. R. TI CATHODOLUMINESCENCE SPECTROSCOPY OF PRESOLAR AND SOLAR AL(2)O(3) GRAINS IN ORDINARY CHONDRITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Takigawa, A.; Alexander, C. M. O'D.] Carnegie Inst Sci, Washington, DC USA. [Takigawa, A.] Kyoto Univ, Kyoto 6068501, Japan. [Vicenzi, E. P.] Smithsonian Inst, Washington, DC 20560 USA. [Huss, G. R.] Univ Hawaii Manoa, Honolulu, HI 96822 USA. EM atakigawa@ciw.edu RI Takigawa, Aki/F-1160-2016 OI Takigawa, Aki/0000-0002-0649-6997 NR 3 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A335 EP A335 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800305 ER PT J AU Velbel, MA Corrigan, CM Vicenzi, EP Konicek, AR Lunning, N AF Velbel, M. A. Corrigan, C. M. Vicenzi, E. P. Konicek, A. R. Lunning, N. TI MODAL ABUNDANCES OF MAJOR PHASES IN THE MILLER RANGE 03346 MARS METEORITE PAIRING GROUP AND COMPARISON WITH OTHER NAKHLITES SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc C1 [Velbel, M. A.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Velbel, M. A.; Corrigan, C. M.; Lunning, N.] Smithsonian Inst, Natl Museum Nat Hist, Dept Mineral Sci, Washington, DC 20013 USA. [Vicenzi, E. P.] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [Konicek, A. R.] NIST, Surface & Microanal Sci Div, Gaithersburg, MD 20899 USA. [Lunning, N.] Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. EM velbel@msu.edu NR 4 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A359 EP A359 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800329 ER PT J AU Williams, CD Hervig, RL Wadhwa, M Bullock, EM MacPherson, GJ AF Williams, C. D. Hervig, R. L. Wadhwa, M. Bullock, E. M. MacPherson, G. J. TI RARE EARTH ELEMENT CONCENTRATIONS IN ALLENDE FUN CAI CMS-1 SO METEORITICS & PLANETARY SCIENCE LA English DT Meeting Abstract CT 76th Annual Meeting of the Meteoritical-Society CY JUL 29-AUG 02, 2013 CL Edmonton, CANADA SP Meteorit Soc ID CHEMICAL FRACTIONATIONS; CONDENSATION; METEORITES C1 [Williams, C. D.; Hervig, R. L.; Wadhwa, M.] Arizona State Univ, Ctr Meteorite Studies, Tempe, AZ USA. [Bullock, E. M.; MacPherson, G. J.] Smithsonian Inst, Washington, DC 20560 USA. EM curtis.williams@asu.edu NR 8 TC 0 Z9 0 U1 0 U2 0 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 2013 VL 48 SU 1 SI SI BP A370 EP A370 PG 1 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 237JN UT WOS:000325865800340 ER PT J AU Lemeshko, M Krems, RV Doyle, JM Kais, S AF Lemeshko, Mikhail Krems, Roman V. Doyle, John M. Kais, Sabre TI Manipulation of molecules with electromagnetic fields SO MOLECULAR PHYSICS LA English DT Review DE molecules in fields; deceleration; focusing; molecular beams; Stark effect; Zeeman effect; AC stark shift; cold molecules; trapping molecules; orientation; adiabatic and non-adiabatic alignment; short laser pulses; combined fields; laser cooling of molecules; many-body physics with dipolar gases; spin models; quantum information processing; ultracold chemistry; molecular collisions; stabilisation of molecules in intense fields; evaporative and sympathetic cooling; entanglement ID INTENSE LASER FIELDS; DIFFERENTIAL CROSS-SECTIONS; RANGE RYDBERG MOLECULES; STRONG ELECTRIC-FIELDS; STATE-SELECTED PHOTODISSOCIATION; INDUCED CONICAL INTERSECTIONS; PERTURBATION-THEORY APPROACH; POTENTIAL-ENERGY SURFACES; TIME-DEPENDENT ALIGNMENT; ASYMMETRIC-TOP MOLECULES AB The goal of the present article is to review the major developments that have led to the current understanding of molecule-field interactions and experimental methods for manipulating molecules with electromagnetic fields. Molecule-field interactions are at the core of several, seemingly distinct areas of molecular physics. This is reflected in the organisation of this article, which includes sections on field control of molecular beams, external field traps for cold molecules, control of molecular orientation and molecular alignment, manipulation of molecules by non-conservative forces, ultracold molecules and ultracold chemistry, controlled many-body phenomena, entanglement of molecules and dipole arrays, and stability of molecular systems in high-frequency super-intense laser fields. The article contains 852 references. C1 [Lemeshko, Mikhail] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lemeshko, Mikhail; Doyle, John M.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Lemeshko, Mikhail; Krems, Roman V.] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Krems, Roman V.] Univ British Columbia, Dept Chem, Vancouver, BC V6T 1Z1, Canada. [Kais, Sabre] Purdue Univ, Dept Chem, W Lafayette, IN 47907 USA. [Kais, Sabre] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. RP Lemeshko, M (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM mikhail.lemeshko@gmail.com OI Kais, Sabre/0000-0003-0574-5346 FU NSF; NSERC of Canada FX This work was supported by NSF through a grant for the Institute for Theoretical Atomic, Molecular, and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory, a grant to the NSF CCI centre 'Quantum Information for Quantum Chemistry', and by NSERC of Canada. M. Lemeshko and R. V. Krems thank KITP for hospitality. NR 847 TC 86 Z9 86 U1 17 U2 165 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 2-4 PARK SQUARE, MILTON PARK, ABINGDON OR14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD JUL 1 PY 2013 VL 111 IS 12-13 SI SI BP 1648 EP 1682 DI 10.1080/00268976.2013.813595 PG 35 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 240CE UT WOS:000326071500004 ER PT J AU Sadeghpour, HR Rittenhouse, ST AF Sadeghpour, H. R. Rittenhouse, S. T. TI How do ultralong-range homonuclear Rydberg molecules get their permanent dipole moments? SO MOLECULAR PHYSICS LA English DT Article DE Rydberg atoms; polar molecules; ultracold Rydberg molecules; permanent dipole moments; symmetry breaking ID ATOMS; TRANSITIONS; DIMERS AB Cold and ultracold Rydberg atoms are in considerable vogue for their ability to creating strong interactions, stemming from their exaggerated and readily tunable properties. Ultralong-range Rydberg molecules have been predicted to form from the interaction of ultracold Rydberg atoms with ground-state atoms and polar molecules. In this work, we discuss and demonstrate how such molecules, which are homonuclear, form substantially large permanent electric dipole moments. A corollary benefit of such strong hybridisation is the realisation of high angular momentum degenerate Rydberg molecules (so-called trilobite molecules) with standard photoassociation techniques. C1 [Sadeghpour, H. R.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Rittenhouse, S. T.] Western Washington Univ, Dept Phys & Astron, Bellingham, WA 98225 USA. RP Sadeghpour, HR (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. EM hsadeghpour@cfa.harvard.edu FU NSF FX This was supported by an NSF grant to ITAMP at the Harvard-Smithsonian Center for Astrophysics. NR 33 TC 6 Z9 6 U1 0 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD JUL 1 PY 2013 VL 111 IS 12-13 SI SI BP 1902 EP 1907 DI 10.1080/00268976.2013.811555 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 240CE UT WOS:000326071500027 ER PT J AU Lin, GD Yelin, SF AF Lin, Guin-Dar Yelin, Susanne F. TI Vibrational spectroscopy of polar molecules with superradiance SO MOLECULAR PHYSICS LA English DT Article DE superradiance; superluminescence; optical depth; vibrational spectroscopy; polar molecule ID SPONTANEOUS EMISSION; SUPER-RADIANCE; SUPERFLUORESCENCE; SYSTEMS; RADIATION; GAS AB We investigate cooperative phenomena and superradiance for vibrational transitions in polar molecule spectroscopy of high optical-depth samples. Such cooperativity comes from the build-up of inter-particle coherence through dipole-dipole interactions and leads to speed-up of decay processes. We compare our calculation to recent work and find very good agreement, suggesting that superradiant effects need to be taken into account in a wide variety of ultracold molecule experiments, including vibrational and rotational states. C1 [Lin, Guin-Dar; Yelin, Susanne F.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, Cambridge, MA 02138 USA. [Lin, Guin-Dar; Yelin, Susanne F.] Harvard Phys Dept, Cambridge, MA 02138 USA. [Yelin, Susanne F.] Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. RP Lin, GD (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys, 60 Garden St, Cambridge, MA 02138 USA. EM guindarl@physics.harvard.edu OI LIN, GUIN-DAR/0000-0002-2243-9490 FU NSF; AFOSR FX We would like to thank NSF and AFOSR for funding, and M. Repp, J. Deiglmayr, and M. Weidemuller for discussions. NR 33 TC 3 Z9 3 U1 1 U2 7 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0026-8976 EI 1362-3028 J9 MOL PHYS JI Mol. Phys. PD JUL 1 PY 2013 VL 111 IS 12-13 SI SI BP 1917 EP 1922 DI 10.1080/00268976.2013.803167 PG 6 WC Chemistry, Physical; Physics, Atomic, Molecular & Chemical SC Chemistry; Physics GA 240CE UT WOS:000326071500029 ER PT J AU Engene, N Gunasekera, SP Paul, VJ AF Engene, N. Gunasekera, S. P. Paul, V. J. TI IDENTIFICATION OF NOVEL BIODIVERSITY FOR MONITORING, SURVEYING, AND CONTROLLING CYANOBACTERIAL HARMFUL ALGAL BLOOMS IN SOUTHERN FLORIDA SO PHYCOLOGIA LA English DT Meeting Abstract C1 [Engene, N.; Gunasekera, S. P.; Paul, V. J.] Smithsonian Inst, Washington, DC 20560 USA. EM engenen@si.edu NR 0 TC 0 Z9 0 U1 1 U2 6 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JUL PY 2013 VL 52 IS 4 SU S MA 75 BP 28 EP 28 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 238QV UT WOS:000325963600076 ER PT J AU Paul, VJ Craft, JD Ritson-Williams, R Langdon, C AF Paul, V. J. Craft, J. D. Ritson-Williams, R. Langdon, C. TI ALGAL CHEMICAL ECOLOGY IN A CHANGING OCEAN SO PHYCOLOGIA LA English DT Meeting Abstract C1 [Paul, V. J.; Craft, J. D.] Smithsonian Inst, Washington, DC 20560 USA. [Ritson-Williams, R.] Univ Hawaii, Honolulu, HI 96822 USA. [Langdon, C.] Univ Miami, Coral Gables, FL 33124 USA. EM paul@si.edu NR 0 TC 0 Z9 0 U1 0 U2 5 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JUL PY 2013 VL 52 IS 4 SU S MA 223 BP 85 EP 85 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 238QV UT WOS:000325963600224 ER PT J AU Soares, AR Duarte, HM Machado, FL Lima, WP Gestinari, LM Rossi-Bergmann, B Fujii, MT Kaiser, CR AF Soares, A. R. Duarte, H. M. Machado, F. L. Lima, W. P. Gestinari, L. M. Rossi-Bergmann, B. Fujii, M. T. Kaiser, C. R. TI WITHIN SPECIES CHEMICAL VARIABILITY IS IMPORTANT TO PHARMACOLOGICAL STUDIES IN LAURENCIA COMPLEX SO PHYCOLOGIA LA English DT Meeting Abstract C1 [Soares, A. R.; Duarte, H. M.] Smithsonian Marine Stn, Ft Pierce, FL USA. [Machado, F. L.; Lima, W. P.; Gestinari, L. M.; Rossi-Bergmann, B.; Kaiser, C. R.] UFRJ, Campinas, SP, Brazil. [Fujii, M. T.] Inst Bot Sao Paulo, Sao Paulo, Brazil. EM angelica.r.soares@gmail.com RI Soares, Angelica/D-7009-2012; Kaiser, Carlos/D-1049-2015 OI Soares, Angelica/0000-0001-9126-3778; NR 0 TC 0 Z9 0 U1 0 U2 0 PU INT PHYCOLOGICAL SOC PI LAWRENCE PA NEW BUSINESS OFFICE, PO BOX 1897, LAWRENCE, KS 66044-8897 USA SN 0031-8884 J9 PHYCOLOGIA JI Phycologia PD JUL PY 2013 VL 52 IS 4 SU S MA 271 BP 103 EP 103 PG 1 WC Plant Sciences; Marine & Freshwater Biology SC Plant Sciences; Marine & Freshwater Biology GA 238QV UT WOS:000325963600272 ER PT J AU Kho, LK Malhi, Y Tan, SKS AF Kho, Lip Khoon Malhi, Yadvinder Tan, Sylvester Kheng San TI Annual budget and seasonal variation of aboveground and belowground net primary productivity in a lowland dipterocarp forest in Borneo SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE Borneo; lowland dipterocarp forest; carbon; net primary productivity; aboveground and belowground biomass; moisture ID TROPICAL RAIN-FOREST; MULU-NATIONAL-PARK; WOOD DENSITY; SPATIAL-PATTERNS; SOUTHWESTERN BORNEO; AMAZONIAN FORESTS; MALAYSIAN BORNEO; WATER-CONTENT; ROOT BIOMASS; LEAF-LITTER AB Tropical forests are thought to have among the highest values of net primary productivity (NPP) on Earth, but comprehensive data on NPP have rarely been collected for tropical forests, especially outside of the Neotropics. In this study, we quantify aboveground and belowground NPP, along with additional environmental factors over a 1-2year period in a lowland dipterocarp forest in Borneo. The site is characterized by high annual rainfall and typically no month of the year when the forest is under water stress. We estimated the total NPP to be 15.890.90Mg C ha(-1)yr(-1) (meanstandard error) for a forest plot on clay soils and 12.790.68Mg C ha(-1)yr(-1) for a forest plot on sandy loam soils. Of this productivity, the allocation to aboveground NPP is 81.86.0%/80.4 +/- 6.0% and to belowground NPP is 18.2 +/- 3.7%/19.6 +/- 2.6% on clay and sandy loam, respectively. Fine root productivity (NPPfine roots) shows stronger seasonal variation relative to other components of NPP. There is evidence suggesting interannual variation in NPPfine roots, leaf flush, NPPlitterfall, and NPPACW. This is the first attempt to describe how the biomass of a Bornean tropical forest is allocated to the various components of NPP over the seasonal cycle. The study highlights the marked seasonality of a tropical forest even under largely aseasonal environmental conditions, as well as the important effect of contrasting seasonality on different soil types. C1 [Kho, Lip Khoon; Malhi, Yadvinder] Univ Oxford, Environm Change Inst, Sch Geog & Environm, Oxford, England. [Tan, Sylvester Kheng San] Harvard Univ, Smithsonian Trop Res Inst, Cambridge, MA 02138 USA. [Tan, Sylvester Kheng San] Harvard Univ, Arnold Arboretum, Ctr Trop Forest Sci, CTFS AA Asia Program, Cambridge, MA 02138 USA. RP Kho, LK (reprint author), Stesen Penyelidikan MPOB Belaga, Tingkat 3,Lot 360 Sublot 71,Jalan Sibiyu,Peti Sur, Bintulu 97013, Sarawak, Malaysia. EM lip.khoon@mpob.gov.my FU Malaysian Palm Oil Board (MPOB); CTFS; MPOB Education Foundation; Jackson Foundation; Oxford Martin School FX The financial support for this study was provided by the Malaysian Palm Oil Board (MPOB) and by CTFS in collaboration with the HSBC Climate Partnership. The authors would like to thank the Forest Department Sarawak, Sarawak Forestry Corporation, and the management of Lambir Hills National Park for their permission to conduct this study in Lambir. We thank Stuart Davies and Helene C. Muller-Landau for their support and for providing the census data; Tomo'omi Kumagai and Tomonori Kume for providing the meteorological data; Hiroko Kurokawa for providing herbivory rate data; and Abilano Deres, Xyxtus Tan, and Nasir Muhi for their field assistance. K. L. K. is supported by the MPOB Education Foundation scholarship. Y.M. is supported by the Jackson Foundation and the Oxford Martin School. This study is part of the Global Ecosystems Monitoring (GEM) network of forest carbon cycle research plots (http://gem.tropicalforests.ox.ac.uk/). NR 110 TC 13 Z9 13 U1 9 U2 40 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 EI 2169-8961 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUL PY 2013 VL 118 IS 3 BP 1282 EP 1296 DI 10.1002/jgrg.20109 PG 15 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 233EV UT WOS:000325549900026 ER PT J AU Vari, RP AF Vari, Richard P. TI Historical Biogeography of Neotropical Freshwater Fishes SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Book Review C1 [Vari, Richard P.] Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Vari, RP (reprint author), Smithsonian Inst, Dept Vertebrate Zool, Natl Museum Nat Hist, Washington, DC 20560 USA. NR 4 TC 0 Z9 0 U1 3 U2 7 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0002-8487 EI 1548-8659 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD JUL 1 PY 2013 VL 142 IS 4 BP 1151 EP 1152 DI 10.1080/00028487.2013.810016 PG 2 WC Fisheries SC Fisheries GA 220VB UT WOS:000324613900025 ER PT J AU Pelletier, J Martin, D Potvin, C AF Pelletier, Johanne Martin, Davy Potvin, Catherine TI REDD plus emissions estimation and reporting: dealing with uncertainty SO ENVIRONMENTAL RESEARCH LETTERS LA English DT Article DE reducing emissions from deforestation and forest degradation in developing countries (REDD plus ); uncertainty analysis; greenhouse gas reporting; forest-related emissions and removals; performance indicators; United Nations Framework Convention on Climate Change; consistency; comparability ID LONG-TERM PLOTS; CARBON EMISSIONS; TROPICAL FOREST; CLIMATE-CHANGE; PERVASIVE ALTERATION; TREE COMMUNITIES; RAIN-FOREST; LAND-USE; BIOMASS; AMAZON AB The United Nations Framework Convention on Climate Change (UNFCCC) defined the technical and financial modalities of policy approaches and incentives to reduce emissions from deforestation and forest degradation in developing countries (REDD+). Substantial technical challenges hinder precise and accurate estimation of forest-related emissions and removals, as well as the setting and assessment of reference levels. These challenges could limit country participation in REDD+, especially if REDD+ emission reductions were to meet quality standards required to serve as compliance grade offsets for developed countries' emissions. Using Panama as a case study, we tested the matrix approach proposed by Bucki et al (2012 Environ. Res. Lett. 7 024005) to perform sensitivity and uncertainty analysis distinguishing between 'modelling sources' of uncertainty, which refers to model-specific parameters and assumptions, and 'recurring sources' of uncertainty, which refers to random and systematic errors in emission factors and activity data. The sensitivity analysis estimated differences in the resulting fluxes ranging from 4.2% to 262.2% of the reference emission level. The classification of fallows and the carbon stock increment or carbon accumulation of intact forest lands were the two key parameters showing the largest sensitivity. The highest error propagated using Monte Carlo simulations was caused by modelling sources of uncertainty, which calls for special attention to ensure consistency in REDD+ reporting which is essential for securing environmental integrity. Due to the role of these modelling sources of uncertainty, the adoption of strict rules for estimation and reporting would favour comparability of emission reductions between countries. We believe that a reduction of the bias in emission factors will arise, among other things, from a globally concerted effort to improve allometric equations for tropical forests. Public access to datasets and methodology used to evaluate reference level and emission reductions would strengthen the credibility of the system by promoting accountability and transparency. To secure conservativeness and deal with uncertainty, we consider the need for further research using real data available to developing countries to test the applicability of conservative discounts including the trend uncertainty and other possible options that would allow real incentives and stimulate improvements over time. Finally, we argue that REDD+ result-based actions assessed on the basis of a dashboard of performance indicators, not only in 'tonnes CO2 equ. per year' might provide a more holistic approach, at least until better accuracy and certainty of forest carbon stocks emission and removal estimates to support a REDD+ policy can be reached. C1 [Pelletier, Johanne; Potvin, Catherine] McGill Univ, Dept Biol, Montreal, PQ H3A 1B1, Canada. [Pelletier, Johanne; Potvin, Catherine] McGill Univ, Global Environm & Climate Change Ctr, Montreal, PQ H3A 1B1, Canada. [Pelletier, Johanne; Potvin, Catherine] Smithsonian Trop Res Inst, Balboa, Panama. [Martin, Davy] Ecole Polytech, Dept Biol, F-91128 Palaiseau, France. RP Pelletier, J (reprint author), McGill Univ, Dept Biol, 1205 Dr Penfield, Montreal, PQ H3A 1B1, Canada. EM johannepelletier@gmail.com RI Pelletier, Johanne/E-3156-2016 OI Pelletier, Johanne/0000-0001-8161-6410 FU Fonds de Recherche Quebecois sur la Nature et les Technologies (FRQNT); Natural Sciences and Engineering Research Council of Canada (NSERC) FX We warmly thank Michael Bucki and Giacomo Grassi for their support in applying the matrix approach along with Bruno Guay and Jonah Busch for their useful comments and revisions on an earlier draft of this manuscript as well as two anonymous reviewers who helped improve this manuscript. JP and DM acknowledge the financial support of the Fonds de Recherche Quebecois sur la Nature et les Technologies (FRQNT) and CP of Natural Sciences and Engineering Research Council of Canada (NSERC) Discover Grant. NR 71 TC 2 Z9 2 U1 3 U2 41 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 2013 VL 8 IS 3 AR 034009 DI 10.1088/1748-9326/8/3/034009 PG 15 WC Environmental Sciences; Meteorology & Atmospheric Sciences SC Environmental Sciences & Ecology; Meteorology & Atmospheric Sciences GA 229FL UT WOS:000325247100015 ER PT J AU Birkebak, JM Mayor, JR Ryberg, KM Matheny, PB AF Birkebak, Joshua M. Mayor, Jordan R. Ryberg, K. Martin Matheny, P. Brandon TI A systematic, morphological and ecological overview of the Clavariaceae (Agaricales) SO MYCOLOGIA LA English DT Article DE biotrophy; evolution; morphology; nutritional mode; taxonomy ID NITROGEN ISOTOPE FRACTIONATION; CLAVARIOID FUNGI; ECTOMYCORRHIZAL FUNGI; MYCORRHIZAL FUNGI; PHYLOGENETIC ANALYSES; PINUS-SYLVESTRIS; RAMARIOPSIS; CARBON; DIVERSITY; SEQUENCES AB The Clavariaceae is a diverse family of mushroom-forming fungi composed of species that produce simple clubs, coralloid, lamellate-stipitate, hydnoid and resupinate sporocarps. Here we present a systematic and ecological overview of the Clavariaceae based on phylogenetic analysis of sequences of the nuclear large subunit ribosomal RNA (nLSU), including nine from type collections. Forty-seven sequences from sporocarps of diverse taxa across the Clavariaceae were merged with 243 environmental sequences from GenBank and analyzed phylogenetically to determine major clades within the family. Four major clades or lineages were recovered: (i) Mucronella, (ii) Ramariopsis-Clavulinopsis, (iii) Hyphodontiella and (iv) Clavaria-Camarophyllopsis-Clavicorona. Clavaria is paraphyletic, within which the lamellate and pileate-stipitate genus Camarophyllopsis is derived and composed of two independent lineages. The monotypic genus Clavicorona also appears nested within Clavaria. The monophyly of Clavaria and Camarophyllopsis, however, cannot be statistically rejected. We compared differing classification schemes for the genera Ramariopsis and Clavulinopsis, most of which are inconsistent with the molecular phylogeny and are statistically rejected. Scytinopogon, a genus classified in the Clavariaceae by several authors, shares phylogenetic affinities with the Trechisporales. Overall 126 molecular operational taxonomic units can be recognized in the Clavariaceae, roughly half of which are known only from environmental sequences, an estimate that exceeds the known number of species in the family. Stable isotope ratios of carbon and nitrogen were measured from specimens representing most major phylogenetic lineages to predict trophic strategies. These results suggest that most non-lignicolous species feature a biotrophic mode of nutrition. Ancestral state reconstruction analysis highlights the taxonomic significance of at least nine morphological traits at various depths in the family tree. C1 [Birkebak, Joshua M.; Ryberg, K. Martin; Matheny, P. Brandon] Univ Tennessee, Dept Ecol & Evolutionary Biol, Knoxville, TN 37996 USA. [Mayor, Jordan R.] Smithsonian Trop Res Inst, Panama City, Panama. RP Birkebak, JM (reprint author), Univ Tennessee, Dept Ecol & Evolutionary Biol, 332 Hesler Biol Bldg, Knoxville, TN 37996 USA. EM jbirkeba@utk.edu FU National Science Foundation [DEB-0949517, OISE-1012703]; NSF [DBI-0748955]; The Mycological Society of America FX This work was financed by a National Science Foundation award DEB-0949517 to PBM and OISE-1012703 to JRM. We would also like to acknowledge NSF DBI-0748955 for research assistantship support to JMB. The Mycological Society of America's international travel award is gratefully acknowledged for helping to finance travel to present and receive feedback concerning this research. We thank curators and staff from herbaria at the University of Washington (WTU), University of Minnesota (MIN) and University of British Columbia (UBC) for their assistance in loans of specimens. We also thank the associate editor, M. Catherine Aime, and two anonymous reviewers for their valuable critiques and suggestions. Michael Wood and D. Jean Lodge are acknowledged for kindly sharing photographs. NR 80 TC 17 Z9 19 U1 4 U2 39 PU ALLEN PRESS INC PI LAWRENCE PA 810 E 10TH ST, LAWRENCE, KS 66044 USA SN 0027-5514 J9 MYCOLOGIA JI Mycologia PD JUL-AUG PY 2013 VL 105 IS 4 BP 896 EP 911 DI 10.3852/12-070 PG 16 WC Mycology SC Mycology GA 197KG UT WOS:000322849500010 PM 23396156 ER PT J AU Meylan, AB Meylan, PA Espinosa, CO AF Meylan, Anne B. Meylan, Peter A. Ordonez Espinosa, Cristina TI Sea Turtles of Bocas del Toro Province and the Comarca Ngobe-Bugle, Republic of Panama SO CHELONIAN CONSERVATION AND BIOLOGY LA English DT Article DE sea turtles; Eretmochelys imbricata; Dermochelys coriacea; Chelonia mydas; Caretta caretta; Bocas del Toro; Comarca Ngobe-Bugle; Panama; threats; life stages; migrations ID CARIBBEAN PANAMA; DEVELOPMENTAL HABITAT; DERMOCHELYS-CORIACEA; CARETTA-CARETTA; CENTRAL-AMERICA; ECOLOGY; ORIGIN; BEACH; COAST AB The Bocas del Toro region of Panama (Bocas del Toro Province and the Comarca Ngobe-Bugle) has been known as an important area for sea turtles since at least the 17th century. Four species occur in the region: the hawksbill (Eretmochelys imbricata), green turtle (Chelonia mydas), loggerhead (Caretta caretta), and leatherback (Dermochelys coriacea). Multiple life stages of these species are supported by the diverse marine habitats and beaches in the region. We summarize the evidence for stages present and their known distributions in the Bocas region. Annual nest numbers, location, and monitoring status are given for 17 nesting beaches. These beaches support regionally significant numbers of leatherback and hawksbill nests, small numbers of green turtle nests and, rarely, loggerhead nests. We review the history of sea turtle use in the Bocas region and describe "velacion," a government-organized system that facilitated the extraction of hawksbills from nesting beaches throughout the Bocas region during the 20th century to supply the market for tortoiseshell. Current threats to sea turtles in the Bocas area include an illegal directed take of turtles at sea and of eggs and turtles on nesting beaches, bycatch in lobster and shark fisheries, and habitat degradation. Coastal development and increasing tourism have gradually become concerns for sea turtle conservation as the economic focus of the region has changed. The history of conservation efforts on behalf of sea turtles in Bocas is also summarized. This contribution was originally written to provide data on sea turtles for a coastal management plan for the region. C1 [Meylan, Anne B.] Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, St Petersburg, FL 33701 USA. [Meylan, Peter A.] Eckerd Coll, Nat Sci Collegium, St Petersburg, FL 33711 USA. [Meylan, Anne B.; Meylan, Peter A.] Smithsonian Trop Res Inst, Balboa, Panama. [Ordonez Espinosa, Cristina] Correo Gen, Sea Turtle Conservancy, Bocas Del Toro, Provincia De Bo, Panama. RP Meylan, AB (reprint author), Fish & Wildlife Res Inst, Florida Fish & Wildlife Conservat Commiss, 100 8th Ave SE, St Petersburg, FL 33701 USA. EM Anne.Meylan@MyFWC.com; meylanpa@eckerd.edu; cristinao@conserveturtles.org FU Wildlife Conservation Society; Busch Gardens Sea World Conservation Fund; Sea Turtle Conservancy; Eckerd College; Florida Fish and Wildlife Conservation Commission (FWC); Molly and Andy Barnes FX Our work in the Bocas region has been possible only because of the assistance of numerous organizations and individuals. The Autoridad Nacional del Ambiente (ANAM) has supported the work since its inception; we thank the ANAM staff: I. Anino, J. Antonio Gonzalez, H. Bonilla, D. Castillo, J. Garcia, and M. Ramos, in particular. The Meylans' work has been supported by the Wildlife Conservation Society since 1988. Additional support has come from the Busch Gardens Sea World Conservation Fund, the Sea Turtle Conservancy, Eckerd College, Florida Fish and Wildlife Conservation Commission (FWC), and Molly and Andy Barnes. C. Ordonez's work in the Comarca Ngobe-Bugle is made possible by special agreement with the General and No Kribo Regional Congress of the Comarca Ngobe-Bugle and has been performed in cooperation with APROR-ENANB (Rio Canaveral) and ACORENANB (Rio Chiriqui). It has been supported through the Sea Turtle Conservancy by the National Fish and Wildlife Foundation, US Fish and Wildlife Service (USFWS), US National Marine Fisheries Service, the Marine Turtle Conservation Act, Disney Worldwide Conservation Fund, World Wildlife Fund, Firedoll Foundation, and the Bay and Paul Foundations. Her work in Bocas del Toro Province has also been supported by Institute for Tropical Ecology and Conservation and Endangered Wildlife Trust. Considerable support has been provided to the authors by the Smithsonian Tropical Research Institute (STRI), in particular, by Z. Alain, O. Arosemena, R. Collin, P. Gondola, U. Gonzalez, G. Jacome, M. Paz, A. Ruiz, and R. Urriola. A. Ruiz has played a critical role in the success of the Bocas sea turtle work by serving as a liaison with Panamanian government offices since 1979. We have been assisted in fieldwork by I. Castillo and his extended family, T. Engstrom, S. Duncan, N. Decastro, R. Fernandez Frances, A. Vasquez Wilches, and numerous local beach monitors and international volunteers. E. Possardt (USFWS), D. Godfrey, S. Troeng, E. Harrison, R. Silman (STC), C. Campbell and C. Lagueux (WCS) have been instrumental to this work. From FWC, B. Brost assisted with database management, R. Hardy, L. French, and K. Wendell helped with the figures. We thank B. Crowder, K. Mansfield, T. O'Meara, A. Ruiz, B. Witherington, and 2 anonymous reviewers for comments on the manuscript. We thank B. Gordon, R. Fernandez, A. Ruiz, D. Suman, and V. Valdes Cadogan for the use of their photographs. S. Buschbaum of Boxwood Press facilitated the use of B. Gordon's published photo. The work was conducted under a series of scientific permits from ANAM, including most recently SE/A-53-10, SE/A132-10 and SE/A38-12, and STRI IACUC agreements, most recently, 2010-110-2013. NR 40 TC 0 Z9 0 U1 3 U2 32 PU CHELONIAN RESEARCH FOUNDATION PI LUNENBURG PA 168 GOODRICH ST., LUNENBURG, MA USA SN 1071-8443 J9 CHELONIAN CONSERV BI JI Chelonian Conserv. Biol. PD JUL PY 2013 VL 12 IS 1 BP 17 EP 33 PG 17 WC Zoology SC Zoology GA 190HN UT WOS:000322330100004 ER PT J AU Shen, CC Lin, J Murphy, NA Raymond, JC AF Shen, Chengcai Lin, Jun Murphy, Nicholas A. Raymond, John C. TI Statistical and spectral properties of magnetic islands in reconnecting current sheets during two-ribbon flares SO PHYSICS OF PLASMAS LA English DT Article ID CORONAL MASS EJECTIONS; SOLAR-FLARE; NUMERICAL EXPERIMENTS; SIMULATIONS; INFLOWS; MODEL; INSTABILITIES; ACCELERATION; TEMPERATURE; RESISTIVITY AB We perform a set of two dimensional resistive magnetohydrodynamic simulations to study the reconnection process occurring in current sheets that develop during solar eruptions. Reconnection commences gradually and produces small-scale structures inside the current sheet, which has one end anchored to the bottom boundary and the other end open. The main features we study include plasmoids (or plasma blobs) flowing in the sheet, and X-points between pairs of adjacent islands. The statistical properties of the fine structure and the dependence of the spectral energy on these properties are examined. The flux and size distribution functions of plasmoids roughly follow inverse square power laws at large scales. The mass distribution function is steep at large scales and shallow at small scales. The size distribution also shows that plasmoids are highly asymmetric soon after being formed, while older plasmoids tend to be more circular. The spectral profiles of magnetic and kinetic energy inside the current sheet are both consistent with a power law. The corresponding spectral indices c are found to vary with the magnetic Reynolds number R-m of the system, but tend to approach a constant for large R-m (> 10(5)). The motion and growth of blobs change the spectral index. The growth of new islands causes the power spectrum to steepen, but it becomes shallower when old and large plasmoids leave the computational domain. (C) 2013 AIP Publishing LLC. C1 [Shen, Chengcai; Lin, Jun] Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China. [Shen, Chengcai; Lin, Jun; Murphy, Nicholas A.; Raymond, John C.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Shen, Chengcai] Chinese Acad Sci, Grad Sch, Beijing 100039, Peoples R China. RP Shen, CC (reprint author), Chinese Acad Sci, Yunnan Astron Observ, POB 110, Kunming 650011, Yunnan, Peoples R China. RI LIN, JUN/B-9890-2017; OI Murphy, Nicholas/0000-0001-6628-8033 FU NASA [NNX11AB61G, NNM0FAB0FC]; NSF SHINE [AGS-1156076]; Program 973 [2011CB811403, 2013CBA01503]; NSFC [11273055]; CAS [KJCX2-EW-T07] FX We think the anonymous referee for very useful comments. This research is supported by NASA Grant NNX11AB61G, NASA Contract NNM0FAB0FC, and NSF SHINE Grant AGS-1156076 to the Smithsonian Astrophysical Observatory. This work was also supported by Program 973 Grants 2011CB811403 and 2013CBA01503, NSFC Grant 11273055, and CAS Grant KJCX2-EW-T07. NR 56 TC 9 Z9 9 U1 0 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 1305 WALT WHITMAN RD, STE 300, MELVILLE, NY 11747-4501 USA SN 1070-664X EI 1089-7674 J9 PHYS PLASMAS JI Phys. Plasmas PD JUL PY 2013 VL 20 IS 7 AR 072114 DI 10.1063/1.4816711 PG 12 WC Physics, Fluids & Plasmas SC Physics GA 193CR UT WOS:000322535400018 ER PT J AU Launius, RD AF Launius, Roger D. TI Imagining Outer Space: European Astroculture in the Twentieth Century SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 [Launius, Roger D.] 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 1 TC 0 Z9 0 U1 0 U2 0 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JUL PY 2013 VL 54 IS 3 BP 689 EP 690 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 209ZH UT WOS:000323798600027 ER PT J AU Chen, H Burnett, RT Kwong, JC Villeneuve, PJ Goldberg, MS Brook, RD van Donkelaar, A Jerrett, M Martin, RV Brook, JR Copes, R AF Chen, Hong Burnett, Richard T. Kwong, Jeffrey C. Villeneuve, Paul J. Goldberg, Mark S. Brook, Robert D. van Donkelaar, Aaron Jerrett, Michael Martin, Randall V. Brook, Jeffrey R. Copes, Ray TI Risk of Incident Diabetes in Relation to Long-term Exposure to Fine Particulate Matter in Ontario, Canada SO ENVIRONMENTAL HEALTH PERSPECTIVES LA English DT Article DE cohort study; diabetes; particulate air pollution ID AMBIENT AIR-POLLUTION; HEALTH ADMINISTRATIVE DATABASES; CARDIOVASCULAR-DISEASE; LOS-ANGELES; MORTALITY; MELLITUS; WOMEN; PREVALENCE; HYPERTENSION; COHORT AB BACKGROUND: Laboratory studies suggest that fine particulate matter (<= 2.5 mu m in diameter; PM2.5) can activate pathophysiological responses that may induce insulin resistance and type 2 diabetes. However, epidemiological evidence relating PM2.5 and diabetes is sparse, particularly for incident diabetes. OBJECTIVES: We conducted a population-based cohort study to determine whether long-term exposure to ambient PM2.5 is associated with incident diabetes. METHODS: We assembled a cohort of 62,012 nondiabetic adults who lived in Ontario, Canada, and completed one of five population-based health surveys between 1996 and 2005. Follow-up extended until 31 December 2010. Incident diabetes diagnosed between 1996 and 2010 was ascertained using the Ontario Diabetes Database, a validated registry of persons diagnosed with diabetes (sensitivity = 86%, specificity = 97%). Six-year average concentrations of PM2.5 at the postal codes of baseline residences were derived from satellite observations. We used Cox proportional hazards models to estimate the associations, adjusting for various individual-level risk factors and contextual covariates such as smoking, body mass index, physical activity, and neighborhood-level household income. We also conducted multiple sensitivity analyses. In addition, we examined effect modification for selected comorbidities and sociodemographic characteristics. RESULTS: There were 6,310 incident cases of diabetes over 484,644 total person-years of follow-up. The adjusted hazard ratio for a 10-mu g/m(3) increase in PM2.5 was 1.11 (95% CI: 1.02, 1.21). Estimated associations were comparable among all sensitivity analyses. We did not find strong evidence of effect modification by comorbidities or sociodemographic covariates. CONCLUSIONS: This study suggests that long-term exposure to PM2.5 may contribute to the development of diabetes. C1 [Chen, Hong; Kwong, Jeffrey C.; Copes, Ray] Publ Hlth Ontario, Toronto, ON M5G 1V2, Canada. [Chen, Hong; Villeneuve, Paul J.; Copes, Ray] Univ Toronto, Dalla Lana Sch Publ Hlth, Toronto, ON, Canada. [Burnett, Richard T.; Villeneuve, Paul J.] Hlth Canada, Populat Studies Div, Ottawa, ON K1A 0L2, Canada. [Kwong, Jeffrey C.] Inst Clin Evaluat Sci, Toronto, ON, Canada. [Kwong, Jeffrey C.] Univ Toronto, Dept Family & Community Med, Toronto, ON M5S 1A1, Canada. [Goldberg, Mark S.] McGill Univ, Dept Med, Montreal, PQ, Canada. [Goldberg, Mark S.] McGill Univ, Ctr Hlth, Div Clin Epidemiol, Montreal, PQ, Canada. [Brook, Robert D.] Univ Michigan, Sch Med, Div Cardiovasc Med, Ann Arbor, MI USA. [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS, Canada. [Jerrett, Michael] Univ Calif Berkeley, Sch Publ Hlth, Div Environm Hlth Sci, Berkeley, CA 94720 USA. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brook, Jeffrey R.] Environm Canada, Air Qual Res Div, Toronto, ON, Canada. RP Chen, H (reprint author), Publ Hlth Ontario, 480 Univ Ave,Suite 300, Toronto, ON M5G 1V2, Canada. EM hong.chen@oahpp.ca RI Martin, Randall/C-1205-2014 OI Martin, Randall/0000-0003-2632-8402 FU Institute for Clinical Evaluative Sciences; Public Health Ontario; Health Canada [4500275504]; Collaborative Health Research Projects grant; Clinician Scientist Award from the Department of Family and Community Medicine, University of Toronto; Ontario Ministry of Health and Long-Term Care FX This work was supported by the Institute for Clinical Evaluative Sciences, operating funds from Public Health Ontario, and a short-form contract (contract 4500275504) from Health Canada. A.v.D. and R.V.M. were supported by Health Canada and a Collaborative Health Research Projects grant. J.C.K. was supported by a Clinician Scientist Award from the Department of Family and Community Medicine, University of Toronto. The Institute for Clinical Evaluative Sciences is funded by an annual grant from the Ontario Ministry of Health and Long-Term Care. NR 49 TC 54 Z9 58 U1 6 U2 47 PU US DEPT HEALTH HUMAN SCIENCES PUBLIC HEALTH SCIENCE PI RES TRIANGLE PK PA NATL INST HEALTH, NATL INST ENVIRONMENTAL HEALTH SCIENCES, PO BOX 12233, RES TRIANGLE PK, NC 27709-2233 USA SN 0091-6765 J9 ENVIRON HEALTH PERSP JI Environ. Health Perspect. PD JUL PY 2013 VL 121 IS 7 BP 804 EP 810 DI 10.1289/ehp.1205958 PG 7 WC Environmental Sciences; Public, Environmental & Occupational Health; Toxicology SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Toxicology GA 208VY UT WOS:000323711000019 PM 23632126 ER PT J AU Tong, CYE Grimes, P Blundell, R Wang, MJ Noguchi, T AF Tong, Cheuk-Yu Edward Grimes, Paul Blundell, Raymond Wang, Ming-Jye Noguchi, Takashi TI Wideband SIS Receivers Using Series Distributed SIS Junction Array SO IEEE TRANSACTIONS ON TERAHERTZ SCIENCE AND TECHNOLOGY LA English DT Article DE Distributed mixers; submillimeter receivers; superconductor-insulator-superconductor (SIS) mixers; ultra wideband receivers ID BANDWIDTH; MIXER AB We have developed an SIS mixer based on a 3-junction series distributed array. In this mixer layout, the three junctions are connected together by passive network elements, such that each junction is subjected to different local oscillator (LO) drive, and slightly different DC bias voltages. This design helps to reduce the output capacitance of the mixer at the intermediate frequency (IF) so as to achieve a wider IF bandwidth, while maintaining adequate RF bandwidth. The receiver performance of this type of mixer was evaluated in the 220 GHz band. The lowest noise temperature measured was 30 K, and the noise temperature remains below 50 K over the IF range from 3 to 11 GHz. Receivers incorporating this new mixer design are currently in routine operation at the Submillimeter Array. C1 [Tong, Cheuk-Yu Edward; Grimes, Paul; Blundell, Raymond] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wang, Ming-Jye] ASIAA, Taipei 10617, Taiwan. [Noguchi, Takashi] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. RP Tong, CYE (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM etong@cfa.har-vard.edu; pgrimes@cfa.harvard.edu; rblundell@cfa.harvard.edu; mingjye@asiaa.sinica.edu.tw; Takashi.Noguchi@nao.ac.jp OI Tong, Edward/0000-0002-7736-4203 NR 10 TC 4 Z9 4 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 2156-342X J9 IEEE T THZ SCI TECHN JI IEEE Trans. Terahertz Sci. Technol. PD JUL PY 2013 VL 3 IS 4 BP 428 EP 432 DI 10.1109/TTHZ.2013.2259624 PG 5 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 210MD UT WOS:000323836700015 ER PT J AU Clough, GW AF Clough, G. Wayne TI Untitled 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 2013 VL 44 IS 4 BP 10 EP 10 PG 1 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA 179NE UT WOS:000321526400006 ER PT J AU Lemeshko, M Weimer, H AF Lemeshko, Mikhail Weimer, Hendrik TI Dissipative binding of atoms by non-conservative forces SO NATURE COMMUNICATIONS LA English DT Article ID QUANTUM SIMULATOR; DRIVEN; OPTICS; GAS AB The formation of molecules and supramolecular structures results from bonding by conservative forces acting among electrons and nuclei and giving rise to equilibrium configurations defined by minima of the interaction potential. Here we show that bonding can also occur by the non-conservative forces responsible for interaction-induced coherent population trapping. The bound state arises in a dissipative process and manifests itself as a stationary state at a preordained interatomic distance. Remarkably, such a dissipative bonding is present even when the interactions among the atoms are purely repulsive. The dissipative bound states can be created and studied spectroscopically in present-day experiments with ultracold atoms or molecules and can potentially serve for cooling strongly interacting quantum gases. C1 [Lemeshko, Mikhail; Weimer, Hendrik] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Lemeshko, Mikhail; Weimer, Hendrik] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Weimer, Hendrik] Leibniz Univ Hannover, Inst Theoret Phys, D-30167 Hannover, Germany. RP Lemeshko, M (reprint author), Harvard Smithsonian Ctr Astrophys, ITAMP, 60 Garden St, Cambridge, MA 02138 USA. EM mlemeshko@cfa.harvard.edu FU National Science Foundation; Smithsonian Astrophysical Observatory; German Academic Exchange Service (DAAD) FX We thank Bretislav Friedrich, Johannes Otterbach, Ignacio Cirac and Hossein Sadegh-pour for insightful discussions. This work was supported by the National Science Foundation through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory and within the Postdoc Program of the German Academic Exchange Service (DAAD). NR 39 TC 14 Z9 14 U1 1 U2 16 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JUL PY 2013 VL 4 AR 2230 DI 10.1038/ncomms3230 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 208YD UT WOS:000323717900010 PM 23896951 ER PT J AU Ettori, S Gastaldello, F Gitti, M O'Sullivan, E Gaspari, M Brighenti, F David, L Edge, AC AF Ettori, S. Gastaldello, F. Gitti, M. O'Sullivan, E. Gaspari, M. Brighenti, F. David, L. Edge, A. C. TI Cold fronts and metal anisotropies in the X-ray cool core of the galaxy cluster Zw 1742+3306 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies: clusters: general; galaxies: clusters: individual: Zw 1742+3306; galaxies: clusters: intracluster medium; X-rays: galaxies: clusters ID ACTIVE GALACTIC NUCLEI; H-ALPHA FILAMENTS; ABUNDANCE PROFILES; INFRARED SURVEY; MULTIPHASE GAS; RADIO-EMISSION; FLOW CLUSTERS; XMM-NEWTON; SKY SURVEY; FEEDBACK AB Context. In recent years, our understanding of the cool cores of galaxy clusters has changed. Once thought to be relatively simple places where gas cools and flows towards the centre, now they are believed to be very dynamic places where heating from the central active galactic nucleus (AGN) and cooling, as inferred from active star formation, molecular gas, and H alpha nebulosity, find an uneasy energetic balance. Aims. We want to characterize the X-ray properties of the nearby cool-core cluster Zw 1742+3306, selected because it is bright at X-ray (with a flux greater than 10(-11) erg s(-1) cm(-2) in the 0.1-2.4 keV band) and H alpha wavelengths (H alpha luminosity > 10(40) erg s(-1)). Methods. We used Chandra data to analyse the spatial and spectral properties of the cool core of Zw 1742+3306, a galaxy cluster at z = 0.0757 that emits in H alpha and presents the brightest central galaxy located in a diffuse X-ray emission with multiple peaks in surface brightness. Results. We show that the X-ray cool core of the galaxy cluster Zw 1742+3306 is thermodynamically very active with evidence of cold fronts and a weak shock in the surface brightness map and of an apparently coherent, elongated structure with metallicity greater than the value measured in the surrounding ambient gas by about 50%. This anisotropic structure is 280 x 90 kpc(2) and is aligned with the cold fronts and with the X-ray emission on larger scales. We suggest that all these peculiarities in the X-ray emission of Zw 1742+3306 are either a very fine-tuned output of a sloshing gas in the cluster core or the product of a metal-rich outflow from the central AGN. C1 [Ettori, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Ettori, S.] Ist Nazl Fis Nucl, Sez Bologna, I-40127 Bologna, Italy. [Gastaldello, F.] IASF, INAF, I-20133 Milan, Italy. [Gastaldello, F.] Univ Calif Irvine, Irvine, CA 92697 USA. [Gitti, M.; Brighenti, F.] Univ Bologna, Dept Phys & Astron, I-40127 Bologna, Italy. [O'Sullivan, E.; David, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gaspari, M.] Max Planck Inst Astrophys, D-85741 Garching, Germany. [Edge, A. C.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Ettori, S (reprint author), Osservatorio Astron Bologna, INAF, Via Ranzani 1, I-40127 Bologna, Italy. EM stefano.ettori@oabo.inaf.it RI Gastaldello, Fabio/N-4226-2015; Ettori, Stefano/N-5004-2015; OI Gastaldello, Fabio/0000-0002-9112-0184; Ettori, Stefano/0000-0003-4117-8617; Gitti, Myriam/0000-0002-0843-3009; Edge, Alastair/0000-0002-3398-6916 FU Chandra grant [GO0-11136X]; Italian Space Agency through ASI/INAF [I/032/10/0]; [ASI-INAF I/023/05/0]; [I/088/06/0]; [247653] FX We thank the anonymous referee for the useful comments that improved the presentation of the work. We acknowledge the financial contribution from contract ASI-INAF I/023/05/0 and I/088/06/0. S. E. acknowledges financial support from Chandra grant GO0-11136X and from FP7-PEOPLE-IRSES-CAFEGroups (grant agreement 247653). F. G. acknowledges financial contributions from the Italian Space Agency through ASI/INAF agreement I/032/10/0 for XMM-Newton operations. NR 48 TC 4 Z9 4 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 JUL PY 2013 VL 555 AR A93 DI 10.1051/0004-6361/201321107 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 185YV UT WOS:000322008600093 ER PT J AU Harsono, D Visser, R Bruderer, S van Dishoeck, EF Kristensen, LE AF Harsono, D. Visser, R. Bruderer, S. van Dishoeck, E. F. Kristensen, L. E. TI Evolution of CO lines in time-dependent models of protostellar disk formation SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE stars: formation; accretion, accretion disks; radiative transfer; astrochemistry; methods: numerical ID YOUNG STELLAR OBJECTS; LOW-MASS PROTOSTARS; SPECTRAL ENERGY-DISTRIBUTIONS; MAGNETIC BRAKING CATASTROPHE; STAR-FORMING REGIONS; CIRCUMSTELLAR DISKS; MOLECULAR-LINE; HL TAURI; SUBMILLIMETER ARRAY; PROTOPLANETARY DISK AB Context. Star and planet formation theories predict an evolution in the density, temperature, and velocity structure as the envelope collapses and forms an accretion disk. While continuum emission can trace the dust evolution, spectrally resolved molecular lines are needed to determine the physical structure and collapse dynamics. Aims. The aim of this work is to model the evolution of the molecular excitation, line profiles, and related observables during low-mass star formation. Specifically, the signatures of disks during the deeply embedded stage (M-env > M-star) are investigated. Methods. The semi-analytic 2D axisymmetric model of Visser and collaborators has been used to describe the evolution of the density, stellar mass, and luminosity from the pre-stellar to the T-Tauri phase. A full radiative transfer calculation is carried out to accurately determine the time-dependent dust temperatures. The time-dependent CO abundance is obtained from the adsorption and thermal desorption chemistry. Non-LTE near-IR (NIR), far-IR (FIR), and submm lines of CO have been simulated at a number of time steps. Results. In single dish (10-20" beams), the dynamics during the collapse are best probed through highly excited (CO)-C-13 and (CO)-O-18 lines, which are significantly broadened by the infall process. In contrast to the dust temperature, the CO excitation temperature derived from submm/FIR data does not vary during the protostellar evolution, consistent with (CO)-O-18 observations obtained with Herschel and from ground-based telescopes. The NIR spectra provide complementary information to the submm lines by probing not only the cold outer envelope but also the warm inner region. The NIR high-J (>= 8) absorption lines are particularly sensitive to the physical structure of the inner few AU, which does show evolution. The models indicate that observations of (CO)-C-13 and (CO)-O-18 low-J submm lines within a <= 1" (at 140 pc) beam are well suited to probe embedded disks in Stage I (M-env < M-star) sources, consistent with recent interferometric observations. High signal-to-noise ratio subarcsec resolution data with ALMA are needed to detect the presence of small rotationally supported disks during the Stage 0 phase and various diagnostics are discussed. The combination of spatially and spectrally resolved lines with ALMA and at NIR is a powerful method to probe the inner envelope and disk formation process during the embedded phase. C1 [Harsono, D.; van Dishoeck, E. F.; Kristensen, L. E.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Harsono, D.] Univ Groningen, SRON Netherlands Inst Space Res, NL-9700 AV Groningen, Netherlands. [Visser, R.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Bruderer, S.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Kristensen, L. E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Harsono, D (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM harsono@strw.leidenuniv.nl RI Kristensen, Lars/F-4774-2011 OI Kristensen, Lars/0000-0003-1159-3721 FU Netherlands Research School for Astronomy (NOVA); Space Research Organization Netherlands (SRON); Netherlands Organisation for Scientific Research (NWO) [614.001.008]; European Community's Seventh Framework Programme FP7 [238258] FX We would like to thank Steve Doty for stimulating discussions on continuum and line radiative transfer and for allowing us to use his chemistry code. We are also grateful to Kees Dullemond for providing RADMC (and RADMC3D) and to Klaus Pontoppidan for RADLite. We thank the anonymous referee for the constructive comments, which have improved this paper. This work is supported by the Netherlands Research School for Astronomy (NOVA) and by the Space Research Organization Netherlands (SRON). Astrochemistry in Leiden is supported by the Netherlands Research School for Astronomy (NOVA), by a Spinoza grant and grant 614.001.008 from the Netherlands Organisation for Scientific Research (NWO), and by the European Community's Seventh Framework Programme FP7/20072013 under grant agreement 238258 (LASSIE). NR 91 TC 9 Z9 9 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 1432-0746 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD JUL PY 2013 VL 555 AR A45 DI 10.1051/0004-6361/201220885 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 185YV UT WOS:000322008600045 ER PT J AU Henrichs, HF de Jong, JA Verdugo, E Schnerr, RS Neiner, C Donati, JF Catala, C Shorlin, SLS Wade, GA Veen, PM Nichols, JS Damen, EMF Talavera, A Hill, GM Kaper, L Tijani, AM Geers, VC Wiersema, K Plaggenborg, B Rygl, KLJ AF Henrichs, H. F. de Jong, J. A. Verdugo, E. Schnerr, R. S. Neiner, C. Donati, J. -F. Catala, C. Shorlin, S. L. S. Wade, G. A. Veen, P. M. Nichols, J. S. Damen, E. M. F. Talavera, A. Hill, G. M. Kaper, L. Tijani, A. M. Geers, V. C. Wiersema, K. Plaggenborg, B. Rygl, K. L. J. TI Discovery of the magnetic field in the pulsating B star beta Cephei SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE magnetic fields; stars: winds, outflows; binaries: spectroscopic; stars: oscillations; stars: early-type ID DRIVEN STELLAR WINDS; H-ALPHA EMISSION; DYNAMICAL SIMULATIONS; O-STAR; SPECKLE INTERFEROMETRY; LINE VARIABILITY; TERM VARIABILITY; LONG-TERM; ROTATION; MUSICOS AB Context. Although the star itself is not helium enriched, the periodicity and the variability in the UV wind lines of the pulsating B1 IV star beta Cephei are similar to what is observed in magnetic helium-peculiar B stars, suggesting that beta Cep is magnetic. Aims. We searched for a magnetic field using high-resolution spectropolarimetry. From UV spectroscopy, we analysed the wind variability and investigated the correlation with the magnetic data. Methods. We used 130 time-resolved circular polarisation spectra that were obtained from 1998 (when beta Cep was discovered to be magnetic) to 2005, with the MuSiCoS echelle spectropolarimeter at the 2 m Telescope Bernard Lyot. We applied the least-square deconvolution method on the Stokes V spectra and derived the longitudinal component of the integrated magnetic field over the visible hemisphere of the star. We performed a period analysis on the magnetic data and on equivalent-width measurements of UV wind lines obtained over 17 years. We also analysed the short-and long-term radial velocity variations, which are due to the pulsations and the 90-year binary motion, respectively. Results. beta Cep hosts a sinusoidally varying magnetic field with an amplitude 97 +/- 4 G and an average value -6 +/- 3 G. From the UV wind line variability, we derive a period of 12.00075(11) days, which is the rotation period of the star, and is compatible with the observed magnetic modulation. Phases of maximum and minimum field match those of maximum emission in the UV wind lines, strongly supporting an oblique magnetic-rotator model. We discuss the magnetic behaviour as a function of pulsation behaviour and UV line variability. Conclusions. This paper presents the analysis of the first confirmed detection of a dipolar magnetic field in an upper main-sequence pulsating star. Maximum wind absorption originates in the magnetic equatorial plane. Maximum emission occurs when the magnetic north pole points to the Earth. Radial velocities agree with the similar to 90-year orbit around its Be-star binary companion. C1 [Henrichs, H. F.; de Jong, J. A.; Schnerr, R. S.; Veen, P. M.; Damen, E. M. F.; Kaper, L.; Tijani, A. M.; Geers, V. C.; Wiersema, K.; Plaggenborg, B.; Rygl, K. L. J.] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [Verdugo, E.] European Space Agcy ESAC, Madrid 28691, Spain. [Neiner, C.] Univ Paris Diderot, UPMC, Observ Paris, LESIA,CNRS UMR 8109, F-92190 Meudon, France. [Donati, J. -F.] Observ Midi Pyrenees, F-31400 Toulouse, France. [Catala, C.] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France. [Shorlin, S. L. S.] Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. [Wade, G. A.] Royal Mil Coll Canada, Dept Phys, Kingston, ON K7K 7B4, Canada. [de Jong, J. A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Nichols, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Talavera, A.] European Space Astron Ctr, Madrid 28691, Spain. [Hill, G. M.] WM Keck Observ, Kamuela, HI 96743 USA. RP Henrichs, HF (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM h.f.henrichs@uva.nl FU Netherlands Foundation for Research in Astronomy (NFRA); Netherlands Organization for Scientific Research (NWO) [781-71-053]; Natural Sciences and Engineering Council of Canada (NSERC) FX We thank D. Lennon, G. Mathys, S. Solanki, J. Telting, and A. ud-Doula for discussions and constructive comments. We also thanks an anonymous referee for useful remarks and comments. H.F.H. thanks his coauthors for their patience and S. Hubrig for encouragement to finish this work. The helpful assistance and support of the observatory staff members at TBL, GSFC, and Vilspa (in particular, the late Dr. Willem Wamsteker) is well remembered and fondly acknowledged. J.D.J. acknowledges support from the Netherlands Foundation for Research in Astronomy (NFRA) with financial aid from the Netherlands Organization for Scientific Research (NWO) under project 781-71-053. G.A.W. acknowledges support from the Natural Sciences and Engineering Council of Canada (NSERC). NR 72 TC 6 Z9 6 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 JUL PY 2013 VL 555 AR A46 DI 10.1051/0004-6361/201321584 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 185YV UT WOS:000322008600046 ER PT J AU Breedy, O Guzman, HM AF Breedy, Odalisca Guzman, Hector M. TI A NEW SPECIES OF THE GENUS EUGORGIA (CNIDARIA: OCTOCORALLIA: GORGONIIDAE) FROM MESOPHOTIC REEFS IN THE EASTERN PACIFIC SO BULLETIN OF MARINE SCIENCE LA English DT Article ID ECOLOGY AB Our knowledge of octocoral diversity in the eastern Pacific has been focused on shallow reef habitats, while the fauna occurring in the mesophotic zone from 40 to 150 m is poorly known. A new species of the gorgoniid Eugorgia was recently obtained with a submersible from the Hannibal Bank, a coastal seamount 60 km off mainland Panama and 15 km from Coiba Island. The morphological characters were analyzed and illustrated by light and scanning electron microscopy. Eugorgia siedenburgae sp. nov. can be distinguished from the other species in the genus by its bushy, multiplanar, bicolored colony, and the sclerites colors, composition, and sizes. This new species increases the number in the genus to 13 and contributes to our understanding of the fragile mesophotic biodiversity. C1 [Breedy, Odalisca] Univ Costa Rica, Ctr Invest Estruct Microscop, Ctr Invest Ciencias Mar & Limnol, San Jose, Costa Rica. [Breedy, Odalisca; Guzman, Hector M.] Smithsonian Trop Res Inst, Panama City, Panama. RP Breedy, O (reprint author), Univ Costa Rica, Ctr Invest Estruct Microscop, Ctr Invest Ciencias Mar & Limnol, POB 11501-2060, San Jose, Costa Rica. EM odaliscab@gmail.com FU International Community Foundation; Smithsonian Tropical Research Institute; Instituto de Investigaciones Cientificas y Servicios de Alta Tecnologia de Panama (INDICASAT); Siedenburg family; Mission Blue's Sylvia Earl Alliance; Vicerrectoria de Investigacion, Universidad de Costa Rica [A9072, B2142] FX We are grateful to anonymous reviewers for critical improvements of the manuscript. We thank crew members of the DEEPSEE submersible and the MV HUNDERSEA HUNTER for making possible the coral collections in Hannibal Bank, and Y Camacho and R Vargas (MZUCR) for collecting specimens during the July 2005 STRI's R/V URRACA Expedition. We thank S Mattson and C Gomez (STRI) for specimen pictures. The expeditions and laboratory work were partially funded by the International Community Foundation, the Smithsonian Tropical Research Institute, the Instituto de Investigaciones Cientificas y Servicios de Alta Tecnologia de Panama (INDICASAT), the Siedenburg family, the Mission Blue's Sylvia Earl Alliance, and the Vicerrectoria de Investigacion (A9072, B2142 projects), Universidad de Costa Rica. NR 11 TC 4 Z9 4 U1 1 U2 13 PU ROSENSTIEL SCH MAR ATMOS SCI PI MIAMI PA 4600 RICKENBACKER CAUSEWAY, MIAMI, FL 33149 USA SN 0007-4977 EI 1553-6955 J9 B MAR SCI JI Bull. Mar. Sci. PD JUL PY 2013 VL 89 IS 3 BP 735 EP 743 DI 10.5343/bms.2013.1014 PG 9 WC Marine & Freshwater Biology; Oceanography SC Marine & Freshwater Biology; Oceanography GA 200RI UT WOS:000323086200006 ER PT J AU Mills, AJ Birch, SJC Stanway, R Huyser, O Chisholm, RA Sirami, C Spear, D AF Mills, Anthony J. Birch, Sarah-Jane C. Stanway, Rosanne Huyser, Onno Chisholm, Ryan A. Sirami, Clelia Spear, Dian TI Sequestering carbon and restoring renosterveld through fallowing: a practical conservation approach for the Overberg, Cape Floristic Region, South Africa SO CONSERVATION LETTERS LA English DT Article DE Biodiversity hotspot; carbon markets; conservation incentives; corridor network; land use changes ID BIODIVERSITY; LAND; SEQUESTRATION; PLAN AB Carbon credits are a potential source of funding for restoration initiatives that contribute to achieving conservation targets in important biodiversity areas. Here we investigated whether fallowing sequesters carbon; a first step in assessing the viability of using carbon financing to promote restoration of threatened vegetation in agricultural landscapes. We used renosterveld, a critically endangered shrubland vegetation of the Cape Floristic Region, as a case study. Carbon stocks of soil and biomass in active fields, fallow fields and intact renosterveld were compared. The total carbon stocks measured in fallow fields (82 Mg C ha(-1)) show that fallowing can sequester carbon lost in the conversion from intact renosterveld (84 Mg C ha(-1)) to active fields (69 Mg C ha(-1)) and that revenues of US$ 10 - 48 ha(-1) yr(-1) from carbon credits could accrue. Our findings suggest that carbon financing could be used to incentivise ecological restoration in marginal agricultural landscapes. C1 [Mills, Anthony J.; Birch, Sarah-Jane C.; Stanway, Rosanne; Sirami, Clelia; Spear, Dian] Univ Stellenbosch, Dept Soil Sci, ZA-7602 Matieland, South Africa. [Huyser, Onno] Kirstenbosch Natl Bot Gardens, WWF South Africa, Ctr Biodivers Conservat, Fynbos & Succulent Karoo & Table Mt Fund, Cape Town, South Africa. [Chisholm, Ryan A.] Smithsonian Trop Res Inst, Balboa Ancon, Panama. RP Mills, AJ (reprint author), Univ Stellenbosch, Dept Soil Sci, ZA-7602 Matieland, South Africa. EM mills@sun.ac.za RI Sirami, Clelia/J-9371-2013; Spear, Dian/B-2469-2009 OI Sirami, Clelia/0000-0003-1741-3082; Spear, Dian/0000-0002-2417-3980 FU Table Mountain Fund FX We thank the Table Mountain Fund for funding this research project; the Overberg land owners for permission to work on their land; SANBI (Kirstenbosch) and Stellenbosch University (Department of Soil Science) for use of their laboratories and ovens; Tanya Medinski for laboratory work assistance; Odette Curtis for site selection assistance and botanical surveys; Peter Coetzee, Omari Asongo and the Bredasdorp team for field assistance; Mireille Lewarne and Willem Hoffmann for information on the economics of land uses in renosterveld; and Weather SA for providing climate data. Three anonymous reviewers are thanked for their constructive comments. NR 38 TC 1 Z9 1 U1 0 U2 14 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1755-263X J9 CONSERV LETT JI Conserv. Lett. PD JUL PY 2013 VL 6 IS 4 BP 255 EP 263 DI 10.1111/conl.12003 PG 9 WC Biodiversity Conservation SC Biodiversity & Conservation GA 200BO UT WOS:000323041600005 ER PT J AU Woodman, N AF Woodman, Neal TI Survival of the Less-fit: A Least Shrew (Mammalia, Soricidae, Cryptotis parvus) Survives a Separated Leg Fracture in the Wild SO JOURNAL OF WILDLIFE DISEASES LA English DT Article ID MICE AB X-rays Of the deformed femur of a least shrew (Cryptotis parvus) revealed an ossified callus enclosing a greatly displaced, spiral fracture. Based on models of fracture healing, this shrew lived for at least 28 days postfracture. Survival of major fractures in the wild may not be uncommon. C1 US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. RP Woodman, N (reprint author), US Geol Survey, Patuxent Wildlife Res Ctr, Natl Museum Nat Hist, Smithsonian Inst, Washington, DC 20013 USA. EM woodmann@si.edu OI Woodman, Neal/0000-0003-2689-7373 NR 14 TC 0 Z9 0 U1 0 U2 0 PU WILDLIFE DISEASE ASSOC, INC PI LAWRENCE PA 810 EAST 10TH ST, LAWRENCE, KS 66044-8897 USA SN 0090-3558 J9 J WILDLIFE DIS JI J. Wildl. Dis. PD JUL PY 2013 VL 49 IS 3 BP 735 EP 737 DI 10.7589/2012-08-218 PG 3 WC Veterinary Sciences SC Veterinary Sciences GA 183FA UT WOS:000321798500039 PM 23778633 ER PT J AU Hopkins, PF Keres, D Murray, N Hernquist, L Narayanan, D Hayward, CC AF Hopkins, Philip F. Keres, Dusan Murray, Norman Hernquist, Lars Narayanan, Desika Hayward, Christopher C. TI Resolving the generation of starburst winds in Galaxy mergers SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: active; galaxies: evolution; galaxies: formation; cosmology: theory ID SMOOTHED PARTICLE HYDRODYNAMICS; ULTRALUMINOUS INFRARED GALAXIES; MOVING-MESH COSMOLOGY; SUPERMASSIVE BLACK-HOLES; ABSORPTION-LINE PROBES; SCALE GASEOUS OUTFLOWS; STAR-FORMING GALAXIES; INITIAL MASS FUNCTION; II ESI SPECTRA; ELLIPTIC GALAXIES AB We study galaxy superwinds driven in major mergers, using pc-scale resolution simulations with detailed models for stellar feedback that can self-consistently follow the generation of winds. The models include molecular cooling, star formation at high densities in giant molecular clouds, and gas recycling and feedback from supernovae (I and II), stellar winds and radiation pressure. We study mergers of systems from Small-Magellanic-Cloud-like dwarfs and Milky Way analogues to z similar to 2 starburst discs. Multiphase superwinds are generated in all passages, with outflow rates up to similar to 1000 M-circle dot yr(-1). However, the wind mass-loading efficiency (outflow rate divided by star formation rate, SFR) is similar to that in the isolated galaxy counterparts of each merger: it depends more on global galaxy properties (mass, size and escape velocity) than on the dynamical state or orbital parameters of the merger. Winds tend to be bi- or unipolar, but multiple 'events' build up complex morphologies with overlapping, differently oriented bubbles and shells at a range of radii. The winds have complex velocity and phase structure, with material at a range of speeds up to similar to 1000 km s(-1) (forming a Hubble-like flow), and a mix of molecular, ionized and hot gas that depends on galaxy properties. We examine how these different phases are connected to different feedback mechanisms. These simulations resolve a problem in some 'subgrid' models, where simple wind prescriptions can dramatically suppress merger-induced starbursts, often making it impossible to form Ultra Luminous Infrared Galaxies (ULIRGs). Despite large mass-loading factors (greater than or similar to 10-20) in the winds simulated here, the peak SFRs are comparable to those in 'no wind' simulations. Wind acceleration does not act equally, so cold dense gas can still lose angular momentum and form stars, while these stars blow out gas that would not have participated in the starburst in the first place. Considerable wind material is not unbound, and falls back on the disc at later times post-merger, leading to higher post-starburst SFRs in the presence of stellar feedback. We consider different simulation numerical methods and their effects on the wind phase structure; while most results are converged, we find that the existence of small clumps in the outflow at large distances from the galaxy is quite sensitive to the methodology. C1 [Hopkins, Philip F.] CALTECH, TAPIR, Pasadena, CA 91125 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Hopkins, Philip F.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Keres, Dusan] Univ Calif San Diego, Dept Phys, Ctr Astrophys & Space Sci, La Jolla, CA 92093 USA. [Murray, Norman] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Murray, Norman] Univ Toronto, Canada Res Chair Astrophys, Toronto, ON M5S 3H8, Canada. [Hernquist, Lars] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Narayanan, Desika] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Hayward, Christopher C.] Heidelberger Inst Theoret Studien, D-69118 Heidelberg, Germany. RP Hopkins, PF (reprint author), CALTECH, TAPIR, Mailcode 350-17, Pasadena, CA 91125 USA. EM phopkins@caltech.edu RI Hayward, Christopher/I-4756-2012 OI Hayward, Christopher/0000-0003-4073-3236 FU NASA [PF1-120083, NAS8-03060, NNG06GI68G]; David and Lucile Packard Foundation FX We thank Eliot Quataert for helpful discussions and contributions motivating this work, and thank the anonymous referee and editor for insightful comments and suggestions. Support for PFH was provided by NASA through Einstein Postdoctoral Fellowship Award Number PF1-120083 issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the NASA under contract NAS8-03060. EQ is supported in part by NASA grant NNG06GI68G and the David and Lucile Packard Foundation. NR 130 TC 28 Z9 28 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2013 VL 433 IS 1 BP 78 EP 97 DI 10.1093/mnras/stt690 PG 20 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200007 ER PT J AU Burningham, B Cardoso, CV Smith, L Leggett, SK Smart, RL Mann, AW Dhital, S Lucas, PW Tinney, CG Pinfield, DJ Zhang, Z Morley, C Saumon, D Aller, K Littlefair, SP Homeier, D Lodieu, N Deacon, N Marley, MS van Spaandonk, L Baker, D Allard, F Andrei, AH Canty, J Clarke, J Day-Jones, AC Dupuy, T Fortney, JJ Gomes, J Ishii, M Jones, HRA Liu, M Magazzu, A Marocco, F Murray, DN Rojas-Ayala, B Tamura, M AF Burningham, Ben Cardoso, C. V. Smith, L. Leggett, S. K. Smart, R. L. Mann, A. W. Dhital, S. Lucas, P. W. Tinney, C. G. Pinfield, D. J. Zhang, Z. Morley, C. Saumon, D. Aller, K. Littlefair, S. P. Homeier, D. Lodieu, N. Deacon, N. Marley, M. S. van Spaandonk, L. Baker, D. Allard, F. Andrei, A. H. Canty, J. Clarke, J. Day-Jones, A. C. Dupuy, T. Fortney, J. J. Gomes, J. Ishii, M. Jones, H. R. A. Liu, M. Magazzu, A. Marocco, F. Murray, D. N. Rojas-Ayala, B. Tamura, M. TI 76 T dwarfs from the UKIDSS LAS: benchmarks, kinematics and an updated space density SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; brown dwarfs; stars: low-mass ID INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; GALACTIC CLUSTERS SURVEY; INFRARED-SURVEY-EXPLORER; INTEGRAL-FIELD SPECTROGRAPH; COOLEST BROWN DWARFS; EARLY DATA RELEASE; LARGE-AREA SURVEY; SOLAR NEIGHBORHOOD; L/T TRANSITION AB We report the discovery of 76 new T dwarfs from the UKIRT Infrared Deep Sky Survey (UKIDSS) Large Area Survey (LAS). Near-infrared broad- and narrow-band photometry and spectroscopy are presented for the new objects, along with Wide-field Infrared Survey Explorer (WISE) and warm-Spitzer photometry. Proper motions for 128 UKIDSS T dwarfs are presented from a new two epoch LAS proper motion catalogue. We use these motions to identify two new benchmark systems: LHS 6176AB, a T8p+M4 pair and HD 118865AB, a T5.5+F8 pair. Using age constraints from the primaries and evolutionary models to constrain the radii, we have estimated their physical properties from their bolometric luminosity. We compare the colours and properties of known benchmark T dwarfs to the latest model atmospheres and draw two principal conclusions. First, it appears that the H - [4.5] and J - W2 colours are more sensitive to metallicity than has previously been recognized, such that differences in metallicity may dominate over differences in T-eff when considering relative properties of cool objects using these colours. Secondly, the previously noted apparent dominance of young objects in the late-T dwarf sample is no longer apparent when using the new model grids and the expanded sample of late-T dwarfs and benchmarks. This is supported by the apparently similar distribution of late-T dwarfs and earlier type T dwarfs on reduced proper motion diagrams that we present. Finally, we present updated space densities for the late-T dwarfs, and compare our values to simulation predictions and those from WISE. C1 [Burningham, Ben; Cardoso, C. V.; Smith, L.; Lucas, P. W.; Pinfield, D. J.; Zhang, Z.; van Spaandonk, L.; Baker, D.; Canty, J.; Clarke, J.; Day-Jones, A. C.; Gomes, J.; Jones, H. R. A.; Marocco, F.] Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. [Burningham, Ben; Andrei, A. H.] Observ Nacl, BR-20921400 Rio De Janeiro, Brazil. [Cardoso, C. V.; Smart, R. L.; Andrei, A. H.] Osserv Astron Torino, Ist Nazl Astrofis, I-10025 Pino Torinese, Italy. [Leggett, S. K.] Gemini Observ, Hilo, HI 96720 USA. [Mann, A. W.; Aller, K.; Liu, M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Dhital, S.] Boston Univ, Dept Astron, Boston, MA 02215 USA. [Tinney, C. G.] Univ New S Wales, Australian Ctr Astrobiol, Sydney, NSW 2052, Australia. [Tinney, C. G.] Univ New S Wales, Sch Phys, Sydney, NSW 2052, Australia. [Morley, C.; Fortney, J. J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Saumon, D.] Los Alamos Natl Lab, Los Alamos, NM 87545 USA. [Littlefair, S. P.] Univ Sheffield, Dept Phys & Astron, Sheffield S3 7RH, S Yorkshire, England. [Homeier, D.] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany. [Homeier, D.] Ecole Normale Super Lyon, CRAL, CNRS, UMR 5574, F-69364 Lyon, France. [Lodieu, N.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Lodieu, N.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Spain. [Deacon, N.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Marley, M. S.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Andrei, A. H.] Shanghai Astron Observatory, CAS, Shanghai 200030, Peoples R China. [Andrei, A. H.] Univ Fed Rio de Janeiro, Observat Valongo, BR-20080090 Rio de Janeiro, Brazil. [Day-Jones, A. C.] Univ Chile, Camino Observ, Santiago, Chile. [Dupuy, T.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ishii, M.] Subaru Telescope, Hilo, HI 96720 USA. [Magazzu, A.] INAF, Fundac Galileo Galilei, E-38700 Santa Cruz De La Palma, Spain. [Rojas-Ayala, B.] Amer Museum Nat Hist, Dept Astrophys, New York, NY 10024 USA. [Tamura, M.] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. RP Burningham, B (reprint author), Univ Hertfordshire, Sci & Technol Res Inst, Ctr Astrophys Res, Hatfield AL10 9AB, Herts, England. EM b.burningham@herts.ac.uk RI Rojas-Ayala, Barbara/G-4382-2015; OI Leggett, Sandy/0000-0002-3681-2989; Rojas-Ayala, Barbara/0000-0002-0149-1302; Littlefair, Stuart/0000-0001-7221-855X; Smart, Richard/0000-0002-4424-4766; Burningham, Ben/0000-0003-4600-5627; Fortney, Jonathan/0000-0002-9843-4354; Homeier, Derek/0000-0002-8546-9128; Magazzu, Antonio/0000-0003-1259-4371; Allard, France/0000-0003-1929-9340; Mann, Andrew/0000-0003-3654-1602; Marley, Mark/0000-0002-5251-2943; Tinney, Christopher/0000-0002-7595-0970 FU Marie Curie 7th European Community Framework Programme [247593]; Fondecyt postdoctorado fellowship [3100098]; proyecto Basal [PB06 (CATA)]; Joint Committee ESO-Government Chile; CNPq [PQ306775/2009-3]; SHAO/CAS; ARC [DP0774000]; Gemini Observatory; RoPACS; Marie Curie Initial Training Network; European Commission; Spanish Ministry of Science and Innovation through the Ramon y Cajal fellowship [08-303-01-02, AYA2010-19136] FX We thank our referee, J. Davy Kirkpatrick, for a helpful review which substantially improved the quality of this manuscript. Based on observations made under project A22TAC96 on the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundacin Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministerio da Ciencia e Tecnologia (Brazil) and Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina). We would like to acknowledge the support of the Marie Curie 7th European Community Framework Programme grant no. 247593 Interpretation and Parametrization of Extremely Red COOL dwarfs (IPERCOOL) International Research Staff Exchange Scheme. ADJ is supported by a Fondecyt postdoctorado fellowship, under project number 3100098, and is also partially supported by the proyecto Basal PB06 (CATA) and the Joint Committee ESO-Government Chile. AHA thanks CNPq grant PQ306775/2009-3 and SHAO/CAS Visiting Professorship grant. CGT is supported by ARC grant DP0774000. SKL's research is supported by the Gemini Observatory. JG is supported by RoPACS, a Marie Curie Initial Training Network funded by the European Commission's Seventh Framework Programme. NL acknowledges funding from the Spanish Ministry of Science and Innovation through the Ramon y Cajal fellowship number 08-303-01-02 and the project number AYA2010-19136. This research has made use of the NASA/IPAC Infrared Science Archive, which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of the SIMBAD data base, operated at CDS, Strasbourg, France, and has benefited from the SpeX Prism Spectral Libraries, maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism. We wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. NR 124 TC 32 Z9 32 U1 0 U2 7 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 JUL PY 2013 VL 433 IS 1 BP 457 EP 497 DI 10.1093/mnras/stt740 PG 41 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200038 ER PT J AU Aravena, M Murphy, EJ Aguirre, JE Ashby, MLN Benson, BA Bothwell, M Brodwin, M Carlstrom, JE Chapman, SC Crawford, TM de Breuck, C Fassnacht, CD Gonzalez, AH Greve, TR Gullberg, B Hezaveh, Y Holder, GP Holzapfel, WL Keisler, R Malkan, M Marrone, DP McIntyre, V Reichardt, CL Sharon, K Spilker, JS Stalder, B Stark, AA Vieira, JD Weiss, A AF Aravena, M. Murphy, E. J. Aguirre, J. E. Ashby, M. L. N. Benson, B. A. Bothwell, M. Brodwin, M. Carlstrom, J. E. Chapman, S. C. Crawford, T. M. de Breuck, C. Fassnacht, C. D. Gonzalez, A. H. Greve, T. R. Gullberg, B. Hezaveh, Y. Holder, G. P. Holzapfel, W. L. Keisler, R. Malkan, M. Marrone, D. P. McIntyre, V. Reichardt, C. L. Sharon, K. Spilker, J. S. Stalder, B. Stark, A. A. Vieira, J. D. Weiss, A. TI Large gas reservoirs and free-free emission in two lensed star-forming galaxies at z=2.7 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: formation; galaxies: high-redshift; galaxies: starburst; cosmology: observations ID SOUTH-POLE TELESCOPE; GREEN BANK TELESCOPE; SUBMILLIMETER GALAXIES; MOLECULAR GAS; INFRARED GALAXIES; HIGH-REDSHIFT; COMPACT STARBURSTS; COSMOS FIELD; RADIO; CO AB We report the detection of CO(1-0) line emission in the bright, lensed star-forming galaxies SPT-S 233227-5358.5 (z = 2.73) and SPT-S 053816-5030.8 (z = 2.78), using the Australia Telescope Compact Array. Both galaxies were discovered in a large-area millimetre survey with the South Pole Telescope (SPT) and found to be gravitationally lensed by intervening structures. The measured CO intensities imply galaxies with molecular gas masses of (3.2 +/- 0.5) x 10(10)(mu/15)(-1)(X-CO/0.8) and (1.7 +/- 0.3) x 10(10)(mu/20)(-1)(X-CO/0.8) M-circle dot, and gas depletion time-scales of 4.9 x 10(7)(X-CO/0.8) and 2.6 x 10(7)(X-CO/0.8) yr, respectively, where mu corresponds to the lens magnification and X-CO is the CO luminosity to gas mass conversion factor. In the case of SPT-S 053816-5030.8, we also obtained significant detections of the rest-frame 115.7 and 132.4 GHz radio continuum. Based on the radio-to-infrared spectral energy distribution and an assumed synchrotron spectral index, we find that 42 +/- 10 and 55 +/- 13 per cent of the flux at rest-frame 115.7 and 132.4 GHz arises from free-free emission. We find a radio-derived intrinsic star formation rate of 470 +/- 170 M-circle dot yr(-1), consistent within the uncertainties with the infrared estimate. Based on the morphology of this object in the source plane, the derived gas mass and the possible flattening of the radio spectral index towards low frequencies, we argue that SPT-S 053816-5030.8 exhibits properties compatible with a scaled-up local ultraluminous infrared galaxy. C1 [Aravena, M.; de Breuck, C.; Gullberg, B.] European So Observ, Casilla, Vitacura Santia, Chile. [Murphy, E. J.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Aguirre, J. E.] Univ Penn, Philadelphia, PA 19104 USA. Univ Penn, Philadelphia, PA 19104 USA. [Ashby, M. L. N.; Stalder, B.; Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Benson, B. A.; Carlstrom, J. E.; Crawford, T. M.; Keisler, R.; Sharon, K.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bothwell, M.; Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bothwell, M.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Crawford, T. M.; Sharon, K.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.] Argonne Natl Lab, Argonne, IL 60439 USA. [Chapman, S. C.] Univ Cambridge Inst Astron, Inst Astron, Cambridge CB3 0HA, England. [Chapman, S. C.] Dalhousie Univ, Halifax B3H 4R2, NS, Canada. [Fassnacht, C. D.] Univ Calif Davis, Dept Phys, Livermore, CA 95616 USA. [Gonzalez, A. H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Greve, T. R.] UCL, Dept Phys & Astron, London WC1E 6BT, England. [Hezaveh, Y.; Holder, G. P.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Holzapfel, W. L.; Reichardt, C. L.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Malkan, M.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [McIntyre, V.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Stalder, B.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Vieira, J. D.] CALTECH, Pasadena, CA 91125 USA. [Weiss, A.] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Aravena, M (reprint author), European So Observ, Casilla, Vitacura Santia, Chile. EM maravena@eso.org RI Aravena, Manuel/O-2361-2014; Holzapfel, William/I-4836-2015; OI Marrone, Daniel/0000-0002-2367-1080; Reichardt, Christian/0000-0003-2226-9169; De Breuck, Carlos/0000-0002-6637-3315; Stark, Antony/0000-0002-2718-9996 FU Marie Curie Actions of the European Commission (FP7-COFUND); Commonwealth of Australia; National Science Foundation [ANT-0638937, PHY-1125897]; Kavli Foundation; Gordon and Betty Moore Foundation FX We thank Andy Biggs for useful discussions. MA and this work was co-funded under the Marie Curie Actions of the European Commission (FP7-COFUND). The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support through PHY-1125897, the Kavli Foundation and the Gordon and Betty Moore Foundation. NR 56 TC 18 Z9 18 U1 0 U2 3 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 JUL PY 2013 VL 433 IS 1 BP 498 EP 505 DI 10.1093/mnras/stt741 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200039 ER PT J AU Mullaney, JR Alexander, DM Fine, S Goulding, AD Harrison, CM Hickox, RC AF Mullaney, J. R. Alexander, D. M. Fine, S. Goulding, A. D. Harrison, C. M. Hickox, R. C. TI Narrow-line region gas kinematics of 24 264 optically selected AGN: the radio connection SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; ISM: kinematics and dynamics; galaxies: active; quasars: emission lines; radio continuum: galaxies ID ACTIVE GALACTIC NUCLEI; DIGITAL-SKY-SURVEY; BLACK-HOLE MASS; HARD X-RAY; EMISSION-LINE; SEYFERT-GALAXIES; HOST GALAXIES; EDDINGTON RATIO; LUMINOSITY FUNCTION; GASEOUS KINEMATICS AB Using a sample of 24 264 optically selected active galactic nuclei (AGNs) from the SDSS DR7 data base, we characterize how the profile of the [O iii] lambda 5007 emission line relates to bolometric luminosity (L-AGN), Eddington ratio, radio loudness, radio luminosity (L-1.4 GHz) and optical class (i.e. broad/narrow-line Seyfert 1, type 2) to determine what drives the kinematics of this kpc-scale line emitting gas. First, we use spectral stacking to characterize how the average [O iii] lambda 5007 profile changes as a function of these five variables. After accounting for the known correlation between L-AGN and L-1.4 GHz, we report that L-1.4 GHz has the strongest influence on the [O iii] lambda 5007 profile, with AGNs of moderate radio luminosity (L-1.4 GHz = 10(23)-10(25) W Hz(-1)) having the broadest [O iii] lambda 5007 profiles. Conversely, we find only a modest change in the [O iii] lambda 5007 profile with increasing radio loudness and find no significant difference between the [O iii] lambda 5007 profiles of broad- and narrow-line Seyfert 1s. When binned according to Eddington ratio, only the AGNs in our highest bin (i.e. > 0.3) show any signs of having broadened [O iii] lambda 5007 profiles, although the small numbers of such extreme AGNs in our sample mean we cannot rule out that other processes (e.g. radio jets) are responsible for this broadening. The [O iii] lambda 5007 profiles of type 1 and type 2 AGNs show the same trends in terms of line width, but type 1 AGNs display a much stronger 'blue wing', which we interpret as evidence of outflowing ionized gas. We perform multicomponent fitting to the H beta, [O iii] lambda lambda 4959, 5007, [N ii] lambda lambda 6548, 6584 and H alpha lines for all the AGNs in our sample to calculate the proportions of AGNs with broad [O iii] lambda 5007 profiles. The individual fits confirm the results from our stacked spectra; AGNs with L-1.4 GHz > 10(23) W Hz(-1) are roughly five times more likely to have extremely broad [O iii] lambda 5007 lines (full width at half-maximum, FWHMAvg > 1000 km s(-1)) compared to lower L-1.4 GHz AGNs, and the width of the [O iii] lambda 5007 line peaks in moderate-radio-luminosity AGNs (L-1.4 GHz similar to 10(24) W Hz(-1)). Our results are consistent with the most disturbed gas kinematics being induced by compact radio cores (rather than powerful radio jets), although broadened [O iii] lambda 5007 lines are also present, but much rarer, in low-L-1.4 GHz systems. Our catalogue of multicomponent fits is freely available as an online resource for statistical studies of the kinematics and luminosities of the narrow- and broad-line AGN regions and the identification of potential targets for follow-up observations at ext-link-type="uri" xlink:href="http://sites.google.com/site/sdssalpaka" xmlns:xlink="http://www.w3.org/1999/xlink">http://sites.google.com/site/sdssalpaka. C1 [Mullaney, J. R.; Alexander, D. M.; Fine, S.; Harrison, C. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Mullaney, J. R.] Univ Paris Diderot, CEA Saclay, Serv Astrophys, Lab AIM,CEA,DSM,CNRS,Irfu, F-91191 Gif Sur Yvette, France. [Goulding, A. D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hickox, R. C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. RP Mullaney, JR (reprint author), Univ Durham, Dept Phys, South Rd, Durham DH1 3LE, England. EM j.r.mullaney@dur.ac.uk OI Alexander, David/0000-0002-5896-6313 FU STFC; Alfred P. Sloan Foundation; National Science Foundation; US Department of Energy; National Aeronautics and Space Administration; Japanese Monbukagakusho; Max Planck Society; Higher Education Funding Council for England FX JRM and DMA acknowledges The Leverhulme Trust. CMH acknowledges funding from STFC. This work has made use of data provided by the SDSS. Funding for the SDSS has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. The SDSS website is http://www.sdss.org/. NR 64 TC 47 Z9 47 U1 0 U2 3 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 JUL PY 2013 VL 433 IS 1 BP 622 EP 638 DI 10.1093/mnras/stt751 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200050 ER PT J AU Heida, M Jonker, PG Torres, MAP Roberts, TP Miniutti, G Fabian, AC Ratti, EM AF Heida, M. Jonker, P. G. Torres, M. A. P. Roberts, T. P. Miniutti, G. Fabian, A. C. Ratti, E. M. TI VLT/FORS2 observations of four high-luminosity ULX candidates(star) SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: distances and redshifts; galaxies: individual: AM 0644-741; galaxies: individual: ESO 306-003; galaxies: individual: NGC 533; galaxies: individual: NGC 741; X-rays: galaxies ID X-RAY SOURCES; MASS BLACK-HOLES; OPTICAL COUNTERPARTS; NEARBY GALAXIES; CHANDRA; SPECTROSCOPY; POPULATION; EMISSION; CLUSTERS; CATALOG AB We obtained Very Large Telescope/FOcal Reducer and low dispersion Spectrograph spectra of the optical counterparts of four high-luminosity (L-X >= 10(40) erg s(-1)) Ultraluminous X-ray sources (ULX) candidates from the catalogue of Walton et al. We first determined accurate positions for the X-ray sources from archival Chandra observations and identified counterparts in archival optical observations that are sufficiently bright for spectroscopy with an 8 m telescope. From the spectra we determine the redshifts to the optical counterparts and emission line ratios. One of the candidate ULXs, in the spiral galaxy ESO 306-003, appears to be a bona fide ULX in an H ii region. The other three sources, near the elliptical galaxies NGC 533 and NGC 741 and in the ring galaxy AM 0644-741, turn out to be background active galactic nuclei (AGN) with redshifts of 1.85, 0.88 or 1.75 and 1.40, respectively. Our findings confirm the trend of a high probability of finding background AGN for systems with a ratio of log(F-X/F-opt) in the range of -1-1. C1 [Heida, M.; Jonker, P. G.; Torres, M. A. P.; Ratti, E. M.] SRON Netherlands Inst Space Res, NL-3584 CA Utrecht, Netherlands. [Heida, M.; Jonker, P. G.] Radboud Univ Nijmegen, Dept Astrophys IMAPP, NL-6500 GL Nijmegen, Netherlands. [Jonker, P. G.; Torres, M. A. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Roberts, T. P.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Miniutti, G.] Ctr Astrobiol CSIC INTA, Dep Astrofis, E-28691 Madrid, Spain. [Miniutti, G.] ESAC, E-28691 Madrid, Spain. [Fabian, A. C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Heida, M (reprint author), SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands. EM m.heida@astro.ru.nl RI Miniutti, Giovanni/L-2721-2014 OI Miniutti, Giovanni/0000-0003-0707-4531 FU Netherlands Organization for Scientific Research; Spanish Plan Nacional de Astronomia y Astrofisica [AYA2010-21490-C02-02]; La Silla Paranal Observatory [088B-0076A] FX PGJ and MAPT acknowledge support from the Netherlands Organization for Scientific Research. GM acknowledges support from the Spanish Plan Nacional de Astronomia y Astrofisica under grant AYA2010-21490-C02-02. This research is based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 088B-0076A. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application package CIAO and of the software packages PAMELA and MOLLY provided by Tom Marsh. NR 44 TC 7 Z9 7 U1 0 U2 3 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 JUL PY 2013 VL 433 IS 1 BP 681 EP 687 DI 10.1093/mnras/stt756 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200054 ER PT J AU Ogrean, GA Bruggen, M van Weeren, RJ Rottgering, H Croston, JH Hoeft, M AF Ogrean, G. A. Brueggen, M. van Weeren, R. J. Rottgering, H. Croston, J. H. Hoeft, M. TI Challenges to our understanding of radio relics: X-ray observations of the Toothbrush cluster SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; galaxies: clusters: individual: 1RXS J0603; 3+4214; X-rays: galaxies: clusters ID MERGING GALAXY CLUSTER; COSMOLOGICAL SHOCK-WAVES; LARGE-SCALE STRUCTURE; XMM-NEWTON; PARTICLE-ACCELERATION; INTERSTELLAR-MEDIUM; HALOS; SIMULATIONS; EMISSION; SPECTRUM AB The cluster 1RXS J0603.3+4214 is a merging galaxy cluster that hosts three radio relics and a giant radio halo. The northern relic, the Toothbrush, is 1.9 Mpc long and has an unusual linear morphology. According to simple diffusive shock acceleration theory, its radio spectral index indicates a Mach number of 3.3-4.6. Here, we present results from a deep XMM-Newton observation of the cluster. We observe two distinct cluster cores that have survived the merger. The presence of three shocks at or near the locations of the radio relics is confirmed by density and temperature discontinuities. However, the observation poses several puzzles that challenge our understanding of radio relics: (i) at the Toothbrush, the shock Mach number is not larger than 2, in apparent conflict with the shock strength predicted from the radio spectrum; (ii) at the Toothbrush, the shock front is, in part, spatially offset from the radio emission; (iii) at the eastern relic, we detect a temperature jump corresponding to a Mach number of approximately 2.5, but there is no associated surface brightness discontinuity. We discuss possible explanations for these findings. C1 [Ogrean, G. A.; Brueggen, M.] Hamburger Sternwarte, D-21029 Hamburg, Germany. [van Weeren, R. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rottgering, H.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hoeft, M.] Thuringer Landessternwarte, D-07778 Tautenburg, Germany. RP Ogrean, GA (reprint author), Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany. EM gogrean@hs.uni-hamburg.de OI van Weeren, Reinout/0000-0002-0587-1660 FU Deutsche Forschungsgemeinschaft (DFG); NASA by Chandra X-ray Center [PF2-130104]; ESA; USA (NASA); research group FOR 1254; NASA [NAS8-03060] FX We thank the referee for helpful comments. GAO thanks Franco Vazza, Annalisa Bonafede and Elke Roediger for helpful discussions. MB and MH acknowledge support by the research group FOR 1254 funded by the Deutsche Forschungsgemeinschaft (DFG). RJvW acknowledges support provided by NASA through the Einstein Postdoctoral Fellowship grant number PF2-130104 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. This research is based on data from observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and the USA (NASA). NR 45 TC 36 Z9 36 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 JUL PY 2013 VL 433 IS 1 BP 812 EP 824 DI 10.1093/mnras/stt776 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200067 ER PT J AU Pan, T Patnaude, D Loeb, A AF Pan, Tony Patnaude, Daniel Loeb, Abraham TI Superluminous X-ray emission from the interaction of supernova ejecta with dense circumstellar shells SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE shock waves; circumstellar matter; supernovae: general; stars: winds; outflows; X-rays: general ID PULSATIONAL PAIR-INSTABILITY; LUMINOUS SUPERNOVAE; SHOCK BREAKOUT; IIN SUPERNOVA; MASS-LOSS; LIGHT CURVES; SN 2005GL; WIND; STAR; OUTBURST AB For supernova (SN) powered by the conversion of kinetic energy into radiation due to the interactions of the ejecta with a dense circumstellar shell, we show that there could be X-ray analogues of optically superluminous SNe with comparable luminosities and energetics. We consider X-ray emission from the forward shock of SN ejecta colliding into an optically thin circumstellar material (CSM) shell, derive simple expressions for the X-ray luminosity as a function of the circumstellar shell characteristics, and discuss the different regimes in which the shock will be radiative or adiabatic, and whether the emission will be dominated by free-free radiation or line cooling. We find that even with normal SN explosion energies of 10(51) erg, there exist CSM shell configurations that can liberate a large fraction of the explosion energy in X-rays, producing unabsorbed X-ray luminosities approaching 10(44) erg s(-1) events lasting a few months, or even 10(45) erg s(-1) flashes lasting days. Although the large column density of the circumstellar shell can absorb most of the flux from the initial shock, the most luminous events produce hard X-rays that are less susceptible to photoelectric absorption, and can counteract such losses by completely ionizing the intervening material. Regardless, once the shock traverses the entire circumstellar shell, the full luminosity could be available to observers. C1 [Pan, Tony; Patnaude, Daniel; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Pan, T (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM span@physics.harvard.edu FU Hertz Foundation; National Science Foundation; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A] FX We thank Sayan Chakraborti, Manos Chatzopoulos, Raffaella Margutti, Takashi Moriya, John Raymond and Randall Smith for useful discussions. TP was supported by the Hertz Foundation and the National Science Foundation via a graduate research fellowship. This work was supported in part by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A. NR 65 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2013 VL 433 IS 1 BP 838 EP 848 DI 10.1093/mnras/stt780 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 178PZ UT WOS:000321461200069 ER PT J AU Wiersma, RPC Ciardi, B Thomas, RM Harker, GJA Zaroubi, S Bernardi, G Brentjens, M de Bruyn, AG Daiboo, S Jelic, V Kazemi, S Koopmans, LVE Labropoulos, P Martinez, O Mellema, G Offringa, A Pandey, VN Schaye, J Veligatla, V Vedantham, H Yatawatta, S AF Wiersma, R. P. C. Ciardi, B. Thomas, R. M. Harker, G. J. A. Zaroubi, S. Bernardi, G. Brentjens, M. de Bruyn, A. G. Daiboo, S. Jelic, V. Kazemi, S. Koopmans, L. V. E. Labropoulos, P. Martinez, O. Mellema, G. Offringa, A. Pandey, V. N. Schaye, J. Veligatla, V. Vedantham, H. Yatawatta, S. TI LOFAR insights into the epoch of reionization from the cross-power spectrum of 21 cm emission and galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: formation; intergalactic medium; cosmology: observations; dark ages; reionization; first stars ID LY-ALPHA EMITTERS; UV LUMINOSITY FUNCTIONS; INTERGALACTIC MEDIUM; COSMIC REIONIZATION; HYDROGEN REIONIZATION; FORMATION HISTORY; STELLAR SOURCES; STAR-FORMATION; 1ST GALAXIES; SIMULATIONS AB Using a combination of N-body simulations, semi-analytic models and radiative transfer calculations, we have estimated the theoretical cross-power spectrum between galaxies and the 21 cm emission from neutral hydrogen during the epoch of reionization. In accordance with previous studies, we find that the 21 cm emission is initially correlated with haloes on large scales (greater than or similar to 30 Mpc), anticorrelated on intermediate (similar to 5 Mpc) and uncorrelated on small (less than or similar to 3 Mpc) scales. This picture quickly changes as reionization proceeds and the two fields become anticorrelated on large scales. The normalization of the cross-power spectrum can be used to set constraints on the average neutral fraction in the intergalactic medium and its shape can be a powerful tool to study the topology of reionization. When we apply a drop-out technique to select galaxies and add to the 21 cm signal the noise expected from the LOw Frequency ARray (LOFAR) telescope, we find that while the normalization of the cross-power spectrum remains a useful tool for probing reionization, its shape becomes too noisy to be informative. On the other hand, for an Ly alpha Emitter (LAE) survey both the normalization and the shape of the cross-power spectrum are suitable probes of reionization. A closer look at a specific planned LAE observing program using Subaru Hyper-Suprime Cam reveals concerns about the strength of the 21 cm signal at the planned redshifts. If the ionized fraction at z similar to 7 is lower than the one estimated here, then using the cross-power spectrum may be a useful exercise given that at higher redshifts and neutral fractions it is able to distinguish between two toy models with different topologies. C1 [Wiersma, R. P. C.; Ciardi, B.] Max Planck Inst Astrophys, D-85748 Garching, Germany. [Thomas, R. M.] Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada. [Thomas, R. M.] Netherlands Inst Neurosci, NL-1105 BA Amsterdam, Netherlands. [Harker, G. J. A.; Yatawatta, S.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Zaroubi, S.; de Bruyn, A. G.; Daiboo, S.; Kazemi, S.; Koopmans, L. V. E.; Labropoulos, P.; Martinez, O.; Offringa, A.; Pandey, V. N.; Veligatla, V.; Vedantham, H.] Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands. [Bernardi, G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brentjens, M.; de Bruyn, A. G.; Jelic, V.; Labropoulos, P.; Pandey, V. N.; Yatawatta, S.] ASTRON, NL-7990 AA Dwingeloo, Netherlands. [Mellema, G.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Mellema, G.] Stockholm Univ, AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Schaye, J.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. RP Wiersma, RPC (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany. EM ciardi@mpa-garching.mpg.de RI Jelic, Vibor/B-2938-2014; Thomas, Rajat/B-7105-2014; Mellema, Garrelt/K-4962-2014; Harker, Geraint/C-4885-2012; Ciardi, Benedetta/N-7625-2015; Yatawatta, Sarod/E-6037-2013 OI Jelic, Vibor/0000-0002-6034-8610; Schaye, Joop/0000-0002-0668-5560; Thomas, Rajat/0000-0002-5362-4816; Mellema, Garrelt/0000-0002-2512-6748; Harker, Geraint/0000-0002-7894-4082; Yatawatta, Sarod/0000-0001-5619-4017 FU DFG [1177]; NASA Lunar Science Institute [NNA09DB30A]; European Research Council under ERC-Starting Grant [FIRSTLIGHT - 258942] FX This work was supported by DFG Priority Program 1177. The authors would like to thank Masami Ouchi for kindly providing observing strategies for the Subaru Hyper-Suprime Cam. GH is a member of the LUNAR consortium, which is funded by the NASA Lunar Science Institute (via Cooperative Agreement NNA09DB30A) to investigate concepts for astrophysical observatories on the Moon. LVEK, HV and SD acknowledge the financial support from the European Research Council under ERC-Starting Grant FIRSTLIGHT - 258942. We would also like to thank the anonymous referee whose comments improved this paper. NR 52 TC 9 Z9 9 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2013 VL 432 IS 3 BP 2615 EP 2624 DI 10.1093/mnras/stt624 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 165AW UT WOS:000320455800059 ER PT J AU Sun, YW Xie, PH Xu, J Zhou, HJ Liu, C Wang, Y Liu, WQ Si, FQ Zeng, Y AF Sun You-Wen Xie Pin-Hua Xu Jin Zhou Hai-Jin Liu Cheng Wang Yang Liu Wen-Qing Si Fu-Qi Zeng Yi TI Measurement of atmospheric CO2 vertical column density using weighting function modified differential optical absorption spectroscopy SO ACTA PHYSICA SINICA LA Chinese DT Article DE environmental pollution Measurements; optical measurement techniques; infrared spectrum; green-house gas ID AIR-MASS-FACTORS; SCIAMACHY; RETRIEVAL; MODEL; DOAS; SPECTROMETER; RADIANCES; NO2; CH4 AB In this paper, we demonstrate a method of atmospheric CO2 vertical column density (VCD) retrieval by using weighting function modified differential optical absorption spectroscopy (WFM-DOAS). Direct sun measurement serves as an example for WFM-DOAS fitting. The atmosphere is divided into 50 layers in the process of WFM-DOAS retrieval, while the simulated sun-normalized radiance and the total weighting functions (CO2, H2O and CH4) for each measurement are computed in terms of the radiative transfer model (RTM) SCIATRAN by using the HITRAN data base and the solar spectrum from Livingston and Wallace (1991). The CO2 vertical column density time series were obtained by utilizing WFM-DOAS fitting method to all direct sun measurement spectra. Fitting errors are all less than 3%. Fitting results for two different DOAS algorithms are compared with each other. It is indicated that the WFM-DOAS technique has the potential of being applied in passive gas remote sensing in the infrared region. C1 [Sun You-Wen; Xie Pin-Hua; Xu Jin; Zhou Hai-Jin; Wang Yang; Liu Wen-Qing; Si Fu-Qi; Zeng Yi] Chinese Acad Sci, Key Lab Environm Opt & Technol, Anhui Inst Opt & Fine Mech, Hefei 230031, Peoples R China. [Liu Cheng] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Liu, C (reprint author), Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. EM chliu@cfa.harvard.edu FU Special Scientific Research Fund of Meteorological Public Welfare Profession of China [GYHY201106045-1, 201109007]; National Natural Science Foundation of China [41275037, 41105011] FX Project supported by the Special Scientific Research Fund of Meteorological Public Welfare Profession of China (Grant Nos. GYHY201106045-1, 201109007), and the National Natural Science Foundation of China (Grant Nos. 41275037, 41105011). NR 26 TC 0 Z9 1 U1 2 U2 15 PU CHINESE PHYSICAL SOC PI BEIJING PA P O BOX 603, BEIJING 100080, PEOPLES R CHINA SN 1000-3290 J9 ACTA PHYS SIN-CH ED JI Acta Phys. Sin. PD JUL PY 2013 VL 62 IS 13 AR 130703 DI 10.7498/aps.62.130703 PG 10 WC Physics, Multidisciplinary SC Physics GA 193NK UT WOS:000322566300022 ER PT J AU Wing, SL Currano, ED AF Wing, Scott L. Currano, Ellen D. TI PLANT RESPONSE TO A GLOBAL GREENHOUSE EVENT 56 MILLION YEARS AGO SO AMERICAN JOURNAL OF BOTANY LA English DT Article DE Paleocene-Eocene Thermal Maximum; PETM; greenhouse climate; floristic change; anthropogenic global warming ID EOCENE THERMAL MAXIMUM; ELEVATED ATMOSPHERIC CO2; CARBON-ISOTOPE EXCURSION; PALEOCENE-EARLY EOCENE; BIGHORN BASIN; CLIMATE-CHANGE; WILLWOOD FORMATION; NORTH-AMERICA; PALAEOCENE/EOCENE BOUNDARY; OXYGEN-ISOTOPE AB Premise of the study: The fossil record provides information about the long-term response of plants to CO2-induced climate change. The Paleocene-Eocene Thermal Maximum (PETM), a 200 000-yr-long period of rapid carbon release and warming that occurred similar to 56 million years ago, is analogous to future anthropogenic global warming. Methods: We collected plant macrofossils in the Bighorn Basin, Wyoming, United States, from a period spanning the PETM and studied changes in floristic composition. We also compiled and summarized published records of floristic change during the PETM. Key results: There was radical floristic change in the Bighorn Basin during the PETM reflecting local or regional extirpation of mesophytic plants, notably conifers, and colonization of the area by thermophilic and dry-tolerant species, especially Fabaceae. This floristic change largely reversed itself as the PETM ended, though some immigrant species persisted and some Paleocene species never returned. Less detailed records from other parts of the world show regional variation in floristic response, but are mostly consistent with the Bighorn Basin trends. Conclusions: Despite geologically rapid extirpation, colonization, and recolonization, we detected little extinction during the PETM, suggesting the rate of climate change did not exceed the dispersal capacity of terrestrial plants. Extrapolating the response of plants from the PETM to future anthropogenic climate change likely underestimates risk because rates of climate change during the PETM may have been an order of magnitude slower than current rates of change and because the abundant, widespread species common as fossils are likely resistant to extinction. C1 [Wing, Scott L.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Currano, Ellen D.] Miami Univ, Dept Geol & Environm Earth Sci, Oxford, OH 45056 USA. RP Wing, SL (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, POB 37012, Washington, DC 20013 USA. EM wings@si.edu OI Wing, Scott/0000-0002-2954-8905 FU Roland Brown Fund; Scholarly Studies Fund of the Smithsonian Institution; NSF [EAR-640192, EAR-0120727] FX The authors acknowledge support from the Roland Brown Fund and Scholarly Studies Fund of the Smithsonian Institution, and NSF grants EAR-640192 and EAR-0120727. Elizabeth C. Lovelock and Erika Gonzalez were centrally involved with collecting and individuating the floras from two critical sites. Colleagues and students too numerous to name assisted with collecting and providing geological context. This is Evolution of Terrestrial Ecosystems publication 240. NR 158 TC 21 Z9 23 U1 7 U2 59 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 JUL PY 2013 VL 100 IS 7 BP 1234 EP 1254 DI 10.3732/ajb.1200554 PG 21 WC Plant Sciences SC Plant Sciences GA 182TF UT WOS:000321766600002 PM 23825133 ER PT J AU Ardila, DR Herczeg, GJ Gregory, SG Ingleby, L France, K Brown, A Edwards, S Johns-Krull, C Linsky, JL Yang, H Valenti, JA Abgrall, H Alexander, RD Bergin, E Bethell, T Brown, JM Calvet, N Espaillat, C Hillenbrand, LA Hussain, G Roueff, E Schindhelm, ER Walter, FM AF Ardila, David R. Herczeg, Gregory J. Gregory, Scott G. Ingleby, Laura France, Kevin Brown, Alexander Edwards, Suzan Johns-Krull, Christopher Linsky, Jeffrey L. Yang, Hao Valenti, Jeff A. Abgrall, Herve Alexander, Richard D. Bergin, Edwin Bethell, Thomas Brown, Joanna M. Calvet, Nuria Espaillat, Catherine Hillenbrand, Lynne A. Hussain, Gaitee Roueff, Evelyne Schindhelm, Eric R. Walter, Frederick M. TI HOT GAS LINES IN T TAURI STARS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE protoplanetary disks; stars: pre-main sequence; stars: variables: T Tauri, Herbig Ae/Be; surveys; ultraviolet: stars ID HUBBLE-SPACE-TELESCOPE; MAIN-SEQUENCE STARS; X-RAY-EMISSION; ETA-CHAMAELEONTIS CLUSTER; FLUORESCENT H-2 EMISSION; HERBIG-AE STAR; MAGNETOCENTRIFUGALLY DRIVEN FLOWS; FAR-ULTRAVIOLET SPECTRA; MEAN RADIAL-VELOCITIES; YOUNG STELLAR OBJECTS AB For Classical T Tauri Stars (CTTSs), the resonance doublets of NV, Si IV, and C IV, as well as the He II 1640 angstrom line, trace hot gas flows and act as diagnostics of the accretion process. In this paper we assemble a large high-resolution, high-sensitivity data set of these lines in CTTSs and Weak T Tauri Stars (WTTSs). The sample comprises 35 stars: 1 Herbig Ae star, 28 CTTSs, and 6 WTTSs. We find that the C IV, Si IV, and N V lines in CTTSs all have similar shapes. We decompose the C IV and He II lines into broad and narrow Gaussian components (BC and NC). The most common (50%) C IV line morphology in CTTSs is that of a low-velocity NC together with a redshifted BC. For CTTSs, a strong BC is the result of the accretion process. The contribution fraction of the NC to the C IV line flux in CTTSs increases with accretion rate, from similar to 20% to up to similar to 80%. The velocity centroids of the BCs and NCs are such that V-BC greater than or similar to 4 V-NC, consistent with the predictions of the accretion shock model, in at most 12 out of 22 CTTSs. We do not find evidence of the post-shock becoming buried in the stellar photosphere due to the pressure of the accretion flow. The He II CTTSs lines are generally symmetric and narrow, with FWHM and redshifts comparable to those of WTTSs. They are less redshifted than the CTTSs C IV lines, by similar to 10 km s(-1). The amount of flux in the BC of the He II line is small compared to that of the C IV line, and we show that this is consistent with models of the pre-shock column emission. Overall, the observations are consistent with the presence of multiple accretion columns with different densities or with accretion models that predict a slow-moving, low-density region in the periphery of the accretion column. For HN Tau A and RW Aur A, most of the C IV line is blueshifted suggesting that the C IV emission is produced by shocks within outflow jets. In our sample, the Herbig Ae star DX Cha is the only object for which we find a P-Cygni profile in the C IV line, which argues for the presence of a hot (105 K) wind. For the overall sample, the Si IV and N V line luminosities are correlated with the C IV line luminosities, although the relationship between Si IV and C IV shows large scatter about a linear relationship and suggests that TW Hya, V4046 Sgr, AA Tau, DF Tau, GM Aur, and V1190 Sco are silicon-poor, while CV Cha, DX Cha, RU Lup, and RW Aur may be silicon-rich. C1 [Ardila, David R.] CALTECH, NASA Herschel Sci Ctr, Pasadena, CA 91125 USA. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Gregory, Scott G.; Hillenbrand, Lynne A.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Gregory, Scott G.] Univ St Andrews, Sch Phys & Astron, St Andrews KY16 9SS, Fife, Scotland. [Ingleby, Laura; Bergin, Edwin; Bethell, Thomas; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [France, Kevin; Brown, Alexander] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [Edwards, Suzan] Smith Coll, Dept Astron, Northampton, MA 01063 USA. [Johns-Krull, Christopher] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. [Linsky, Jeffrey L.] Univ Colorado, JILA, Boulder, CO 80309 USA. [Linsky, Jeffrey L.] NIST, Boulder, CO 80309 USA. [Yang, Hao] Cent China Normal Univ, Inst Astrophys, Wuhan 430079, Peoples R China. [Valenti, Jeff A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Abgrall, Herve; Roueff, Evelyne] CNRS, Observ Paris, Sect Meudon, UMR 8102, F-92195 Meudon, France. [Abgrall, Herve; Roueff, Evelyne] CNRS, Observ Paris, Sect Meudon, LUTH, F-92195 Meudon, France. [Alexander, Richard D.] Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. [Brown, Joanna M.; Espaillat, Catherine] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hussain, Gaitee] ESO, D-85748 Garching, Germany. [Schindhelm, Eric R.] Southwest Res Inst, Dept Space Studies, Boulder, CO 80303 USA. [Walter, Frederick M.] SUNY Stony Brook, Dept Phys & Astron, Stony Brook, NY 11794 USA. RP Ardila, DR (reprint author), CALTECH, NASA Herschel Sci Ctr, MC 100-22, Pasadena, CA 91125 USA. EM ardila@ipac.caltech.edu RI Yang, Hao/F-8396-2014; OI Yang, Hao/0000-0002-9423-2333; Gregory, Scott/0000-0003-3674-5568; Herczeg, Gregory/0000-0002-7154-6065 FU NASA through Space Telescope Science Institute (STScI) [HST-GO-11616.10, HST-GO-12161.01]; NASA [NAS 5-26555]; Science & Technology Facilities Council (STFC) [ST/J003255/1]; UK's Science & Technology Facilities Council (STFC) [ST/G00711X/1]; HST GTO [11533, 12036] FX Based on observations made with the NASA/ESA Hubble Space Telescope. Support for this paper was provided by NASA through grant numbers HST-GO-11616.10 and HST-GO-12161.01 from the Space Telescope Science Institute (STScI), which is operated by Association of Universities for Research in Astronomy, Inc. (AURA) under NASA contract NAS 5-26555. S. G. G. acknowledges support from the Science & Technology Facilities Council (STFC) via an Ernest Rutherford Fellowship [ST/J003255/1]. R. D. A. acknowledges support from the UK's Science & Technology Facilities Council (STFC) through an Advanced Fellowship (ST/G00711X/1).; We thank the team from HST GTO programs 11533 and 12036 (PI: J. Green) for allowing us early access to their data. NR 202 TC 28 Z9 28 U1 0 U2 10 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2013 VL 207 IS 1 AR UNSP 1 DI 10.1088/0067-0049/207/1/1 PG 43 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194KJ UT WOS:000322631500001 ER PT J AU Massaro, F Paggi, A Errando, M D'Abrusco, R Masetti, N Tosti, G Funk, S AF Massaro, F. Paggi, A. Errando, M. D'Abrusco, R. Masetti, N. Tosti, G. Funk, S. TI BL LAC CANDIDATES FOR TeV OBSERVATIONS SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non-thermal; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; DIGITAL SKY SURVEY; GAMMA-RAY SOURCES; LACERTAE OBJECTS; SOURCE CATALOG; DATA RELEASE; 20 CENTIMETERS; RADIO-SOURCES; 1ST SURVEY AB BL Lac objects are the most numerous class of extragalactic TeV-detected sources. One of the biggest difficulties in investigating their TeV emission is due to their limited number, since only 47 BL Lac objects are known to be TeV emitters. In this paper, we propose new criteria to select TeV BL Lac candidates based on infrared and X-ray observations. We apply our selection criteria to the BL Lac objects listed in the ROMA-BZCAT catalog, thereby identifying 41 potential TeV emitters. We then perform a search over a more extended sample combining the ROSAT bright source catalog and the WISE all-sky survey, revealing 54 additional candidates for TeV observations. Our investigation also led to a tentative classification of 16 unidentified X-ray sources as BL Lac candidates. This analysis provides new interesting BL Lac targets for future observations with ground-based Cherenkov telescopes. C1 [Massaro, F.; Funk, S.] SLAC Natl Lab, Menlo Pk, CA 94025 USA. [Massaro, F.; Funk, S.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Paggi, A.; D'Abrusco, R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Errando, M.] Columbia Univ, Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Masetti, N.] INAF Ist Astrofis Spaziale & Fis Cosm Bologna, I-40129 Bologna, Italy. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. RP Massaro, F (reprint author), SLAC Natl Lab, 2575 Sand Hill Rd, Menlo Pk, CA 94025 USA. RI Funk, Stefan/B-7629-2015; D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI Funk, Stefan/0000-0002-2012-0080; D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Errando, Manel/0000-0002-1853-863X; Masetti, Nicola/0000-0001-9487-7740 FU NASA [NNX12AO97G, NNX12AJ30G]; US Virtual Astronomical Observatory; National Science Foundation; National Aeronautics and Space Administration; ASI/INAF [I/005/12/0] FX We thank the anonymous referee for useful comments that improved the presentation of our work. We are grateful to R. Mukherjee for her valuable comments and suggestions that improved the manuscript as well as to S. Digel, P. Giommi, D. Harris, and J. Grindlay for their helpful discussions. The work is supported by NASA grant NNX12AO97G. R. D. gratefully acknowledges the financial support of the US Virtual Astronomical Observatory, which is sponsored by the National Science Foundation and the National Aeronautics and Space Administration. The work by G. T. is supported by ASI/INAF contract I/005/12/0. M. E. acknowledges support from NASA grant NNX12AJ30G. TOPCAT10 (Taylor 2005) was used extensively in this work for the preparation and manipulation of the tabular data and the images. Part of this work is based on archival data, software, or online services provided by the ASI Science Data Center. This research has made use of data obtained from the High Energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA's Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; and the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Part of this work is based on NVSS (NRAO VLA Sky Survey); The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. NR 53 TC 16 Z9 16 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2013 VL 207 IS 1 AR UNSP 16 DI 10.1088/0067-0049/207/1/16 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194KJ UT WOS:000322631500016 ER PT J AU Silverman, JM Nugent, PE Gal-Yam, A Sullivan, M Howell, DA Filippenko, AV Arcavi, I Ben-Ami, S Bloom, JS Cenko, SB Cao, Y Chornock, R Clubb, KI Coil, AL Foley, RJ Graham, ML Griffith, CV Horesh, A Kasliwal, MM Kulkarni, SR Leonard, DC Li, WD Matheson, T Miller, AA Modjaz, M Ofek, EO Pan, YC Perley, DA Poznanski, D Quimby, RM Steele, TN Sternberg, A Xu, D Yaron, O AF Silverman, Jeffrey M. Nugent, Peter E. Gal-Yam, Avishay Sullivan, Mark Howell, D. Andrew Filippenko, Alexei V. Arcavi, Iair Ben-Ami, Sagi Bloom, Joshua S. Cenko, S. Bradley Cao, Yi Chornock, Ryan Clubb, Kelsey I. Coil, Alison L. Foley, Ryan J. Graham, Melissa L. Griffith, Christopher V. Horesh, Assaf Kasliwal, Mansi M. Kulkarni, Shrinivas R. Leonard, Douglas C. Li, Weidong Matheson, Thomas Miller, Adam A. Modjaz, Maryam Ofek, Eran O. Pan, Yen-Chen Perley, Daniel A. Poznanski, Dovi Quimby, Robert M. Steele, Thea N. Sternberg, Assaf Xu, Dong Yaron, Ofer TI TYPE Ia SUPERNOVAE STRONGLY INTERACTING WITH THEIR CIRCUMSTELLAR MEDIUM SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE circumstellar matter; supernovae: general; supernovae: individual (SN 1997cy, SN 1999E, SN 2002ic, SN 2005gj, SN 2008J, SN 2008cg, SN 2011jb, CSS120327:110520-015205, PTF11kx, PTF10htz, PTF10iuf, PTF10yni, PTF11dsb, PTF11hzx, PTF12efc) ID CORE-COLLAPSE SUPERNOVAE; WHITE-DWARF STAR; HOST GALAXY; SN 2011FE; FACTORY OBSERVATIONS; SODIUM-ABSORPTION; II SUPERNOVAE; MASSIVE STAR; PROGENITOR; LUMINOSITY AB Owing to their utility for measurements of cosmic acceleration, Type Ia supernovae (SNe Ia) are perhaps the best-studied class of SNe, yet the progenitor systems of these explosions largely remain a mystery. A rare subclass of SNe Ia shows evidence of strong interaction with their circumstellar medium (CSM), and in particular, a hydrogen-rich CSM; we refer to them as SNe Ia-CSM. In the first systematic search for such systems, we have identified 16 SNe Ia-CSM, and here we present new spectra of 13 of them. Six SNe Ia-CSM have been well studied previously, three were previously known but are analyzed in depth for the first time here, and seven are new discoveries from the Palomar Transient Factory. The spectra of all SNe Ia-CSM are dominated by H alpha emission (with widths of similar to 2000 km s(-1)) and exhibit large H alpha/H beta intensity ratios (perhaps due to collisional excitation of hydrogen via the SN ejecta overtaking slower-moving CSM shells); moreover, they have an almost complete lack of He I emission. They also show possible evidence of dust formation through a decrease in the red wing of H alpha 75-100 days past maximum brightness, and nearly all SNe Ia-CSM exhibit strong Na ID absorption from the host galaxy. The absolute magnitudes (uncorrected for host-galaxy extinction) of SNe Ia-CSM are found to be -21.3 mag <= M-R <= -19 mag, and they also seem to show ultraviolet emission at early times and strong infrared emission at late times (but no detected radio or X-ray emission). Finally, the host galaxies of SNe Ia-CSM are all late-type spirals similar to the Milky Way, or dwarf irregulars like the Large Magellanic Cloud, which implies that these objects come from a relatively young stellar population. This work represents the most detailed analysis of the SN Ia-CSM class to date. C1 [Silverman, Jeffrey M.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Silverman, Jeffrey M.; Filippenko, Alexei V.; Bloom, Joshua S.; Cenko, S. Bradley; Clubb, Kelsey I.; Li, Weidong; Miller, Adam A.; Steele, Thea N.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Nugent, Peter E.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Gal-Yam, Avishay; Arcavi, Iair; Ben-Ami, Sagi; Ofek, Eran O.; Xu, Dong; Yaron, Ofer] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Sullivan, Mark] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Howell, D. Andrew; Graham, Melissa L.] Las Cumbres Observ Global Telescope Network, Goleta, CA 93117 USA. [Howell, D. Andrew; Graham, Melissa L.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Cao, Yi; Horesh, Assaf; Kulkarni, Shrinivas R.] CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA. [Chornock, Ryan; Foley, Ryan J.; Perley, Daniel A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Coil, Alison L.] Univ Calif San Diego, Dept Phys, La Jolla, CA 92093 USA. [Griffith, Christopher V.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Kasliwal, Mansi M.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Leonard, Douglas C.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. [Matheson, Thomas] Natl Optic Astron Observ, Tucson, AZ 85719 USA. [Modjaz, Maryam] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Pan, Yen-Chen] Univ Oxford, Dept Phys Astrophys, Oxford OX1 3RH, England. [Poznanski, Dovi] Tel Aviv Univ, Sch Phys & Astron, Tel Aviv, Israel. [Quimby, Robert M.] Univ Tokyo, Kavli IPMU, Kashiwa, Chiba 2778583, Japan. [Steele, Thea N.] Kutztown Univ Pennsylvania, Dept Comp Sci, Kutztown, PA 19530 USA. [Sternberg, Assaf] Max Planck Inst Astrophys, D-85741 Garching, Germany. RP Silverman, JM (reprint author), Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. EM jsilverman@astro.as.utexas.edu RI Horesh, Assaf/O-9873-2016; OI Horesh, Assaf/0000-0002-5936-1156; Sullivan, Mark/0000-0001-9053-4820 FU W. M. Keck Foundation; NASA; Alfred P. Sloan Foundation; National Science Foundation; U.S. Department of Energy Office of Science; Gary and Cynthia Bengier; Richard and Rhoda Goldman Fund; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-0908886, AST-1211916]; ISF; BSF; GIF; Minerva; FP7/ERC grant; Helen and Martin Kimmel Award for Innovative Investigation FX We thank K. Alatalo, T. Barlow, E. Bellm, B. Cobb, A. Cucchiara, M. Ganeshalingam, Y. Green, M. Hidas, L. Kewley, N. Konidaris, S. Lazarevic, N. Lee, D. Levitan, M. McCourt, K. Mooley, R. Mostardi, D. Perley, A. G. Riess, B. Sesar, R. Street, T. Treu, V. Viscomi, and X. Wang for their assistance with some of the observations and data reduction; B. Dilday, O. Fox, and L. Wang for helpful discussions; and D. Balam, M. Stritzinger, J. Vinko, and J. C. Wheeler for providing unpublished spectra of possible SNe Ia-CSM. We are grateful to the staffs at the Isaac Newton Group of Telescopes and the Lick, Keck, Palomar, and Kitt Peak National Observatories for their support. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration (NASA); the observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community; we are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy Office of Science. The SDSS-III Web site is http://www.sdss3.org/. Supernova research by A.V.F.'s group at UC Berkeley is supported by Gary and Cynthia Bengier, the Richard and Rhoda Goldman Fund, the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grants AST-0908886 and AST-1211916. Work by A.G.-Y. and his group is supported by grants from the ISF, BSF, GIF, Minerva, an FP7/ERC grant, and the Helen and Martin Kimmel Award for Innovative Investigation. M. M. K. acknowledges generous support from a Hubble Fellowship and a Carnegie-Princeton Fellowship. NR 89 TC 58 Z9 58 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0067-0049 J9 ASTROPHYS J SUPPL S JI Astrophys. J. Suppl. Ser. PD JUL PY 2013 VL 207 IS 1 AR UNSP 3 DI 10.1088/0067-0049/207/1/3 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 194KJ UT WOS:000322631500003 ER PT J AU Thomas, RM Ubelaker, DH Byrd, JE AF Thomas, Richard M. Ubelaker, Douglas H. Byrd, John E. TI Tables for the Metric Evaluation of Pair-Matching of Human Skeletal Elements SO JOURNAL OF FORENSIC SCIENCES LA English DT Article DE forensic science; forensic anthropology; pair-matching; osteometric sorting; commingling; bilateral asymmetry ID BILATERAL ASYMMETRY; BONES; LIMB AB A common task in forensic anthropology involves pair-matching of left and right skeletal elements. This can be achieved through visual pair-matching by evaluating similarities in morphology, and through osteometric sorting, a quantitative technique. To simplify the process of osteometric sorting, this article explains the use of a statistic (M), which captures the amount of size variation found between homologous bones from single individuals. A database of skeletal measurements for all major paired postcranial bones is used to calculate values of M from a variety of sources. The maximum value and the 90th and 95th percentiles of M are provided in tabular format, and values of M from forensic cases can be compared to these tables as an objective means for determining whether homologous bones could have originated from the same individual. This simple technique can be combined with visual pair-matching to be particularly effective in cases involving commingling of skeletons. C1 [Thomas, Richard M.] Fed Bur Invest, Trace Evidence Unit, Lab Div, Quantico, VA USA. [Ubelaker, Douglas H.] Natl Museum Nat Hist, Smithsonian Inst, Dept Anthropol, Washington, DC 20560 USA. [Byrd, John E.] Joint POW MIA Accounting Command, Cent Identificat Lab, Hickam Afb, HI USA. RP Thomas, RM (reprint author), FBI Lab, Trace Evidence Unit, 2501 Invest Pkwy, Quantico, VA 22135 USA. EM richard.m.thomas@ic.fbi.gov NR 12 TC 5 Z9 5 U1 0 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-1198 J9 J FORENSIC SCI JI J. Forensic Sci. PD JUL PY 2013 VL 58 IS 4 BP 952 EP 956 DI 10.1111/1556-4029.12133 PG 5 WC Medicine, Legal SC Legal Medicine GA 179BH UT WOS:000321491200016 PM 23682771 ER PT J AU Forshage, M Nordlander, G Buffington, ML AF Forshage, Mattias Nordlander, Goran Buffington, Matthew L. TI EUCOILINAE OF NORTH AMERICA: A REVISED CATALOG OF GENERA AND DESCRIBED SPECIES SO PROCEEDINGS OF THE ENTOMOLOGICAL SOCIETY OF WASHINGTON LA English DT Article DE Tetramerocera; Ganaspis; Bewelda; Aporeucoela; Hexacola; Pentaplastidia; Trybliographa; Figitidae; Cynipoidea ID HYMENOPTERA FIGITIDAE EUCOILINAE; AGROSTOCYNIPS-DIAZ HYMENOPTERA; CYNIPOIDEA; GENUS; FORSTER; BUFFINGTON; PHYLOGENY; CIRCUMSCRIPTION; EVOLUTION AB We present an updated catalog of North American Eucoilinae, bearing little resemblance to previous regional catalogs, which have been lagging behind in the recent systematic work in the group. The current catalog comprises 34 genera, arranged in six tribes. Of these genera, 9 are represented wholly by unidentified or undescribed species in the region, while the other 25 include 108 species recorded from the region. In comparison with previous catalogs, 24 genera and 41 species are added, and 34 species-level names are recombined, while 7 genera, five subgenera and 11 species are removed from the list of North American taxa. A modern, phylogenetically stable and type-based classification is implemented, as well as a tribal classification. In terms of nomenclatural acts, 25 new combinations are made (one is a reinstatement of an old combination); four new genus-levels synonymies are made (Tetramerocera Ashmead junior synonym of Ganaspis Forster, Bewelda Quinlan and Aporeucoela Kieffer junior synonyms of Hexacola Forster, Pentaplastidia Weld junior synonym of Trybliographa Forster); eight new species-level synonymies are made; two species names are removed from synonymy; one new replacement name given (Hexacola pennsylvanicus for Hexacola subaperta Kieffer 1907 nec (Kieffer 1901a)). C1 [Forshage, Mattias] Swedish Museum Nat Hist, Dept Entomol, SE-10405 Stockholm, Sweden. [Nordlander, Goran] Swedish Univ Agr Sci, Dept Ecol, SE-75007 Uppsala, Sweden. [Buffington, Matthew L.] ARS, Systemat Entomol Lab, USDA, Smithsonian Inst,Natl Museum Nat Hist, Washington, DC 20560 USA. RP Forshage, M (reprint author), Swedish Museum Nat Hist, Dept Entomol, Box 50007, SE-10405 Stockholm, Sweden. EM Mattias.Forshage@nrm.se; Goran.Nordlander@slu.se; matt.buffington@ars.usda.gov NR 130 TC 3 Z9 3 U1 0 U2 8 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 2013 VL 115 IS 3 BP 225 EP 255 DI 10.4289/0013-8797.115.3.225 PG 31 WC Entomology SC Entomology GA 194CJ UT WOS:000322608300001 ER PT J AU Tang, SM Sasselov, D Grindlay, J Los, E Servillat, M AF Tang, Sumin Sasselov, Dimitar Grindlay, Jonathan Los, Edward Servillat, Mathieu TI 100-year DASCH Light Curves of Kepler Planet-Candidate Host Stars SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID ATMOSPHERIC CHARACTERIZATION; CHROMOSPHERIC ACTIVITY; HOT JUPITERS; DISCOVERY; FIELD; II. AB We present 100 year light curves of Kepler planet-candidate host stars from the Digital Access to a Sky Century at Harvard (DASCH) project. 261 out of 997 host stars have at least 10 good measurements on DASCH scans of the Harvard plates. 109 of them have at least 100 good measurements, including 70% ( 73 out of 104) of all host stars with g <= 13 mag, and 44% ( 100 out of 228) of all host stars with g <= 14 mag. Our typical photometric uncertainty is similar to 0.1-0.15 mag. No variation is found at 3 sigma level for these host stars, including 21 confirmed or candidate hot Jupiter systems which might be expected to show enhanced flares from magnetic interactions between dwarf primaries and their close and relatively massive planet companions. C1 [Tang, Sumin; Sasselov, Dimitar; Grindlay, Jonathan; Los, Edward; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tang, Sumin] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Tang, Sumin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Servillat, Mathieu] Univ Paris Diderot, CEA Saclay, CNRS, CEA DSM IRFU SAp,Lab AIM, F-91191 Gif Sur Yvette, France. RP Tang, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST0407380, AST0909073]; Cornel and Cynthia K. Sarosdy Fund FX We thank the anonymous referee for suggestions that have helped improve this article. We thank Alison Doane, Jaime Pepper, David Sliski and Robert J. Simcoe at CfA for their work on DASCH, and many volunteers who have helped digitize log-books, clean and scan plates (http://hea-www.harvard.edu/DASCH/team.php). This work was supported in part by NSF grants AST0407380 and AST0909073 and now also the Cornel and Cynthia K. Sarosdy Fund for DASCH. NR 30 TC 1 Z9 1 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 JUL PY 2013 VL 125 IS 929 BP 793 EP 797 DI 10.1086/671759 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 188TT UT WOS:000322217800005 ER PT J AU Tang, SM Grindlay, J Los, E Servillat, M AF Tang, Sumin Grindlay, Jonathan Los, Edward Servillat, Mathieu TI Improved Photometry for the DASCH Pipeline SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Article ID CATALOG; DISCOVERY AB The Digital Access to a Sky Century@Harvard (DASCH) project is digitizing the similar to 500, 000 glass plate images obtained (full sky) by the Harvard College Observatory from 1885 to 1992. Astrometry and photometry for each resolved object are derived with photometric rms values of similar to 0.15 mag for the initial photometry analysis pipeline. Here we describe new developments for DASCH photometry, applied to the Kepler field, that have yielded further improvements, including better identification of image blends and plate defects by measuring image profiles and astrometric deviations. A local calibration procedure using nearby stars in a similar magnitude range as the program star (similar to what has been done for visual photometry from the plates) yields additional improvement for a net photometric rms of similar to 0.1 mag. We also describe statistical measures of light curves that are now used in the DASCH pipeline processing to identify new variables autonomously. The DASCH photometry methods described here are used in the pipeline processing for the data releases of DASCH data, 5 as well as for a forthcoming paper on the long-term variables discovered by DASCH in the Kepler field. C1 [Tang, Sumin; Grindlay, Jonathan; Los, Edward; Servillat, Mathieu] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tang, Sumin] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA. [Tang, Sumin] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. [Servillat, Mathieu] Univ Paris Diderot, Commissariat Energie Atom & Energies Alternat CEA, CNRS, Lab Astrophys Instrumentat & Modelisat CEA DSM IR, F-91191 Gif Sur Yvette, France. RP Tang, SM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NSF [AST0407380, AST0909073]; Cornel and Cynthia K. Sarosdy Fund; Robert Martin Ayers Sciences Fund FX We thank the referee, George Djorgovski, for many helpful comments and suggestions that improved the paper. There are many colleagues who have helped out. In particular we thank our team members Alison Doane, Bob Simcoe, Jaime Pepper, David Sliski, and Silas Laycock for their work on DASCH. We would also like to thank many volunteers who have helped digitize logbooks, clean and scan plates (http://hea-www.harvard.edu/DASCH/team.php). This work was supported in part by NSF grants AST0407380 and AST0909073 and now also the Cornel and Cynthia K. Sarosdy Fund for DASCH. This research has made use of the APASS database, located at the AAVSO Web site. Funding for APASS has been provided by the Robert Martin Ayers Sciences Fund. NR 21 TC 5 Z9 5 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 2013 VL 125 IS 929 BP 857 EP 865 DI 10.1086/671760 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 188TT UT WOS:000322217800010 ER PT J AU Kerr, KCR Dove, CJ AF Kerr, Kevin C. R. Dove, Carla J. TI Delimiting shades of gray: phylogeography of the Northern Fulmar, Fulmarus glacialis SO ECOLOGY AND EVOLUTION LA English DT Article DE Arctic; Atlantic; DNA barcodes; MC1R; Pacific; polymorphism ID DNA BARCODES; MELANOCORTIN-1 RECEPTOR; SEQUENCE VARIATION; PLUMAGE COLOR; GEOGRAPHICAL VARIATION; PHYLOGENETIC ANALYSES; SPECIES RECOGNITION; GENETIC-STRUCTURE; NATURAL-HISTORY; LIFE-HISTORY AB The Northern Fulmar (Fulmarus glacialis) is a common tube-nosed seabird with a disjunct Holarctic range. Taxonomic divisions within the Northern Fulmar have historically been muddled by geographical variation notably including highly polymorphic plumage. Recent molecular analyses (i.e., DNA barcoding) have suggested that genetic divergence between Atlantic and Pacific populations could be on par with those typically observed between species. We employ a multigene phylogenetic analysis to better explore the level of genetic divergence between these populations and to test an old hypothesis on the origin of the modern distribution of color morphs across their range. Additionally, we test whether mutations in the melanocortin-1 receptor gene (MC1R) are associated with dark plumage in the Northern Fulmar. We confirmed that mitochondrial lineages in the Atlantic and Pacific populations are highly divergent, but nuclear markers revealed incomplete lineage sorting. Genetic divergence between these populations is consistent with that observed between many species of Procellariiformes and we recommend elevating these two forms to separate species. We also find that MC1R variation is not associated with color morph but rather is better explained by geographical divergence. C1 [Kerr, Kevin C. R.; Dove, Carla J.] Smithsonian Inst, Natl Museum Nat Hist, Div Birds, Washington, DC 20560 USA. RP Kerr, KCR (reprint author), Royal Ontario Museum, Dept Nat Hist, 100 Queens Pk, Toronto, ON M5S 2C6, Canada. EM kevink@rom.on.ca FU Smithsonian post-doctoral fellowship FX Funding was provided through a Smithsonian post-doctoral fellowship NR 97 TC 7 Z9 8 U1 1 U2 25 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 2045-7758 J9 ECOL EVOL JI Ecol. Evol. PD JUL PY 2013 VL 3 IS 7 BP 1915 EP 1915 DI 10.1002/ece3.597 PG 1 WC Ecology; Evolutionary Biology SC Environmental Sciences & Ecology; Evolutionary Biology GA 185WY UT WOS:000322002400008 PM 23919139 ER PT J AU Hayek, LAC Buzas, MA AF Hayek, Lee-Ann C. Buzas, Martin A. TI ON THE PROPER AND EFFICIENT USE OF DIVERSITY MEASURES WITH INDIVIDUAL FIELD SAMPLES SO JOURNAL OF FORAMINIFERAL RESEARCH LA English DT Article ID BENTHIC FORAMINIFERAL ASSEMBLAGES; PLANKTONIC-FORAMINIFERA; BENTHONIC FORAMINIFERA; SPECIES DIVERSITY; NORTH-ATLANTIC; NEW-ZEALAND; DEEP-SEA; BAY; ENVIRONMENTS; COMMUNITIES AB It is common to find that authors use more than one diversity measure in published research without providing interpretation or explanation. We use a survey of the last three years of articles published in this journal along with a classic data set of Parker from the Gulf of Mexico to show that the familiar practice of citing multiple indices, e.g., Shannon's and Simpson's diversity indices and/or Fisher's alpha, each calculated for the same samples, is redundant and singularly uninformative. In addition, authors often register surprise at the performance of indices when describing diversity over gradients such as depth or time. We show that there is no requirement that the values of the indices be concordant over any gradient and the behavior of a measure can be mathematically determined by the distribution of the observed species. The measures we found to be the most common in current use were S, alpha, H, lambda, and max p(i). The mathematical equivalence of measures is shown through simple plots and description and a standard set of non-redundant measures on a log scale, lnS, H, and ln (1/ max p(i)) is recommended. Use of standardized analytical approaches to the study of problems of change in biodiversity removes limitations on the potential for inference concerning local as well as regional and global scales. C1 [Hayek, Lee-Ann C.; Buzas, Martin A.] Smithsonian Inst, NMNH MRC 121, Washington, DC 20013 USA. RP Hayek, LAC (reprint author), Smithsonian Inst, NMNH MRC 121, POB 7012, Washington, DC 20013 USA. EM hayekl@si.edu NR 46 TC 11 Z9 11 U1 0 U2 19 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 2013 VL 43 IS 3 BP 305 EP 313 PG 9 WC Paleontology SC Paleontology GA 186ON UT WOS:000322054100008 ER PT J AU Turner, BL Yavitt, JB Harms, KE Garcia, MN Romero, TE Wright, SJ AF Turner, Benjamin L. Yavitt, Joseph B. Harms, Kyle E. Garcia, Milton N. Romero, Tania E. Wright, S. Joseph TI Seasonal Changes and Treatment Effects on Soil Inorganic Nutrients Following a Decade of Fertilizer Addition in a Lowland Tropical Forest SO SOIL SCIENCE SOCIETY OF AMERICA JOURNAL LA English DT Article ID RAIN-FOREST; MICROBIAL BIOMASS; MOIST FOREST; PHOSPHORUS AVAILABILITY; LITTER DECOMPOSITION; NITROGEN-FIXATION; LEAF-LITTER; DYNAMICS; TREE; PANAMA AB We conducted monthly measurements of extractable soil nutrients, including N, P, base cations, and micronutrients, as well as the potential toxin Al, in a long-term fertilization experiment in lowland tropical rain forest in the Republic of Panama. Our prediction was that the response of individual nutrients to seasonal climate and fertilizer addition would vary depending on the nature of their biogeochemical cycles. We detected significant seasonal variation in soil pH and all nutrients measured, although only extractable K concentrations were greater in the early wet season, while extractable phosphate varied little in plots that did not receive P addition. A decade of N addition increased soil nitrate, had no effect on extractable ammonium, and decreased soil pH (similar to 0.8 units in plots receiving only N). The decline in pH caused a corresponding decline in extractable base cations (Ca and K) and increased extractable Al, highlighting an important but poorly understood consequence of long-term atmospheric N deposition onto tropical forests. A decade of P addition increased extractable phosphate by 50-fold, indicating that chronic fertilizer addition has overcome the high phosphate sorption capacity of the soil. Potassium addition without N increased extractable soil K by 91%, but only by 25% when K was added in combination with N, suggesting that the previously reported N x K interactive effect on trunk growth rates could be a true response to N addition. Extractable Cu and Zn were increased twofold by micronutrient fertilizer addition, were reduced in the dry season, but were not affected by N addition (i.e., soil acidification). We conclude that the response of extractable nutrients to seasonal climate and fertilizer addition varies among nutrients, and suggest that greater attention be paid to the biological implications of acidification in response to long-term atmospheric N deposition onto strongly-weathered tropical forest soils. C1 [Turner, Benjamin L.; Harms, Kyle E.; Garcia, Milton N.; Romero, Tania E.; Wright, S. Joseph] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Yavitt, Joseph B.] Cornell Univ, Dept Nat Resources, Ithaca, NY 14853 USA. [Harms, Kyle E.] Louisiana State Univ, Dept Biol Sci, Baton Rouge, LA 70803 USA. RP Turner, BL (reprint author), Smithsonian Trop Res Inst, Apartado 0843-03092, Balboa, Ancon, Panama. EM TurnerBL@si.edu RI Turner, Benjamin/E-5940-2011; Wright, Stuart/M-3311-2013 OI Turner, Benjamin/0000-0002-6585-0722; Wright, Stuart/0000-0003-4260-5676 NR 73 TC 19 Z9 19 U1 1 U2 93 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 2013 VL 77 IS 4 BP 1357 EP 1369 DI 10.2136/sssaj2012.0128 PG 13 WC Soil Science SC Agriculture GA 186YZ UT WOS:000322083200023 ER PT J AU Ackermann, M Ajello, M Albert, A Allafort, A Antolini, E Baldini, L Ballet, J Barbiellini, G Bastieri, D Bechtol, K Bellazzini, R Blandford, RD Bloom, ED Bonamente, E Bottacini, E Bouvier, A Brandt, TJ Bregeon, J Brigida, M Bruel, P Buehler, R Buson, S Caliandro, GA Cameron, RA Caraveo, PA Cavazzuti, E Cecchi, C Charles, E Chekhtman, A Cheung, CC Chiang, J Chiaro, G Ciprini, S Claus, R Cohen-Tanugi, J Conrad, J Cutini, S Dalton, M D'Ammando, F de Angelis, A de Palma, F Dermer, CD Di Venere, L Drell, PS Drlica-Wagner, A Favuzzi, C Fegan, SJ Ferrara, EC Focke, WB Franckowiak, A Fukazawa, Y Funk, S Fusco, P Gargano, F Gasparrini, D Germani, S Giglietto, N Giordano, F Giroletti, M Glanzman, T Godfrey, G Grenier, IA Grondin, MH Grove, JE Guiriec, S Hadasch, D Hanabata, Y Harding, AK Hayashida, M Hays, E Hewitt, J Hill, AB Horan, D Hou, X Hughes, RE Inoue, Y Jackson, MS Jogler, T Johannesson, G Johnson, WN Kamae, T Kataoka, J Kawano, T Knoedlseder, J Kuss, M Lande, J Larsson, S Latronico, L Lemoine-Goumard, M Longo, F Loparco, F Lott, B Lovellette, MN Lubrano, P Mayer, M Mazziotta, MN McEnery, JE Michelson, PF Mitthumsiri, W Mizuno, T Monte, C Monzani, ME Morselli, A Moskalenko, IV Murgia, S Nemmen, R Nuss, E Ohsugi, T Okumura, A Omodei, N Orienti, M Orlando, E Ormes, JF Paneque, D Panetta, JH Perkins, JS Pesce-Rollins, M Piron, F Pivato, G Porter, TA Raino, S Rando, R Razzano, M Reimer, A Reimer, O Romoli, C Roth, M Sanchez-Conde, M Scargle, JD Schulz, A Sgro, C Siskind, EJ Spandre, G Spinelli, P Suson, DJ Takahashi, H Takeuchi, Y Thayer, JG Thayer, JB Thompson, DJ Tibaldo, L Tinivella, M Torres, DF Tosti, G Troja, E Tronconi, V Usher, TL Vandenbroucke, J Vasileiou, V Vianello, G Vitale, V Winer, BL Wood, KS Wood, M Yang, Z AF Ackermann, M. Ajello, M. Albert, A. Allafort, A. Antolini, E. Baldini, L. Ballet, J. Barbiellini, G. Bastieri, D. Bechtol, K. Bellazzini, R. Blandford, R. D. Bloom, E. D. Bonamente, E. Bottacini, E. Bouvier, A. Brandt, T. J. Bregeon, J. Brigida, M. Bruel, P. Buehler, R. Buson, S. Caliandro, G. A. Cameron, R. A. Caraveo, P. A. Cavazzuti, E. Cecchi, C. Charles, E. Chekhtman, A. Cheung, C. C. Chiang, J. Chiaro, G. Ciprini, S. Claus, R. Cohen-Tanugi, J. Conrad, J. Cutini, S. Dalton, M. D'Ammando, F. de Angelis, A. de Palma, F. Dermer, C. D. Di Venere, L. Drell, P. S. Drlica-Wagner, A. Favuzzi, C. Fegan, S. J. Ferrara, E. C. Focke, W. B. Franckowiak, A. Fukazawa, Y. Funk, S. Fusco, P. Gargano, F. Gasparrini, D. Germani, S. Giglietto, N. Giordano, F. Giroletti, M. Glanzman, T. Godfrey, G. Grenier, I. A. Grondin, M-H. Grove, J. E. Guiriec, S. Hadasch, D. Hanabata, Y. Harding, A. K. Hayashida, M. Hays, E. Hewitt, J. Hill, A. B. Horan, D. Hou, X. Hughes, R. E. Inoue, Y. Jackson, M. S. Jogler, T. Johannesson, G. Johnson, W. N. Kamae, T. Kataoka, J. Kawano, T. Knoedlseder, J. Kuss, M. Lande, J. Larsson, S. Latronico, L. Lemoine-Goumard, M. Longo, F. Loparco, F. Lott, B. Lovellette, M. N. Lubrano, P. Mayer, M. Mazziotta, M. N. McEnery, J. E. Michelson, P. F. Mitthumsiri, W. Mizuno, T. Monte, C. Monzani, M. E. Morselli, A. Moskalenko, I. V. Murgia, S. Nemmen, R. Nuss, E. Ohsugi, T. Okumura, A. Omodei, N. Orienti, M. Orlando, E. Ormes, J. F. Paneque, D. Panetta, J. H. Perkins, J. S. Pesce-Rollins, M. Piron, F. Pivato, G. Porter, T. A. Raino, S. Rando, R. Razzano, M. Reimer, A. Reimer, O. Romoli, C. Roth, M. Sanchez-Conde, M. Scargle, J. D. Schulz, A. Sgro, C. Siskind, E. J. Spandre, G. Spinelli, P. Suson, D. J. Takahashi, H. Takeuchi, Y. Thayer, J. G. Thayer, J. B. Thompson, D. J. Tibaldo, L. Tinivella, M. Torres, D. F. Tosti, G. Troja, E. Tronconi, V. Usher, T. L. Vandenbroucke, J. Vasileiou, V. Vianello, G. Vitale, V. Winer, B. L. Wood, K. S. Wood, M. Yang, Z. TI THE FERMI ALL-SKY VARIABILITY ANALYSIS: A LIST OF FLARING GAMMA-RAY SOURCES AND THE SEARCH FOR TRANSIENTS IN OUR GALAXY SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: general; BL Lacertae objects: general; catalogs; galaxies: active; stars: flare; surveys ID LARGE-AREA TELESCOPE; ACTIVE GALACTIC NUCLEI; ETA-CARINAE; CRAB-NEBULA; SOURCE CATALOG; LS 5039; EMISSION; BINARY; DISCOVERY; HESS AB In this paper, we present the Fermi All-sky Variability Analysis (FAVA), a tool to systematically study the variability of the gamma-ray sky measured by the Large Area Telescope on board the Fermi Gamma-ray Space Telescope. For each direction on the sky, FAVA compares the number of gamma-rays observed in a given time window to the number of gamma-rays expected for the average emission detected from that direction. This method is used in weekly time intervals to derive a list of 215 flaring gamma-ray sources. We proceed to discuss the 27 sources found at Galactic latitudes smaller than 10 degrees and show that, despite their low latitudes, most of them are likely of extragalactic origin. C1 [Ackermann, M.; Buehler, R.; Mayer, M.; Schulz, A.] Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. [Ajello, M.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Albert, A.; Hughes, R. E.; Winer, B. L.] Ohio State Univ, Dept Phys, Ctr Cosmol & Astro Particle Phys, Columbus, OH 43210 USA. [Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Dept Phys, Stanford, CA 94305 USA. [Allafort, A.; Bechtol, K.; Blandford, R. D.; Bloom, E. D.; Bottacini, E.; Cameron, R. A.; Charles, E.; Chiang, J.; Claus, R.; Di Venere, L.; Drell, P. S.; Drlica-Wagner, A.; Focke, W. B.; Franckowiak, A.; Funk, S.; Glanzman, T.; Godfrey, G.; Hayashida, M.; Hill, A. B.; Inoue, Y.; Jogler, T.; Kamae, T.; Lande, J.; Michelson, P. F.; Mitthumsiri, W.; Monzani, M. E.; Moskalenko, I. V.; Murgia, S.; Okumura, A.; Omodei, N.; Orlando, E.; Paneque, D.; Panetta, J. H.; Porter, T. A.; Reimer, A.; Reimer, O.; Sanchez-Conde, M.; Thayer, J. G.; Thayer, J. B.; Tibaldo, L.; Usher, T. L.; Vandenbroucke, J.; Vianello, G.; Wood, M.] Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA. [Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Antolini, E.; Bonamente, E.; Cecchi, C.; Germani, S.; Lubrano, P.; Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. [Baldini, L.] Univ Pisa, I-56127 Pisa, Italy. [Baldini, L.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Ballet, J.; Grenier, I. A.] Univ Paris Diderot, Lab AIM, CEA IRFU, CNRS,Serv Astrophys,CEA Saclay, F-91191 Gif Sur Yvette, France. [Barbiellini, G.; Longo, F.] Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy. [Barbiellini, G.; Longo, F.] Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy. [Bastieri, D.; Buson, S.; Rando, R.] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy. [Bastieri, D.; Buson, S.; Chiaro, G.; Pivato, G.; Rando, R.; Romoli, C.; Tronconi, V.] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy. [Bellazzini, R.; Bregeon, J.; Kuss, M.; Pesce-Rollins, M.; Razzano, M.; Sgro, C.; Spandre, G.; Tinivella, M.] Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy. [Bouvier, A.; Razzano, M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Razzano, M.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Giglietto, N.; Giordano, F.; Loparco, F.; Monte, C.; Raino, S.; Spinelli, P.] Politecn Bari, I-70126 Bari, Italy. [Brigida, M.; de Palma, F.; Favuzzi, C.; Fusco, P.; Gargano, F.; Giglietto, N.; Giordano, F.; Loparco, F.; Mazziotta, M. N.; Monte, C.; Raino, S.; Spinelli, P.] Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy. [Bruel, P.; Fegan, S. J.; Horan, D.] Ecole Polytech, CNRS, Lab Leprince Ringuet, IN2P3, F-91128 Palaiseau, France. [Caliandro, G. A.; Hadasch, D.; Torres, D. F.] Inst Ciencies Espai IEEE CSIC, E-08193 Barcelona, Spain. [Caraveo, P. A.] INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy. [Cavazzuti, E.; Ciprini, S.; Cutini, S.; Gasparrini, D.] Agenzia Spaziale Italiana ASI Sci Data Ctr, I-00044 Frascati, Roma, Italy. [Chekhtman, A.] George Mason Univ, Ctr Earth Observing & Space Res, Coll Sci, Fairfax, VA 22030 USA. [Cheung, C. C.; Dermer, C. D.; Grove, J. E.; Johnson, W. N.; Lovellette, M. N.; Wood, K. S.] Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Ciprini, S.; Cutini, S.; Gasparrini, D.] Osserv Astron Roma, Ist Nazl Astrofis, I-00040 Monte Porzio Catone, Roma, Italy. [Cohen-Tanugi, J.; Nuss, E.; Piron, F.; Vasileiou, V.] Univ Montpellier 2, Lab Univers & Particules Montpellier, CNRS IN2P3, Montpellier, France. [Conrad, J.; Larsson, S.; Yang, Z.] Stockholm Univ, Dept Phys, SE-10691 Stockholm, Sweden. [Conrad, J.; Jackson, M. S.; Larsson, S.; Yang, Z.] Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden. [Conrad, J.] Royal Swedish Acad Sci, SE-10405 Stockholm, Sweden. [Dalton, M.; Hou, X.; Lemoine-Goumard, M.; Lott, B.] Univ Bordeaux 1, CNRS IN2p3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France. [D'Ammando, F.; Giroletti, M.; Orienti, M.] INAF Ist Radioastron, I-40129 Bologna, Italy. [de Angelis, A.] Univ Udine, Dipartimento Fis, I-33100 Udine, Italy. [de Angelis, A.] Grp Collegato Udine, Ist Nazl Fis Nucl, I-33100 Udine, Italy. [Fukazawa, Y.; Hanabata, Y.; Kawano, T.; Takahashi, H.] Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan. [Grondin, M-H.; Knoedlseder, J.] IRAP, CNRS, F-31028 Toulouse 4, France. [Grondin, M-H.; Knoedlseder, J.] Univ Toulouse, GAHEC, UPS OMP, IRAP, Toulouse, France. [Hayashida, M.] Kyoto Univ, Grad Sch Sci, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Hill, A. B.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Jackson, M. S.] Royal Inst Technol KTH, Dept Phys, SE-10691 Stockholm, Sweden. [Johannesson, G.] Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland. [Kataoka, J.; Takeuchi, Y.] Waseda Univ, Res Inst Sci & Engn, Shinjuku Ku, Tokyo 1698555, Japan. [Larsson, S.] Stockholm Univ, Dept Astron, SE-10691 Stockholm, Sweden. [Latronico, L.] Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy. [McEnery, J. E.] Univ Maryland, Dept Phys, College Pk, MD 20742 USA. [McEnery, J. E.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Mizuno, T.; Ohsugi, T.] Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan. [Morselli, A.; Vitale, V.] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy. [Okumura, A.] Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan. [Ormes, J. F.] Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA. [Paneque, D.] Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany. [Perkins, J. S.] Univ Maryland Baltimore Cty, Baltimore, MD 21250 USA. [Perkins, J. S.] Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA. [Perkins, J. S.] CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Perkins, J. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria. [Reimer, A.; Reimer, O.] Leopold Franzens Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria. [Scargle, J. D.] Univ Washington, Dept Phys, Seattle, WA 98195 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.] Inst Catalana Recerca & Estudis Avancats ICREA, Barcelona, Spain. [Vianello, G.] CIFS, I-10133 Turin, Italy. [Vitale, V.] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy. [Chekhtman, A.] Naval Res Lab, Washington, DC 20375 USA. [Conrad, J.] Royal Swedish Acad Sci, Stockholm, Sweden. [Troja, E.] NASA, Postdoctoral Program, Washington, DC USA. RP Ackermann, M (reprint author), Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany. EM allafort@stanford.edu; rolf.buehler@desy.de RI Torres, Diego/O-9422-2016; Orlando, E/R-5594-2016; Di Venere, Leonardo/C-7619-2017; Rando, Riccardo/M-7179-2013; Mazziotta, Mario /O-8867-2015; Sgro, Carmelo/K-3395-2016; Hays, Elizabeth/D-3257-2012; Reimer, Olaf/A-3117-2013; Morselli, Aldo/G-6769-2011; Nemmen, Rodrigo/O-6841-2014; Funk, Stefan/B-7629-2015; Johannesson, Gudlaugur/O-8741-2015; Loparco, Francesco/O-8847-2015; Gargano, Fabio/O-8934-2015; giglietto, nicola/I-8951-2012; Moskalenko, Igor/A-1301-2007 OI Pesce-Rollins, Melissa/0000-0003-1790-8018; orienti, monica/0000-0003-4470-7094; Giroletti, Marcello/0000-0002-8657-8852; Gasparrini, Dario/0000-0002-5064-9495; Baldini, Luca/0000-0002-9785-7726; Torres, Diego/0000-0002-1522-9065; Di Venere, Leonardo/0000-0003-0703-824X; Inoue, Yoshiyuki/0000-0002-7272-1136; Giordano, Francesco/0000-0002-8651-2394; De Angelis, Alessandro/0000-0002-3288-2517; Caraveo, Patrizia/0000-0003-2478-8018; Sgro', Carmelo/0000-0001-5676-6214; SPINELLI, Paolo/0000-0001-6688-8864; Rando, Riccardo/0000-0001-6992-818X; Hill, Adam/0000-0003-3470-4834; Bastieri, Denis/0000-0002-6954-8862; Omodei, Nicola/0000-0002-5448-7577; Mazziotta, Mario /0000-0001-9325-4672; Reimer, Olaf/0000-0001-6953-1385; Morselli, Aldo/0000-0002-7704-9553; Funk, Stefan/0000-0002-2012-0080; Johannesson, Gudlaugur/0000-0003-1458-7036; Loparco, Francesco/0000-0002-1173-5673; Gargano, Fabio/0000-0002-5055-6395; giglietto, nicola/0000-0002-9021-2888; Moskalenko, Igor/0000-0001-6141-458X FU Istituto Nazionale di Astrofisica in Italy; Centre National d'Etudes Spatiales in France FX Rolf Buhler acknowledges generous support from the Fermi guest investigator program. 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 47 TC 16 Z9 17 U1 0 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 57 DI 10.1088/0004-637X/771/1/57 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200057 ER PT J AU Faigler, S Tal-Or, L Mazeh, T Latham, DW Buchhave, LA AF Faigler, S. Tal-Or, L. Mazeh, T. Latham, D. W. Buchhave, L. A. TI BEER ANALYSIS OF KEPLER AND CoRoT LIGHT CURVES. I. DISCOVERY OF KEPLER-76b: A HOT JUPITER WITH EVIDENCE FOR SUPERROTATION SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; methods: data analysis; planets and satellites: detection; planets and satellites: individual (KIC 4570949b, Kepler-76b) ID CORALIE ECHELLE SPECTROGRAPH; RADIAL-VELOCITY MEASUREMENTS; PLANETARY TRANSIT SEARCHES; MULTI-ORDER TODCOR; ELLIPSOIDAL VARIATIONS; ECLIPSING BINARIES; SYSTEM HD-41004; Y-2 ISOCHRONES; INPUT CATALOG; DATA RELEASE AB We present the first case in which the BEER algorithm identified a hot Jupiter in the Kepler light curve, and its reality was confirmed by orbital solutions based on follow-up spectroscopy. The companion Kepler-76b was identified by the BEER algorithm, which detected the BEaming (sometimes called Doppler boosting) effect together with the Ellipsoidal and Reflection/emission modulations (BEER), at an orbital period of 1.54 days, suggesting a planetary companion orbiting the 13.3mag F star. Further investigation revealed that this star appeared in the Kepler eclipsing binary catalog with estimated primary and secondary eclipse depths of 5 x 10(-3) and 1 x 10(-4), respectively. Spectroscopic radial velocity follow-up observations with Tillinghast Reflector Echelle Spectrograph and SOPHIE confirmed Kepler-76b as a transiting 2.0 +/- 0.26 M-Jup hot Jupiter. The mass of a transiting planet can be estimated from either the beaming or the ellipsoidal amplitude. The ellipsoidal-based mass estimate of Kepler-76b is consistent with the spectroscopically measured mass while the beaming-based estimate is significantly inflated. We explain this apparent discrepancy as evidence for the superrotation phenomenon, which involves eastward displacement of the hottest atmospheric spot of a tidally locked planet by an equatorial superrotating jet stream. This phenomenon was previously observed only for HD 189733b in the infrared. We show that a phase shift of 10 degrees.3 +/- 2 degrees.0 of the planet reflection/emission modulation, due to superrotation, explains the apparently inflated beaming modulation, resolving the ellipsoidal/ beaming amplitude discrepancy. Kepler-76b is one of very few confirmed planets in the Kepler light curves that show BEER modulations and the first to show superrotation evidence in the Kepler band. Its discovery illustrates for the first time the ability of the BEER algorithm to detect short-period planets and brown dwarfs. C1 [Faigler, S.; Tal-Or, L.; Mazeh, T.] Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel. [Latham, D. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. RP Faigler, S (reprint author), Tel Aviv Univ, Sch Phys & Astron, Raymond & Beverly Sackler Fac Exact Sci, IL-69978 Tel Aviv, Israel. OI Buchhave, Lars A./0000-0003-1605-5666 FU European Research Council under the EU's Seventh Framework Programme (FP7)/ERC [291352]; ISRAEL SCIENCE FOUNDATION [1423/11]; NASA [NAS5-26555, NNX11AB99A]; NASA Office of Space Science [NNX09AF08G]; Smithsonian Astrophysical Observatory, DWL PI; OPTICON network; European Community's Seventh Framework Programme FX We are indebted to Shay Zucker for numerous helpful discussions, and to Ignasi Ribas for discussing the thermal phase shift. We thank the referee Steven Bloemen for his valuable remarks and suggestions, and especially for his comment about the alphabeam calculation. The research leading to these results has received funding from the European Research Council under the EU's Seventh Framework Programme (FP7/(2007-2013)/ERC grant Agreement No. 291352). This research was supported by the ISRAEL SCIENCE FOUNDATION (grant No. 1423/11). We feel deeply indebted to the team of the Kepler mission that enabled us to search and analyze their unprecedentedly accurate photometric data. All the photometric data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. We thank the Kepler mission for partial support of the spectroscopic observations under NASA Cooperative Agreement NNX11AB99A with the Smithsonian Astrophysical Observatory, DWL PI. We are indebted to Andrew H. Szentgyorgyi, who led the TRES project, and to Gabor Furesz for his many contributions to the success of the instrument. We thank Robert P. Stefanik, Perry Berlind, Gilbert A. Esquerdo, and Michael L. Calkins for obtaining the TRES observations, and Allyson Bieryla and Jessica Mink for help with the data analysis. This paper is based in part on observations made at Observatoire de Haute Provence (CNRS), France. We are grateful to the OHP director and team for the allocation of the SOPHIE observing time. We are also thankful for the help of the night assistants that enabled us to obtain the spectra presented here. OHP observations were supported by the OPTICON network. OPTICON has received research funding from the European Community's Seventh Framework Programme. NR 62 TC 24 Z9 24 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 26 DI 10.1088/0004-637X/771/1/26 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200026 ER PT J AU Frebel, A Lunnan, R Casey, AR Norris, JE Wyse, RFG Gilmore, G AF Frebel, Anna Lunnan, Ragnhild Casey, Andrew R. Norris, John E. Wyse, Rosemary F. G. Gilmore, Gerard TI THE 300 km s(-1) STELLAR STREAM NEAR SEGUE 1: INSIGHTS FROM HIGH-RESOLUTION SPECTROSCOPY OF ITS BRIGHTEST STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: halo; Galaxy: kinematics and dynamics; stars: abundances ID METAL-POOR STARS; DWARF SPHEROIDAL GALAXY; MILKY-WAY; CHEMICAL-COMPOSITION; ABUNDANCE PATTERNS; GLOBULAR-CLUSTERS; ORPHAN STREAM; DISK STARS; SKY SURVEY; FIELD AB We present a chemical abundance analysis of 300S(-1), the brightest likely member star of the 300 km s(-1) stream near the faint satellite galaxy Segue 1. From a high-resolution Magellan/MIKE spectrum, we determine a metallicity of [Fe/H] = -1.46 +/- 0.05 +/- 0.23 (random and systematic uncertainties) for star 300S-1, and find an abundance pattern similar to typical halo stars at this metallicity. Comparing our stellar parameters to theoretical isochrones, we estimate a distance of 18 +/- 7 kpc. Both the metallicity and distance estimates are in good agreement with what can be inferred from comparing the Sloan Digital Sky Survey photometric data of the stream stars to globular cluster sequences. While several other structures overlap with the stream in this part of the sky, the combination of kinematic, chemical, and distance information makes it unlikely that these stars are associated with either the Segue 1 galaxy, the Sagittarius Stream, or the Orphan Stream. Streams with halo-like abundance signatures, such as the 300 km s(-1) stream, present another observational piece for understanding the accretion history of the Galactic halo. C1 [Frebel, Anna; Casey, Andrew R.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Lunnan, Ragnhild] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Casey, Andrew R.; Norris, John E.] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Wyse, Rosemary F. G.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Gilmore, Gerard] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Frebel, A (reprint author), MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA. FU Smithsonian Astrophysical Observatory; Australian Research Council Laureate [0992131]; Australian Prime Minister's Endeavour Award Research Fellowship; Australian Research Council [DP063563, DP0984924]; NSF [AST-0908326, CDI-1124403] FX A.F. acknowledges support of an earlier Clay Fellowship administered by the Smithsonian Astrophysical Observatory. A.R.C. acknowledges the financial support through the Australian Research Council Laureate Fellowship 0992131, and from the Australian Prime Minister's Endeavour Award Research Fellowship, which has facilitated his research at MIT. J.E.N. acknowledges support from the Australian Research Council (grants DP063563 and DP0984924) for studies of the Galaxy's most metal-poor stars and ultra-faint satellite systems. R.F.G.W. acknowledges support from NSF grants AST-0908326 and CDI-1124403. NR 49 TC 4 Z9 4 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 JUL 1 PY 2013 VL 771 IS 1 AR 39 DI 10.1088/0004-637X/771/1/39 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200039 ER PT J AU Gunther, HM Wolter, U Robrade, J Wolk, SJ AF Guenther, H. M. Wolter, U. Robrade, J. Wolk, S. J. TI MN Lup: X-RAYS FROM A WEAKLY ACCRETING T TAURI STAR SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: formation; stars: pre-main sequence; X-rays: stars ID YOUNG STELLAR OBJECTS; SPITZER C2D SURVEY; LOW-MASS STARS; EMISSION-LINES; BROWN DWARFS; FAR-ULTRAVIOLET; ATOMIC DATABASE; XMM-NEWTON; DISK; MULTIWAVELENGTH AB Young T Tauri stars (TTS) are surrounded by an accretion disk, which over time disperses due to photoevaporation, accretion, and possibly planet formation. The accretion shock on the central star produces an UV/optical veiling continuum, line emission, and X-ray signatures. As the accretion rate decreases, the impact on the central star must change. In this article we study MN Lup, a young star where no indications of a disk are seen in IR observations. We present XMM-Newton and VLT/UVES observations, some of them taken simultaneously. The X-ray data show that MN Lup is an active star with L-X/L-bol close to the saturation limit. However, we find high densities (n(e) > 3 x 10(10) cm(-3)) in the X-ray grating spectrum. This can be well fitted using an accretion shock model with an accretion rate of 2 x 10(-11) M-circle dot yr(-1). Despite the simple Ha line profile which has a broad component, but no absorption signatures as typically seen on accreting TTS, we find rotational modulation in Ca II K and in photospheric absorption lines. These line profile modulations do not clearly indicate the presence of a localized hot accretion spot on the star. In the Ha line we see a prominence in absorption about 2R* above the stellar surface-the first of its kind on a TTS. MN Lup is also the only TTS where accretion is seen, but no dust disk is detected that could fuel it. We suggest that MN Lup presents a unique and short-lived state in the disk evolution. It may have lost its dust disk only recently and is now accreting the remaining gas at a very low rate. C1 [Guenther, H. M.; Wolk, S. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wolter, U.; Robrade, J.] Univ Hamburg, Hamburger Sternwarte, D-21029 Hamburg, Germany. RP Gunther, HM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM hguenther@cfa.harvard.edu OI Gunther, Hans Moritz/0000-0003-4243-2840; Wolk, Scott/0000-0002-0826-9261 FU ESA Member States; NASA; ESO Telescopes at the La Silla Paranal Observatory [087.V0991(A)]; ESO VLT; National Aeronautics and Space Administration [NNX11AD12G] FX Based on observations made with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, and ESO Telescopes at the La Silla Paranal Observatory under program ID 087.V0991(A).; Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA and the ESO VLT. H. M. G. was supported by the National Aeronautics and Space Administration under Grant no. NNX11AD12G issued through the Astrophysics Data Analysis Program. NR 84 TC 2 Z9 2 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 70 DI 10.1088/0004-637X/771/1/70 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200070 ER PT J AU Lin, YT Brodwin, M Gonzalez, AH Bode, P Eisenhardt, PRM Stanford, SA Vikhlinin, A AF Lin, Yen-Ting Brodwin, Mark Gonzalez, Anthony H. Bode, Paul Eisenhardt, Peter R. M. Stanford, S. A. Vikhlinin, Alexey TI THE STELLAR MASS GROWTH OF BRIGHTEST CLUSTER GALAXIES IN THE IRAC SHALLOW CLUSTER SURVEY SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: clusters: general; galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: luminosity function, mass function ID X-RAY DATA; LUMINOSITY FUNCTION; EVOLUTION; SIMULATIONS; POPULATION; COSMOLOGY; REDSHIFT; SCATTER AB The details of the stellar mass assembly of brightest cluster galaxies (BCGs) remain an unresolved problem in galaxy formation. We have developed a novel approach that allows us to construct a sample of clusters that form an evolutionary sequence, and have applied it to the Spitzer IRAC Shallow Cluster Survey (ISCS) to examine the evolution of BCGs in progenitors of present-day clusters with mass of (2.5-4.5) x 10(14) M-circle dot. We follow the cluster mass growth history extracted from a high resolution cosmological simulation, and then use an empirical method that infers the cluster mass based on the ranking of cluster luminosity to select high-z clusters of appropriate mass from ISCS to be progenitors of the given set of z = 0 clusters. We find that, between z = 1.5 and 0.5, the BCGs have grown in stellar mass by a factor of 2.3, which is well-matched by the predictions from a state-of-the-art semi-analytic model. Below z = 0.5 we see hints of differences in behavior between the model and observation. C1 [Lin, Yen-Ting] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. [Lin, Yen-Ting] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe, Kashiwa, Chiba, Japan. [Brodwin, Mark] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Gonzalez, Anthony H.] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Bode, Paul] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Eisenhardt, Peter R. M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Stanford, S. A.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Stanford, S. A.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Vikhlinin, Alexey] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lin, YT (reprint author), Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan. EM ytl@asiaa.sinica.edu.tw FU National Science Council [NSC 102-2112-M-001-001-MY3]; WPI Research Center Initiative, MEXT, Japan; National Science Foundation [AST-0707731, AST-0908292]; Pittsburgh Supercomputing Center [AST070015]; NASA FX We thank Laurie Shaw and Antonio Vale for constructing the merger trees used in this work. We are grateful to the anonymous referee for a report that improved the paper. Y.T.L. thanks Gabriella De Lucia, David Spergel, and Jerry Ostriker for helpful discussions, and I. H. for constant encouragement. Y.T.L. acknowledges supports from the National Science Council grant NSC 102-2112-M-001-001-MY3, as well as WPI Research Center Initiative, MEXT, Japan, during the course of this work. This work was supported by National Science Foundation grants AST-0707731 and AST-0908292. Computer simulations and analysis were supported by the NSF through resources provided by XSEDE and the Pittsburgh Supercomputing Center, under grant AST070015; computations were also performed at the TIGRESS high performance computer center at Princeton University, which is jointly supported by the Princeton Institute for Computational Science and Engineering and the Princeton University Office of Information Technology. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the JPL/Caltech under a contract with NASA. This publication makes use of data products from WISE, a joint project of UCLA and JPL/Caltech, funded by NASA. The Millennium Simulation databases were constructed as part of the activities of the GAVO. NR 32 TC 30 Z9 30 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 61 DI 10.1088/0004-637X/771/1/61 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200061 ER PT J AU Liu, HB Qiu, KP Zhang, QZ Girart, JM Ho, PTP AF Liu, Hauyu Baobab Qiu, Keping Zhang, Qizhou Girart, Josep M. Ho, Paul T. P. TI GAS KINEMATICS AND THE DRAGGED MAGNETIC FIELD IN THE HIGH-MASS MOLECULAR OUTFLOW SOURCE G192.16-3.84: AN SMA VIEW SO ASTROPHYSICAL JOURNAL LA English DT Article DE evolution; ISM: individual objects (G192.16-3.84); stars: formation ID STAR-FORMING REGIONS; ROTATING-DISK; PROTOSTAR G192.16-3.82; ACCRETION DISK; YOUNG STAR; CORES; IRAS-20126+4104; COLLAPSE; SYSTEM; SAMPLE AB We report Submillimeter Array (SMA) observations of polarized 0.88 mm thermal dust emission and various molecular line transitions toward the early B-type (L* similar to 2 x 10(3) L-circle dot) star-forming region G192.16-3.84 (IRAS 05553+1631). The peak of the continuum Stokes-I emission coincides with a hot rotating disk/envelope (SO2 rotational temperature T-rot(2)SO similar to 84(-13)(+18) K), with a north-south velocity gradient. Joint analysis of the rotation curve traced by HCO+ 4-3 and SO2 19(1,19)-18(0,18) suggests that the dense molecular gas is undergoing a spinning-up rotation, marginally bound by the gravitational force of an enclosed mass M*(+gas+dust) similar to 11.2-25.2 M-circle dot. Perpendicular to the rotational plane, a greater than or similar to 100/cos(i) km s(-1) (i similar to 63 degrees) high velocity molecular jet and a similar to 15-20 km s(-1) expanding biconical cavity were revealed in the CO 3-2 emission. The polarization percentage of the 0.88 mm continuum emission decreases toward the central rotating disk/envelope. The polarization angle in the inner similar to 2 '' (0.015 pc) disk/envelope is perpendicular to the plane of the rotation. The magnetic field lines, which are predominantly in the toroidal direction along the disk plane, are likely to be dragged by the gravitationally accelerated rotation. C1 [Liu, Hauyu Baobab; Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Qiu, Keping] Nanjing Univ, Sch Astron & Space Sci, Nanjing 210093, Jiangsu, Peoples R China. [Zhang, Qizhou; Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Girart, Josep M.] Fac Ciencies, CSIC IEEC, Inst Ciencies Espai, E-08193 Bellaterra, Catalonia, Spain. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. RI Girart, Josep/O-1638-2014; OI Girart, Josep/0000-0002-3829-5591; Zhang, Qizhou/0000-0003-2384-6589 FU Smithsonian Institution; Academia Sinica; Spanish MINECO [AYA2011-30228-C03-02]; Catalan AGAUR [2009SGR1172] FX The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics, and is funded by the Smithsonian Institution and the Academia Sinica (Ho et al. 2004).; The SMA data were taken as part of the Large SMA Dust Polarization Survey (PI: Qizhou Zhang). We acknowledge the supports from the SMA staffs. H. B. L. thanks Vivien H.-R. Chen for useful discussions. J.M.G. is supported by the Spanish MINECO AYA2011-30228-C03-02 and the Catalan AGAUR 2009SGR1172 grants. NR 38 TC 10 Z9 10 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 71 DI 10.1088/0004-637X/771/1/71 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200071 ER PT J AU Martinez-Sykora, J De Pontieu, B Leenaarts, J Pereira, TMD Carlsson, M Hansteen, V Stern, JV Tian, H McIntosh, SW van der Voort, LR AF Martinez-Sykora, Juan De Pontieu, Bart Leenaarts, Jorrit Pereira, Tiago M. D. Carlsson, Mats Hansteen, Viggo Stern, Julie V. Tian, Hui McIntosh, Scott W. van der Voort, Luc Rouppe TI A DETAILED COMPARISON BETWEEN THE OBSERVED AND SYNTHESIZED PROPERTIES OF A SIMULATED TYPE II SPICULE SO ASTROPHYSICAL JOURNAL LA English DT Article DE magnetohydrodynamics (MHD); radiative transfer; Sun: atmosphere; Sun: chromosphere; Sun: corona; Sun: transition region ID HIGH-RESOLUTION OBSERVATIONS; FLUX TUBE EMERGENCE; TRANSITION REGION; SOLAR CORONA; EXTREME-ULTRAVIOLET; ALFVENIC WAVES; MAGNETOHYDRODYNAMIC SIMULATIONS; NONEQUILIBRIUM IONIZATION; NUMERICAL SIMULATIONS; HYDROGEN IONIZATION AB We have performed a three-dimensional radiative MHD simulation of the solar atmosphere. This simulation shows a jet-like feature that shows similarities to the type II spicules observed for the first time with Hinode's Solar Optical Telescope. Rapid blueshifted events (RBEs) on the solar disk are associated with these spicules. Observational results suggest they may contribute significantly in supplying the corona with hot plasma. We perform a detailed comparison of the properties of the simulated jet with those of type II spicules (observed with Hinode) and RBEs (with ground-based instruments). We analyze a wide variety of synthetic emission and absorption lines from the simulations including chromospheric (Ca II 8542 angstrom, Ca II H, and H alpha) to transition region and coronal temperatures (10,000 K to several million K). We compare their synthetic intensities, line profiles, Doppler shifts, line widths, and asymmetries with observations from Hinode/SOT and EIS, SOHO/SUMER, the Swedish 1 m Solar Telescope, and SDO/AIA. Many properties of the synthetic observables resemble the observations, and we describe in detail the physical processes that lead to these observables. Detailed analysis of the synthetic observables provides insight into how observations should be analyzed to derive information about physical variables in such a dynamic event. For example, we find that line-of-sight superposition in the optically thin atmosphere requires the combination of Doppler shifts and spectral line asymmetry to determine the velocity in the jet. In our simulated type II spicule, the lifetime of the asymmetry of the transition region lines is shorter than that of the coronal lines. Other properties differ from the observations, especially in the chromospheric lines. The mass density of the part of the spicule with a chromospheric temperature is too low to produce significant opacity in chromospheric lines. The synthetic Ca II 8542 angstrom and H alpha profiles therefore do not show signal resembling RBEs. These and other discrepancies are described in detail, and we discuss which mechanisms and physical processes may need to be included in the MHD simulations to mimic the thermodynamic processes of the chromosphere and corona, in particular to reproduce type II spicules. C1 [Martinez-Sykora, Juan; De Pontieu, Bart; Pereira, Tiago M. D.; Stern, Julie V.] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, Juan; Leenaarts, Jorrit; Carlsson, Mats; Hansteen, Viggo; van der Voort, Luc Rouppe] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Martinez-Sykora, Juan] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Pereira, Tiago M. D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Tian, Hui] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [McIntosh, Scott W.] Natl Ctr Atmospher Res, High Altitude Observ, Boulder, CO 80307 USA. RP Martinez-Sykora, J (reprint author), Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. EM j.m.sykora@astro.uio.no RI Pereira, Tiago/G-4079-2014; OI Pereira, Tiago/0000-0003-4747-4329; Leenaarts, Jorrit/0000-0003-4936-4211 FU European Research Council under the European Union's Seventh Framework Programme/ERC [291058]; NASA [NNX08AH45G, NNX08BA99G, NNX11AN98G, NNM07AA01C, NNG09FA40C]; NASA Post-doctoral Program at Ames Research Center [NNH06CC03B]; Lockheed-Martin [8100002705]; High End Computing (HEC) division of NASA [s1061]; Research Council of Norway [170935/V30]; Programme for Supercomputing FX The research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 291058. We gratefully acknowledge support by NASA grants NNX08AH45G, NNX08BA99G, NNX11AN98G, NNM07AA01C (Hinode), and NNG09FA40C (IRIS). T.M.D.P.'s research was supported by the NASA Post-doctoral Program at Ames Research Center through Contract No. NNH06CC03B. H.T.'s work at CfA is supported under contract 8100002705 from Lockheed-Martin to SAO. The 3D simulation and synthesis have been run on clusters from the Notur project, and the Pleiades cluster through the computing project s1061 from the High End Computing (HEC) division of NASA. We thankfully acknowledge the computer and super-computer resources of the Research Council of Norway through grant 170935/V30 and through grants of computing time from the Programme for Supercomputing. The Swedish 1 m Solar Telescope is operated by the Institute for Solar Physics of the Royal Swedish Academy of Sciences in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. NR 74 TC 8 Z9 8 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 66 DI 10.1088/0004-637X/771/1/66 PG 25 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200066 ER PT J AU Matsuoka, K Silverman, JD Schramm, M Steinhardt, CL Nagao, T Kartaltepe, J Sanders, DB Treisters, E Hasinger, G Akiyama, M Ohta, K Ueda, Y Bongiorno, A Brandt, WN Brusa, M Capak, P Civano, F Comastri, A Elvis, M Lilly, SJ Mainieri, V Masters, D Mignoli, M Salvato, M Trump, JR Taniguchi, Y Zamorani, G Alexander, DM Schawinski, K AF Matsuoka, K. Silverman, J. D. Schramm, M. Steinhardt, C. L. Nagao, T. Kartaltepe, J. Sanders, D. B. Treisters, E. Hasinger, G. Akiyama, M. Ohta, K. Ueda, Y. Bongiorno, A. Brandt, W. N. Brusa, M. Capak, P. Civano, F. Comastri, A. Elvis, M. Lilly, S. J. Mainieri, V. Masters, D. Mignoli, M. Salvato, M. Trump, J. R. Taniguchi, Y. Zamorani, G. Alexander, D. M. Schawinski, K. TI A COMPARATIVE ANALYSIS OF VIRIAL BLACK HOLE MASS ESTIMATES OF MODERATE-LUMINOSITY ACTIVE GALACTIC NUCLEI USING SUBARU/FMOS SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; galaxies: active; quasars: emission lines ID DEEP FIELD-SOUTH; DIGITAL SKY SURVEY; BROAD-LINE REGION; HIGH-REDSHIFT QUASARS; COSMOS SURVEY. I.; SIMILAR-TO 1.4; EMISSION-LINE; EDDINGTON RATIO; OPTICAL SPECTROSCOPY; SOURCE CATALOGS AB We present an analysis of broad emission lines observed in moderate-luminosity active galactic nuclei (AGNs), typical of those found in X-ray surveys of deep fields, with the goal of testing the validity of single-epoch virial black hole mass estimates. We have acquired near-infrared spectra of AGNs up to z similar to 1.8 in the COSMOS and Extended Chandra Deep Field-South Survey, with the Fiber Multi-Object Spectrograph mounted on the Subaru telescope. These near-infrared spectra provide a significant detection of the broad H alpha line, shown to be a reliable probe of black hole mass at low redshift. Our sample has existing optical spectroscopy that provides a detection of Mg II, typically used for black hole mass estimation at z greater than or similar to 1. We carry out a spectral-line fitting procedure using both H alpha and Mg II to determine the virial velocity of gas in the broad-line region, the continuum luminosity at 3000 angstrom, and the total H alpha line luminosity. With a sample of 43 AGNs spanning a range of two decades in luminosity, we find a tight correlation between the ultraviolet and emission-line luminosity. There is also a close one-to-one relationship between the full width at half-maximum of H alpha and Mg II. Both of these then lead to there being very good agreement between H alpha- and Mg II-based masses over a wide range in black hole mass, i.e., M-BH similar to 10(7-9) M-circle dot. In general, these results demonstrate that local scaling relations, using Mg II or H alpha, are applicable for AGNs at moderate luminosities and up to z similar to 2. C1 [Matsuoka, K.] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Matsuoka, K.; Taniguchi, Y.] Ehime Univ, Res Ctr Space & Cosm Evolut, Matsuyama, Ehime 7908577, Japan. [Silverman, J. D.; Schramm, M.; Steinhardt, C. L.] Univ Tokyo, Todai Inst Adv Study, Kavli Inst Phys & Math Universe Kavli IPMU WPI, Kashiwa, Chiba 2778583, Japan. [Nagao, T.] Kyoto Univ, Hakubi Ctr Adv Res, Sakyo Ku, Kyoto 6068302, Japan. [Nagao, T.; Ohta, K.; Ueda, Y.] Kyoto Univ, Dept Astron, Sakyo Ku, Kyoto 6068502, Japan. [Kartaltepe, J.] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Sanders, D. B.; Hasinger, G.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Treisters, E.] Univ Concepcion, Dept Astron, Concepcion, Chile. [Akiyama, M.] Tohoku Univ, Inst Astron, Aoba Ku, Sendai, Miyagi 9808578, Japan. [Bongiorno, A.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Bongiorno, A.] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy. [Brandt, W. N.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brusa, M.; Salvato, M.] Max Planck Inst Extraterr Phys, D-84571 Garching, Germany. [Brusa, M.] Univ Bologna, Dipartimento Fis & Astron, I-40127 Bologna, Italy. [Brusa, M.; Comastri, A.; Mignoli, M.; Zamorani, G.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Capak, P.] CALTECH, NASA JPL Spitzer Sci Ctr, Pasadena, CA 91125 USA. [Civano, F.; Elvis, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lilly, S. J.; Schawinski, K.] ETH, Inst Astron, CH-8093 Zurich, Switzerland. [Mainieri, V.] European So Observ, D-85748 Garching, Germany. [Masters, D.] Observ Carnegie Inst Sci, Pasadena, CA 91101 USA. [Trump, J. R.] Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. [Trump, J. R.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Alexander, D. M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. RP Matsuoka, K (reprint author), Seoul Natl Univ, Dept Phys & Astron, 599 Gwanak Ro, Seoul 151742, South Korea. EM kenta@astro.snu.ac.kr RI Brandt, William/N-2844-2015; Mignoli, Marco/O-9426-2015; Comastri, Andrea/O-9543-2015; OI Brandt, William/0000-0002-0167-2453; Mignoli, Marco/0000-0002-9087-2835; Comastri, Andrea/0000-0003-3451-9970; Bongiorno, Angela/0000-0002-0101-6624; Schawinski, Kevin/0000-0001-5464-0888; Zamorani, Giovanni/0000-0002-2318-301X; Alexander, David/0000-0002-5896-6313 FU Japan Society for the Promotion of Science (JSPS); JSPS [23654068] FX We thank Kentaro Aoki and Naoyuki Tamura for their invaluable assistance during our Subaru/FMOS observations. K. M. acknowledges financial support from the Japan Society for the Promotion of Science (JSPS). T.N. is financially supported by JSPS (grant No. 23654068). Data analyses were carried out in part on common-use data analysis computer system at the Astronomy Data Center, ADC, of the National Astronomical Observatory of Japan (NAOJ). NR 67 TC 14 Z9 14 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 64 DI 10.1088/0004-637X/771/1/64 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200064 ER PT J AU Patel, B Di Stefano, R Nelson, T Primini, FA Liu, J Scoles, S AF Patel, B. Di Stefano, R. Nelson, T. Primini, F. A. Liu, J. Scoles, S. TI ANALYSIS OF A STATE CHANGING SUPERSOFT X-RAY SOURCE IN M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: individual (M31); X-rays: binaries ID ACCRETING WHITE-DWARFS; HIGH-RESOLUTION CAMERA; LARGE-MAGELLANIC-CLOUD; MASS BLACK-HOLE; POINT SOURCES; CATACLYSMIC VARIABLES; OPTICAL NOVAE; IA SUPERNOVAE; SOFT SOURCES; QUASI-SOFT AB We report on observations of a luminous supersoft X-ray source (SSS) in M31, r1-25, that has exhibited spectral changes to harder X-ray states. We document these spectral changes. In addition, we show that they have important implications for modeling the source. Quasisoft states in a source that has been observed as an SSS represent a newly discovered phenomenon. We show how such state changers could prove to be examples of unusual black hole or neutron star accretors. Future observations of this and other state changers can provide the information needed to determine the nature(s) of these intriguing new sources. C1 [Patel, B.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Di Stefano, R.; Primini, F. A.; Liu, J.; Scoles, S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Nelson, T.] Univ Maryland, Dept Phys, Baltimore, MD 21250 USA. RP Patel, B (reprint author), Rutgers State Univ, Dept Phys & Astron, POB 849, Piscataway, NJ 08854 USA. OI Primini, Francis/0000-0002-6077-0643 FU HST [AR-10948.01-A-0]; Smithsonian Institution IR D award; NSF [AST-0847157] FX We thank the Swift team for approving our ToO request (Target ID: 35336). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, Caltech, under contract with the National Aeronautics and Space Administration. This research was supported by HST Grant AR-10948.01-A-0 and the Smithsonian Institution IR & D award. B. P. is supported at Rutgers University in part by NSF award by AST-0847157. We thank the anonymous referee for comments that have helped to improve the paper. NR 63 TC 0 Z9 0 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 6 DI 10.1088/0004-637X/771/1/6 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200006 ER PT J AU Sironi, L Spitkovsky, A Arons, J AF Sironi, Lorenzo Spitkovsky, Anatoly Arons, Jonathan TI THE MAXIMUM ENERGY OF ACCELERATED PARTICLES IN RELATIVISTIC COLLISIONLESS SHOCKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma-ray burst: general; pulsars: general; radiation mechanisms: non-thermal; shock waves ID GAMMA-RAY BURST; ELECTRON-POSITRON PLASMAS; PULSAR WIND NEBULAE; CRAB-NEBULA; MAGNETIC-FIELD; ELECTROMAGNETIC INSTABILITIES; ASTROPHYSICAL SHOCKS; SUPERNOVA-REMNANTS; FERMI OBSERVATIONS; TERMINATION SHOCK AB The afterglow emission from gamma-ray bursts (GRBs) is usually interpreted as synchrotron radiation from electrons accelerated at the GRB external shock that propagates with relativistic velocities into the magnetized interstellar medium. By means of multi-dimensional particle-in-cell simulations, we investigate the acceleration performance of weakly magnetized relativistic shocks, in the magnetization range 0 less than or similar to sigma less than or similar to 10(-1). The pre-shock magnetic field is orthogonal to the flow, as generically expected for relativistic shocks. We find that relativistic perpendicular shocks propagating in electron-positron plasmas are efficient particle accelerators if the magnetization is sigma less than or similar to 10(-3). For electron-ion plasmas, the transition to efficient acceleration occurs for sigma less than or similar to 3 x 10(-5). Here, the acceleration process proceeds similarly for the two species, since the electrons enter the shock nearly in equipartition with the ions, as a result of strong pre-heating in the self-generated upstream turbulence. In both electron-positron and electron-ion shocks, we find that the maximum energy of the accelerated particles scales in time as epsilon(max) alpha t(1/2). This scaling is shallower than the so-called (and commonly assumed) Bohm limit epsilon(max) alpha t, and it naturally results from the small-scale nature of the Weibel turbulence generated in the shock layer. In magnetized plasmas, the energy of the accelerated particles increases until it reaches a saturation value epsilon(sat)/gamma(0)m(i)c(2) similar to sigma(--1/4), where gamma(0)m(i)c(2) is the mean energy per particle in the upstream bulk flow. Further energization is prevented by the fact that the self-generated turbulence is confined within a finite region of thickness alpha sigma(-1/2) around the shock. Our results can provide physically grounded inputs for models of non-thermal emission from a variety of astrophysical sources, with particular relevance to GRB afterglows. C1 [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spitkovsky, Anatoly] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Arons, Jonathan] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Arons, Jonathan] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Arons, Jonathan] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. RP Sironi, L (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM lsironi@cfa.harvard.edu FU NASA [PF1-120090, NNX12AD01G]; Chandra X-ray Center; Smithsonian Astrophysical Observatory for NASA [NAS803060]; NSF [AST-0807381]; XSEDE [TG-AST120010, TG-AST100035] FX L.S. gratefully thanks D. Giannios and L. Nava for comments that helped to improve the manuscript. We gratefully thank G. Pelletier and I. Plotnikov for fruitful discussions, supported by ISSI. L.S. is supported by NASA through Einstein Post-doctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS803060. A.S. is supported by NSF grant AST-0807381 and NASA grant NNX12AD01G. The simulations were performed on the PICSciE-OIT High Performance Computing Center and Visualization Laboratory at Princeton University, on XSEDE resources under contract Nos. TG-AST120010 and TG-AST100035, and on NASA High-End Computing (HEC) resources through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. NR 72 TC 79 Z9 79 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 54 DI 10.1088/0004-637X/771/1/54 PG 22 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200054 ER PT J AU Tobin, JJ Hartmann, L Chiang, HF Wilner, DJ Looney, LW Loinard, L Calvet, N D'Alessio, P AF Tobin, John J. Hartmann, Lee Chiang, Hsin-Fang Wilner, David J. Looney, Leslie W. Loinard, Laurent Calvet, Nuria D'Alessio, Paola TI MODELING THE RESOLVED DISK AROUND THE CLASS 0 PROTOSTAR L1527 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: individual objects (L1527); protoplanetary disks; stars: formation ID YOUNG STELLAR OBJECTS; SUBMILLIMETER CONTINUUM OBSERVATIONS; SPECTRAL ENERGY-DISTRIBUTIONS; MAGNETIC BRAKING CATASTROPHE; MAIN ACCRETION PHASE; LOW-MASS PROTOSTARS; T-TAURI STARS; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISK; SCATTERED-LIGHT AB We present high-resolution sub/millimeter interferometric imaging of the Class 0 protostar L1527 IRS (IRAS 04368+2557) at lambda = 870 mu m and 3.4 mm from the Submillimeter Array and Combined Array for Research in Millimeter Astronomy. We detect the signature of an edge-on disk surrounding the protostar with an observed diameter of 180 AU in the sub/millimeter images. The mass of the disk is estimated to be 0.007M(circle dot), assuming optically thin, isothermal dust emission. The millimeter spectral index is observed to be quite shallow at all the spatial scales probed: alpha similar to 2, implying a dust opacity spectral index beta similar to 0. We model the emission from the disk and surrounding envelope using Monte Carlo radiative transfer codes, simultaneously fitting the sub/millimeter visibility amplitudes, sub/millimeter images, resolved L' image, spectral energy distribution, and mid-infrared spectrum. The best-fitting model has a disk radius of R = 125 AU, is highly flared (H alpha R-1.3), has a radial density profile rho alpha R-2.5, and has a mass of 0.0075M(circle dot). The scale height at 100 AU is 48 AU, about a factor of two greater than vertical hydrostatic equilibrium. The resolved millimeter observations indicate that disks may grow rapidly throughout the Class 0 phase. The mass and radius of the young disk around L1527 are comparable to disks around pre-main-sequence stars; however, the disk is considerably more vertically extended, possibly due to a combination of lower protostellar mass, infall onto the disk upper layers, and little settling of similar to 1 mu m-sized dust grains. C1 [Tobin, John J.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Hartmann, Lee; Calvet, Nuria] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Chiang, Hsin-Fang; Looney, Leslie W.] Univ Illinois, Dept Astron, Urbana, IL 61801 USA. [Chiang, Hsin-Fang] Univ Hawaii Manoa, Inst Astron, Hilo, HI 96720 USA. [Chiang, Hsin-Fang] Univ Hawaii Manoa, NASA Astrobiol Inst, Hilo, HI 96720 USA. [Wilner, David J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Loinard, Laurent; D'Alessio, Paola] UNAM, Ctr Radioastron & Astrofis, Morelia 58089, Michoacan, Mexico. [Loinard, Laurent] Max Planck Inst Radioastron, D-53121 Bonn, Germany. RP Tobin, JJ (reprint author), Natl Radio Astron Observ, Edgemont Rd, Charlottesville, VA 22903 USA. EM jtobin@nrao.edu FU NASA through Hubble Fellowship [HST-HF-51300.01-A]; Space Telescope Science Institute; Association of Universities for Research in Astronomy, Inc., for NASA [NAS 5-26555]; University of Michigan; National Aeronautics and Space Administration through the NASA Astrobiology Institute [NNA09DA77A]; Laboratory for Astronomical Imaging at the University of Illinois; NSF [AST-07-09206]; PAPIIT-UNAM; DGAPA; UNAM; CONACyT (Mexico); Alexander von Humboldt Stiftung; CARMA FX The authors wish to thank the anonymous referee for comments which improved the manuscript. J.T. acknowledges support provided by NASA through Hubble Fellowship grant HST-HF-51300.01-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. L. H. and J.T. acknowledge partial support from the University of Michigan. H.-F.C. acknowledges support from the National Aeronautics and Space Administration through the NASA Astrobiology Institute under cooperative agreement No. NNA09DA77A issued through the Office of Space Science. L. W. L. and H.-F.C. acknowledge support from the Laboratory for Astronomical Imaging at the University of Illinois and the NSF under grant AST-07-09206. P.D. acknowledges a grant from PAPIIT-UNAM. L.L. acknowledges the support of DGAPA, UNAM, CONACyT (Mexico), and the Alexander von Humboldt Stiftung for financial support. Support for CARMA construction was derived from the states of Illinois, California, and Maryland, the James S. McDonnell Foundation, the Gordon and Betty Moore Foundation, the Kenneth T. and Eileen L. Norris Foundation, the University of Chicago, the Associates of the California Institute of Technology, and the National Science Foundation. Ongoing CARMA development and operations are supported by the National Science Foundation under a cooperative agreement, and by the CARMA partner universities. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. NR 93 TC 32 Z9 32 U1 0 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 48 DI 10.1088/0004-637X/771/1/48 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200048 ER PT J AU Uchida, H Yamaguchi, H Koyama, K AF Uchida, Hiroyuki Yamaguchi, Hiroya Koyama, Katsuji TI ASYMMETRIC EJECTA DISTRIBUTION IN SN 1006 SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances; ISM: individual objects (SN 1006); ISM: supernova remnants; X-rays: ISM ID X-RAY-SPECTRUM; IA SUPERNOVAE; ABSORPTION-LINES; CARBON IGNITION; SN-1006 REMNANT; PROPER MOTIONS; LUPUS REGION; EMISSION; SPECTROSCOPY; EXPLOSION AB We present the results from deep X-ray observations (similar to 400 ks in total) of SN 1006 with Suzaku. The thermal spectrum from the entire supernova remnant (SNR) exhibits prominent emission lines of O, Ne, Mg, Si, S, Ar, Ca, and Fe. The observed abundance pattern in the ejecta components is in good agreement with that predicted by a standard model of Type Ia supernovae (SNe). The spatially resolved analysis reveals that the distribution of the O-burning and incomplete Si-burning products (Si, S, and Ar) is asymmetric, while that of the C-burning products (O, Ne, and Mg) is relatively uniform in the SNR interior. The peak position of the former is clearly shifted by 5' (similar to 3.2 pc at the distance of 2.2 kpc) to the southeast (SE) from the SNR's geometric center. Using the SNR age of similar to 1000 yr, we constrain that the velocity asymmetry (in projection) of the ejecta is similar to 3100 km s(-1). The Fe abundance is also significantly higher in the SE region than in the northwest. Given that the non-uniformity is observed only in the heavier elements (Si through Fe), we argue that SN 1006 originates from an asymmetric explosion, as is expected from recent multidimensional simulations of Type Ia SNe, although we cannot eliminate the possibility that inhomogeneous ambient medium had induced the apparent non-uniformity. Possible evidence for the Cr-K-shell line and line broadening in the Fe-K-shell emission is also found. C1 [Uchida, Hiroyuki; Koyama, Katsuji] Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. [Yamaguchi, Hiroya] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Koyama, Katsuji] Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. RP Uchida, H (reprint author), Kyoto Univ, Grad Sch Sci, Dept Phys, Sakyo Ku, Kitashirakawa Oiwake Cho, Kyoto 6068502, Japan. EM uchida@cr.scphys.kyoto-u.ac.jp RI XRAY, SUZAKU/A-1808-2009 FU Japan Society for the Promotion of Science (JSPS) Research Fellowship for Young Scientists; JSPS KAKENHI [23000004, 24540229]; Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan FX The authors thank Dr. T.G. Tsuru and Dr. M. Nobukawa for carefully reading our manuscript. H.U. is supported by Japan Society for the Promotion of Science (JSPS) Research Fellowship for Young Scientists. K. K. is supported by JSPS KAKENHI grant Nos. 23000004 and 24540229. This work was supported by the Grant-in-Aid for the Global COE Program "The Next Generation of Physics, Spun from Universality and Emergence" from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan. NR 47 TC 11 Z9 11 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 56 DI 10.1088/0004-637X/771/1/56 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200056 ER PT J AU Winebarger, AR Walsh, RW Moore, R De Pontieu, B Hansteen, V Cirtain, J Golub, L Kobayashi, K Korreck, K DeForest, C Weber, M Title, A Kuzin, S AF Winebarger, Amy R. Walsh, Robert W. Moore, Ronald De Pontieu, Bart Hansteen, Viggo Cirtain, Jonathan Golub, Leon Kobayashi, Ken Korreck, Kelly DeForest, Craig Weber, Mark Title, Alan Kuzin, Sergey TI DETECTING NANOFLARE HEATING EVENTS IN SUBARCSECOND INTER-MOSS LOOPS USING Hi-C SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona ID ACTIVE-REGION LOOPS; TRANSITION-REGION; CORONAL-EXPLORER; ATMOSPHERIC LOOP; SOLAR CORONA; TRACE; TEMPERATURE; HINODE; CONSTRAINTS; EVOLUTION AB The High-resolution Coronal Imager (Hi-C) flew aboard a NASA sounding rocket on 2012 July 11 and captured roughly 345 s of high-spatial and temporal resolution images of the solar corona in a narrowband 193 angstrom channel. In this paper, we analyze a set of rapidly evolving loops that appear in an inter-moss region. We select six loops that both appear in and fade out of the Hi-C images during the short flight. From the Hi-C data, we determine the size and lifetimes of the loops and characterize whether these loops appear simultaneously along their length or first appear at one footpoint before appearing at the other. Using co-aligned, co-temporal data from multiple channels of the Atmospheric Imaging Assembly on the Solar Dynamics Observatory, we determine the temperature and density of the loops. We find the loops consist of cool (similar to 10(5) K), dense (similar to 10(10) cm(-3)) plasma. Their required thermal energy and their observed evolution suggest they result from impulsive heating similar in magnitude to nanoflares. Comparisons with advanced numerical simulations indicate that such dense, cold and short-lived loops are a natural consequence of impulsive magnetic energy release by reconnection of braided magnetic field at low heights in the solar atmosphere. C1 [Winebarger, Amy R.; Moore, Ronald; Cirtain, Jonathan] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Walsh, Robert W.] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England. [De Pontieu, Bart; Title, Alan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Hansteen, Viggo] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Golub, Leon; Korreck, Kelly; Weber, Mark] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kobayashi, Ken] Univ Alabama, Ctr Space Plasma & Aeron Res, Huntsville, AL 35805 USA. [DeForest, Craig] Southwest Res Inst, Boulder, CO 80302 USA. [Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. RP Winebarger, AR (reprint author), NASA, George C Marshall Space Flight Ctr, ZP 13, Huntsville, AL 35812 USA. EM amy.r.winebarger@nasa.gov RI Kuzin, Sergey/M-3435-2015 FU NASA FX We acknowledge the High-resolution Coronal Imager instrument grant funded by the NASA's Low Cost Access to Space program. MSFC/NASA led the mission and partners include the Smithsonian Astrophysical Observatory in Cambridge, Massachusetts; Lockheed Martin's Solar Astrophysical Laboratory in Palo Alto, California; the University of Central Lancashire in Lancashire, England; and the Lebedev Physical Institute of the Russian Academy of Sciences in Moscow. NR 37 TC 26 Z9 26 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUL 1 PY 2013 VL 771 IS 1 AR 21 DI 10.1088/0004-637X/771/1/21 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 176AD UT WOS:000321274200021 ER PT J AU Joyce, WG Parham, JF Lyson, TR Warnock, RCM Donoghue, PCJ AF Joyce, Walter G. Parham, James F. Lyson, Tyler R. Warnock, Rachel C. M. Donoghue, Philip C. J. TI A DIVERGENCE DATING ANALYSIS OF TURTLES USING FOSSIL CALIBRATIONS: AN EXAMPLE OF BEST PRACTICES SO JOURNAL OF PALEONTOLOGY LA English DT Article ID SOFT-SHELLED TURTLES; MULTIPLE SEQUENCE ALIGNMENT; HELL CREEK FORMATION; SIDE-NECKED TURTLES; MOLECULAR CLOCK; SANTANA FORMATION; SEA-TURTLE; TIME-ESTIMATION; NORTH-AMERICA; EARLY EOCENE AB Turtles have served as a model system for molecular divergence dating studies using fossil calibrations. However, because some parts of the fossil record of turtles are very well known, divergence age estimates from molecular phylogenies often do not differ greatly from those observed directly from the fossil record alone. Also, the phylogenetic position and age of turtle fossil calibrations used in previous studies have not been adequately justified. We provide the first explicitly justified minimum and soft maximum age constraints on 22 clades of turtles following best practice protocols. Using these data we undertook a Bayesian relaxed molecular clock analysis establishing a timescale for the evolution of crown Testudines that we exploit in attempting to address evolutionary questions that cannot be resolved with fossils alone. Some of these questions, such as whether the turtle crown originated in the Triassic or Jurassic, cannot be resolved by our analysis. However, our results generate novel age-of-origination estimates for clades within crown Testudines. Finally, we compare our fossil calibrations and posterior age estimates to those from other studies, revealing substantial differences in results and interpretation. C1 [Joyce, Walter G.] Univ Tubingen, Inst Geowissensch, D-72076 Tubingen, Germany. [Joyce, Walter G.; Lyson, Tyler R.] Yale Peabody Museum Nat Hist, New Haven, CT 06511 USA. [Parham, James F.] Calif State Univ Fullerton, Dept Geol Sci, John Cooper Archaeol & Paleontol Ctr, Fullerton, CA 92834 USA. [Lyson, Tyler R.] Smithsonian Inst, Dept Vertebrate Zool, Washington, DC 20013 USA. [Lyson, Tyler R.] Marmarth Res Fdn, Marmarth, ND 58643 USA. [Warnock, Rachel C. M.] Natl Evolutionary Synth Ctr, Durham, NC 27705 USA. [Warnock, Rachel C. M.; Donoghue, Philip C. J.] Univ Bristol, Dept Earth Sci, Bristol, Avon, England. RP Joyce, WG (reprint author), Univ Tubingen, Inst Geowissensch, D-72076 Tubingen, Germany. EM walter.joyce@uni-tuebingen.de RI Donoghue, Philip/A-3873-2008; OI Donoghue, Philip/0000-0003-3116-7463 FU University of Tubingen; Biotechnology and Bioscience Research Council; Natural Environment Research Council; National Evolutionary Synthesis Center (NESCent) (National Science Foundation) [EF-0905606] FX We would like to thank D. Brinkman, I. Danilov, M. Everhart, M. Rabi, and I. Werneburg for useful discussions regarding fossil turtles and M. dos Reis and Z. Yang for their insights regarding molecular calibration studies. J. Sterli and C. Brochu provided constructive criticisms that helped improve the quality of the final manuscript. L. Martin and M. Carrano provided generous access to fossils under their care. This study was funded by a grant from the University of Tubingen to WGJ, a Biotechnology and Bioscience Research Council grant to PCJD, a studentship funded by the Natural Environment Research Council to RCMW, and further facilitated by a fossil calibration working group funded by the National Evolutionary Synthesis Center (NESCent) (National Science Foundation no. EF-0905606). NR 251 TC 41 Z9 41 U1 3 U2 38 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0022-3360 EI 1937-2337 J9 J PALEONTOL JI J. Paleontol. PD JUL PY 2013 VL 87 IS 4 BP 612 EP 634 DI 10.1666/12-149 PG 23 WC Paleontology SC Paleontology GA 184HP UT WOS:000321881000006 ER PT J AU Rick, TC Lowery, DL AF Rick, Torben C. Lowery, Darrin L. TI ACCELERATOR MASS SPECTROMETRY C-14 DATING AND THE ANTIQUITY OF SHELL-TEMPERED CERAMICS FROM THE CHESAPEAKE BAY AND MIDDLE ATLANTIC SO AMERICAN ANTIQUITY LA English DT Article ID NORTH-AMERICA; RADIOCARBON; POTTERY AB Ceramics typologies have long been used to build artifact, site, and regional chronologies. Direct accelerator mass spectrometry (AMS) C-14 dating of shell-tempered ceramics offers a promising tool for updating and improving these chronologies. Few studies have C-14 dated shell fragments from shell-tempered pottery, however, and questions remain about potential biases from "old shell," the reservoir effect, and other variables. Forty-five direct AMS C-14 assays on shell-tempered pottery and associated shell, charcoal, and bone from nine archaeological sites in Virginia and Maryland provide a framework to test this method. AMS C-14 assays from one site may have problems with old shell, but most of the calibrated direct and associated age estimates overlap. One of our samples is the oldest securely dated shell-tempered pottery in North America at similar to 1000 cal B.C. Our study demonstrates the promise of AMS C-14 dating shell-tempered pottery for refining ceramic and regional chronologies in coastal and other areas around the world. C1 [Rick, Torben C.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. [Lowery, Darrin L.] Chesapeake Watershed Archaeol Res Fdn, Easton, MD 21601 USA. RP Rick, TC (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Program Human Ecol & Archaeobiol, Washington, DC 20013 USA. EM rickt@si.edu; darrinlowery@yahoo.com NR 31 TC 2 Z9 2 U1 0 U2 12 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 JUL PY 2013 VL 78 IS 3 BP 570 EP 579 PG 10 WC Anthropology; Archaeology SC Anthropology; Archaeology GA 177ZX UT WOS:000321415000009 ER PT J AU Scheidt, SP Lancaster, N AF Scheidt, Stephen P. Lancaster, Nick TI The application of COSI-Corr to determine dune system dynamics in the southern Namib Desert using ASTER data SO EARTH SURFACE PROCESSES AND LANDFORMS LA English DT Article DE aeolian processes; dune migration; remote sensing; COSI-Corr; sand transport; Namib Sand Sea ID GROUND DEFORMATION MEASUREMENTS; SAND SEA; VELOCITIES; TRANSPORT; ACCURACY; IMAGERY; MODELS AB The Coregistration of Optically Sensed Images and Correlation (COSI-Corr) algorithm was used to estimate dune migration and sand flux rates from a series of remotely-sensed optical image pairs. Several areas of barchan and transverse dunes transport sand along definite pathways, feeding the southern part of the Namib Sand Sea from beaches and deflationary basins in the Sperrgebiet. We give a detailed description of the pre- and post-processing routines used for our COSI-Corr analysis, and we evaluate the sub-pixel dune migration results at the dune and dune-field scales. The best set of parameters for the application of the algorithm was systematically derived, resulting in methodological refinements of the cross-correlation windows. The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) sensor aboard the Terra satellite provided the remote sensing imagery. Few comparisons have been made between dune migration measurements using COSI-Corr and other types of change detection analysis, and few dune fields have served as test cases for COSI-Corr. We suggest that analysis and interpretation of COSI-Corr output from ASTER data is more valuable if combined with other image analysis techniques, such as manual digitization of dunes in a geographic information system (GIS), processing of write memory function insertion (WMFI) imagery and multispectral image (MSI) analysis of composition. The dune migrations estimated from COSI-Corr results were validated using GIS and WMFI, and later MSI analysis added an important regional, contextual framework of sand transport pathways. The synthesis of these works lends more confidence to understanding the Namib dune system's dynamics and provides a basis for future comparisons to other dune fields. Copyright (c) 2013 John Wiley & Sons, Ltd. C1 [Scheidt, Stephen P.] Natl Air & Space Museum, Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Lancaster, Nick] Univ Nevada, Desert Res Inst, Div Earth & Ecosyst Sci, Reno, NV 89506 USA. RP Scheidt, SP (reprint author), Natl Air & Space Museum, Smithsonian Inst, Ctr Earth & Planetary Studies, MRC 315, POB 37012, Washington, DC 20013 USA. EM sscheidt77@gmail.com FU NASA EPSCoR [NNX07AT65A] FX This work was supported in part by NASA EPSCoR Award NNX07AT65A to the Nevada System of Higher Education. The authors thank the reviewers for their helpful comments and suggestions to improve the manuscript. NR 42 TC 2 Z9 2 U1 1 U2 19 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0197-9337 J9 EARTH SURF PROC LAND JI Earth Surf. Process. Landf. PD JUL PY 2013 VL 38 IS 9 BP 1004 EP 1019 DI 10.1002/esp.3383 PG 16 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 178HC UT WOS:000321435800009 ER PT J AU Puerta-Pinero, C Muller-Landau, HC Calderon, O Wright, SJ AF Puerta-Pinero, Carolina Muller-Landau, Helene C. Calderon, Osvaldo Joseph Wright, S. TI Seed arrival in tropical forest tree fall gaps SO ECOLOGY LA English DT Article DE animal-dispersed species; Barro Colorado Island; canopy gaps; dispersal syndrome; gap dependence; lianas; Panama; tropical forest; wind-dispersed species ID NEOTROPICAL FORESTS; PHASE REGENERATION; SPECIES-DIVERSITY; UNDERSTORY BIRDS; PIONEER TREES; WET FOREST; DISPERSAL; RECRUITMENT; PATTERNS; LIANAS AB Tree deaths open gaps in closed-canopy forests, which allow light to reach the forest floor and promote seed germination and seedling establishment. Gap dependence of regeneration is an important axis of life history variation among forest plant species, and many studies have evaluated how plant species differ in seedling and sapling performance in gaps. However, relatively little is known about how seed arrival in gaps compares with seed arrival in the understory, even though seed dispersal by wind and animals is expected to be altered in gaps. We documented seed arrival for the first seven years after gap formation in the moist tropical forests of Barro Colorado Island (BCI), Panama, and evaluated how the amount and functional composition of arriving seeds compared with understory sites. On average, in the first three years after gap formation, 72% fewer seeds arrived in gaps than in the understory (207 vs. 740 seedsm(-2)yr(-1)). The reduction in number of arriving seeds fell disproportionately on animal-dispersed species, which suffered an 86% reduction in total seed number, while wind-dispersed species experienced only a 47% reduction, and explosively dispersed species showed increased seed numbers arriving. The increase in explosively dispersed seeds consisted entirely of the seeds of several shrub species, a result consistent with greater in situ seed production by explosively dispersed shrubs that survived gap formation or recruited immediately thereafter. Lianas did relatively better in seed arrival into gaps than did trees, suffering less of a reduction in seed arrival compared with understory sites. This result could in large part be explained by the greater predominance of wind dispersal among lianas: there were no significant differences between lianas and trees when controlling for dispersal syndromes. Our results show that seed arrival in gaps is very different from seed arrival in the understory in both total seeds arriving and functional composition. Differential seed arrival in gaps will help to maintain wind-dispersed, explosively dispersed, and possibly other understory species in the community of plants that regenerate in gaps. C1 [Puerta-Pinero, Carolina; Muller-Landau, Helene C.; Calderon, Osvaldo; Joseph Wright, S.] Smithsonian Trop Res Inst, Panama City, Panama. RP Puerta-Pinero, C (reprint author), Autonomous Univ Barcelona, Ctr Ecol Res & Forestry Applicat, CREAF, E-08193 Barcelona, Spain. EM cpuertapinero@gmail.com RI Puerta Pinero, Carolina/B-3186-2012; Wright, Stuart/M-3311-2013 OI Puerta Pinero, Carolina/0000-0002-0584-7548; Wright, Stuart/0000-0003-4260-5676 FU Fundacion Caja Madrid; Spanish Ministry of Education [EX-2009-0703] FX Rufino Gonzalez helped collect the seed rain data. Jim Dalling and Eugene Schupp improved the manuscript with valuable reviews. Fundacion Caja Madrid and a postdoctoral fellowship from the Spanish Ministry of Education (EX-2009-0703) supported C. Puerta-Pinero. NR 35 TC 10 Z9 10 U1 2 U2 61 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 JUL PY 2013 VL 94 IS 7 BP 1552 EP 1562 DI 10.1890/12-1012.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 180SY UT WOS:000321618400013 PM 23951715 ER PT J AU Altieri, AH Bertness, MD Coverdale, TC Axelman, EE Herrmann, NC Szathmary, PL AF Altieri, Andrew H. Bertness, Mark D. Coverdale, Tyler C. Axelman, Eric E. Herrmann, Nicholas C. Szathmary, P. Lauren TI Feedbacks underlie the resilience of salt marshes and rapid reversal of consumer-driven die-off SO ECOLOGY LA English DT Article DE alternate community state; cordgrass die-off; facilitation; feedback; group benefits; herbivory; human impact; phase shift; resilience; salt marsh recovery; Sesarma reticulatum; Spartina alterniflora ID NEW-ENGLAND; POSITIVE INTERACTIONS; ECOLOGICAL-SYSTEMS; STABLE STATES; GLOBAL CHANGE; ECOSYSTEM; CONSERVATION; RECOVERY; BIODIVERSITY; FACILITATION AB Understanding ecosystem resilience to human impacts is critical for conservation and restoration. The large-scale die-off of New England salt marshes was triggered by overfishing and resulted from decades of runaway crab grazing. In 2009, however, cordgrass began to recover, decreasing die-off approximate to 40% by 2010. We used surveys and experiments to test whether plant-substrate feedbacks underlie marsh resilience. Initially, grazer-generated die-off swept through the cordgrass, creating exposed, stressful peat banks that inhibited plant growth. This desertification cycle broke when banks eroded and peat transitioned into mud with fewer herbivores, less grazing, and lower physical stress. Cordgrass reestablished in these areas through a feedback where it engineered a recovery zone by further ameliorating physical stresses and facilitating additional revegetation. Our results reveal that feedbacks can play a critical role in rapid, reversible ecosystem shifts associated with human impacts, and that the interplay of facilitative and consumer interactions should be incorporated into resilience theory. C1 [Altieri, Andrew H.; Bertness, Mark D.; Coverdale, Tyler C.; Axelman, Eric E.; Herrmann, Nicholas C.; Szathmary, P. Lauren] Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. [Altieri, Andrew H.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Altieri, AH (reprint author), Brown Univ, Dept Ecol & Evolutionary Biol, Providence, RI 02912 USA. EM AltieriA@si.edu OI Coverdale, Tyler/0000-0003-0910-9187 FU NSF FX We thank Dov Sax, Qiang He, Stephanie Yin, and Natividad Chen for their comments on the manuscript, and the NSF Biological Oceanography program for financial support. NR 54 TC 15 Z9 16 U1 8 U2 90 PU ECOLOGICAL SOC AMER PI WASHINGTON PA 1990 M STREET NW, STE 700, WASHINGTON, DC 20036 USA SN 0012-9658 EI 1939-9170 J9 ECOLOGY JI Ecology PD JUL PY 2013 VL 94 IS 7 BP 1647 EP 1657 DI 10.1890/12-1781.1 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 180SY UT WOS:000321618400022 PM 23951724 ER PT J AU McKeon, CS Summers, K AF McKeon, C. Seabird Summers, Kyle TI Predator driven reproductive behavior in a tropical frog SO EVOLUTIONARY ECOLOGY LA English DT Article DE Larval habitat; Life history evolution; Phytotelmata; Predation; Indirect effects ID DART-POISON FROG; COMPLEX LIFE-CYCLES; PARENTAL CARE; EPIPEDOBATES-FEMORALIS; ADAPTIVE SIGNIFICANCE; INTRAGUILD PREDATION; OVIPOSITION BEHAVIOR; MATING STRATEGIES; PATERNAL CARE; CHEMICAL CUES AB Life history trade-offs in reproductive strategy are often invoked as ecological agents of evolutionary change, despite a limited amount of experimental data from the field. The larval deposition strategy of Allobates femoralis was tested in Southeastern Peru using a blocked, fully crossed experimental design. Arrays of four pools were used to test the effects of pool size and the presence of a predatory insect (Belostomatid) on the deposition behavior of A. femoralis. Further experiments investigated the colonization of insect predators into potential larval habitats and interactions between predatory insects. Results suggest that pool size, the presence of predatory aquatic insects, and interactions between predators, influence larval deposition in A. femoralis. Similar ecological interactions may have driven toxic dendrobatids to the use of arboreal phytotelmata and associated derived reproductive strategies. C1 [McKeon, C. Seabird] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. [Summers, Kyle] E Carolina Univ, Dept Biol, Greenville, NC 27858 USA. RP McKeon, CS (reprint author), Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. EM mckeons@si.edu; summersk@ecu.edu FU National Geographic Society [7243-02]; East Carolina University FX The authors would like to express thanks to those who have assisted in the preparation of this manuscript. Nat Seavy, Michael McCoy, Hope Klug, Gustav Paulay, Trip Lamb, Carol Goodwillie and Brian Silliman offered critical reviews. Jan Caldwell and four anonymous reviewers provided critical reviews. This work would not have been possible without funding provided by National Geographic Society (Research Grant 7243-02) and East Carolina University. Support in Peru was generously provided by Pantiacolla Nature Tours, Madre de Dios Explorations, and the Yine Project. NR 58 TC 6 Z9 6 U1 2 U2 31 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 2013 VL 27 IS 4 SI SI BP 725 EP 737 DI 10.1007/s10682-013-9641-3 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 175VX UT WOS:000321262800006 ER PT J AU Richards-Zawacki, CL Yeager, J Bart, HPS AF Richards-Zawacki, Corinne L. Yeager, Justin Bart, Henry P. S. TI No evidence for differential survival or predation between sympatric color morphs of an aposematic poison frog SO EVOLUTIONARY ECOLOGY LA English DT Article DE Color polymorphism; Polytypism; Aposematism; Bocas del Toro; Dendrobates pumilio; Predation; Survival ID DENDROBATES-PUMILIO; MATE-CHOICE; DART FROG; SEXUAL SELECTION; OOPHAGA-PUMILIO; FIDDLER-CRAB; UCA-VOMERIS; SIGNALS; MIMICRY; DIVERGENCE AB Because variation in warning signals slows down the predator education process, aposematic theory predicts that animal warning signals should be monomorphic. Yet, warning color polytypisms are not uncommon in aposematic species. In cases where warning signal variants are separated geographically, adaptation to local predators could explain this variation. However, this cannot explain the persistence of sympatric polymorphisms in aposematic taxa. The strawberry poison frog (Oophaga pumilio) exhibits both allopatric and sympatric warning color variation in and around the Bocas del Toro archipelago of Panama. One explanation that has been proposed for the rapid diversification of O. pumilio coloration in this archipelago is low predation; if island populations have few predators, stabilizing selection would be relaxed opening the door for diversification via selection or genetic drift. Using a combination of mark-recapture and clay model studies, we tested for differences in survival and predation among sympatric red and yellow color morphs of O. pumilio from Bastimentos Island. We found no evidence for differential survival or predation in this population, despite the fact that one morph (red) is more common and widely distributed than the other (yellow). Even in an area of the island where the yellow morph is not found, predator attack rates were similar among morphs. Visual modeling suggests that yellow and red morphs are distinguishable and conspicuous against a variety of backgrounds and by viewers with different visual systems. Our results suggest that general avoidance by predators of red and yellow, both of which are typical warning colors used throughout the animal kingdom, may be contributing to the apparent stability of this polymorphism. C1 [Richards-Zawacki, Corinne L.; Yeager, Justin; Bart, Henry P. S.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Richards-Zawacki, Corinne L.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. RP Richards-Zawacki, CL (reprint author), Tulane Univ, Dept Ecol & Evolutionary Biol, 400 Lindy Boggs Bldg, New Orleans, LA 70118 USA. EM cori@tulane.edu RI Richards-Zawacki, Corinne/F-2731-2011 OI Richards-Zawacki, Corinne/0000-0002-4212-041X FU STRI; National Science Foundation [0801165]; University of California President's office; Tulane Dean's grant FX We thank Narissa Bax, Sebastian Castillo, Ricardo Cossio, Anisha Devar, Deyvis Gonzalez, Eli Hornstein, Danny Lenger, Tom Richards, Becky Richards, Eric Rightley, Tracy Stetzinger, Geoff Zawacki and Amanda Zellmer for help with the mark-recapture study and to Anisha Devar for help with the predation experiment. The STRI provided logistical support for this project and we are particularly grateful to Gabriel Jacome and Plinio Gondola of the Bocas del Toro Field Station. This study was financially supported by short-term fellowships from STRI to CLRZ and JY, postdoctoral fellowships from the National Science Foundation (Award No. 0801165) and the University of California President's office to CLRZ, and a Tulane Dean's grant to HPSB. The Panamanian National Authority for the Environment (ANAM) provided research permission for this study. This work complied with IACUC protocols (University of Michigan No. 09765, Tulane University No. 0832 and STRI No. 2007-17-12-15-07). NR 48 TC 19 Z9 20 U1 5 U2 56 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 2013 VL 27 IS 4 SI SI BP 783 EP 795 DI 10.1007/s10682-013-9636-0 PG 13 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 175VX UT WOS:000321262800010 ER PT J AU Williams, RME Irwin, RP Burr, DM Harrison, T McClelland, P AF Williams, Rebecca M. E. Irwin, Rossman P., III Burr, Devon M. Harrison, Tanya McClelland, Phillip TI Variability in martian sinuous ridge form: Case study of Aeolis Serpens in the Aeolis Dorsa, Mars, and insight from the Mirackina paleoriver, South Australia SO ICARUS LA English DT Article DE Mars, Surface; Geological processes; Earth ID MEDUSAE FOSSAE FORMATION; CHANNEL DIMENSIONS; ICE-SHEET; DEPOSITS; SEDIMENTATION; MELTWATER; DISCHARGE; SYSTEM; REGION; BASIN AB In the largest known population of sinuous ridges on Mars, Aeolis Serpens stands out as the longest (similar to 500 km) feature in Aeolis Dorsa. The formation of this landform, whether from fluvial or glacio-fluvial processes, has been debated in the literature. Here we examine higher-resolution data and use a terrestrial analog (the Mirackina paleoriver, South Australia) to show that both the morphology and contextual evidence for Aeolis Serpens are consistent with development of an inverted fluvial landform from differential erosion of variably cemented deposits. The results of this study demonstrate that the induration mechanism can affect preservation of key characteristics of the paleoriver morphology. For groundwater cemented inverted fluvial landforms, like the Mirackina example, isolated remnants of the paleoriver are preserved because of the temporal and spatial variability of cementation sites. Upon landscape inversion, the result is a landform comprised of aligned mesas and ridges with an undulating longitudinal profile. Recognizing how different induration mechanisms affect preservation of fluvial sediments in denuded regions is relevant to the interpretation of sinuous ridges at other locations on Mars. In particular, double ridge transverse shape may be an instrumental aspect in identifying potential inverted fluvial landforms. There are significant limitations on determining former channel parameters for inverted fluvial landforms that form as a result of variable cementation. Radius of curvature can be accurately determined and an upper-bound constraint for former channel wavelength and width can be made, but it is not possible to reconstruct the paleoslope. Thus, the number of applicable paleohydrologic models is restricted and only first order estimates of flow magnitude can be made. Paleodischarge estimates range between 10(2) and 10(3) m(3)/s for both Aeolis Serpens and the Mirackina paleoriver. Located near the base of the Medusae Fossae Formation (MFF), Aeolis Serpens provides insight into the fluvial environment early in the development of that deposit. When Aeolis Serpens was active, climate conditions must have included at least a period conducive to channelized flow for several hundred kilometers. (C) 2013 Elsevier Inc. All rights reserved. C1 [Williams, Rebecca M. E.] Planetary Sci Inst, Tucson, AZ 85719 USA. [Irwin, Rossman P., III] Smithsonian Inst, Ctr Earth & Planetary Studies, Washington, DC 20013 USA. [Burr, Devon M.] Univ Tennessee, Knoxville, TN 37996 USA. [Harrison, Tanya] Malin Space Sci Syst, San Diego, CA 92121 USA. [McClelland, Phillip] Ultramag Geophys, Mt Hutton, NSW 2280, Australia. RP Williams, RME (reprint author), Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA. EM williams@psi.edu FU National Aeronautics and Space Administration [NNX06AB21G]; Mars Data Analysis Program for investigation of the Aeolis Dorsa sinuous ridge [NNX08AK97G, NNX08BA24G] FX We thank Patrick and Stephanie Williams for generously granting access to portions of the Mirackina paleoriver located on Mount Barry Station, Dr. Cliff Oilier (University of Western Australia) for valuable discussions on silcrete and ferricrete formation, David Shean (University of Washington) for software contributions and discussion of CTX DEM products, Frank Chuang (PSI) for assistance with Landsat and ASTER data for the Mirackina site, and Dr. Alexandra Lefort (University of Tennessee) for discussion of Aeolis Dorsa sinuous ridges. We thank Jim Zimbelman and Edwin Kite for their careful review of this manuscript. This material is based upon work supported by the National Aeronautics and Space Administration through the Mars Fundamental Research Program for investigation of the Mirackina paleoriver (Grant NNX06AB21G, Principal Investigator Williams), and the Mars Data Analysis Program for investigation of the Aeolis Dorsa sinuous ridge (Grant NNX08AK97G, Principal Investigator Williams, and grant NNX08BA24G, Principal Investigator Burr). This is PSI contribution #602. NR 86 TC 12 Z9 12 U1 3 U2 10 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 JUL PY 2013 VL 225 IS 1 BP 308 EP 324 DI 10.1016/j.icarus.2013.03.016 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 174ND UT WOS:000321161800027 ER PT J AU Rodriguez, JJ Fernandez-Triana, JL Smith, MA Janzen, DH Hallwachs, W Erwin, TL Whitfield, JB AF Rodriguez, Josephine J. Fernandez-Triana, Jose L. Smith, M. Alex Janzen, Daniel H. Hallwachs, Winnie Erwin, Terry L. Whitfield, James B. TI Extrapolations from field studies and known faunas converge on dramatically increased estimates of global microgastrine parasitoid wasp species richness (Hymenoptera: Braconidae) SO INSECT CONSERVATION AND DIVERSITY LA English DT Article DE Biodiversity; extrapolation; lepidoptera; microgastrinae; parasitism; parasitoid wasps; species richness ID COSTA-RICA; DIVERSITY; LEPIDOPTERA; INTEGRATION; FORESTS AB 1. We extrapolate a new range of estimates of the species richness of Microgastrinae (Hymenoptera: Braconidae) wasps, a diverse group of small parasitoids that attack caterpillars of Lepidoptera. 2. Our estimates, using an array of focal study faunas to provide reasonable bounds for minimum and maximum values, range from 17000 to 46000+ species. These calculations make use of a geographically relatively constant proportion of the total number of local caterpillar species to species of Microgastrinae, and extend what is known from better studied areas to those less thoroughly studied. 3. This new estimate of species richness for Microgastrinae is 8-20 times that of the approximate to 2000 currently described species, and 2-10 times greater than that of previously published estimates. C1 [Rodriguez, Josephine J.] Univ Calif Santa Barbara, Natl Ctr Ecol Anal & Synth NCEAS, Santa Barbara, CA 93106 USA. [Fernandez-Triana, Jose L.; Smith, M. Alex] Univ Guelph, Dept Integrat Biol, Guelph, ON N1G 2W1, Canada. [Fernandez-Triana, Jose L.; Smith, M. Alex] Univ Guelph, Biodivers Inst Ontario, Guelph, ON N1G 2W1, Canada. [Fernandez-Triana, Jose L.] Canadian Natl Collect Insects, Ottawa, ON, Canada. [Janzen, Daniel H.; Hallwachs, Winnie] Univ Penn, Dept Biol, Philadelphia, PA 19104 USA. [Erwin, Terry L.] Natl Museum Nat Hist, Dept Entomol, Smithsonian Inst, Washington, DC 20560 USA. [Whitfield, James B.] Univ Illinois, Dept Entomol, Urbana, IL 61801 USA. RP Whitfield, JB (reprint author), Univ Illinois, Dept Entomol, 320 Morrill Hall,505 S Goodwin Ave, Urbana, IL 61801 USA. EM jwhitfie@life.illinois.edu RI Smith, M Alex/B-4468-2013; OI Smith, M Alex/0000-0002-8650-2575; Quicke, Donald/0000-0003-4471-6775 FU National Center for Ecological Analysis and Synthesis; U.S. N.S.F. [EF-0553768, DEB 1020510, BSR 9024770, DEB 9306296, 9400829, 9705072, 0072730, 0515699]; University of California, Santa Barbara; State of California; NSF Doctoral Dissertation Enhancement Program [OISE-0809175]; U.S. Department of Agriculture [2009-35302-05250]; Government of Canada through Genome Canada; Ontario Genomics Institute [2008-0GI-ICI-03]; Natural Sciences and Engineering Research Council of Canada (NSERC); Wege Foundation; International Conservation Fund of Canada; Jessie B. Cox Charitable Trust; Blue Moon Fund; Guanacaste Dry Forest Conservation Fund; Area de Conservacion Guanacaste; University of Pennsylvania FX JJR was supported by the National Center for Ecological Analysis and Synthesis, a Center funded by U.S. N.S.F. (Grant #EF-0553768), the University of California, Santa Barbara, and the State of California and NSF Doctoral Dissertation Enhancement Program award OISE-0809175. JBW was supported by U.S. N.S.F. grants DEB 1020510 and U.S. Department of Agriculture grant 2009-35302-05250. JFT and laboratory analyses on sequences generated since 2009 were funded by the Government of Canada through Genome Canada and the Ontario Genomics Institute (2008-0GI-ICI-03). MAS was supported by a Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant. DHJ and WH were supported by U.S. N.S.F. grants BSR 9024770 and DEB 9306296, 9400829, 9705072, 0072730, and 0515699, and grants from the Wege Foundation, International Conservation Fund of Canada, Jessie B. Cox Charitable Trust, Blue Moon Fund, Guanacaste Dry Forest Conservation Fund, Area de Conservacion Guanacaste, and University of Pennsylvania. NR 35 TC 21 Z9 21 U1 2 U2 24 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1752-458X EI 1752-4598 J9 INSECT CONSERV DIVER JI Insect. Conserv. Divers. PD JUL PY 2013 VL 6 IS 4 BP 530 EP 536 DI 10.1111/icad.12003 PG 7 WC Biodiversity Conservation; Entomology SC Biodiversity & Conservation; Entomology GA 179EH UT WOS:000321501800009 ER PT J AU Fabre, AC Cornette, R Slater, G Argot, C Peigne, S Goswami, A Pouydebat, E AF Fabre, A. -C. Cornette, R. Slater, G. Argot, C. Peigne, S. Goswami, A. Pouydebat, E. TI Getting a grip on the evolution of grasping in musteloid carnivorans: a three-dimensional analysis of forelimb shape SO JOURNAL OF EVOLUTIONARY BIOLOGY LA English DT Article DE ecomorphology; geometric morphometrics; grasping; musteloids ID CHIMPANZEES PAN-TROGLODYTES; FUNCTIONAL-MORPHOLOGY; LOCOMOTOR BEHAVIOR; FALSE-THUMB; MOVEMENTS; MANIPULATION; ANATOMY; HAND; PATTERN; DIDELPHIDAE AB The ability to grasp and manipulate is often considered a hallmark of hominins and associated with the evolution of their bipedal locomotion and tool use. Yet, many other mammals use their forelimbs to grasp and manipulate objects. Previous investigations have suggested that grasping may be derived from digging behaviour, arboreal locomotion or hunting behaviour. Here, we test the arboreal origin of grasping and investigate whether an arboreal lifestyle could confer a greater grasping ability in musteloid carnivorans. Moreover, we investigate the morphological adaptations related to grasping and the differences between arboreal species with different grasping abilities. We predict that if grasping is derived from an arboreal lifestyle, then the anatomical specializations of the forelimb for arboreality must be similar to those involved in grasping. We further predict that arboreal species with a well-developed manipulation ability will have articulations that facilitate radio-ulnar rotation. We use ancestral character state reconstructions of lifestyle and grasping ability to understand the evolution of both traits. Finally, we use a surface sliding semi-landmark approach capable of quantifying the articulations in their full complexity. Our results largely confirm our predictions, demonstrating that musteloids with greater grasping skills differ markedly from others in the shape of their forelimb bones. These analyses further suggest that the evolution of an arboreal lifestyle likely preceded the development of enhanced grasping ability. C1 [Fabre, A. -C.; Argot, C.; Peigne, S.] Univ Paris 06, CNRS, Museum Natl Hist Nat, Ctr Rech Paleobiodivers & Paleoenvironm,UMR 7207, Paris, France. [Fabre, A. -C.] Univ Paris Diderot, Paris, France. [Fabre, A. -C.; Goswami, A.] UCL, Dept Genet Evolut & Environm, London, England. [Fabre, A. -C.; Goswami, A.] UCL, Dept Earth Sci, London, England. [Cornette, R.] Museum Natl Hist Nat, CNRS, UMR 7205, F-75005 Paris 5, France. [Slater, G.] Smithsonian Inst NHB MRC 121, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC USA. [Pouydebat, E.] Museum Natl Hist Nat, CNRS, Dept Ecol & Gest Biodivers, UMR 7179, F-75005 Paris 5, France. RP Fabre, AC (reprint author), Museum Natl Hist Nat, Ctr Rech Paleobiodivers & Paleoenvironm, UMR 7207, 8 Rue Buffon,CP 38, F-75005 Paris 5, France. EM acfabre@mnhn.fr RI Pouydebat, Emmanuelle/D-3150-2013; Fabre, Anne-Claire/J-4492-2014 OI Fabre, Anne-Claire/0000-0001-7310-1775 FU UCL IMPACT FX We thank Jacques Cuisin, Geraldine Veron, Julie Villemain, Celine Bens and Tarik for access to specimens from the collections Mammiferes et Oiseaux, MNHN, Paris. We also thank Loic Costeur for allowing us to scan the material from the Naturhistorisches Museum, Basel; Judy Chupasko for allowing us to scan the material from the Harvard Museum of Comparative Zoology, Cambridge, Massachusetts; and Suzanne Peurach for allowing us to scan the material from the Smithsonian National Museum of Natural History, Washington, D. C. We thank the 'plate-forme de morphometrie' of the UMS 2700 (CNRS, MNHN) for access to the surface scanner. ACF thanks the doctoral school FdV, the Fondation Bettencourt-Schueller, and, Andrew Murray and Mary Collins to help her to obtain a UCL IMPACT scholarship for funding. We also thank Andrew Murray, Mary Collins, Anthony Herrel, Livia Bascher, Marcela Randau, Sybile Moulin and Celine Houssin for their helpful discussions and comments on this manuscript. NR 61 TC 21 Z9 22 U1 0 U2 33 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1010-061X J9 J EVOLUTION BIOL JI J. Evol. Biol. PD JUL PY 2013 VL 26 IS 7 BP 1521 EP 1535 DI 10.1111/jeb.12161 PG 15 WC Ecology; Evolutionary Biology; Genetics & Heredity SC Environmental Sciences & Ecology; Evolutionary Biology; Genetics & Heredity GA 185XC UT WOS:000322003000012 PM 23662594 ER PT J AU Shadwick, RE Goldbogen, JA Potvin, J Pyenson, ND Vogl, AW AF Shadwick, Robert E. Goldbogen, Jeremy A. Potvin, Jean Pyenson, Nicholas D. Vogl, A. Wayne TI Novel muscle and connective tissue design enables high extensibility and controls engulfment volume in lunge-feeding rorqual whales SO JOURNAL OF EXPERIMENTAL BIOLOGY LA English DT Article DE ventral groove blubber; collagen; elastin; muscle morphology; Balaenopteridae ID FIN WHALES; SKELETAL-MUSCLE; TERRESTRIAL LOCOMOTION; BALAENOPTERA-PHYSALUS; VENTRAL POUCH; BODY; KINEMATICS; MOUTHFUL; CAPACITY; INCLINE AB Muscle serves a wide variety of mechanical functions during animal feeding and locomotion, but the performance of this tissue is limited by how far it can be extended. In rorqual whales, feeding and locomotion are integrated in a dynamic process called lunge feeding, where an enormous volume of prey-laden water is engulfed into a capacious ventral oropharyngeal cavity that is bounded superficially by skeletal muscle and ventral groove blubber (VGB). The great expansion of the cavity wall presents a mechanical challenge for the physiological limits of skeletal muscle, yet its role is considered fundamental in controlling the flux of water into the mouth. Our analyses of the functional properties and mechanical behaviour of VGB muscles revealed a crimped microstructure in an unstrained, non-feeding state that is arranged in parallel with dense and straight elastin fibres. This allows the muscles to accommodate large tissue deformations of the VGB yet still operate within the known strain limits of vertebrate skeletal muscle. VGB transverse strains in routine-feeding rorquals were substantially less than those observed in dead ones, where decomposition gas stretched the VGB to its elastic limit, evidence supporting the idea that eccentric muscle contraction modulates the rate of expansion and ultimate size of the ventral cavity during engulfment. C1 [Shadwick, Robert E.] Univ British Columbia, Dept Zool, Vancouver, BC V6T 1Z4, Canada. [Goldbogen, Jeremy A.] Cascadia Res Collect, Olympia, WA 98501 USA. [Potvin, Jean] St Louis Univ, Dept Phys, St Louis, MO 63103 USA. [Pyenson, Nicholas D.] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Vogl, A. Wayne] Univ British Columbia, Dept Cellular & Physiol Sci, Vancouver, BC V6T 1Z3, Canada. RP Shadwick, RE (reprint author), Univ British Columbia, Dept Zool, 6270 Univ Blvd, Vancouver, BC V6T 1Z4, Canada. EM shadwick@zoology.ubc.ca OI Goldbogen, Jeremy/0000-0002-4170-7294 FU Natural Sciences and Engineering Research Council (NSERC) of Canada; University of British Columbia; Scripps Institution of Oceanography; NSERC; Smithsonian Institution; Remington Kellogg Fund FX R.E.S. and A. W. V. acknowledge funding from the Natural Sciences and Engineering Research Council (NSERC) of Canada Discovery Grants Program. J.A.G. was supported by a Graduate Fellowship from the University of British Columbia and a Postdoctoral Fellowship from the Scripps Institution of Oceanography. N.D.P. was supported by an NSERC Postdoctoral Research Fellowship, the Smithsonian Institution, and its Remington Kellogg Fund. NR 35 TC 5 Z9 5 U1 1 U2 20 PU COMPANY OF BIOLOGISTS LTD PI CAMBRIDGE PA BIDDER BUILDING CAMBRIDGE COMMERCIAL PARK COWLEY RD, CAMBRIDGE CB4 4DL, CAMBS, ENGLAND SN 0022-0949 J9 J EXP BIOL JI J. Exp. Biol. PD JUL PY 2013 VL 216 IS 14 BP 2691 EP 2701 DI 10.1242/jeb.081752 PG 11 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 172FN UT WOS:000320985500022 PM 23580724 ER PT J AU Hatala, KG Dingwall, HL Wunderlich, RE Richmond, BG AF Hatala, Kevin G. Dingwall, Heather L. Wunderlich, Roshna E. Richmond, Brian G. TI The relationship between plantar pressure and footprint shape SO JOURNAL OF HUMAN EVOLUTION LA English DT Article DE Biomechanics; Foot function; Locomotion; Ileret; Human evolution ID PLIOCENE HOMINID FOOTPRINTS; NORTHERN TANZANIA; HUMAN LOCOMOTION; LAETOLI; FOOT; WALKING; AUSTRALOPITHECUS; PRESERVATION; MORPHOLOGY; MOVEMENTS AB Fossil footprints preserve the only direct evidence of the external foot morphologies and gaits of extinct hominin taxa. However, their interpretation requires an understanding of the complex interaction among foot anatomy, foot function, and soft sediment mechanics. We applied an experimental approach aimed at understanding how one measure of foot function, the distribution of plantar pressure, influences footprint topography. Thirty-eight habitually unshod and minimally shod Daasanach individuals (19 male, 19 female) walked across a pressure pad and produced footprints in sediment directly excavated from the geological layer that preserves 1.5 Ma fossil footprints at Ileret, Kenya. Calibrated pressure data were collected and three-dimensional models of all footprints were produced using photogrammetry. We found significant correlations (Spearman's rank, p < 0.0001) between measurements of plantar pressure distribution and relative footprint depths at ten anatomical regions across the foot. Furthermore, plantar pressure distributions followed a pattern similar to footprint topography, with areas of higher pressure tending to leave deeper impressions. This differs from the results of experimental studies performed in different types of sediment, supporting the hypothesis that sediment type influences the relationship between plantar pressure and footprint topography. Our results also lend support to previous interpretations that the shapes of the Ileret footprints preserve evidence of a medial transfer of plantar pressure during late stance phase, as seen in modern humans. However, the weakness of the correlations indicates that much of the variation in relative depths within footprints is not explained by pressure distributions under the foot when walking on firm ground, using the methods applied here. This warrants caution when interpreting the unique foot anatomies and foot functions of extinct hominins evidenced by their footprint structures. Further research is necessary to clarify how anatomical, functional, and sedimentary variables influence footprint formation and how each can be inferred from footprint morphology. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Hatala, Kevin G.] George Washington Univ, Hominid Paleobiol Doctoral Program, Washington, DC 20052 USA. [Hatala, Kevin G.; Dingwall, Heather L.; Richmond, Brian G.] George Washington Univ, Ctr Adv Study Hominid Paleobiol, Dept Anthropol, Washington, DC 20052 USA. [Dingwall, Heather L.] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Wunderlich, Roshna E.] James Madison Univ, Dept Biol, Harrisonburg, VA 22807 USA. [Richmond, Brian G.] Smithsonian Inst, Human Origins Program, Natl Museum Nat Hist, Washington, DC 20560 USA. RP Hatala, KG (reprint author), George Washington Univ, Hominid Paleobiol Doctoral Program, 2110 G St NW, Washington, DC 20052 USA. EM kevin.g.hatala@gmail.com FU National Science Foundation [BCS-0924476, BCS-1128170, DGE-0801634] FX We thank David Green, David Braun, Jack Harris, Purity Kiura, Emmanuel Ndiema, the Koobi Fora Field School, the National Museums of Kenya, the town of Ileret, Kenya, and our Daasanach subjects for their contributions to this project. We also thank three anonymous reviewers who provided insightful and constructive comments and advice during the preparation of this manuscript. This study was funded by the National Science Foundation, grants BCS-0924476, BCS-1128170, and DGE-0801634. NR 41 TC 7 Z9 7 U1 0 U2 29 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 JUL PY 2013 VL 65 IS 1 BP 21 EP 28 DI 10.1016/j.jhevol.2013.03.009 PG 8 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 179RL UT WOS:000321538900003 PM 23725794 ER PT J AU Meijer, HJM Sutikna, T Saptomo, EW Awe, RD Jatmiko Wasisto, S James, HF Morwood, MJ Tocheri, MW AF Meijer, Hanneke J. M. Sutikna, Thomas Saptomo, E. Wahyu Awe, Rokhus Due Jatmiko Wasisto, Sri James, Helen F. Morwood, Michael J. Tocheri, Matthew W. TI LATE PLEISTOCENE-HOLOCENE NON-PASSERINE AVIFAUNA OF LIANG BUA (FLORES, INDONESIA) SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID HOMO-FLORESIENSIS; HOMININ EVOLUTION; PARROTS AVES; NEW-ZEALAND; BIOGEOGRAPHY; MORPHOLOGY; MIOCENE; FAUNA; PSITTACIFORMES; AFFINITIES AB Liang Bua, a limestone cave on the Indonesian island of Flores, has a depositional sequence that spans the last 95,000years and includes well-preserved faunal remains. Birds are well represented throughout the stratigraphic sequence at Liang Bua. Here, we present the results of the first comprehensive study of avian remains retrieved from Sector XI, a 2m by 2m archaeological excavation along the east wall of the cave. A total of 579 specimens were identified as avian, with 244 belonging to at least 26 non-passerine taxa in 13 families. The late Pleistocene assemblage (23 taxa) includes the first recorded occurrence of vultures in Wallacea, as well as kingfishers, snipes, plovers, parrots, pigeons, and swiftlets. Together, these taxa suggest that during this time the surrounding environment was floristically diverse and included several habitat types. Two of these taxa, the giant marabou Leptoptilos robustus and the vulture Trigonoceps sp., are extinct. Eight taxa were identified in the Holocene assemblage, and five of these were also present in the late Pleistocene. Imperial pigeons Ducula sp. and the Island Collared Dove Streptopelia cf. bitorquata appear only in the Holocene assemblage. The differences in faunal composition between the late Pleistocene and Holocene assemblages may reflect a change in avifaunal composition due to climatic and environmental changes near the Pleistocene-Holocene transition, possibly amplified by impacts associated with the arrival of modern humans; however, the small Holocene sample prevents a firm conclusion about faunal turnover from being made. C1 [Meijer, Hanneke J. M.; James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Div Birds, Washington, DC 20013 USA. [Meijer, Hanneke J. M.] Nat Biodivers Ctr, NL-2333 CR Leiden, Netherlands. [Sutikna, Thomas; Saptomo, E. Wahyu; Awe, Rokhus Due; Jatmiko; Wasisto, Sri] Natl Res & Dev Ctr Archaeol, Jakarta 12510, Indonesia. [Sutikna, Thomas; Morwood, Michael J.] Univ Wollongong, Sch Earth & Environm Sci, GeoQuEST Res Ctr, Wollongong, NSW 2522, Australia. [Tocheri, Matthew W.] Smithsonian Inst, Natl Museum Nat Hist, Dept Anthropol, Human Origins Program, Washington, DC 20013 USA. RP Meijer, HJM (reprint author), Inst Catala Paleontol Miquel Crusafont, Barcelona 08193, Spain. EM hanneke.meijer@icp.cat; thomasutikna@yahoo.com; wahyu_saptomo@yahoo.com; ako_jatmiko90@yahoo.com; sriwasisto@yahoo.com; jamesh@si.edu; mikem@uow.edu.au; tocherim@si.edu RI Meijer, Hanneke/A-1912-2013; OI Meijer, Hanneke/0000-0001-7066-6869; Tocheri, Matthew/0000-0001-7600-8998 FU Netherlands Centre for Biodiversity; Smithsonian Institution Postdoctoral Fellowship Award FX We express our gratitude to T. Djubiantono, former Director of the National Research and Development Centre for Archaeology (ARKENAS), for permission to study the Liang Bua bird material. We thank Z. Zhang and M. Spitzer for their help in identifying the bird material and discussions on fossil storks, vultures, and (insular) fossil avifaunas. We gratefully acknowledge K. M. Helgen for discussion on the bat fauna of Flores; G. F. Mees for discussions on the extant Flores avifauna; M. Schellekens for providing unpublished observations on the extant birds of Flores; C. Stimpson for insightful discussions on Southeast Asian swiftlets and providing unpublished data on swiftlet bone material; and B. Pobiner for examining possible gnaw and cut marks. We greatly appreciate the insightful comments and suggestions made by two anonymous reviewers. This research was supported by the Netherlands Centre for Biodiversity and a Smithsonian Institution Postdoctoral Fellowship Award to H.J.M.M. NR 99 TC 10 Z9 10 U1 0 U2 19 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JUL 1 PY 2013 VL 33 IS 4 BP 877 EP 894 DI 10.1080/02724634.2013.746941 PG 18 WC Paleontology SC Paleontology GA 170XX UT WOS:000320889600012 ER PT J AU Fitzgerald, EMG Velez-Juarbe, J Wells, RT AF Fitzgerald, Erich M. G. Velez-Juarbe, Jorge Wells, Roderick T. TI MIOCENE SEA COW (SIRENIA) FROM PAPUA NEW GUINEA SHEDS LIGHT ON SIRENIAN EVOLUTION IN THE INDO-PACIFIC SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID SOUTHEASTERN AUSTRALIA; CARIBBEAN REGION; FOSSIL SIRENIA; WEST ATLANTIC; MAMMALIA; BASIN; ASIA; DUGONGINAE; VICTORIA; EOCENE AB A partial postcranial skeleton (vertebrae and ribs) of an indeterminate sirenian is described from Selminum Tem cave in the Hindenburg Range, Western Province of Papua New Guinea. It was derived from a section of the Darai Limestone dating to the Burdigalian-Serravallian (early-middle Miocene) and representing shallow platform carbonates. The thoracic vertebrae are remarkably small, being comparable in size to the vertebrae of Nanosiren garciae and implying small body size, although it is uncertain whether the specimen represents a diminutive adult or juvenile individual. These fossils represent the geologically earliest mammal recorded from the island of New Guinea and the earliest evidence of Sirenia in Australasia. Thus, this fossil evidence provides a minimum date (similar to 11.8 Ma) for the earliest presence of sirenians in Australasian coastal marine ecosystems, as well as their primary food source, seagrasses. C1 [Fitzgerald, Erich M. G.] Museum Victoria, Melbourne, Vic 3001, Australia. [Fitzgerald, Erich M. G.; Velez-Juarbe, Jorge] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Velez-Juarbe, Jorge] Howard Univ, Coll Med, Dept Anat, Washington, DC 20059 USA. [Wells, Roderick T.] Flinders Univ S Australia, Sch Biol Sci, Adelaide, SA 5001, Australia. RP Fitzgerald, EMG (reprint author), Museum Victoria, GPO Box 666, Melbourne, Vic 3001, Australia. EM efitzgerald@museum.vic.gov.au; velezjuarbe@gmail.com; rod.wells@flinders.edu.au FU Smithsonian Postdoctoral Fellowship; Harold Mitchell Foundation; Museum Victoria; WBHR Louis Stokes Alliance for Minority Participation Bridge to the Doctorate Program at Howard University; National Museum of Natural History; NSF Earth Sciences grant [0929117] FX We thank M.-A. Binnie (South Australian Museum), D. Bohaska (National Museum of Natural History), and G. Mosuwadoga (National Museum and Art Gallery of Papua New Guinea) for access to collections; and two referees for comments on the manuscript. This work was initiated during a Smithsonian Postdoctoral Fellowship awarded to E.M.G.F., and continued with support from the Harold Mitchell Foundation and Museum Victoria. E.M.G.F. thanks the South Australian Museum for facilitating research on its collections. J.V.G.'s contribution was partially supported by WBHR Louis Stokes Alliance for Minority Participation Bridge to the Doctorate Program at Howard University; a predoctoral fellowship from the National Museum of Natural History; and NSF Earth Sciences grant 0929117 awarded to Daryl P. Domning. NR 50 TC 1 Z9 1 U1 1 U2 8 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JUL 1 PY 2013 VL 33 IS 4 BP 956 EP 963 DI 10.1080/02724634.2013.753081 PG 8 WC Paleontology SC Paleontology GA 170XX UT WOS:000320889600017 ER PT J AU Sues, HD Schoch, RR AF Sues, Hans-Dieter Schoch, Rainer R. TI FIRST RECORD OF COLOGNATHUS (?AMNIOTA) FROM THE MIDDLE TRIASSIC OF EUROPE SO JOURNAL OF VERTEBRATE PALEONTOLOGY LA English DT Article ID REPTILIA C1 [Sues, Hans-Dieter] Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Schoch, Rainer R.] Staatliches Museum Nat Kunde Stuttgart, D-70191 Stuttgart, Germany. RP Sues, HD (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Paleobiol, MRC 121,POB 37012, Washington, DC 20013 USA. EM suesh@si.edu; rainer.schoch@smns-bw.de NR 29 TC 2 Z9 2 U1 0 U2 0 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0272-4634 J9 J VERTEBR PALEONTOL JI J. Vertebr. Paleontol. PD JUL 1 PY 2013 VL 33 IS 4 BP 998 EP 1002 DI 10.1080/02724634.2013.732977 PG 5 WC Paleontology SC Paleontology GA 170XX UT WOS:000320889600021 ER PT J AU Ferrari, MA Campagna, C Condit, R Lewis, MN AF Ferrari, Mariano A. Campagna, Claudio Condit, Richard Lewis, Mirtha N. TI The founding of a southern elephant seal colony SO MARINE MAMMAL SCIENCE LA English DT Article DE Mirounga leonina; southern elephant seal; population trends; Bayesian state space models ID MIROUNGA-LEONINA; POPULATION-DYNAMICS; TIME-SERIES; MODELS; GROWTH; VERTEBRATES; ISLAND; SIZE AB The only large mainland colony of southern elephant seals (Mirounga leonina) is on Peninsula Valdes, at 42 degrees S, in Argentine Patagonia. Censuses of pups have been carried out regularly there since 1970, and the population grew five-fold by 2010. Here we use Bayesian modeling tools to make rigorous estimates of the rate of population growth, r, and to estimate survival and recruitment parameters that could account for the growth, incorporating observation error across different census methods. In the 1970s, r= 8%/yr, but has slowed to <1%/yr over the past decade. Using explicit demographic models, we established that the high growth of the 1970s was consistent with adult and juvenile survival at the upper end of published values (0.87/yr adult female survival; 0.40 juvenile survivorship to age four); the decline in the rate of population growth from 1970 to 2010 can be described by density-dependent reductions in adult and juvenile survival that fall well within published variation. Extrapolating empirical models of population growth rate backwards illustrates that the population could have been an established colony, with 100 pups born per year, between 1915 and 1945, consistent with qualitative observations prior to 1950. We conclude that the Valdes colony was founded by a few immigrants early in the 20th century and has been growing mostly by internal recruitment, with unknown density-dependent processes causing a reduction in growth and stabilization at 15,000-16,000 pups born. C1 [Ferrari, Mariano A.; Campagna, Claudio; Lewis, Mirtha N.] Consejo Nacl Invest Cient & Tecn, Ctr Nacl Patagon, RA-9120 Puerto Madryn, Chubut, Argentina. [Ferrari, Mariano A.] Univ Nacl Patagonia San Juan Bosco, Fac Ingn, RA-9120 Puerto Madryn, Chubut, Argentina. [Campagna, Claudio] WCS Argentina, Marine Program, Wildlife Conservat Soc, RA-1426 Buenos Aires, Argentina. [Condit, Richard] Smithsonian Trop Res Inst, Unit 0948, Panama City, Panama. RP Ferrari, MA (reprint author), Consejo Nacl Invest Cient & Tecn, Ctr Nacl Patagon, Bv Brown 2915, RA-9120 Puerto Madryn, Chubut, Argentina. EM ferrari@cenpat.edu.ar OI Campagna, Claudio/0000-0002-7971-5062 FU Agencia Nacional de Promocion Cientifica y Tecnologica [PICT 01-11749, 07-06420]; Wildlife Conservation Society FX We thank John Van den Hoff for their comments on an early version of the manuscript. This work was funded by grants from the Agencia Nacional de Promocion Cientifica y Tecnologica (grants PICT 01-11749 and 07-06420) and by the Wildlife Conservation Society. NR 51 TC 6 Z9 6 U1 2 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0824-0469 J9 MAR MAMMAL SCI JI Mar. Mamm. Sci. PD JUL PY 2013 VL 29 IS 3 BP 407 EP 423 DI 10.1111/j.1748-7692.2012.00585.x PG 17 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 179CP UT WOS:000321496100011 ER PT J AU Woc-Colburn, AM Murray, S Lock, J Dragoo, JW Guglielmo, D Maldonado, JE AF Woc-Colburn, Ana Margarita Murray, Suzan Lock, Justin Dragoo, Jerry W. Guglielmo, Dell Maldonado, Jesus E. TI A minimally invasive method for gender determination in the prehensile-tailed porcupine (Coendou prehensilis) SO ZOO BIOLOGY LA English DT Article DE Coendou prehensilis; sex determining zinc finger region; ZFX/ZFY; gender identification; molecular sexing ID PANDA AILUROPODA-MELANOLEUCA; SEX IDENTIFICATION; SAMPLES AB Prehensile-tailed porcupines (Coendou prehensilis), like other rodents, lack external sexual traits, making it difficult to non-invasively determine their gender. By exploiting genetic differences between the X and the Y chromosome, we developed a simple genetic test to determine the gender of Coendous from shed quills. We Sanger sequenced a short portion (195bp) of the zinc finger protein gene of known male (XY) Coendous to identify positions that are polymorphic between the X and Y chromosomes at this locus. By directly sequencing this fragment, we were able to correctly determine (confirmed via anatomical sexing) the gender of male and female Coendous by the presences or absence of polymorphisms in the resulting chromatograms. This assay is simple, quick and is applicable to other porcupine species. (c) 2013 Wiley Periodicals Inc. C1 [Woc-Colburn, Ana Margarita; Murray, Suzan] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. [Lock, Justin; Maldonado, Jesus E.] Smithsonian Conservat Biol Inst, Ctr Conservat & Evolutionary Genet, Natl Zool Pk, Washington, DC USA. [Lock, Justin; Maldonado, Jesus E.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Dragoo, Jerry W.] Univ New Mexico, Dept Biol, Albuquerque, NM 87131 USA. [Guglielmo, Dell] Smithsonian Conservat Biol Inst, Natl Zool Pk, Dept Anim Program, Washington, DC USA. RP Woc-Colburn, AM (reprint author), Nashville Zoo, 3777 Nolensville Pike, Nashville, TN 37211 USA. EM mwoccolburn@nashville-zoo.org RI Dragoo, Jerry/B-5486-2011 FU NIH [P20GM103452] FX Grant Sponsor: NIH; Grant number: P20GM103452 NR 12 TC 0 Z9 0 U1 2 U2 13 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0733-3188 J9 ZOO BIOL JI Zoo Biol. PD JUL PY 2013 VL 32 IS 4 BP 463 EP 466 DI 10.1002/zoo.21063 PG 4 WC Veterinary Sciences; Zoology SC Veterinary Sciences; Zoology GA 183NU UT WOS:000321824000016 PM 23447467 ER PT J AU Taufik, E Sekii, N Senda, A Fukuda, K Saito, T Eisert, R Oftedal, OT Urashima, T AF Taufik, Epi Sekii, Nobuhiro Senda, Akitsugu Fukuda, Kenji Saito, Tadao Eisert, Regina Oftedal, Olav T. Urashima, Tadasu TI Neutral and acidic milk oligosaccharides of the striped skunk (Mephitidae: Mephitis mephitis) SO ANIMAL SCIENCE JOURNAL LA English DT Article DE lactose; Mephitidae; milk oligosaccharides; striped skunk ID URSUS-THIBETANUS-JAPONICUS; JAPANESE BLACK BEAR; CHEMICAL-CHARACTERIZATION; MOLECULAR PHYLOGENY; POLAR BEAR; BLOOD TYPE; CARNIVORA; COLOSTRUM; MAMMALIA; BADGERS AB The biological significance of the tremendous variation in proportions of oligosaccharides and lactose among mammalian milks is poorly understood. We investigated milk oligosaccharides of the striped skunk (Mephitis mephitis) and compared these results to other species of the clade Mustelida. Individual oligosaccharides were identified by proton nuclear magnetic resonance spectroscopy. In the striped skunk, six oligosaccharides were identified: isoglobotriose, 2'-fucosyllactose, A-tetrasaccharide, Galili pentasaccharide, 3'-sialyllactose and monosialyl monogalactosyl lacto-N-neohexaose. Four of these have been found in related Mustelida and the other two in more distantly related carnivorans. The neutral and acidic oligosaccharides derive from three core structures: lactose (Gal(beta 1-4)Glc), lacto-N-neotetraose (Gal(beta 1-4)GlcNAc(beta 1-3)Gal(beta 1-4)Glc) and lacto-N-neohexaose (Gal(beta 1-4)GlcNAc(beta 1-3)[Gal(beta 1-4)GlcNAc(beta 1-6)]Gal(beta 1-4)Glc). C1 [Taufik, Epi; Sekii, Nobuhiro; Senda, Akitsugu; Fukuda, Kenji; Urashima, Tadasu] Obihiro Univ Agr & Vet Med, Grad Sch Anim & Food Hyg, Obihiro, Hokkaido 0808555, Japan. [Saito, Tadao] Tohoku Univ, Grad Sch Agr, Sendai, Miyagi 980, Japan. [Eisert, Regina; Oftedal, Olav T.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Eisert, Regina] Univ Canterbury, Gateway Antarctica, Christchurch 1, New Zealand. RP Urashima, T (reprint author), Obihiro Univ Agr & Vet Med, Grad Sch Anim & Food Hyg, Obihiro, Hokkaido 0808555, Japan. EM urashima@obihiro.ac.jp OI Taufik, Epi/0000-0003-4617-9037 FU Ministry of Education, Culture, Sports, Science, and Technology, Japan FX We would like to thank Dr. Milo Richmond and the New York State Cooperative Wildlife Unit at Cornell University for access to the skunk breeding colony, and Catherine (Missy) Mink for assistance in milk collection. We also gratefully acknowledge funding from the Global COE Program 'Frontier Program for Animal Global Health and Hygiene', Ministry of Education, Culture, Sports, Science, and Technology, Japan. NR 44 TC 4 Z9 4 U1 1 U2 8 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1344-3941 J9 ANIM SCI J JI Anim. Sci. J. PD JUL PY 2013 VL 84 IS 7 BP 569 EP 578 DI 10.1111/asj.12040 PG 10 WC Agriculture, Dairy & Animal Science SC Agriculture GA 176ZG UT WOS:000321344700008 PM 23607515 ER PT J AU Cerruti, M Dermer, CD Lott, B Boisson, C Zech, A AF Cerruti, Matteo Dermer, Charles D. Lott, Benoit Boisson, Catherine Zech, Andreas TI GAMMA-RAY BLAZARS NEAR EQUIPARTITION AND THE ORIGIN OF THE GeV SPECTRAL BREAK IN 3C 454.3 SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE galaxies: active; galaxies: individual: 3C454.3; gamma rays: general; radiation mechanisms: non-thermal ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; MULTIWAVELENGTH OBSERVATIONS; RADIO QUASARS; AGILE DETECTION; 2010 NOVEMBER; 3C-454.3; OUTBURST; EMISSION; CAMPAIGN AB Observations performed with the Fermi-LAT telescope have revealed the presence of a spectral break in the GeV spectrum of flat-spectrum radio quasars (FSRQs) and other low-and intermediate-synchrotron peaked blazars. We propose that this feature can be explained by Compton scattering of broad-line region photons by a non-thermal population of electrons described by a log-parabolic function. We consider in particular a scenario in which the energy densities of particles, magnetic field, and soft photons in the emitting region are close to equipartition. We show that this model can satisfactorily account for the overall spectral energy distribution of the FSRQ 3C 454.3, reproducing the GeV spectral cutoff due to Klein-Nishina effects and a curving electron distribution. C1 [Cerruti, Matteo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Cerruti, Matteo; Boisson, Catherine; Zech, Andreas] Univ Paris Diderot, CNRS, LUTII, Observ Paris, F-92190 Meudon, France. [Dermer, Charles D.] US Naval Res Lab, Div Space Sci, Washington, DC 20375 USA. [Lott, Benoit] Univ Bordeaux, CENBG, IN2P3, CNRS,UMR 7595, F-33175 Gradignan, France. RP Cerruti, M (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM matteo.cerruti@cfa.harvard.edu; charles.dermer@nrl.navy.mil FU Office of Naval Research; Fermi Guest Investigator Program FX The work of C.D.D. is supported by the Office of Naval Research and the Fermi Guest Investigator Program. NR 37 TC 26 Z9 26 U1 1 U2 12 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 JUL 1 PY 2013 VL 771 IS 1 AR L4 DI 10.1088/2041-8205/771/1/L4 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169WL UT WOS:000320811300004 ER PT J AU Greenhill, LJ Goddi, C Chandler, CJ Matthews, LD Humphreys, EML AF Greenhill, L. J. Goddi, C. Chandler, C. J. Matthews, L. D. Humphreys, E. M. L. TI DYNAMICAL EVIDENCE FOR A MAGNETOCENTRIFUGAL WIND FROM A 20 M-circle dot BINARY YOUNG STELLAR OBJECT (vol 770, pg L32, 2013) SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Correction C1 [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goddi, C.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Chandler, C. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. [Humphreys, E. M. L.] European So Observ, D-85748 Garching, Germany. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM greenhill@cfa.harvard.edu NR 1 TC 0 Z9 0 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 JUL 1 PY 2013 VL 771 IS 1 AR L18 DI 10.1088/2041-8205/771/1/L18 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169WL UT WOS:000320811300018 ER PT J AU Hermes, JJ Kepler, SO Castanheira, BG Gianninas, A Winget, DE Montgomery, MH Brown, WR Harrold, ST AF Hermes, J. J. Kepler, S. O. Castanheira, Barbara G. Gianninas, A. Winget, D. E. Montgomery, M. H. Brown, Warren R. Harrold, Samuel T. TI DISCOVERY OF AN ULTRAMASSIVE PULSATING WHITE DWARF SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE stars: evolution; stars: individual (GD 518); stars: oscillations; stars: variables: general; supernovae: general; white dwarfs ID ELECTRON-CAPTURE SUPERNOVAE; DIGITAL SKY SURVEY; STARS; EVOLUTION; MASS; CORES; CRYSTALLIZATION; PROGENITORS; TELESCOPE AB We announce the discovery of the most massive pulsating hydrogen-atmosphere white dwarf (WD) ever discovered, GD 518. Model atmosphere fits to the optical spectrum of this star show it is a 12,030 +/- 210 K WD with a log g = 9.08 +/- 0.06, which corresponds to a mass of 1.20 +/- 0.03M(circle dot). Stellar evolution models indicate that the progenitor of such a high-mass WD endured a stable carbon-burning phase, producing an oxygen-neon-core WD. The discovery of pulsations in GD 518 thus offers the first opportunity to probe the interior of a WD with a possible oxygen-neon core. Such a massive WD should also be significantly crystallized at this temperature. The star exhibits multi-periodic luminosity variations at timescales ranging from roughly 425 to 595 s and amplitudes up to 0.7%, consistent in period and amplitude with the observed variability of typical ZZ Ceti stars, which exhibit non-radial g-mode pulsations driven by a hydrogen partial ionization zone. Successfully unraveling both the total mass and core composition of GD 518 provides a unique opportunity to investigate intermediate-mass stellar evolution, and can possibly place an upper limit to the mass of a carbon-oxygen-core WD, which in turn constrains Type Ia supernovae progenitor systems. C1 [Hermes, J. J.; Castanheira, Barbara G.; Winget, D. E.; Montgomery, M. H.; Harrold, Samuel T.] Univ Texas Austin, Dept Astron, Austin, TX 78712 USA. [Hermes, J. J.; Castanheira, Barbara G.; Winget, D. E.; Montgomery, M. H.; Harrold, Samuel T.] McDonald Observ, Ft Davis, TX 79734 USA. [Kepler, S. O.] Univ Fed Rio Grande do Sul, Inst Fis, Porto Alegre, RS, Brazil. [Gianninas, A.] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Brown, Warren R.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Hermes, JJ (reprint author), Univ Texas Austin, Dept Astron, RLM 15308, Austin, TX 78712 USA. EM jjhermes@astro.as.utexas.edu RI Kepler, S. O. /H-5901-2012; Alexandros, Gianninas/B-8352-2016 OI Kepler, S. O. /0000-0002-7470-5703; Alexandros, Gianninas/0000-0002-8655-4308 FU Norman Hackerman Advanced Research Program [003658-0252-2009]; National Science Foundation [AST-0909107] FX We thank R. E. Falcon and E. L. Robinson for useful comments. This work is supported by the Norman Hackerman Advanced Research Program, under grant 003658-0252-2009, and by the National Science Foundation, under grant AST-0909107. We acknowledge the McDonald Observatory staff for their support, especially John Kuehne and Dave Doss. NR 44 TC 11 Z9 11 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2013 VL 771 IS 1 AR L2 DI 10.1088/2041-8205/771/1/L2 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169WL UT WOS:000320811300002 ER PT J AU Holder, GP Viero, MP Zahn, O Aird, KA Benson, BA Bhattacharya, S Bleem, LE Bock, J Brodwin, M Carlstrom, JE Chang, CL Cho, HM Conley, A Crawford, TM Crites, AT de Haan, T Dobbs, MA Dudley, J George, EM Halverson, NW Holzapfel, WL Hoover, S Hou, Z Hrubes, JD Keisler, R Knox, L Lee, AT Leitch, EM Lueker, M Luong-Van, D Marsden, G Marrone, DP McMahon, JJ Mehl, J Meyer, SS Millea, M Mohr, JJ Montroy, TE Padin, S Plagge, T Pryke, C Reichardt, CL Ruhl, JE Sayre, JT Schaffer, KK Schulz, B Shaw, L Shirokoff, E Spieler, HG Staniszewski, Z Stark, AA Story, KT van Engelen, A Vanderlinde, K Vieira, JD Williamson, R Zemcov, M AF Holder, G. P. Viero, M. P. Zahn, O. Aird, K. A. Benson, B. A. Bhattacharya, S. Bleem, L. E. Bock, J. Brodwin, M. Carlstrom, J. E. Chang, C. L. Cho, H-M. Conley, A. Crawford, T. M. Crites, A. T. de Haan, T. Dobbs, M. A. Dudley, J. George, E. M. Halverson, N. W. Holzapfel, W. L. Hoover, S. Hou, Z. Hrubes, J. D. Keisler, R. Knox, L. Lee, A. T. Leitch, E. M. Lueker, M. Luong-Van, D. Marsden, G. Marrone, D. P. McMahon, J. J. Mehl, J. Meyer, S. S. Millea, M. Mohr, J. J. Montroy, T. E. Padin, S. Plagge, T. Pryke, C. Reichardt, C. L. Ruhl, J. E. Sayre, J. T. Schaffer, K. K. Schulz, B. Shaw, L. Shirokoff, E. Spieler, H. G. Staniszewski, Z. Stark, A. A. Story, K. T. van Engelen, A. Vanderlinde, K. Vieira, J. D. Williamson, R. Zemcov, M. TI A COSMIC MICROWAVE BACKGROUND LENSING MASS MAP AND ITS CORRELATION WITH THE COSMIC INFRARED BACKGROUND SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE cosmic background radiation; galaxies: structure ID SOUTH-POLE TELESCOPE; GALAXIES AB We use a temperature map of the cosmic microwave background (CMB) obtained using the South Pole Telescope at 150 GHz to construct a map of the gravitational convergence to z similar to 1100, revealing the fluctuations in the projected mass density. This map shows individual features that are significant at the similar to 4 sigma level, providing the first image of CMB lensing convergence. We cross-correlate this map with Herschel/SPIRE maps covering 90 deg(2) at wavelengths of 500, 350, and 250 mu m. We show that these submillimeter (submm) wavelength maps are strongly correlated with the lensing convergence map, with detection significances in each of the three submm bands ranging from 6.7 sigma to 8.8 sigma. We fit the measurement of the cross power spectrum assuming a simple constant bias model and infer bias factors of b = 1.3-1.8, with a statistical uncertainty of 15%, depending on the assumed model for the redshift distribution of the dusty galaxies that are contributing to the Herschel/SPIRE maps. C1 [Holder, G. P.; de Haan, T.; Dobbs, M. A.; Dudley, J.; Shaw, L.; van Engelen, A.; Vanderlinde, K.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Viero, M. P.; Bock, J.; Lueker, M.; Padin, S.; Schulz, B.; Vieira, J. D.; Zemcov, M.] CALTECH, Pasadena, CA 91125 USA. [Zahn, O.] Univ Calif Berkeley, Dept Phys, Berkeley Ctr Cosmol Phys, Berkeley, CA 94720 USA. [Zahn, O.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Aird, K. A.; Hrubes, J. D.; Luong-Van, D.] Univ Chicago, Chicago, IL 60637 USA. [Benson, B. A.; Bhattacharya, S.; Bleem, L. E.; Carlstrom, J. E.; Chang, C. L.; Crawford, T. M.; Crites, A. T.; Hoover, S.; Keisler, R.; Leitch, E. M.; Mehl, J.; Meyer, S. S.; Padin, S.; Plagge, T.; Schaffer, K. K.; Story, K. T.; Williamson, R.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Benson, B. A.; Carlstrom, J. E.; Chang, C. L.; Meyer, S. S.; Schaffer, K. K.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Bhattacharya, S.] Argonne Natl Lab, Div High Energy Phys, Argonne, IL 60440 USA. [Bleem, L. E.; Carlstrom, J. E.; Hoover, S.; Keisler, R.; Meyer, S. S.; Story, K. T.] Univ Chicago, Dept Phys, Chicago, IL 60637 USA. [Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Brodwin, M.] Univ Missouri, Dept Phys & Astron, Kansas City, MO 64110 USA. [Carlstrom, J. E.; Crawford, T. M.; Crites, A. T.; Leitch, E. M.; Meyer, S. S.; Padin, S.; Plagge, T.; Williamson, R.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Carlstrom, J. E.; Chang, C. L.; Mehl, J.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cho, H-M.] NIST Quantum Devices Grp, Boulder, CO 80305 USA. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. [George, E. M.; Holzapfel, W. L.; Lee, A. T.; Reichardt, C. L.; Shirokoff, E.] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. [Halverson, N. W.] Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. [Halverson, N. W.] Univ Colorado, Dept Phys, Boulder, CO 80309 USA. [Hou, Z.; Knox, L.; Millea, M.] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. [Lee, A. T.; Spieler, H. G.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Div Phys, Berkeley, CA 94720 USA. [Marsden, G.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Marrone, D. P.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [McMahon, J. J.] Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA. [Mohr, J. J.] Univ Munich, Dept Phys, D-81679 Munich, Germany. [Mohr, J. J.] Excellence Cluster Universe, D-85748 Garching, Germany. [Mohr, J. J.] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Montroy, T. E.; Ruhl, J. E.; Sayre, J. T.; Staniszewski, Z.] Case Western Reserve Univ, Ctr Educ & Res Cosmol & Astrophys, Dept Phys, Cleveland, OH 44106 USA. [Pryke, C.] Univ Minnesota, Dept Phys, Minneapolis, MN 55455 USA. [Schaffer, K. K.] Sch Art Inst Chicago, Liberal Arts Dept, Chicago, IL 60603 USA. [Schulz, B.] CALTECH, JPL, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Stark, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Vanderlinde, K.] Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Vanderlinde, K.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. RP Holder, GP (reprint author), McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. RI Williamson, Ross/H-1734-2015; Holzapfel, William/I-4836-2015; OI Williamson, Ross/0000-0002-6945-2975; Reichardt, Christian/0000-0003-2226-9169; Stark, Antony/0000-0002-2718-9996; Marrone, Daniel/0000-0002-2367-1080; Aird, Kenneth/0000-0003-1441-9518 FU National Science Foundation [ANT-0638937]; NSF [PHY-1125897, AST-1009811]; Kavli Foundation; Gordon and Betty Moore Foundation; National Sciences and Engineering Research Council of Canada; Canada Research Chairs program; Canadian Institute for Advanced Research; NASA Hubble Fellowship [HF-51275.01]; KICP Fellowship; Alfred P. Sloan Research Fellowship; BCCP fellowship; [AST-1009012] FX The SPT is supported by the National Science Foundation through grant ANT-0638937, with partial support provided by NSF grant PHY-1125897, the Kavli Foundation, and the Gordon and Betty Moore Foundation. The McGill group acknowledges funding from the National Sciences and Engineering Research Council of Canada, Canada Research Chairs program, and the Canadian Institute for Advanced Research. Work at Harvard is supported by grant AST-1009012. S. Bhattacharya acknowledges support from NSF grant AST-1009811, R. Keisler from NASA Hubble Fellowship grant HF-51275.01, B. Benson from a KICP Fellowship, M. Dobbs from an Alfred P. Sloan Research Fellowship, and O. Zahn from a BCCP fellowship. NR 26 TC 39 Z9 39 U1 1 U2 9 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2013 VL 771 IS 1 AR L16 DI 10.1088/2041-8205/771/1/L16 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169WL UT WOS:000320811300016 ER PT J AU McLaughlin, BM Ballance, CP Bowen, KP Gardenghi, DJ Stolte, WC AF McLaughlin, B. M. Ballance, C. P. Bowen, K. P. Gardenghi, D. J. Stolte, W. C. TI HIGH PRECISION K-SHELL PHOTOABSORPTION CROSS SECTIONS FOR ATOMIC OXYGEN: EXPERIMENT AND THEORY SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE atomic data; atomic processes; ISM: abundances; photon-dominated region (PDR); stars: Wolf-Rayet; Sun: X-rays; gamma rays ID RAY-ABSORPTION SPECTROSCOPY; INTERSTELLAR-MEDIUM; PHOTOIONIZATION; RESONANCES; SPECTRUM; LINES; IONS; IONIZATION; EMISSION; PROGRAM AB Photoabsorption of atomic oxygen in the energy region below the 1s(-1) threshold in X-ray spectroscopy from Chandra and XMM-Newton is observed in a variety of X-ray binary spectra. Photoabsorption cross sections determined from an R-matrix method with pseudo-states and new, high precision measurements from the Advanced Light Source (ALS) are presented. High-resolution spectroscopy with E/Delta E approximate to 4250 +/- 400 was obtained for photon energies from 520 eV to 555 eV at an energy resolution of 124 +/- 12 meV FWHM. K-shell photoabsorption cross section measurements were made with a re-analysis of previous experimental data on atomic oxygen at the ALS. Natural line widths G are extracted for the 1s(-1)2s(2)2p(4)(4P) np P-3. and 1s(-1)2s(2)2p(4)(2P) np P-3. Rydberg resonances series and compared with theoretical predictions. Accurate cross sections and line widths are obtained for applications in X-ray astronomy. Excellent agreement between theory and the ALS measurements is shown which will have profound implications for the modeling of X-ray spectra and spectral diagnostics. C1 [McLaughlin, B. M.] Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. [McLaughlin, B. M.] Harvard Smithsonian Ctr Astrophys, ITAMP, Cambridge, MA 02138 USA. [Ballance, C. P.] Auburn Univ, Dept Phys, Allison Lab 206, Auburn, AL 36849 USA. [Bowen, K. P.; Gardenghi, D. J.; Stolte, W. C.] Univ Nevada, Dept Chem, Las Vegas, NV 89154 USA. [Stolte, W. C.] Univ Nevada, Harry Reid Ctr Environm Studies, Las Vegas, NV 89154 USA. [Stolte, W. C.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Adv Light Source, Berkeley, CA 94720 USA. RP McLaughlin, BM (reprint author), Queens Univ Belfast, Sch Math & Phys, CTAMOP, Belfast BT7 1NN, Antrim, North Ireland. EM b.mclaughlin@qub.ac.uk; ballance@physics.auburn.edu; bowenk4@gmail.com; dgardenghi@gmail.com; wcstolte@lbl.gov FU National Science Foundation; U.S. Department of Energy (DoE) grants through Auburn University; National Science Foundation under NSF [PHY-01-40375]; National Science Foundation [OCI-1053575]; Director, Office of Science, Office of Basic Energy Sciences, of the U. S. Department of Energy [DE-AC02-05CH11231] FX B.M.M. and C.P.B. thank the Institute for Theoretical Atomic and Molecular Physics (ITAMP) at the Harvard-Smithsonian Center for Astrophysics for their hospitality and support (B.M.M.) under the visitor's program. ITAMP is supported by a grant from the National Science Foundation. C.P.B. acknowledges support by U.S. Department of Energy (DoE) grants through Auburn University. W.C.S. acknowledges support from the National Science Foundation under NSF Grant No. PHY-01-40375. We thank Professor Alex Dalgarno FRS, Dr. John C Raymond, Dr. Randall K Smith, Dr. Jeremy J Drake and Dr. Brad Wargelin for discussions on the astrophysical applications and the LETG Chandra calibration. Grants of computational time at the National Energy Research Scientific Computing Center in Oakland, CA, USA, the Kraken XT5 facility at the National Institute for Computational Science (NICS) in Knoxville, TN, USA and at the High Performance Computing Center Stuttgart (HLRS) of the University of Stuttgart are gratefully acknowledged. The Kraken XT5 facility is a resource of the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by National Science Foundation Grant No. OCI-1053575. The help of Hendrik Blum and Tolek Tyliszczak in setting up the experiment on beamline 11 at the ALS is gratefully acknowledged. The Advanced Light Source in Berkeley, CA, USA, is supported by the Director, Office of Science, Office of Basic Energy Sciences, of the U. S. Department of Energy under Contract No. DE-AC02-05CH11231. NR 49 TC 15 Z9 15 U1 0 U2 18 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUL 1 PY 2013 VL 771 IS 1 AR L8 DI 10.1088/2041-8205/771/1/L8 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 169WL UT WOS:000320811300008 ER PT J AU Zeigler, SL De Vleeschouwer, KM Raboy, BE AF Zeigler, Sara L. De Vleeschouwer, Kristel M. Raboy, Becky E. TI Assessing Extinction Risk in Small Metapopulations of Golden-headed Lion Tamarins (Leontopithecus chrysomelas) in Bahia State, Brazil SO BIOTROPICA LA English DT Article DE Atlantic Forest; habitat fragmentation; habitat loss; logistic sensitivity analysis; population viability analysis; small population size ID BRAZILIAN ATLANTIC FOREST; LEONTOPITHECUS-CHRYSOMELAS; BIODIVERSITY CONSERVATION; HABITAT FRAGMENTATION; FUNCTIONAL CONNECTIVITY; POPULATION VIABILITY; SOUTHERN BAHIA; LANDSCAPE; DYNAMICS; PRIMATE AB Golden-headed lion tamarins (GHLTs; Leontopithecus chrysomelas) are endangered primates endemic to the Brazilian Atlantic Forest, where loss of forest and its connectivity threaten species survival. Understanding the role of habitat availability and configuration on population declines is critical for guiding proactive conservation for this, and other, endangered species. We conducted population viability analysis to assess vulnerability of ten GHLT metapopulations to habitat loss and small population size. Seven metapopulations had a low risk of extirpation (or local extinction) over the next 100 years assuming no further forest loss, and even small populations could persist with immediate protection. Three metapopulations had a moderate/high risk of extirpation, suggesting extinction debt may be evident in parts of the species' range. When deforestation was assumed to continue at current rates, extirpation risk significantly increased while abundance and genetic diversity decreased for all metapopulations. Extirpation risk was significantly negatively correlated with the size of the largest patch available to metapopulations, underscoring the importance of large habitat patches for species persistence. Finally, we conducted sensitivity analysis using logistic regression, and our results showed that local extinction risk was sensitive to percentage of females breeding, adult female mortality, and dispersal rate and survival; conservation or research programs that target these aspects of the species' biology/ecology could have a disproportionately important impact on species survival. We stress that efforts to protect populations and tracts of habitat of sufficient size throughout the species' distribution will be important in the near-term to protect the species from continuing decline and extinction. C1 [Zeigler, Sara L.] Univ Maryland, Dept Geog Sci, College Pk, MD 20742 USA. [De Vleeschouwer, Kristel M.; Raboy, Becky E.] Royal Zool Soc Antwerp, Ctr Res & Conservat, B-2018 Antwerp, Belgium. [De Vleeschouwer, Kristel M.; Raboy, Becky E.] Inst Estudos Socioambientais Sul Bahia, Ilheus, Brazil. [Raboy, Becky E.] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC USA. RP Zeigler, SL (reprint author), Univ Maryland, Dept Geog Sci, 2181 Samuel J LeFrak Hall, College Pk, MD 20742 USA. EM szeigler23@gmail.com FU Ann G. Wylie Dissertation Fellowship through the University of Maryland FX Long-term demographic data on GHLTs were obtained by B. Raboy, J. Dietz, K. De Vleeschouwer, and their field assistants from studies in and around Una Biological Reserve (authorized by IBAMA and CNPq). Reserve directors Saturnino Souza and Paulo Cruz provided instrumental support. We also thank Nayara Cardoso and Leonardo Neves from Conexao Mico Leao (Smithsonian/IESB). S. Zeigler was supported by an Ann G. Wylie Dissertation Fellowship through the University of Maryland. NR 62 TC 5 Z9 6 U1 9 U2 130 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0006-3606 J9 BIOTROPICA JI Biotropica PD JUL PY 2013 VL 45 IS 4 BP 528 EP 535 DI 10.1111/btp.12037 PG 8 WC Ecology SC Environmental Sciences & Ecology GA 175DQ UT WOS:000321210900016 ER PT J AU Cerqueira, MC Cohn-Haft, M Vargas, CF Nader, CE Andretti, CB Costa, TVV Sberze, M Hines, JE Ferraz, G AF Cerqueira, Marconi C. Cohn-Haft, Mario Vargas, Claudeir F. Nader, Carlos E. Andretti, Christian B. Costa, Thiago V. V. Sberze, Monica Hines, James E. Ferraz, Goncalo TI Rare or elusive? A test of expert knowledge about rarity of Amazon forest birds SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE Acoustic sampling; birds; detection; expert knowledge; occupancy; rarity ID HIERARCHICAL BAYES ESTIMATION; SPECIES DISTRIBUTIONS; EXTINCTION RISK; OCCUPANCY; CONSERVATION; MODELS; ABUNDANCE; JUDGMENT; ECOLOGY; UNCERTAINTY AB Aim To offer a test of expert knowledge about rarity of twenty Amazon forest bird species following an approach that equates rarity with low site occupancy and formally accounts for imperfect species detection. We define ten pairs of closely related species, each pair with one hypothetically common and one hypothetically rare species. Our null hypothesis is that members of each pair have similar occupancy, with hypothesized differences due to detection errors alone. Location A 1000-ha plot of primary rainforest in the central Brazilian Amazon. Methods We visited each of 55 sampling sites multiple times per season for three field seasons and estimated the probability of site occupancy by each species following a maximum likelihood state-space approach that also estimates the probability that a species is present yet undetected at a site. To maximize detection and account for its variation, we employed three different sampling techniques while systematically training and testing observer's ability to recognize species. Results Occupancy estimates agree with expert predictions in all but two species pairs and show no evidence of clear temporal variation in occupancy between sampling seasons. Detection probability had a positive relation with observer ability, a strong relation to time of day across species, and a strong relation with the use of playback for some species. Detection with point counts and with autonomous recorders varied between species pairs. Main conclusions We reject the null hypothesis of equal occupancy within pairs, concluding that expert knowledge on species rarity is useful and worth eliciting. Our results replace qualitative ratings of rarity with statistical estimates of occupancy, establishing a reliable baseline for future comparisons. Besides illustrating the relevance of expert knowledge, this application to Amazonian birds illustrates a flexible approach that can be used for testing knowledge about rarity for a variety of species groups and spatial scales. C1 [Costa, Thiago V. V.] Univ Sao Paulo, Dept Zool, Inst Biociencias, BR-05508 Sao Paulo, Brazil. [Costa, Thiago V. V.] Univ Sao Paulo, Museu Zool, BR-05508 Sao Paulo, Brazil. [Hines, James E.] US Geol Survey, Patuxent Wildlife Res Ctr, Laurel, MD 20708 USA. [Ferraz, Goncalo] Smithsonian Trop Res Inst, Panama City 084303092, Panama. RP Ferraz, G (reprint author), Inst Nacl de Pesquisas da Amazonia, Biol Dynam Forest Fragments Project, CP 478,Av Andre Araujo, BR-29366908 Manaus, Amazonas, Brazil. EM ferrazg@si.edu RI Costa, Thiago/F-7931-2013; Ferraz, Goncalo/C-3860-2008; Museu de Zoologia da USP, MZ-USP/Q-2192-2016; OI Ferraz, Goncalo/0000-0001-8748-0462; Campos-Cerqueira, Marconi/0000-0001-6561-5864 FU Brazil's Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq); Smithsonian Tropical Research Institute; State of Amazonas Fundacao de Amparoa Pesquisa (FAPEAM) FX We are thankful to Angela Pacheco, Thiago Orsi, Gisiane Rodrigues, Jefferson Valsko, Marcelo dos Santos, Catherine Bechtoldt, JoaoVitor Campos e Silva, Mariana Tolentino, Francisco Villa-Marin and Andre Zumak for their help with bird sampling and gracious submission to bird sound memory tests. Fieldwork was made lighter by Eduarda Benicio's cooking and Jairo Lopes' assistance. MCC was supported by a M.Sc. grant from Brazil's Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) and equipment donations by Idea Wild and Birders' Exchange. Field expenses were paid by the Smithsonian Tropical Research Institute and the State of Amazonas Fundacao de Amparoa Pesquisa (FAPEAM). This is contribution 605 of the BDFFP technical series and contribution 25 of the INPA Scientific Collections Amazonian Ornithology series. NR 59 TC 5 Z9 5 U1 0 U2 30 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD JUL PY 2013 VL 19 IS 7 BP 710 EP 721 DI 10.1111/ddi.12033 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 163HU UT WOS:000320327500006 ER PT J AU Dutta, T Sharma, S Maldonado, JE Wood, TC Panwar, HS Seidensticker, J AF Dutta, Trishna Sharma, Sandeep Maldonado, Jesus E. Wood, Thomas C. Panwar, H. S. Seidensticker, John TI Fine-scale population genetic structure in a wide-ranging carnivore, the leopard (Panthera pardus fusca) in central India SO DIVERSITY AND DISTRIBUTIONS LA English DT Article DE corridors; faecal DNA genetic structure; habitat fragmentation; India; non-invasive sampling ID HUMAN-DOMINATED LANDSCAPES; MULTILOCUS GENOTYPE DATA; MICROSATELLITE DATA; COMPUTER-PROGRAM; INTERPOPULATION DISPERSAL; NATURAL-POPULATIONS; ASSIGNMENT METHODS; NATIONAL-PARK; ONE-MIGRANT; SOFTWARE AB Aim Habitat loss and fragmentation can influence the genetic structure of biological populations. Large terrestrial predators can often avoid genetic subdivision due to fragmentation because they have high rates of dispersal-mediated gene flow. Leopards (Panthera pardus) are found in a variety of habitats and are the most widely distributed of the large and middle-sized felids. We investigated the genetic diversity and population substructure of leopards (P.p fusca) in a fragmented meta-population comprised of four populations from five protected areas and inter-connecting corridors spread over an area of 45,000km2 in central India. Location Kanha, Pench, Satpura and Melghat Tiger Reserves, and interconnecting corridors in the Satpura-Maikal Landscape of Central India. Methods We collected faecal samples and used genetic methods to identify individuals, estimate the genetic variation and evaluate the patterns of genetic substructuring within this meta-population of leopards. Results We identified 217 individual leopards using a panel of seven microsatellite loci. Leopards showed high levels of genetic diversity in all sampled populations. Spatial and non-spatial Bayesian analysis revealed at least two admixed genetic populations with indications of ongoing genetic subdivision. Genetic differentiation between populations was not explained by geographic distance. We identified nine individuals as migrants, most of which were assigned to reserves connected by corridors. Main conclusions Our study demonstrates that the leopard, an adaptable and vagile species, can become genetically differentiated with increased habitat fragmentation. Contrary to our hypothesis of panmixia, our results indicate that although leopards in this landscape are admixed, there is genetic substructuring at both the landscape and the fine-scale level. We conclude that this is due to habitat fragmentation and corridors are of immense value in maintaining genetic connectivity in this landscape. C1 [Dutta, Trishna; Sharma, Sandeep; Maldonado, Jesus E.; Seidensticker, John] Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. [Dutta, Trishna; Sharma, Sandeep; Wood, Thomas C.] George Mason Univ, Dept Environm Sci & Policy, Fairfax, VA 22030 USA. [Panwar, H. S.] Peace Inst Charitable Trust, Delhi 110091, India. RP Dutta, T (reprint author), Smithsonian Conservat Biol Inst, Natl Zool Pk, Washington, DC 20013 USA. EM trishnad@gmail.com FU Smithsonian Conservation Biology Institute (SCBI); Friends of the National Zoo; George Mason University; International Bear Association (IBA) FX Funding was provided by Smithsonian Conservation Biology Institute (SCBI), Friends of the National Zoo, George Mason University and International Bear Association (IBA). We thank the Principal Chief Conservator of Forests (PCCF) Wildlife, Madhya Pradesh and Maharashtra, and field directors and staff of all five tiger reserves (Kanha, Satpura, Melghat, Pench MP and Mh) for providing research permissions and logistical help. We thank Robert Fleischer, Center for Conservation and Evolutionary Genetics, SCBI, and Yogesh S. Shouche, National Center for Cell Sciences (NCCS), Pune, Maharashtra, India, for providing laboratory space and facilitating lab work. We thank Nancy Rotzel, Libby Dougan, and Hitendra Munot for logistical support, and Susan Lumpkin and Christine Bozarth for comments on the manuscript. We would like to thank the Associate Editor and two anonymous reviewers for their inputs. NR 82 TC 18 Z9 19 U1 4 U2 72 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1366-9516 J9 DIVERS DISTRIB JI Divers. Distrib. PD JUL PY 2013 VL 19 IS 7 BP 760 EP 771 DI 10.1111/ddi.12024 PG 12 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 163HU UT WOS:000320327500010 ER PT J AU Abed, RMM Dobretsov, S Al-Fori, M Gunasekera, SP Sudesh, K Paul, VJ AF Abed, Raeid M. M. Dobretsov, Sergey Al-Fori, Marwan Gunasekera, Sarath P. Sudesh, Kumar Paul, Valerie J. TI Quorum-sensing inhibitory compounds from extremophilic microorganisms isolated from a hypersaline cyanobacterial mat SO JOURNAL OF INDUSTRIAL MICROBIOLOGY & BIOTECHNOLOGY LA English DT Article DE Quorum-sensing inhibition; Antimicrobial, extreme halophiles; Diketopiperazines; Cyanobacterial mats; Biofouling ID AEROBIC HETEROTROPHIC BACTERIA; SULTANATE-OF-OMAN; HALOPHILIC ARCHAEON; MARINE-BACTERIA; MICROBIAL MAT; STRUCTURE ELUCIDATION; ANTIFOULING ACTIVITY; CROSS-TALK; SP-NOV.; DIKETOPIPERAZINES AB In this study, extremely halophilic and moderately thermophilic microorganisms from a hypersaline microbial mat were screened for their ability to produce antibacterial, antidiatom, antialgal, and quorum-sensing (QS) inhibitory compounds. Five bacterial strains belonging to the genera Marinobacter and Halomonas and one archaeal strain belonging to the genus Haloterrigena were isolated from a microbial mat. The strains were able to grow at a maximum salinity of 22-25 % and a maximum temperature of 45-60 A degrees C. Hexanes, dichloromethane, and butanol extracts from the strains inhibited the growth of at least one out of nine human pathogens. Only butanol extracts of supernatants of Halomonas sp. SK-1 inhibited growth of the microalga Dunaliella salina. Most extracts from isolates inhibited QS of the acyl homoserine lactone producer and reporter Chromobacterium violaceum CV017. Purification of QS inhibitory dichloromethane extracts of Marinobacter sp. SK-3 resulted in isolation of four related diketopiperazines (DKPs): cyclo(l-Pro-l-Phe), cyclo(l-Pro-l-Leu), cyclo(l-Pro-l-isoLeu), and cyclo(l-Pro-d-Phe). QS inhibitory properties of these DKPs were tested using C. violaceum CV017 and Escherichia coli-based QS reporters (pSB401 and pSB1075) deficient in AHL production. Cyclo(l-Pro-l-Phe) and cyclo(l-Pro-l-isoLeu) inhibited QS-dependent production of violacein by C. violaceum CV017. Cyclo(l-Pro-l-Phe), cyclo(l-Pro-l-Leu), and cyclo(l-Pro-l-isoLeu) reduced QS-dependent luminescence of the reporter E. coli pSB401 induced by 3-oxo-C6-HSL. Our study demonstrated the ability of halophilic and moderately thermophilic strains from a hypersaline microbial mat to produce biotechnologically relevant compounds that could be used as antifouling agents. C1 [Abed, Raeid M. M.] Sultan Qaboos Univ, Dept Biol, Coll Sci, Al Khoud, Oman. [Dobretsov, Sergey; Al-Fori, Marwan] Sultan Qaboos Univ, Marine Sci & Fisheries Dept, Coll Agr & Marine Sci, Al Khoud, Oman. [Gunasekera, Sarath P.; Paul, Valerie J.] Smithsonian Marine Stn, Ft Pierce, FL USA. [Sudesh, Kumar] Univ Sains Malaysia, Sch Biol Sci, George Town 11800, Malaysia. RP Dobretsov, S (reprint author), Sultan Qaboos Univ, Marine Sci & Fisheries Dept, Coll Agr & Marine Sci, Al Khoud, Oman. EM sergey@squ.edu.om RI Sudesh, Kumar/C-2942-2011; OI Sudesh, Kumar/0000-0003-4756-9192 FU Sultan Qaboos University (SQU) [IG/AGR/FISH/12/01]; HM Sultan Qaboos Research Trust Fund [SR/AGR/FISH/10/01]; George E. Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution (USA); Hanse-Wissenschaftskolleg (HWK), Institute for Advanced Study, Germany FX The work of SD was supported by a Sultan Qaboos University (SQU) internal grant IG/AGR/FISH/12/01, by a HM Sultan Qaboos Research Trust Fund SR/AGR/FISH/10/01 and by the George E. Burch Fellowship in Theoretical Medicine and Affiliated Sciences at the Smithsonian Institution (USA). SD acknowledges Professor Ricardo Coutinho (IEAPM, Arraial do Cabo, Brazil) and the program science without frontiers (CNPq). RA would like to thank the Hanse-Wissenschaftskolleg (HWK), Institute for Advanced Study, Germany, for their support. The authors acknowledge help with QS bioassays by Dr. Max Teplitski (University of Florida, USA) and with strain isolation by Mrs. Samiha Al Kharusi. This is contribution No. 910 of the Smithsonian Marine Station at Fort Pierce. NR 64 TC 8 Z9 11 U1 6 U2 56 PU SPRINGER HEIDELBERG PI HEIDELBERG PA TIERGARTENSTRASSE 17, D-69121 HEIDELBERG, GERMANY SN 1367-5435 J9 J IND MICROBIOL BIOT JI J. Ind. Microbiol. Biotechnol. PD JUL PY 2013 VL 40 IS 7 BP 759 EP 772 DI 10.1007/s10295-013-1276-4 PG 14 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA 164GB UT WOS:000320396000011 PM 23645384 ER PT J AU Wagner, K Bogusch, W Zotz, G AF Wagner, Katrin Bogusch, Wiebke Zotz, Gerhard TI The role of the regeneration niche for the vertical stratification of vascular epiphytes SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE Anthurium; Araceae; Bromeliaceae; Catopsis; Central America; germination; Guzmania; microclimatic gradient; seedlings; Tillandsia; tropical rain forest; Werauhia ID HUMID MONTANE FOREST; WATER RELATIONS; RAIN-FOREST; CLOUD-FOREST; BROMELIADS; CANOPY; GERMINATION; MICROCLIMATE; SURVIVAL; GROWTH AB Vertical stratification of vascular epiphytes is frequently attributed to niche partitioning along microclimatic gradients but experimental confirmations of this notion are rare. This study investigates the role of the regeneration phase for the stratification of five bromeliad (Catopsis sessiliflora, Guzmania subcorymbosa, Tillandsia anceps, T. bulbosa and Werauhia gladioliflora) and seven aroid species (Anthurium acutangulum, A. brownii, A. clavigerum, A. durandii, A. friedrichsthalii, A. hacumense and A. scandens) in a Panamanian rain forest. We documented gradients of temperature, vapour pressure deficit and light (n = 10d) as well as species height distributions (n = 11-120). Microclimatic gradients were substantial (maximal T and RH differences between strata: 5 degrees C and 18%, respectively) and mean attachment heights of the study species (range = 4-21 m) differed significantly. We tested sensitivity to recurrent drought (four treatments) during germination (all species, cumulative germination of 20 seeds, n = 3) and seedling growth (four aroid species, n = 25). Seedling survival of six aroid species transplanted to three heights (n = 27) was monitored in situ. Some species did not germinate under severe recurrent drought while others germinated at the same rate in all treatments. Seedlings of the most exposed species grew fastest under intermediate recurrent drought while those of the other three species grew fastest when kept constantly wet. Survival of transplanted seedlings did not depend on species attachment height, but this may be attributable to insufficient statistical power. Taken together, the results suggest that the stratification can be explained to a large degree by differential sensitivity to the vertical moisture gradient during the regeneration phase. C1 [Wagner, Katrin; Bogusch, Wiebke; Zotz, Gerhard] Carl von Ossietzky Univ Oldenburg, Inst Biol & Umweltwissensch, AG Funkt Okol, D-26111 Oldenburg, Germany. [Zotz, Gerhard] Smithsonian Trop Res Inst, Panama City, Panama. RP Wagner, K (reprint author), Carl von Ossietzky Univ Oldenburg, Inst Biol & Umweltwissensch, AG Funkt Okol, Postfach 2503, D-26111 Oldenburg, Germany. EM ka.wagner@uni-oldenburg.de FU DFG [Zo 94/5-1] FX We thank the Republic of Panama for making its natural resources available for science (research permits: SE/P-32-09, SE/P-14-10, SC/P-26-10, and SE/P-3-11). Thanks to Dr S. J. Wright (STRI, Panama) for the opportunity to work at the crane, to Argelis Ruiz and Mirna Sarmaniego for organizing crane work and to Edwin Andrade and Jose Herrera for manoeuvring us through the canopy. Many thanks to Catherine Brunton for laboratory assistance, to Eduardo Sanchez for assistance in the field and to Juliano Sarmento Cabral and Gunnar Petter for rechecking the transplants in October 2012. The bromeliad experiments were part of Wiebke Bogusch's master's thesis. This work was funded by the DFG (Zo 94/5-1). NR 44 TC 14 Z9 15 U1 2 U2 58 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JUL PY 2013 VL 29 BP 277 EP 290 DI 10.1017/S0266467413000291 PN 4 PG 14 WC Ecology SC Environmental Sciences & Ecology GA 175BF UT WOS:000321203600001 ER PT J AU Zalamea, PC Sarmiento, C Stevenson, PR Rodriguez, M Nicolini, E Heuret, P AF Zalamea, Paul-Camilo Sarmiento, Carolina Stevenson, Pablo R. Rodriguez, Manuel Nicolini, Eric Heuret, Patrick TI Effect of rainfall seasonality on the growth of Cecropia sciadophylla: intra-annual variation in leaf production and node length SO JOURNAL OF TROPICAL ECOLOGY LA English DT Article DE leaf phenology; Neotropics; pioneer plants; plant growth; plant morphology; rainfall seasonality; Urticaceae ID PHENOLOGY; TREE; FOREST; PATTERNS AB Patterns of leaf production and leaf fall directly influence leaf area index and forest productivity. Here, we focused on Cecropia sciadophylla individuals inhabiting the extremes of the gradient in seasonality in rainfall at which C. sciadophylla occurs. In Colombia and French Guiana we compared the intra-annual variation in leaf production as well as the intra-annual fluctuation in internode length on a total of 69 saplings ranging in size from 1 to 2 m. The mean rate of leaf production was similar to 2 leaves mo(-1) in both populations, and the rate of leaf production was constant throughout the year. Our results showed monthly variation in internode length and the number of live leaves per sapling in the seasonal habitat and variation only in internode length in the everwet habitat. Because the rate of leaf production is constant at both localities, the difference in number of live leaves per sapling at the seasonal site must reflect seasonal variation in leaf life span. We show that in Cecropia, internode length can serve as an indicator of precipitation seasonality. Finally an open question is whether leaf production in other pioneer species is also independent of climatic seasonal cues. This information could allow us to link growth and climate of secondary forest species and better understand how past and future climate can affect plant growth trajectories. C1 [Zalamea, Paul-Camilo] IRD, UMR AMAP, F-34000 Montpellier, France. [Sarmiento, Carolina; Stevenson, Pablo R.; Rodriguez, Manuel] Univ Los Andes, Dept Ciencias Biol, Bogota, Colombia. [Zalamea, Paul-Camilo; Sarmiento, Carolina] Smithsonian Trop Res Inst, Ancon, Panama. [Nicolini, Eric] CIRAD, UMR AMAP, F-34000 Montpellier, France. [Heuret, Patrick] INRA, UMR ECOFOG, F-97310 Kourou, French Guiana. RP Zalamea, PC (reprint author), IRD, UMR AMAP, F-34000 Montpellier, France. EM camilozalamea@gmail.com OI Sarmiento, Carolina/0000-0002-8575-7170 FU Ecos-Nord; Colciencias; Paris 13 University [C08A01]; IRD (Institut de Recherche pour le Developpement, France) FX The authors are most grateful to A. Rodriguez and B. Leudet de la Vallee for their assistance in the field. We thank F. Munoz and A. Berthouly for enlightening discussions during data analyses. We also thank J. Dalling, E. V. J. Tanner, E. Leigh Jr., N. Rowe, D. Roche, B. Wolfe and one anonymous reviewer for helpful comments on earlier versions of this manuscript. This research was partially supported by an Ecos-Nord, Colciencias, and Paris 13 University grant (C08A01), an IRD (Institut de Recherche pour le Developpement, France) doctoral grant to P-C Z. NR 14 TC 1 Z9 1 U1 4 U2 37 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0266-4674 J9 J TROP ECOL JI J. Trop. Ecol. PD JUL PY 2013 VL 29 BP 361 EP 365 DI 10.1017/S0266467413000394 PN 4 PG 5 WC Ecology SC Environmental Sciences & Ecology GA 175BF UT WOS:000321203600010 ER PT J AU Podorvanyuk, NY Chilingarian, IV Katkov, IY AF Podorvanyuk, Nikolay Yu. Chilingarian, Igor V. Katkov, Ivan Yu. TI A new technique for the determination of the initial mass function in unresolved stellar populations SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: data analysis; globular clusters: general; galaxies: dwarf; galaxies: kinematics and dynamics; galaxies: star clusters: general; galaxies: stellar content ID COMPACT DWARF GALAXIES; GALACTIC GLOBULAR-CLUSTERS; DARK-MATTER CONTENT; TO-LIGHT RATIOS; STAR-CLUSTERS; EVOLUTIONARY SYNTHESIS; GAS EXPULSION; METALLICITY; SPECTRA; SEGREGATION AB We present a new technique for the determination of the low-mass slope (alpha(1); M-* < 0.5 M-circle dot) of the present-day stellar mass function (PDMF) using the pixel-space fitting of integrated light spectra. The technique can be used to constrain the initial mass function (IMF) of stellar systems with relaxation time-scales exceeding the Hubble time and to test the IMF universality hypothesis. We provide two versions of the technique: (i) a fully unconstrained determination of the age, metallicity and alpha(1); and (ii) a constrained fitting by imposing the externally determined mass-to-light ratio of the stellar population. We tested our approach with Monte Carlo simulations using mock spectra and conclude that: (i) age, metallicity and alpha(1) can be precisely determined by applying the unconstrained version of the code to high signal-to-noise ratio data sets (S/N = 100, R = 7000 yields delta alpha(1) approximate to 0.1); (ii) the M/L constraint significantly improves the precision and reduces the degeneracies; however, its systematic errors cause biased alpha(1) estimates; (iii) standard Lick indices cannot constrain the PDMF because they miss most of the mass function-sensitive spectral features; (iv) the alpha(1) determination remains unaffected by the high-mass IMF shape (alpha(3); M-* >= 1 M-circle dot) variation for stellar systems older than 8 Gyr, while the intermediate-mass IMF slope (alpha(2); 0.5 < M-* < 1 M-circle dot) may introduce biases into the best-fitting alpha(1) values if it is different from the canonical value alpha(2) = 2.3. We analysed observed intermediate-resolution spectra of ultracompact dwarf galaxies with our technique and demonstrated its applicability to real data. C1 [Podorvanyuk, Nikolay Yu.; Chilingarian, Igor V.; Katkov, Ivan Yu.] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia. [Chilingarian, Igor V.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Podorvanyuk, NY (reprint author), Moscow MV Lomonosov State Univ, Sternberg Astron Inst, 13 Univ Prospect, Moscow 119992, Russia. EM nicola@sai.msu.ru RI Katkov, Ivan/A-1867-2014; Chilingarian, Igor/N-5117-2016 OI Katkov, Ivan/0000-0002-6425-6879; Chilingarian, Igor/0000-0002-7924-3253 FU Russian Federation [MD-3288.2012.2]; Russian Foundation for Basic Research [12-02-31452]; M.V. Lomonosov Moscow State University Program of Development FX This work was supported by the Russian Federation President's grant MD-3288.2012.2, the Russian Foundation for Basic Research (project no. 12-02-31452) and the M.V. Lomonosov Moscow State University Program of Development. We thank the anonymous referee for valuable comments. IYK is grateful to Dmitry Zimin's non-profit Dynasty Foundation. NR 34 TC 2 Z9 2 U1 0 U2 0 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUL PY 2013 VL 432 IS 4 BP 2632 EP 2638 DI 10.1093/mnras/stt419 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 173BR UT WOS:000321053500002 ER PT J AU Martin, FA Blake, C Poole, GB McBride, CK Brough, S Colless, M Contreras, C Couch, W Croton, DJ Croom, S Davis, T Drinkwater, MJ Forster, K Gilbank, D Gladders, M Glazebrook, K Jelliffe, B Jurek, RJ Li, IH Madore, B Martin, DC Pimbblet, K Pracy, M Sharp, R Wisnioski, E Woods, D Wyder, TK Yee, HKC AF Martin, Felipe A. Blake, Chris Poole, Gregory B. McBride, Cameron K. Brough, Sarah Colless, Matthew Contreras, Carlos Couch, Warrick Croton, Darren J. Croom, Scott Davis, Tamara Drinkwater, Michael J. Forster, Karl Gilbank, David Gladders, Mike Glazebrook, Karl Jelliffe, Ben Jurek, Russell J. Li, I-hui Madore, Barry Martin, D. Christopher Pimbblet, Kevin Pracy, Michael Sharp, Rob Wisnioski, Emily Woods, David Wyder, Ted K. Yee, H. K. C. TI The WiggleZ Dark Energy Survey: constraining galaxy bias and cosmic growth with three-point correlation functions SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE methods: statistical; cosmological parameters; cosmology: observations; large-scale structure of; Universe ID LARGE-SCALE STRUCTURE; DIGITAL SKY SURVEY; LUMINOUS RED GALAXIES; BARYON ACOUSTIC-OSCILLATIONS; POWER-SPECTRUM ANALYSIS; REDSHIFT SURVEY; SDSS GALAXIES; STATISTICAL-ANALYSIS; COSMOLOGICAL IMPLICATIONS; COLOR DEPENDENCE AB Higher order statistics are a useful and complementary tool for measuring the clustering of galaxies, containing information on the non-Gaussian evolution and morphology of large-scale structure in the Universe. In this work we present measurements of the three-point correlation function (3PCF) for 187 000 galaxies in the WiggleZ spectroscopic galaxy survey. We explore the WiggleZ 3PCF scale and shape dependence at three different epochs z = 0.35, 0.55 and 0.68, the highest redshifts where these measurements have been made to date. Using N-body simulations to predict the clustering of dark matter, we constrain the linear and non-linear bias parameters of WiggleZ galaxies with respect to dark matter, and marginalize over them to obtain constraints on Sigma(8)(z), the variance of perturbations on a scale of 8 h(-1) Mpc and its evolution with redshift. These measurements of Sigma(8)(z), which have 10-20 per cent accuracies, are consistent with the predictions of the Lambda cold dark matter concordance cosmology and test this model in a new way. C1 [Martin, Felipe A.; Blake, Chris; Poole, Gregory B.; Contreras, Carlos; Couch, Warrick; Croton, Darren J.; Glazebrook, Karl; Pracy, Michael; Wisnioski, Emily] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122, Australia. [Poole, Gregory B.] Univ Melbourne, Sch Phys, Parksville, Vic 3010, Australia. [McBride, Cameron K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brough, Sarah; Colless, Matthew] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Croom, Scott; Jelliffe, Ben; Pracy, Michael] Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia. [Davis, Tamara; Drinkwater, Michael J.] Univ Queensland, Sch Math & Phys, Brisbane, Qld 4072, Australia. [Forster, Karl; Martin, D. Christopher; Wyder, Ted K.] CALTECH, Pasadena, CA 91125 USA. [Gilbank, David] S African Astron Observ, ZA-7935 Cape Town, South Africa. [Gladders, Mike] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Jurek, Russell J.] CSIRO, Australia Telescope Natl Facil, Epping, NSW 1710, Australia. [Li, I-hui; Yee, H. K. C.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Madore, Barry] Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. [Pimbblet, Kevin] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Sharp, Rob] Australian Natl Univ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia. [Wisnioski, Emily] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Woods, David] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Martin, FA (reprint author), Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia. EM fmarin@astro.swin.edu.au RI Drinkwater, Michael/A-2201-2008; Glazebrook, Karl/N-3488-2015; Davis, Tamara/A-4280-2008; OI Drinkwater, Michael/0000-0003-4867-0022; Glazebrook, Karl/0000-0002-3254-9044; Davis, Tamara/0000-0002-4213-8783; Colless, Matthew/0000-0001-9552-8075 FU Australian Research Council; Australian Research Council through a QEII Fellowship; Centre for All-sky Astrophysics, an Australian Research Council Centre of Excellence; [CE11000102] FX We thank Eyal Kazin for fruitful discussions and suggestions, and the anonymous referee for valuable comments and suggestions. We acknowledge financial support from the Australian Research Council through Discovery Project grants which have funded the positions of MP, GP, TD and FM. SMC acknowledges the support of the Australian Research Council through a QEII Fellowship. CB acknowledges the financial support of the ARC through a Future Fellowship award. We are also grateful for support from the Centre for All-sky Astrophysics, an Australian Research Council Centre of Excellence funded by grant CE11000102. NR 74 TC 36 Z9 36 U1 1 U2 8 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 JUL PY 2013 VL 432 IS 4 BP 2654 EP 2668 DI 10.1093/mnras/stt520 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 173BR UT WOS:000321053500005 ER PT J AU Forgan, D Kipping, D AF Forgan, Duncan Kipping, David TI Dynamical effects on the habitable zone for Earth-like exomoons SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE astrobiology; methods: numerical; planets and satellites: general ID EXTRASOLAR GIANT PLANETS; MOONS; EXOPLANETS; EVOLUTION; ORBITS; SATELLITES; CAPTURE; SYSTEMS; LIMITS; STARS AB With the detection of extrasolar moons (exomoons) on the horizon, it is important to consider their potential for habitability. If we consider the circumstellar habitable zone (HZ, often described in terms of planet semi-major axis and orbital eccentricity), we can ask, 'How does the HZ for an Earth-like exomoon differ from the HZ for an Earth-like exoplanet?' For the first time, we use 1D latitudinal energy balance modelling to address this question. The model places an Earth-like exomoon in an orbit around a Jupiter mass planet, which in turn orbits a Sun-like star. The exomoon's surface is decomposed into latitudinal strips, and the temperature of each strip is evolved under the action of stellar insolation, atmospheric cooling, heat diffusion, eclipses of the star by the planet and tidal heating. We use this model to carry out two separate investigations. In the first investigation, four test cases are run to investigate in detail the dependence of the exomoon climate on the orbital direction, orbital inclination and the frequency of the stellar eclipse by the host planet. We find that lunar orbits which are retrograde to the planetary orbit exhibit greater climate variations than prograde orbits, with global mean temperatures around 0.1 K higher due to the geometry of eclipses. If eclipses become frequent relative to the atmospheric thermal inertia time-scale, climate oscillations become extremely small. In the second investigation, we carry out an extensive parameter study, running the model many times to study the habitability of the exomoon in the four-dimensional space composed of the planet semi-major axis and eccentricity, and the moon semi-major axis and eccentricity. We find that for zero moon eccentricity, frequent eclipses allow the moon to remain habitable in regions of high planet eccentricity, but tidal heating severely constrains habitability in the limit of high moon eccentricity, making the HZ a sensitive function of the moon semi-major axis. C1 [Forgan, Duncan] Univ Edinburgh, Inst Astron, SUPA, Edinburgh EH9 3HJ, Midlothian, Scotland. [Kipping, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Forgan, D (reprint author), Univ Edinburgh, Inst Astron, SUPA, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland. EM dhf@roe.ac.uk OI Forgan, Duncan/0000-0003-1175-4388 FU STFC [ST/J001422/1]; NASA FX DF gratefully acknowledges support from the STFC grant ST/J001422/1. DMK is supported by the NASA Carl Sagan Fellowships. NR 43 TC 17 Z9 18 U1 0 U2 14 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 JUL PY 2013 VL 432 IS 4 BP 2994 EP 3004 DI 10.1093/mnras/stt662 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 173BR UT WOS:000321053500032 ER PT J AU Sanchez-Monge, A Palau, A Fontani, F Busquet, G Juarez, C Estalella, R Tan, JC Sepulveda, I Ho, PTP Zhang, QZ Kurtz, S AF Sanchez-Monge, Alvaro Palau, Aina Fontani, Francesco Busquet, Gemma Juarez, Carmen Estalella, Robert Tan, Jonathan C. Sepulveda, Inma Ho, Paul T. P. Zhang, Qizhou Kurtz, Stan TI Properties of dense cores in clustered massive star-forming regions at high angular resolution SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE stars: early-type; stars: formation; ISM: molecules; radio lines: ISM ID ULTRACOMPACT HII-REGIONS; YOUNG STELLAR OBJECTS; SPECTRAL ENERGY-DISTRIBUTION; (PROTO)STAR IRAS 20126+4104; HIGH-SPATIAL-RESOLUTION; INFRARED DARK CLOUDS; MOLECULAR CLOUDS; INITIAL CONDITIONS; PROTOSTELLAR CANDIDATES; IMAGING SURVEY AB We aim at characterizing dense cores in the clustered environments associated with intermediate-/high-mass star-forming regions. For this, we present a uniform analysis of Very Large Array NH3 (1,1) and (2,2) observations towards a sample of 15 intermediate-/high-mass star-forming regions, where we identify a total of 73 cores, classify them as protostellar, quiescent starless, or perturbed starless, and derive some physical properties. The average sizes and ammonia column densities of the total sample are similar to 0.06 pc and similar to 10(15) cm(-2), respectively, with no significant differences between the starless and protostellar cores, while the linewidth and rotational temperature of quiescent starless cores are smaller, similar to 1.0 km s(-1) and 16 K, than linewidths and temperatures of protostellar (similar to 1.8 km s(-1) and 21 K), and perturbed starless (similar to 1.4 km s(-1) and 19 K) cores. Such linewidths and temperatures for these quiescent starless cores in the surroundings of intermediate-/high-mass stars are still significantly larger than the typical linewidths and rotational temperatures measured in starless cores of low-mass star-forming regions, implying an important non-thermal component. We confirm at high angular resolutions (spatial scales similar to 0.05 pc) the correlations previously found with single-dish telescopes (spatial scales greater than or similar to 0.1 pc) between the linewidth and the rotational temperature of the cores, as well as between the rotational temperature and the linewidth with respect to the bolometric luminosity. In addition, we find a correlation between the temperature of each core and the incident flux from the most massive star in the cluster, suggesting that the large temperatures measured in the starless cores of our sample could be due to heating from the nearby massive star. A simple virial equilibrium analysis seems to suggest a scenario of a self-similar, self-gravitating, turbulent, virialized hierarchy of structures from clumps (similar to 0.1-10 pc) to cores (similar to 0.05 pc). A closer inspection of the dynamical state taking into account external pressure effects reveals that relatively strong magnetic field support may be needed to stabilize the cores, or that they are unstable and thus on the verge of collapse. C1 [Sanchez-Monge, Alvaro; Fontani, Francesco] Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. [Sanchez-Monge, Alvaro; Juarez, Carmen; Estalella, Robert; Sepulveda, Inma] Univ Barcelona, Dpt Astron & Meteorol IEEC UB, ICC, E-08028 Barcelona, Spain. [Palau, Aina; Juarez, Carmen] Inst Ciencies & Espai CSIC IEEC, Fac Ciencies, E-08193 Barcelona, Spain. [Busquet, Gemma] INAF Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Tan, Jonathan C.] Univ Florida, Dept Phys & Astron, Gainesville, FL 32611 USA. [Ho, Paul T. P.] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Ho, Paul T. P.; Zhang, Qizhou] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kurtz, Stan] Univ Nacl Autonoma Mexico, Ctr Radioastron & Astrofs, Morelia 58090, Michoacan, Mexico. RP Sanchez-Monge, A (reprint author), Osserv Astrofis Arcetri, INAF, Largo Enrico Fermi 5, I-50125 Florence, Italy. EM asanchez@arcetri.astro.it OI Fontani, Francesco/0000-0003-0348-3418; Zhang, Qizhou/0000-0003-2384-6589 FU JAE-Doc CSIC fellowship; European Social Fund under the programme 'Junta para la Ampliacion de Estudios', by the Spanish MICINN [AYA2011-30228-C03-02]; FEDER; AGAUR grant (Catalonia) [2009SGR1172]; Italian Space Agency (ASI) fellowship [I/005/11/0] FX We are grateful to James di Francesco for support with SCUBA data. We thank the anonymous referee for his/her constructive criticisms. The figures of this paper have been done in GREG of the GILDAS software package developed at the Institut de Radioastronomie Millimetrique (IRAM) and the Observatoire de Grenoble. AP is supported by a JAE-Doc CSIC fellowship co-funded with the European Social Fund under the programme 'Junta para la Ampliacion de Estudios', by the Spanish MICINN grant AYA2011-30228-C03-02 (co-funded with FEDER funds), and by the AGAUR grant 2009SGR1172 (Catalonia). GB is funded by an Italian Space Agency (ASI) fellowship under contract number I/005/11/0. NR 109 TC 24 Z9 24 U1 0 U2 4 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 PY 2013 VL 432 IS 4 BP 3288 EP 3319 DI 10.1093/mnras/stt679 PG 32 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 173BR UT WOS:000321053500056 ER PT J AU Harkey, MA Asano, A Zoulas, ME Torok-Storb, B Nagashima, J Travis, A AF Harkey, Michael A. Asano, Atsushi Zoulas, Mary Ellen Torok-Storb, Beverly Nagashima, Jennifer Travis, Alexander TI Isolation, genetic manipulation, and transplantation of canine spermatogonial stem cells: progress toward transgenesis through the male germ-line SO REPRODUCTION LA English DT Article ID ADULT-MOUSE TESTIS; IN-VITRO; SELF-RENEWAL; TESTICULAR CELLS; RHESUS MACAQUES; GROWTH-FACTORS; KNOCKOUT MICE; BONE-MARROW; DOG-MODELS; CULTURE AB The dog is recognized as a highly predictive model for preclinical research. Its size, life span, physiology, and genetics more closely match human parameters than do those of the mouse model. Investigations of the genetic basis of disease and of new regenerative treatments have frequently taken advantage of canine models. However, full utility of this model has not been realized because of the lack of easy transgenesis. Blastocyst-mediated transgenic technology developed in mice has been very slow to translate to larger animals, and somatic cell nuclear transfer remains technically challenging, expensive, and low yield. Spermatogonial stem cell (SSC) transplantation, which does not involve manipulation of ova or blastocysts, has proven to be an effective alternative approach for generating transgenic offspring in rodents and in some large animals. Our recent demonstration that canine testis cells can engraft in a host testis, and generate donor-derived sperm, suggests that SSC transplantation may offer a similar avenue to transgenesis in the canine model. Here, we explore the potential of SSC transplantation in dogs as a means of generating canine transgenic models for preclinical models of genetic diseases. Specifically, we i) established markers for identification and tracking canine spermatogonial cells; ii) established methods for enrichment and genetic manipulation of these cells; iii) described their behavior in culture; and iv) demonstrated engraftment of genetically manipulated SSC and production of transgenic sperm. These findings help to set the stage for generation of transgenic canine models via SSC transplantation. C1 [Harkey, Michael A.; Torok-Storb, Beverly] Fred Hutchinson Canc Res Ctr, Seattle, WA 98109 USA. [Asano, Atsushi; Nagashima, Jennifer; Travis, Alexander] Cornell Univ, Coll Vet Med, Baker Inst Anim Hlth, Ithaca, NY 14853 USA. [Asano, Atsushi; Nagashima, Jennifer; Travis, Alexander] Smithsonian Conservat Biol Inst, Natl Zool Pk, Joint Grad Training Program, Washington, DC 20008 USA. [Zoulas, Mary Ellen] Seattle Anim Shelter Spay & Neuter Clin, W Seattle, WA 98119 USA. RP Harkey, MA (reprint author), Fred Hutchinson Canc Res Ctr, Mail Stop D1-100,1100 Fairview Ave North,POB 1902, Seattle, WA 98109 USA. EM mharkey@fhcrc.org FU Northwest Genome Engineering Consortium [20003812]; NIH [1-UL1-RR024921-01, NHBLI-1-RC1-HL100270-01, 3P30DK056465-11S2] FX This work was supported in part by Pilot grant 20003812 from the Northwest Genome Engineering Consortium (NIH grant 1-UL1-RR024921-01) and by NIH Challenge grant: NHBLI-1-RC1-HL100270-01.; The authors acknowledge the services of the Core Center of Excellence in Hematology (funded by NIH grant 3P30DK056465-11S2) for provision of canine mRNAs and reporter constructs, as well as design of RT-PCR primers and isolation of DNA and RNA samples. The authors thank Dr Margaret McEntee and her staff at the Jane M Turrel Radiation Therapy Suite at Cornell's College of Veterinary Medicine for their generous assistance with recipient preparation. They also thank Deborah Higginbotham, Gretchen Johnson, Emily Meyer, and Darlene John for technical assistance. They also thank Bonnie Larson and Helen Crawford for assistance with the preparation and editing of the manuscript. NR 99 TC 4 Z9 4 U1 1 U2 15 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 2013 VL 146 IS 1 BP 75 EP 90 DI 10.1530/REP-13-0086 PG 16 WC Developmental Biology; Reproductive Biology SC Developmental Biology; Reproductive Biology GA 175OL UT WOS:000321239900010 PM 23690628 ER PT J AU Young, HS McCauley, DJ Helgen, KM Goheen, JR Otarola-Castillo, E Palmer, TM Pringle, RM Young, TP Dirzo, R AF Young, Hillary S. McCauley, Douglas J. Helgen, Kristofer M. Goheen, Jacob R. Otarola-Castillo, Erik Palmer, Todd M. Pringle, Robert M. Young, Truman P. Dirzo, Rodolfo TI Effects of mammalian herbivore declines on plant communities: observations and experiments in an African savanna SO JOURNAL OF ECOLOGY LA English DT Article DE abiotic gradients; community structure; East Africa; exclosure experiment; herbivory; livestock-wildlife interactions; plant species richness; plant-herbivore interactions; wildlife decline ID ECOSYSTEM PROCESSES; DIVERSITY DEPENDS; TALLGRASS PRAIRIE; SEMIARID SAVANNA; LAND-USE; CATTLE; SCALE; PRODUCTIVITY; LIVESTOCK; UNGULATE AB Herbivores influence the structure and composition of terrestrial plant communities. However, responses of plant communities to herbivory are variable and depend on environmental conditions, herbivore identity and herbivore abundance. As anthropogenic impacts continue to drive large declines in wild herbivores, understanding the context dependence of herbivore impacts on plant communities becomes increasingly important. Exclosure experiments are frequently used to assess how ecosystems reorganize in the face of large wild herbivore defaunation. Yet in many landscapes, declines in large wildlife are often accompanied by other anthropogenic activities, especially land conversion to livestock production. In such cases, exclosure experiments may not reflect typical outcomes of human-driven extirpations of wild herbivores. Here, we examine how plant community responses to changes in the identity and abundance of large herbivores interact with abiotic factors (rainfall and soil properties). We also explore how effects of wild herbivores on plant communities differ between large-scale herbivore exclosures and landscape sites where anthropogenic activity has caused wildlife declines, often accompanied by livestock increases. Abiotic context modulated the responses of plant communities to herbivore declines with stronger effect sizes in lower-productivity environments. Also, shifts in plant community structure, composition and species richness following wildlife declines differed considerably between exclosure experiments and landscape sites in which wild herbivores had declined and were often replaced by livestock. Plant communities in low wildlife landscape sites were distinct in both composition and physical structure from both exclosure and control sites in experiments. The power of environmental (soil and rainfall) gradients in influencing plant response to herbivores was also greatly dampened or absent in the landscape sites. One likely explanation for these observed differences is the compensatory effect of livestock associated with the depression or extirpation of wildlife. Synthesis. Our results emphasize the importance of abiotic environmental heterogeneity in modulating the effects of mammalian herbivory on plant communities and the importance of such covariation in understanding effects of wild herbivore declines. They also suggest caution when extrapolating results from exclosure experiments to predict the consequences of defaunation as it proceeds in the Anthropocene. C1 [Young, Hillary S.; Helgen, Kristofer M.] Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. [Young, Hillary S.; Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Young, Hillary S.; McCauley, Douglas J.; Goheen, Jacob R.; Palmer, Todd M.; Pringle, Robert M.; Young, Truman P.] Mpala Res Ctr, Nanyuki, Kenya. [Young, Hillary S.] Harvard Univ, Ctr Environm, Cambridge, MA 02138 USA. [McCauley, Douglas J.] Univ Calif Berkeley, Dept Environm Sci Policy & Management, Berkeley, CA 94720 USA. [Goheen, Jacob R.] Univ Wyoming, Dept Zool & Physiol, Laramie, WY 82071 USA. [Otarola-Castillo, Erik] Harvard Univ, Dept Human Evolutionary Biol, Cambridge, MA 02138 USA. [Otarola-Castillo, Erik] Iowa State Univ, Dept Ecol Evolut & Organismal Biol, Ames, IA 50010 USA. [Palmer, Todd M.] Univ Florida, Dept Zool, Gainesville, FL 32611 USA. [Pringle, Robert M.] Princeton Univ, Dept Ecol & Evolutionary Biol, Princeton, NJ 08544 USA. [Young, Truman P.] Univ Calif Davis, Dept Plant Sci, Davis, CA 95616 USA. RP Young, HS (reprint author), Smithsonian Inst, Div Mammals, Washington, DC 20013 USA. EM younghs@si.edu OI Palmer, Todd/0000-0001-5710-9750 FU Stanford's Woods Institute for the Environment; James Smithson Fund of the Smithsonian Institution; National Geographic Society [4691-91, 8846-10, 9106-12]; National Science Foundation [LTREB BSR-97-07477, 03-16402, 08-16453, DEB-09-09670]; Natural Sciences and Engineering Council of Canada; African Elephant Program of the U.S. Fish and Wildlife Service [98210-0-G563]; Smithsonian Institution Women's Committee [SWC 44] FX This research is facilitated by grants from Stanford's Woods Institute for the Environment, the James Smithson Fund of the Smithsonian Institution (to A.P. Smith), the National Geographic Society (Grants 4691-91, 8846-10, 9106-12), the National Science Foundation (LTREB BSR-97-07477, 03-16402, 08-16453, DEB-09-09670), the Natural Sciences and Engineering Council of Canada, the African Elephant Program of the U.S. Fish and Wildlife Service (98210-0-G563) and the Smithsonian Institution Women's Committee (SWC 44). For assistance in the field, we thank Cara Brook, Jack Silanje, Peter Lokeny, Everlyn Ndinda, Frederick Erii, John Lochikuya, Matthew Namoni, Jackson Ekadeli, Abdikadir Ali Hassan, Simon Lima and Patrick Etelej. We also thank the Kenyan Government, Mpala Research Centre, Ol Jogi Ranch, Ol Pejeta Ranch, Segera Ranch, Ol Maisor Ranch, and Lekiji, Il Motiok, Koija, Lododo, Narok, Il Polei, Thome, Marura and Kimugandura communities for facilitating this research. We thank two anonymous reviewers for their careful revisions, which greatly improved this manuscript. The authors declare no conflicts of interest. NR 62 TC 28 Z9 29 U1 9 U2 123 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-0477 J9 J ECOL JI J. Ecol. PD JUL PY 2013 VL 101 IS 4 BP 1030 EP 1041 DI 10.1111/1365-2745.12096 PG 12 WC Plant Sciences; Ecology SC Plant Sciences; Environmental Sciences & Ecology GA 171OG UT WOS:000320938100020 ER PT J AU Rowcliffe, JM Kays, R Carbone, C Jansen, PA AF Rowcliffe, J. Marcus Kays, Roland Carbone, Chris Jansen, Patrick A. TI Clarifying assumptions behind the estimation of animal density from camera trap rates SO JOURNAL OF WILDLIFE MANAGEMENT LA English DT Letter C1 [Rowcliffe, J. Marcus; Carbone, Chris] ZSL Inst Zool, London NW 4RY, England. [Kays, Roland] North Caolina Museum Nat Sci, Nat Res Ctr, Raleigh, NC 27601 USA. [Kays, Roland] N Carolina State Univ, Fisheries Wildlife & Conservat Program, Raleigh, NC 27695 USA. [Jansen, Patrick A.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. Wageningen Univ, Dept Environm Sci, NL-6700 AA Wageningen, Netherlands. RP Rowcliffe, JM (reprint author), ZSL Inst Zool, Regents Pk, London NW 4RY, England. EM marcus.rowcliffe@ioz.ac.uk RI Jansen, Patrick/G-2545-2015 OI Jansen, Patrick/0000-0002-4660-0314 NR 5 TC 11 Z9 12 U1 5 U2 98 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0022-541X EI 1937-2817 J9 J WILDLIFE MANAGE JI J. Wildl. Manage. PD JUL PY 2013 VL 77 IS 5 BP 876 EP 876 DI 10.1002/jwmg.533 PG 1 WC Ecology; Zoology SC Environmental Sciences & Ecology; Zoology GA 171NV UT WOS:000320937000002 ER PT J AU Ashford, OS Foster, WA Turner, BL Sayer, EJ Sutcliffe, L Tanner, EVJ AF Ashford, O. S. Foster, W. A. Turner, B. L. Sayer, E. J. Sutcliffe, L. Tanner, E. V. J. TI Litter manipulation and the soil arthropod community in a lowland tropical rainforest SO SOIL BIOLOGY & BIOCHEMISTRY LA English DT Article DE Litter manipulation; Soil fauna; Neotropics; Community composition; Chemical parameters; Physical parameters ID HIGHER-TAXON RICHNESS; SPECIES RICHNESS; EXPERIMENTAL PERTURBATIONS; NUTRIENT CONCENTRATIONS; DECIDUOUS FOREST; DIVERSITY; ECOSYSTEM; INVERTEBRATES; ABUNDANCE; QUALITY AB Tropical soil arthropod communities are highly diverse and provide a number of important ecosystem services, including the maintenance of soil structure, regulation of hydrological processes, nutrient cycling and decomposition. Experiments in temperate regions suggest that litter dynamics are important in determining the abundance, richness and community composition of soil fauna, but there is little information for lowland tropical forests. We used a long-term litter manipulation experiment (removing, doubling and control) in a neotropical forest to investigate the consequences of changing litter dynamics on the soil arthropod community. The abundance and biomass of arthropods were reduced significantly by the removal of litter, but not affected by litter addition. Litter manipulation had no effect on simple measures of taxonomic richness or diversity, but multivariate ordination techniques revealed a significant shift in arthropod community composition with the removal, but not addition, of litter. This suggests the overall importance of top-down controls on the arthropod community in this ecosystem, with bottom-up influences only important following the removal of large quantities of litter. Of the parameters measured, the faunal composition of experimental plots was best predicted by litter depth and the concentrations of total carbon and readily-exchangeable phosphorus (in order of importance), highlighting the influential role of soil chemical properties, in addition to the physical properties of litter, in shaping soil arthropod communities. Comparison with the results of a previous study of litter-dwelling fauna in the same litter manipulation experiment suggested that the soil and litter arthropod communities are influenced by different parameters: total carbon and litter depth for the soil community, but sodium and calcium for the litter community, although phosphorus was important in both environments. We conclude that arthropod community composition is controlled by different factors in the soil than in the litter and is affected by decreasing, but not increasing, depth of litter. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ashford, O. S.; Foster, W. A.; Sutcliffe, L.] Univ Cambridge, Dept Zool, Cambridge CB2 3EJ, England. [Tanner, E. V. J.] Univ Cambridge, Dept Plant Sci, Cambridge CB2 3EA, England. [Turner, B. L.] Smithsonian Trop Res Inst, Balboa 084303092, Ancon, Panama. [Sayer, E. J.] Open Univ, Dept Environm Earth & Ecosyst, Milton Keynes MK7 6AA, Bucks, England. RP Ashford, OS (reprint author), 10 Church Lane, Chichester PO18 9LH, W Sussex, England. EM osa22@cantab.net RI Turner, Benjamin/E-5940-2011; Sayer, Emma/B-2514-2010 OI Turner, Benjamin/0000-0002-6585-0722; Sayer, Emma/0000-0002-3322-4487 NR 62 TC 12 Z9 14 U1 14 U2 96 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0038-0717 J9 SOIL BIOL BIOCHEM JI Soil Biol. Biochem. PD JUL PY 2013 VL 62 BP 5 EP 12 DI 10.1016/j.soilbio.2013.03.001 PG 8 WC Soil Science SC Agriculture GA 164QY UT WOS:000320425800002 ER PT J AU de Queiroz, K AF de Queiroz, Kevin TI Nodes, Branches, and Phylogenetic Definitions SO SYSTEMATIC BIOLOGY LA English DT Article ID TAXON NAMES; SYSTEMATICS C1 [de Queiroz, Kevin] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. RP de Queiroz, K (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Div Amphibians & Reptiles, NHB, POB 37012,WG 7,MRC 162, Washington, DC 20013 USA. EM dequeirozk@si.edu NR 21 TC 1 Z9 1 U1 3 U2 14 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1063-5157 J9 SYST BIOL JI Syst. Biol. PD JUL PY 2013 VL 62 IS 4 BP 625 EP 632 DI 10.1093/sysbio/syt027 PG 8 WC Evolutionary Biology SC Evolutionary Biology GA 164IJ UT WOS:000320402300010 PM 23619174 ER PT J AU Strait, DS Constantino, P Lucas, PW Richmond, BG Spencer, MA Dechow, PC Ross, CF Grosse, IR Wright, BW Wood, BA Weber, GW Wang, Q Byron, C Slice, DE Chalk, J Smith, AL Smith, LC Wood, S Berthaume, M Benazzi, S Dzialo, C Tamvada, K Ledogar, JA AF Strait, David S. Constantino, Paul Lucas, Peter W. Richmond, Brian G. Spencer, Mark A. Dechow, Paul C. Ross, Callum F. Grosse, Ian R. Wright, Barth W. Wood, Bernard A. Weber, Gerhard W. Wang, Qian Byron, Craig Slice, Dennis E. Chalk, Janine Smith, Amanda L. Smith, Leslie C. Wood, Sarah Berthaume, Michael Benazzi, Stefano Dzialo, Christine Tamvada, Kelli Ledogar, Justin A. TI Viewpoints: Diet and dietary adaptations in early hominins: The hard food perspective SO AMERICAN JOURNAL OF PHYSICAL ANTHROPOLOGY LA English DT Article DE Australopithecus; Paranthropus; microwear; carbon isotope; biomechanics ID FINITE-ELEMENT-ANALYSIS; DENTAL MICROWEAR TEXTURE; VIVO BONE STRAIN; AUSTRALOPITHECUS-AFRICANUS; FUNCTIONAL-MORPHOLOGY; ISOTOPIC EVIDENCE; MOLAR MICROWEAR; FALLBACK FOODS; EARLY HOMO; GEOMETRIC MORPHOMETRICS AB Recent biomechanical analyses examining the feeding adaptations of early hominins have yielded results consistent with the hypothesis that hard foods exerted a selection pressure that influenced the evolution of australopith morphology. However, this hypothesis appears inconsistent with recent reconstructions of early hominin diet based on dental microwear and stable isotopes. Thus, it is likely that either the diets of some australopiths included a high proportion of foods these taxa were poorly adapted to consume (i.e., foods that they would not have processed efficiently), or that aspects of what we thought we knew about the functional morphology of teeth must be wrong. Evaluation of these possibilities requires a recognition that analyses based on microwear, isotopes, finite element modeling, and enamel chips and cracks each test different types of hypotheses and allow different types of inferences. Microwear and isotopic analyses are best suited to reconstructing broad dietary patterns, but are limited in their ability to falsify specific hypotheses about morphological adaptation. Conversely, finite element analysis is a tool for evaluating the mechanical basis of form-function relationships, but says little about the frequency with which specific behaviors were performed or the particular types of food that were consumed. Enamel chip and crack analyses are means of both reconstructing diet and examining biomechanics. We suggest that current evidence is consistent with the hypothesis that certain derived australopith traits are adaptations for consuming hard foods, but that australopiths had generalized diets that could include high proportions of foods that were both compliant and tough. Am J Phys Anthropol 151:339-355, 2013.(c) 2013 Wiley Periodicals, Inc. C1 [Strait, David S.; Smith, Amanda L.; Tamvada, Kelli; Ledogar, Justin A.] SUNY Albany, Dept Anthropol, Albany, NY 12222 USA. [Constantino, Paul] Marshall Univ, Dept Biol Sci, Huntington, WV 25755 USA. [Lucas, Peter W.] Kuwait Univ, Fac Dent, Dept Bioclin Sci, Kuwait, Kuwait. [Richmond, Brian G.; Wood, Bernard A.] George Washington Univ, Dept Anthropol, Ctr Adv Study Hominid Paleobiol, Washington, DC 20052 USA. [Richmond, Brian G.; Wood, Bernard A.] Smithsonian Inst, Natl Museum Nat Hist, Human Origins Program, Washington, DC 20560 USA. [Spencer, Mark A.] Arizona State Univ, Inst Human Origins, Sch Human Evolut & Social Change, Tempe, AZ 85287 USA. [Dechow, Paul C.; Smith, Leslie C.] Baylor Coll Dent, Texas A&M Hlth Sci Ctr, Dept Biomed Sci, Dallas, TX 75246 USA. [Ross, Callum F.] Univ Chicago, Dept Organismal Biol & Anat, Chicago, IL 60637 USA. [Grosse, Ian R.; Wood, Sarah; Berthaume, Michael; Dzialo, Christine] Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. [Wright, Barth W.] Kansas City Univ Med & Biosci, Dept Anat, Kansas City, MO 64106 USA. [Weber, Gerhard W.] Univ Vienna, Dept Anthropol, A-1090 Vienna, Austria. [Wang, Qian] Mercer Univ, Sch Med, Div Basic Med Sci, Macon, GA 31207 USA. [Byron, Craig] Mercer Univ, Dept Biol, Macon, GA 31207 USA. [Slice, Dennis E.] Florida State Univ, Sch Computat Sci, Tallahassee, FL 32306 USA. [Slice, Dennis E.] Florida State Univ, Dept Biol Sci, Tallahassee, FL 32306 USA. [Chalk, Janine] Duke Univ, Dept Evolutionary Anthropol, Durham, NC 27708 USA. [Benazzi, Stefano] Max Planck Inst Evolutionary Anthropol, Dept Human Evolut, D-04103 Leipzig, Germany. RP Strait, DS (reprint author), SUNY Albany, Dept Anthropol, 1400 Washington Ave, Albany, NY 12222 USA. EM dstrait@albany.edu RI Weber, Gerhard/F-2583-2010; OI Benazzi, Stefano/0000-0003-4305-6920 FU National Science Foundation Physical Anthropology HOMINID program [NSF BCS 0725219, 0725183, 0725147, 0725141, 0725136, 0725126, 0725122, 0725078]; EU [MRTN-CT-2005-019564 "EVAN"] FX Grant sponsor: National Science Foundation Physical Anthropology HOMINID program; Grant numbers: NSF BCS 0725219, 0725183, 0725147, 0725141, 0725136, 0725126, 0725122, and 0725078; Grant sponsor: EU FP6 Marie Curie Actions; Grant number: MRTN-CT-2005-019564 "EVAN." NR 124 TC 25 Z9 26 U1 11 U2 112 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0002-9483 J9 AM J PHYS ANTHROPOL JI Am. J. Phys. Anthropol. PD JUL PY 2013 VL 151 IS 3 BP 339 EP 355 DI 10.1002/ajpa.22285 PG 17 WC Anthropology; Evolutionary Biology SC Anthropology; Evolutionary Biology GA 169JC UT WOS:000320775300003 PM 23794330 ER PT J AU Adams, ER Dupree, AK Kulesa, C McCarthy, D AF Adams, E. R. Dupree, A. K. Kulesa, C. McCarthy, D. TI ADAPTIVE OPTICS IMAGES. II. 12 KEPLER OBJECTS OF INTEREST AND 15 CONFIRMED TRANSITING PLANETS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: general; instrumentation: adaptive optics; planets and satellites: detection ID HOT JUPITER; STAR; CANDIDATES; SUPERWASP AB All transiting planet observations are at risk of contamination from nearby, unresolved stars. Blends dilute the transit signal, causing the planet to appear smaller than it really is, or producing a false positive detection when the target star is blended with an eclipsing binary. High spatial resolution adaptive optics images are an effective way of resolving most blends. Here we present visual companions and detection limits for 12 Kepler planet candidate host stars, of which 4 have companions within 4 ''. One system (KOI 1537) consists of two similar-magnitude stars separated by 0 ''.1, while KOI 174 has a companion at 0 ''.5. In addition, observations were made of 15 transiting planets that were previously discovered by other surveys. The only companion found within 1 '' of a known planet is the previously identified companion to WASP-2b. An additional four systems have companions between 1 '' and 4 '': HAT-P-30b (3 ''.7, Delta Ks = 2.9), HAT-P-32b (2 ''.9, Delta Ks = 3.4), TrES-1b (2 ''.3, Delta Ks = 7.7), and WASP-P-33b (1 ''.9, Delta Ks = 5.5), some of which have not been reported previously. Depending on the spatial resolution of the transit photometry for these systems, these companion stars may require a reassessment of the planetary parameters derived from transit light curves. For all systems observed, we report the limiting magnitudes beyond which additional fainter objects located 0 ''.1-4 '' from the target may still exist. C1 [Adams, E. R.; Dupree, A. K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kulesa, C.; McCarthy, D.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Adams, ER (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. FU NASA [NNX10AK54A] FX Authors gratefully acknowledge partial support from NASA grant NNX10AK54A. Thanks also go to David Ciardi for coordination of the Kepler Follow-on Program (KFOP), and to Steve Bryson for helpful conversations about centroid offsets. We thank an anonymous referee for suggested improvements. NR 18 TC 35 Z9 35 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 JUL PY 2013 VL 146 IS 1 AR UNSP 9 DI 10.1088/0004-6256/146/1/9 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166JP UT WOS:000320551000009 ER PT J AU Zhang, ZW Lehner, MJ Wang, JH Wen, CY Wang, SY King, SK Granados, AP Alcock, C Axelrod, T Bianco, FB Byun, YI Chen, WP Coehlo, NK Cook, KH de Pater, I Kim, DW Lee, T Lissauer, JJ Marshall, SL Protopapas, P Rice, JA Schwamb, ME AF Zhang, Z. -W. Lehner, M. J. Wang, J. -H. Wen, C. -Y. Wang, S. -Y. King, S. -K. Granados, A. P. Alcock, C. Axelrod, T. Bianco, F. B. Byun, Y. -I. Chen, W. P. Coehlo, N. K. Cook, K. H. de Pater, I. Kim, D. -W. Lee, T. Lissauer, J. J. Marshall, S. L. Protopapas, P. Rice, J. A. Schwamb, M. E. TI THE TAOS PROJECT: RESULTS FROM SEVEN YEARS OF SURVEY DATA SO ASTRONOMICAL JOURNAL LA English DT Article DE comets: general; Kuiper Belt: general; occultations; planets and satellites: formation ID KUIPER-BELT OBJECTS; JUPITER-FAMILY COMETS; TRANS-NEPTUNIAN OBJECTS; OUTER SOLAR-SYSTEM; AMERICAN OCCULTATION SURVEY; SIZE DISTRIBUTION; STELLAR OCCULTATIONS; COLLISIONAL EVOLUTION; LUMINOSITY FUNCTION; MILLISECOND DIPS AB The Taiwanese-American Occultation Survey (TAOS) aims to detect serendipitous occultations of stars by small (similar to 1 km diameter) objects in the Kuiper Belt and beyond. Such events are very rare (<10(-3) events per star per year) and short in duration (similar to 200 ms), so many stars must be monitored at a high readout cadence. TAOS monitors typically similar to 500 stars simultaneously at a 5 Hz readout cadence with four telescopes located at Lulin Observatory in central Taiwan. In this paper, we report the results of the search for small Kuiper Belt objects (KBOs) in seven years of data. No occultation events were found, resulting in a 95% c. l. upper limit on the slope of the faint end of the KBO size distribution of q = 3.34-3.82, depending on the surface density at the break in the size distribution at a diameter of about 90 km. C1 [Zhang, Z. -W.; Lehner, M. J.; Wang, J. -H.; Wen, C. -Y.; Wang, S. -Y.; King, S. -K.; Cook, K. H.; Lee, T.] Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, Taipei 10617, Taiwan. [Lehner, M. J.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Lehner, M. J.; Alcock, C.; Protopapas, P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Granados, A. P.] Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico. [Axelrod, T.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Bianco, F. B.] NYU, Ctr Cosmol & Particle Phys, New York, NY 10003 USA. [Byun, Y. -I.] Yonsei Univ, Dept Astron, Seoul 120749, South Korea. [Byun, Y. -I.] Yonsei Univ, Univ Observ, Seoul 120749, South Korea. [Chen, W. P.] Natl Cent Univ, Inst Astron, Jhongli 320, Taoyuan County, Taiwan. [Coehlo, N. K.; Rice, J. A.] Univ Calif Berkeley, Dept Stat, Berkeley, CA 94720 USA. [de Pater, I.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Kim, D. -W.] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Lissauer, J. J.] NASA, Space Sci & Astrobiol Div 245 3, Ames Res Ctr, Moffett Field, CA 94035 USA. [Marshall, S. L.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [Protopapas, P.] Harvard Univ, Initiat Innovat Comp, Cambridge, MA 02138 USA. [Schwamb, M. E.] Yale Univ, Dept Phys, New Haven, CT 06511 USA. [Schwamb, M. E.] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. RP Zhang, ZW (reprint author), Natl Taiwan Univ, Acad Sinica, Inst Astron & Astrophys, 11F Astron Math Bldg,1,Sec 4,Roosevelt Rd, Taipei 10617, Taiwan. EM zwzhang@asiaa.sinica.edu.tw RI Lee, Typhoon/N-8347-2013; OI Lehner, Matthew/0000-0003-4077-0985; Schwamb, Megan/0000-0003-4365-1455 FU thematic research program [AS-88-TP-A02]; NSF [AST-0501681, DMS-0636667]; NASA [NNG04G113G]; NRF [2011-0030875]; USDOE [DE-AC02-76SF00515]; NASA's Planetary Geology and Geophysics Program; [NSC101-2628-M-008-002]; [NSC 96-2112-M-008-024-MY3] FX Work at ASIAA was supported in part by the thematic research program AS-88-TP-A02. Work at NCU and at Lulin Observatory was supported in part by grant NSC101-2628-M-008-002. Work at the CfA was supported in part by the NSF under grant AST-0501681 and by NASA under grant NNG04G113G. Work at Yonsei was supported by the NRF grant 2011-0030875. Work at NCU was supported by the grant NSC 96-2112-M-008-024-MY3. Work at Berkeley was supported in part by NSF grant DMS-0636667. Work at SLAC was performed under USDOE contract DE-AC02-76SF00515. Work at NASA Ames was supported by NASA's Planetary Geology and Geophysics Program. NR 56 TC 14 Z9 14 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 J9 ASTRON J JI Astron. J. PD JUL PY 2013 VL 146 IS 1 AR 14 DI 10.1088/0004-6256/146/1/14 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 166JP UT WOS:000320551000014 ER PT J AU Nottingham, AT Turner, BL Winter, K Chamberlain, PM Stott, A Tanner, EVJ AF Nottingham, Andrew T. Turner, Benjamin L. Winter, Klaus Chamberlain, Paul M. Stott, Andrew Tanner, Edmund V. J. TI Root and arbuscular mycorrhizal mycelial interactions with soil microorganisms in lowland tropical forest SO FEMS MICROBIOLOGY ECOLOGY LA English DT Article DE arbuscular mycorrhizal fungi; hydrolytic enzymes; phospholipid fatty acids; Pseudobombax septenatum; soil microorganisms; soil organic matter; tropical forest ID FUNGUS GLOMUS-INTRARADICES; MICROBIAL BIOMASS-C; ORGANIC-MATTER; COMMUNITY STRUCTURE; RAIN-FOREST; LITTER DECOMPOSITION; CARBON DECOMPOSITION; ELEVATED CO2; RHIZOSPHERE; PLANT AB Tropical forests have high rates of soil carbon cycling, but little information is available on how roots, arbuscular mycorrhizal fungi (AMF), and free-living microorganisms interact and influence organic matter mineralization in these ecosystems. We used mesh ingrowth cores and isotopic tracers in phospholipid fatty acid biomarkers to investigate the effects of roots and AMF mycelia on (1) microbial community composition, microbial carbon utilization, and hydrolytic enzyme activities for large, potted tropical trees and (2) enzyme activities and litter mass loss in a lowland tropical forest. Under the tropical tree, plant-derived carbon was incorporated predominantly into bacterial groups in both rhizosphere and AMF-only soils. Gram-positive bacteria incorporated additional soil-derived carbon in rhizosphere soils, which also contained the highest microbial biomass. For hydrolytic enzymes, -glucosidase and N-acetyl -glucosaminidase activities were highest in rhizosphere soils, while phosphomonoesterase activity was highest in AMF-only soil. In the forest, leaf litter mass loss was increased by the presence of roots, but not by the presence of AMF mycelia only. Root-microbial interactions influenced organic matter cycling, with evidence for rhizosphere priming and accelerated leaf litter decomposition in the presence of roots. Although AMF mycelia alone did not stimulate organic matter mineralization, they were a conduit of carbon to other soil microorganisms. C1 [Nottingham, Andrew T.; Tanner, Edmund V. J.] Univ Cambridge, Dept Plant Sci, Cambridge, England. [Turner, Benjamin L.; Winter, Klaus] Smithsonian Trop Res Inst, Panama City, Panama. [Chamberlain, Paul M.; Stott, Andrew] Lancaster Environm Ctr, Ctr Ecol & Hydrol, Lancaster, England. RP Nottingham, AT (reprint author), Univ Edinburgh, Sch Geosci, Drummond St, Edinburgh EH8 9XP, Midlothian, Scotland. EM anotting@staffmail.ed.ac.uk RI Turner, Benjamin/E-5940-2011; STOTT, ANDREW /I-7920-2012 OI Turner, Benjamin/0000-0002-6585-0722; FU NERC [NER/S/A/2004/12241A]; Smithsonian Tropical Research Institute FX We thank Jorge Aranda, Lucas Cernusak, Scott Mangan, Catherine Potvin, Ludo Luckerhoff, Tania Romero, Emma Sayer, Michael Tobin, and Didimo Urena for their support. We thank two anonymous reviewers for comments on an early draft of the manuscript. The project was funded by a NERC grant (NER/S/A/2004/12241A) and a Smithsonian Tropical Research Institute Short-Term Fellowship to ATN. NR 90 TC 11 Z9 14 U1 7 U2 171 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0168-6496 EI 1574-6941 J9 FEMS MICROBIOL ECOL JI FEMS Microbiol. Ecol. PD JUL PY 2013 VL 85 IS 1 BP 37 EP 50 DI 10.1111/1574-6941.12096 PG 14 WC Microbiology SC Microbiology GA 166LQ UT WOS:000320556500004 PM 23406337 ER PT J AU Young, HS McCauley, DJ Guevara, R Dirzo, R AF Young, Hillary S. McCauley, Douglas J. Guevara, Roger Dirzo, Rodolfo TI Consumer preference for seeds and seedlings of rare species impacts tree diversity at multiple scales SO OECOLOGIA LA English DT Article DE Plant-herbivore interactions; Plant diversity; Density dependence; Seed predation; Seedling predation ID JANZEN-CONNELL MODEL; DENSITY-DEPENDENCE; TROPICAL FORESTS; RAIN-FOREST; LAND CRABS; PLANT DIVERSITY; RECRUITMENT; COEXISTENCE; PATTERNS; DISPERSAL AB Positive density-dependent seed and seedling predation, where herbivores selectively eat seeds or seedlings of common species, is thought to play a major role in creating and maintaining plant community diversity. However, many herbivores and seed predators are known to exhibit preferences for rare foods, which could lead to negative density-dependent predation. In this study, we first demonstrate the occurrence of increased predation of locally rare tree species by a widespread group of insular seed and seedling predators, land crabs. We then build computer simulations based on these empirical data to examine the effects of such predation on diversity patterns. Simulations show that herbivore preferences for locally rare species are likely to drive scale-dependent effects on plant community diversity: at small scales these foraging patterns decrease plant community diversity via the selective consumption of rare plant species, while at the landscape level they should increase diversity, at least for short periods, by promoting clustered local dominance of a variety of species. Finally, we compared observed patterns of plant diversity at the site to those obtained via computer simulations, and found that diversity patterns generated under simulations were highly consistent with observed diversity patterns. We posit that preference for rare species by herbivores may be prevalent in low- or moderate-diversity systems, and that these effects may help explain diversity patterns across different spatial scales in such ecosystems. C1 [Young, Hillary S.; Dirzo, Rodolfo] Stanford Univ, Dept Biol, Stanford, CA 94305 USA. [Young, Hillary S.] Smithsonian Inst, Div Vertebrate Zool, Washington, DC 20013 USA. [McCauley, Douglas J.] Stanford Univ, Hopkins Marine Stn, Pacific Grove, CA 93950 USA. [Guevara, Roger] Inst Ecol AC, Red Biol Evolut, Xalapa, Veracruz, Mexico. RP Young, HS (reprint author), Harvard Univ, Ctr Environm, 11 Oxford St, Cambridge, MA 02138 USA. EM hyoung@fas.harvard.edu RI Guevara, Roger/F-3287-2010 OI Guevara, Roger/0000-0003-0768-3580 FU National Science Foundation [0639185]; National Geographic Society; Stanford's Woods Institute for the Environment FX We thank the National Science Foundation, the National Geographic Society, and Stanford's Woods Institute for the Environment for their financial support. We also thank the US Fish and Wildlife Service for permission to work in the Palmyra Atoll National Wildlife Refuge. For assistance in the field we are very grateful to L. Anderegg, P. DeSalles, C. Hanson, A. Meyer, A. McInturff, A. Miller-ter Kuile, L. Palumbi, and T. C. Robbins. We thank A. Wegmann for advice and insight throughout. Finally, we thank three anonymous reviewers for their comments, which greatly improved the quality of this manuscript. This is publication number PARC-0092 of the Palmyra Atoll Research Consortium (PARC), and was based on collaboration and networking across multiple partner organizations in PARC, which is supported in part by the National Science Foundation under grant no. 0639185. The experiments comply with the current laws of the country (USA) in which the experiments were performed. NR 42 TC 6 Z9 6 U1 2 U2 60 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0029-8549 J9 OECOLOGIA JI Oecologia PD JUL PY 2013 VL 172 IS 3 BP 857 EP 867 DI 10.1007/s00442-012-2542-2 PG 11 WC Ecology SC Environmental Sciences & Ecology GA 164KX UT WOS:000320409100021 PM 23229391 ER PT J AU Rojas-Sandoval, J Melendez-Ackerman, E AF Rojas-Sandoval, Julissa Melendez-Ackerman, Elvia TI Population dynamics of a threatened cactus species: general assessment and effects of matrix dimensionality SO POPULATION ECOLOGY LA English DT Article DE Columnar cacti; Demography; Elasticity; Matrix dimension; Mona Island; Projection matrix models ID COMPARATIVE PLANT DEMOGRAPHY; PROJECTION MATRIX; COLUMNAR CACTUS; CATEGORY SIZE; CACTACEAE; MEXICO; RARE; ELASTICITIES; CONSERVATION; REGENERATION AB Harrisia portoricensis is an endemic Caribbean cactus currently under threatened status. In this study we used population projection matrices to evaluate the conservation status of this species and we performed a systematic analysis of the effects of matrix dimensionality on the inferred demographic parameters. Results revealed that population growth rates (lambda) were 0.946 and 0.961 for the 2007-2008 and 2008-2009 periods respectively, suggesting a declining population with limited persistence ability. Even when the highest elasticity values corresponded to the survival of adults, numerical simulations suggested that increases in either seedling establishment or fecundity could render lambda > 1. Our empirical-based analysis using raw demographic data revealed a clear trend for lambda values to decrease with increasing matrix dimension. Stasis and fecundity elasticities were also found to decrease whereas retrogression and growth elasticitites increased with increasing matrix dimension. These results are roughly insensitive to the method used to create matrices of different dimensions. For H. portoricensis, large matrices with narrow classifications were required to minimize variations in lambda, highlighting the need for large data sets to assess the convergence of results with matrix dimensionality. Our combined results emphasize that under current scenarios the ability of H. portoricensis for population growth is severely limited. Any management strategy designed for the conservation of this species should consider long-term monitoring of populations as well as programs that enhance seedling establishment and adult survival. C1 [Rojas-Sandoval, Julissa; Melendez-Ackerman, Elvia] Univ Puerto Rico, Ctr Appl Trop Ecol & Conservat, San Juan, PR 00936 USA. [Melendez-Ackerman, Elvia] Univ Puerto Rico, Inst Trop Ecosyst Studies, San Juan, PR 00936 USA. RP Rojas-Sandoval, J (reprint author), Natl Museum Nat Hist, Smithsonian Inst, Dept Bot, Room W526B,POB 37012, Washington, DC 20013 USA. EM julirs07@gmail.com FU NSF-CREST through the Center for Applied Tropical Ecology and Conservation of the University of Puerto Rico [HRD-0206200, HRD 0734826] FX We thank D. Angles-Alcazar for valuable help in data analysis. Comments by J.M. Nassar, J.D. Ackerman, R. L. Tremblay and two anonymous reviewers significantly improved this manuscript. This study was funded by the NSF-CREST (HRD-0206200 and HRD 0734826) through the Center for Applied Tropical Ecology and Conservation of the University of Puerto Rico. NR 39 TC 5 Z9 5 U1 2 U2 42 PU SPRINGER JAPAN KK PI TOKYO PA CHIYODA FIRST BLDG EAST, 3-8-1 NISHI-KANDA, CHIYODA-KU, TOKYO, 101-0065, JAPAN SN 1438-3896 J9 POPUL ECOL JI Popul. Ecol. PD JUL PY 2013 VL 55 IS 3 BP 479 EP 491 DI 10.1007/s10144-013-0378-1 PG 13 WC Ecology SC Environmental Sciences & Ecology GA 166NK UT WOS:000320561600008 ER PT J AU Pogue, MG AF Pogue, Michael G. TI Revised status of Chloridea Duncan and (Westwood), 1841, for the Heliothis virescens species group (Lepidoptera: Noctuidae: Heliothinae) based on morphology and three genes SO SYSTEMATIC ENTOMOLOGY LA English DT Article AB The Heliothinae comprise some of the world's most injurious agricultural pests. This study reanalyses a subsample of the Heliothis group to determine the monophyly of Chloridea (Heliothis virescens and H.subflexa). Two nuclear gene regions, elongation factor-1 (EF-1; 1240bp) and dopa decarboylase (DDC; 687bp), and the barcoding region of mitochondrial cytochrome oxidase I (COI; 708bp) were used in this analysis for a total of 2635bp and a morphological dataset of 20 characters and 62 character states. Sixteen species representing five genera plus two outgroup species were used in the analysis. Analyses used were Maximum Parsimony (MP), Maximum Likelihood (ML) and Bayesian Inference (BI). The revised status for the monophyletic genus Chloridea Duncan and (Westwood) was supported by a very strong bootstrap support (BP=98-100). Larval host-plant usage is discussed within the Heliothis clade. Polyphagy is most likely the ancestral condition with a host shift to monophagy and oligophagy. Based on known larval hosts, Heliocheilus is oligophagous on Poaceae. Traits of host plant use in Helicoverpa and Chloridea where both polyphagy and oligophagy occur in closely related species are discussed. C1 [Pogue, Michael G.] ARS, USDA, Systemat Entomol Lab, PSI,US, Washington, DC 20013 USA. RP Pogue, MG (reprint author), ARS, USDA, Systemat Entomol Lab, PSI,US,Smithsonian Inst,NMNH, POB 37012,MRC 168, Washington, DC 20013 USA. EM michael.pogue@ars.usda.gov NR 0 TC 6 Z9 6 U1 2 U2 16 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 J9 SYST ENTOMOL JI Syst. Entomol. PD JUL PY 2013 VL 38 IS 3 BP 523 EP 542 DI 10.1111/syen.12010 PG 20 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 166MX UT WOS:000320560100006 ER PT J AU Ang, Y Puniamoorthy, J Pont, AC Bartak, M Blanckenhorn, WU Eberhard, WG Puniamoorthy, N Silva, VC Munari, L Meier, R AF Ang, Yuchen Puniamoorthy, Jayanthi Pont, Adrian C. Bartak, Miroslav Blanckenhorn, Wolf U. Eberhard, William G. Puniamoorthy, Nalini Silva, Vera C. Munari, Lorenzo Meier, Rudolf TI A plea for digital reference collections and other science-based digitization initiatives in taxonomy: Sepsidnet as exemplar SO SYSTEMATIC ENTOMOLOGY LA English DT Article ID MICROSEPSIS-ARMILLATA DIPTERA; NATURAL-HISTORY COLLECTIONS; SEXUAL SIZE DIMORPHISM; DUNG FLY; FLIES DIPTERA; BODY-SIZE; MORPHOLOGICAL COEVOLUTION; FLUCTUATING ASYMMETRY; QUANTITATIVE GENETICS; HERBARIUM SPECIMENS C1 [Ang, Yuchen; Puniamoorthy, Jayanthi; Puniamoorthy, Nalini; Meier, Rudolf] Natl Univ Singapore, Dept Biol Sci, Fac Sci, Singapore 117543, Singapore. [Pont, Adrian C.] Univ Oxford, Museum Nat Hist, Oxford, England. [Pont, Adrian C.] Nat Hist Museum, London SW7 5BD, England. [Bartak, Miroslav] Czech Univ Life Sci Prague, Dept Zool & Fisheries, Fac Agrobiol Food & Nat Resources, Prague, Czech Republic. [Blanckenhorn, Wolf U.; Puniamoorthy, Nalini] Univ Zurich, Inst Evolutionary Biol & Environm Studies, Zurich, Switzerland. [Eberhard, William G.] Univ Costa Rica, Escuela Biol, San Pedro, Costa Rica. [Eberhard, William G.] Smithsonian Trop Res Inst, Balboa, Panama. [Silva, Vera C.] Univ Estadual Paulista, Fac Ciencias Agr & Vet, Dept Morfol & Fisiol Anim, Sao Paulo, Brazil. [Munari, Lorenzo] Nat Hist Museum, Entomol Sect, Venice, Italy. [Meier, Rudolf] Natl Univ Singapore, Univ Scholars Programme, Singapore 117543, Singapore. RP Meier, R (reprint author), Natl Univ Singapore, Dept Biol Sci, 14 Sci Dr 4, Singapore 117543, Singapore. EM meier@nus.edu.sg RI Puniamoorthy, Nalini/M-1642-2013; Silva, Vera/H-1011-2012; Meier, Rudolf/A-7099-2011 OI Puniamoorthy, Nalini/0000-0003-0651-8356; Meier, Rudolf/0000-0002-4452-2885 FU MOE [R-154-000-476-112] FX We would like to acknowledge the help from numerous colleagues who collected specimens or helped with species identifications for this project. Special thanks go to A. L. Ozerov who confirmed many identifications. The construction of Sepsidnet was supported by MOE grant R-154-000-476-112. We thank Peter Cranston, who as editor of Systematic Entomology encouraged this contribution, as well as his coeditors for their comments on earlier drafts. NR 78 TC 16 Z9 19 U1 1 U2 23 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0307-6970 EI 1365-3113 J9 SYST ENTOMOL JI Syst. Entomol. PD JUL PY 2013 VL 38 IS 3 BP 637 EP 644 DI 10.1111/syen.12015 PG 8 WC Evolutionary Biology; Entomology SC Evolutionary Biology; Entomology GA 166MX UT WOS:000320560100013 ER PT J AU Anderson-Teixeira, KJ Miller, AD Mohan, JE Hudiburg, TW Duval, BD DeLucia, EH AF Anderson-Teixeira, Kristina J. Miller, Adam D. Mohan, Jacqueline E. Hudiburg, Tara W. Duval, Benjamin D. DeLucia, Evan H. TI Altered dynamics of forest recovery under a changing climate SO GLOBAL CHANGE BIOLOGY LA English DT Review DE biogeochemistry; climate feedback; FACE; irrigation; regime shift; succession; throughfall manipulation; warming ID ALTERNATIVE STABLE STATES; ATMOSPHERIC CARBON-DIOXIDE; SCRUB-OAK ECOSYSTEM; DIVERSITY-DISTURBANCE RELATIONSHIPS; NET PRIMARY PRODUCTIVITY; PONDEROSA PINE FORESTS; FINE-ROOT RESPONSES; CO2 ENRICHMENT FACE; BOREAL BLACK SPRUCE; OLD-GROWTH FORESTS AB Forest regeneration following disturbance is a key ecological process, influencing forest structure and function, species assemblages, and ecosystem-climate interactions. Climate change may alter forest recovery dynamics or even prevent recovery, triggering feedbacks to the climate system, altering regional biodiversity, and affecting the ecosystem services provided by forests. Multiple lines of evidence - including global-scale patterns in forest recovery dynamics; forest responses to experimental manipulation of CO2, temperature, and precipitation; forest responses to the climate change that has already occurred; ecological theory; and ecosystem and earth system models - all indicate that the dynamics of forest recovery are sensitive to climate. However, synthetic understanding of how atmospheric CO2 and climate shape trajectories of forest recovery is lacking. Here, we review these separate lines of evidence, which together demonstrate that the dynamics of forest recovery are being impacted by increasing atmospheric CO2 and changing climate. Rates of forest recovery generally increase with CO2, temperature, and water availability. Drought reduces growth and live biomass in forests of all ages, having a particularly strong effect on seedling recruitment and survival. Responses of individual trees and whole-forest ecosystems to CO2 and climate manipulations often vary by age, implying that forests of different ages will respond differently to climate change. Furthermore, species within a community typically exhibit differential responses to CO2 and climate, and altered community dynamics can have important consequences for ecosystem function. Age- and species-dependent responses provide a mechanism by which climate change may push some forests past critical thresholds such that they fail to recover to their previous state following disturbance. Altered dynamics of forest recovery will result in positive and negative feedbacks to climate change. Future research on this topic and corresponding improvements to earth system models will be a key to understanding the future of forests and their feedbacks to the climate system. C1 [Anderson-Teixeira, Kristina J.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Anderson-Teixeira, Kristina J.] Smithsonian Trop Res Inst, Smithsonian Inst Global Earth Observ, Ctr Trop Forest Sci, Panama City, Panama. [Miller, Adam D.; DeLucia, Evan H.] Univ Illinois, Inst Genom Biol, Chicago, IL 60680 USA. [Mohan, Jacqueline E.] Univ Georgia, Odum Sch Ecol, Athens, GA 30602 USA. [Hudiburg, Tara W.; DeLucia, Evan H.] Univ Illinois, Energy Biosci Inst, Urbana, IL 61801 USA. [Hudiburg, Tara W.; DeLucia, Evan H.] Univ Illinois, Urbana, IL 61801 USA. [Duval, Benjamin D.] USDA ARS, US Dairy Forage Res Ctr, Madison, WI 53706 USA. RP Anderson-Teixeira, KJ (reprint author), Natl Zool Pk, Smithsonian Conservat Biol Inst, Natl Zool Pk,1500 Remount Rd, Front Royal, VA 22630 USA. EM TeixeiraK@si.edu FU DOE [DE-SC0008085] FX Thanks to Jonathan Thompson and Sean McMahon for helpful discussion and to three anonymous reviewers for helpful comments. This research was supported by DOE grant #DE-SC0008085 to KJAT, EHD, and BDD. NR 224 TC 47 Z9 47 U1 21 U2 322 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1354-1013 EI 1365-2486 J9 GLOBAL CHANGE BIOL JI Glob. Change Biol. PD JUL PY 2013 VL 19 IS 7 BP 2001 EP 2021 DI 10.1111/gcb.12194 PG 21 WC Biodiversity Conservation; Ecology; Environmental Sciences SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 158IT UT WOS:000319963500004 PM 23529980 ER PT J AU Stopar, JD Taylor, GJ Velbel, MA Norman, MD Vicenzi, EP Hallis, LJ AF Stopar, Julie D. Taylor, G. Jeffrey Velbel, Michael A. Norman, Marc D. Vicenzi, Edward P. Hallis, Lydia J. TI Element abundances, patterns, and mobility in Nakhlite Miller Range 03346 and implications for aqueous alteration SO GEOCHIMICA ET COSMOCHIMICA ACTA LA English DT Article ID RARE-EARTH-ELEMENTS; MARTIAN METEORITE; MINERAL ASSEMBLAGES; REE MOBILIZATION; IGNEOUS ROCKS; MARS; TRACE; DISSOLUTION; IDDINGSITE; PETROLOGY AB Nakhlite Miller Range (MIL) 03346 contains many secondary phases resulting from aqueous processes, including formation of poorly crystalline iddingsite-like veins in olivine, the precipitation of Ca-sulfates and Fe,K-sulfates from evaporating fluids, alteration of titanomagnetite to secondary Fe-oxides, and the dissolution of magmatic Ca-phosphates and residual glass in the mesostasis. A surprising variety of alteration products occur in association with olivine in MIL 03346, including: patches of incipiently-altered olivine, large Si-enriched olivine-hosted veins (up to 10 mu m across) some of which are complex in morphology and are composed of several phases, small Fe, S(+/- K)-rich veinlets that crosscut the Si-enriched veins, Ca-sulfates filling cracks in olivine, and secondary Ca-phosphates. Elemental abundances and distributions in these alteration products are consistent with the mobilization of elements from readily dissolved phases in the mesostasis such as phosphates and residual glass. Under favorable weathering conditions, these phases dissolve more readily than pyroxenes, plagioclase, and even olivine at low pH. The occurrence (crosscut and devolatilized by the fusion crust) and composition of Si-enriched alteration veins in olivine are consistent with their formation on Mars. Si-enriched, poorly crystalline alteration products and secondary Ca-sulfates commonly occur in nakhlites, but the habit and composition of these alteration products differ between meteorites. Elemental distributions in these secondary phases suggest at least two episodes of alteration have affected MIL 03346, and subtle differences in secondary minerals and chemistry indicate that each nakhlite experienced its own unique alteration history either on Mars, Earth, or both. The variable Al content and range of morphologies of the olivine-hosted Si-enriched veins suggest variable alteration conditions consistent with a water-limited regime. If the secondary phases in MIL 03346 can be shown to have formed on Mars, their chemistry will provide important clues to the aqueous environments and processes at the time of their formation. However, elevated S and REEs, Ce anomalies, and association of secondary minerals with post-impact cracks and voids indicate that terrestrial weathering has significantly affected MIL 03346. This work highlights the difficulty in distinguishing pre-terrestrial aqueous alteration from later chemical weathering of susceptible mineral phases even in meteorites with limited terrestrial modification. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Stopar, Julie D.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ USA. [Taylor, G. Jeffrey; Hallis, Lydia J.] Univ Hawaii, Sch Ocean & Earth Sci & Technol, Honolulu, HI 96822 USA. [Velbel, Michael A.] Michigan State Univ, Dept Geol Sci, E Lansing, MI 48824 USA. [Norman, Marc D.] Australian Natl Univ, Res Sch Earth Sci, Canberra, ACT, Australia. [Vicenzi, Edward P.] Museum Conservat Inst, Smithsonian Inst, Suitland, MD USA. RP Stopar, JD (reprint author), LROC ASU, POB 873603, Tempe, AZ 85287 USA. EM jstopar@asu.edu OI Stopar, Julie/0000-0003-1578-3688 FU NASA Graduate Student Researcher Program; NASA Mars Fundamental Research Program [NNG05GL77G]; NASA Astrobiology Institute [NNA09DA77A] FX This research was primarily funded by a Grant from the NASA Graduate Student Researcher Program (J.D. Stopar, Awardee). Additional support was provided by NASA Mars Fundamental Research Program grant NNG05GL77G (M.A. Velbel, P.I.) and the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A (J.G. Taylor). Helpful reviews were provided by Bradley L. Jolliff (Washington University in St. Louis, MO, USA) and an anonymous reviewer. NR 75 TC 9 Z9 9 U1 2 U2 25 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 JUL 1 PY 2013 VL 112 BP 208 EP 225 DI 10.1016/j.gca.2013.02.024 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 144WP UT WOS:000318972800014 ER PT J AU Langa, LA Monaco, P Subramaniam, M Jaeger, PT Shanahan, K Ziebarth, B AF Langa, Lesley A. Monaco, Pino Subramaniam, Mega Jaeger, Paul T. Shanahan, Katie Ziebarth, Beth TI Improving the Museum Experiences of Children with Autism Spectrum Disorders and Their Families: An Exploratory Examination of Their Motivations and Needs and Using Web-based Resources to Meet Them SO CURATOR-THE MUSEUM JOURNAL LA English DT Article AB Through a partnership with a local school, the Smithsonian Institution and the Information Policy and Access Center at the University of Maryland conducted an exploratory study to examine the motivations and needs of families visiting museums with children with Autism Spectrum Disorders (ASDs). This study represents one of the first undertakings to study visitors with ASDs, especially children, through a primarily qualitative data collection. Interest-driven enjoyment emerged as a primary motivation, though to relax and to socialize outside of the family boundaries were not ranked as important motives for visiting museums. Children, who were directly interviewed, gave positive assessments of their museum experiences, while parents commented that challenges, both museum- and family-related (crowds, loud noise, not feeling welcome, and a child's unpredictable behavior) surfaced in public settings like museums. Parents desired a "typical family outing" with their ASDs child, stating that manageable and safe environments helped families experience a museum. C1 [Langa, Lesley A.] Univ Maryland, Coll Informat, Informat Policy & Access Ctr, College Pk, MD 20742 USA. [Monaco, Pino] Smithsonian Ctr Educ & Museum Studies, Program Evaluat & Audience Res, Washington, DC USA. [Subramaniam, Mega] Univ Maryland, Coll Informat Studies, Informat Policy & Access Ctr, College Pk, MD 20742 USA. [Jaeger, Paul T.] Univ Maryland, Coll Informat Studies, College Pk, MD 20742 USA. [Jaeger, Paul T.] Univ Maryland, Informat Policy & Access Ctr, College Pk, MD 20742 USA. [Shanahan, Katie] Robert Frost Middle Sch, Rockville, MD USA. [Ziebarth, Beth] Smithsonian Inst, Accessibil Program, Washington, DC 20560 USA. RP Langa, LA (reprint author), Univ Maryland, Coll Informat, Informat Policy & Access Ctr, College Pk, MD 20742 USA. EM lesleylanga@gmail.com; monacop@si.edu; mmsubram@umd.edu; pjaeger@umd.edu; Kate.Shana@gmail.com; ziebarth@si.edu NR 58 TC 4 Z9 4 U1 3 U2 5 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2013 VL 56 IS 3 SI SI BP 323 EP 335 DI 10.1111/cura.12031 PG 13 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V41AW UT WOS:000209520100004 ER PT J AU Davis, D AF Davis, Daniel TI New Ways of "Seeing": The Evocative Power of Audio and the Empowerment of Crowdsourcing in Exhibitions SO CURATOR-THE MUSEUM JOURNAL LA English DT Article C1 Smithsonian Natl Museum Amer Indian, Media Grp, Washington, DC 20560 USA. RP Davis, D (reprint author), Smithsonian Natl Museum Amer Indian, Media Grp, Washington, DC 20560 USA. EM DavisDan@si.edu NR 0 TC 0 Z9 0 U1 1 U2 2 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2013 VL 56 IS 3 SI SI BP 371 EP 373 DI 10.1111/cura.12037 PG 3 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V41AW UT WOS:000209520100010 ER PT J AU Werb, SR AF Werb, Shari Rosenstein TI My Body Politic, A Memoir SO CURATOR-THE MUSEUM JOURNAL LA English DT Book Review C1 [Werb, Shari Rosenstein] Smithsonian Natl Museum Nat Hist, Educ & Outreach, Washington, DC 20560 USA. RP Werb, SR (reprint author), Smithsonian Natl Museum Nat Hist, Educ & Outreach, Washington, DC 20560 USA. NR 3 TC 0 Z9 0 U1 0 U2 0 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 0011-3069 EI 2151-6952 J9 CURATOR JI Curator PD JUL PY 2013 VL 56 IS 3 SI SI BP 385 EP 389 DI 10.1111/cura.12039 PG 5 WC Humanities, Multidisciplinary SC Arts & Humanities - Other Topics GA V41AW UT WOS:000209520100012 ER PT J AU Henry, TJ Johnson, CA AF Henry, Thomas J. Johnson, Christine A. TI RANDALL TOBIAS SCHUH: A CELEBRATION OF HIS CAREER AND ACCOMPLISHMENTS ON THE OCCASION OF HIS 70TH BIRTHDAY SO ENTOMOLOGICA AMERICANA LA English DT Article C1 [Henry, Thomas J.] ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, Washington, DC 20013 USA. [Johnson, Christine A.] Amer Museum Nat Hist, Div Invertebrate Zool, New York, NY 10024 USA. RP Henry, TJ (reprint author), ARS, Systemat Entomol Lab, USDA, Natl Museum Nat Hist,Smithsonian Inst, MRC-168, Washington, DC 20013 USA. EM thomas.henry@ars.usda.gov; cjohnson@amnh.org FU American Museum of Natural History FX We are grateful to the many authors who contributed to this Festschrift volume, especially those who wrote personal tributes, including Toby's wife Brenda Massie, his daughter Ella Massie-Schuh, Gerry Cassis (University of New South Wales, Sydney), Katrina Menard (Sam Noble Museum, University of Oklahoma, Norman), and Ruth Salas (The American Museum of American History, New York). We also thank The New York Entomological Society for supporting this special volume and The American Museum of Natural History for funding; without this support this publication would not have been possible. NR 96 TC 0 Z9 0 U1 0 U2 0 PU NEW YORK ENTOMOLOGICAL SOC INC PI NEW YORK PA C/O AMER MUSEUM NAT HIST 79TH & CENTRAL PARK WEST, NEW YORK, NY 10024 USA SN 1947-5136 EI 1947-5144 J9 ENTOMOL AM-NY JI Entomol. Am. PD JUL PY 2013 VL 119 IS 1-2 BP 1 EP 6 DI 10.1664/13-SN-005.1 PG 6 WC Entomology SC Entomology GA V35YA UT WOS:000209179800001 ER PT J AU Montaser, R Paul, VJ Luesch, H AF Montaser, R. Paul, V. J. Luesch, H. TI Modular Strategies for Structure and Function Employed by Marine Cyanobacteria: Characterization and Synthesis of Pitinoic Acids SO PLANTA MEDICA LA English DT Meeting Abstract CT Annual Meeting of the American-Society-of-Pharmacognosy on Natural Products at a Crossroad - Current and Future Directions CY JUL 14-17, 2013 CL St Louis, MO SP Amer Soc Pharmacognosy C1 [Montaser, R.; Luesch, H.] Univ Florida, Dept Med Chem, Gainesville, FL 32610 USA. [Paul, V. J.] Smithsonian Marine Stn, Ft Pierce, FL 34949 USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU GEORG THIEME VERLAG KG PI STUTTGART PA RUDIGERSTR 14, D-70469 STUTTGART, GERMANY SN 0032-0943 EI 1439-0221 J9 PLANTA MED JI Planta Med. PD JUL PY 2013 VL 79 IS 10 MA CL14 BP 822 EP 822 PG 1 WC Plant Sciences; Chemistry, Medicinal; Integrative & Complementary Medicine; Pharmacology & Pharmacy SC Plant Sciences; Pharmacology & Pharmacy; Integrative & Complementary Medicine GA AK8RG UT WOS:000338695100062 ER PT J AU Ruckelshaus, M Doney, SC Galindo, HM Barry, JP Chan, F Duffy, JE English, CA Gaines, SD Grebmeier, JM Hollowed, AB Knowlton, N Polovina, J Rabalais, NN Sydeman, WJ Talley, LD AF Ruckelshaus, M. Doney, S. C. Galindo, H. M. Barry, J. P. Chan, F. Duffy, J. E. English, C. A. Gaines, S. D. Grebmeier, J. M. Hollowed, A. B. Knowlton, N. Polovina, J. Rabalais, N. N. Sydeman, W. J. Talley, L. D. TI Securing ocean benefits for society in the face of climate change SO MARINE POLICY LA English DT Article DE Ecosystem services; Climate adaptation; Coastal hazards; Fisheries; Tourism; Trade-offs ID MARINE PROTECTED AREAS; ECOSYSTEM SERVICES; FISHERIES MANAGEMENT; COASTAL VEGETATION; MANGROVE FORESTS; CORAL-REEFS; IMPACTS; RESILIENCE; RECOVERY; TSUNAMI AB Benefits humans rely on from the ocean - marine ecosystem services - are increasingly vulnerable under future climate. This paper reviews how three valued services have, and will continue to, shift under climate change: (1) capture fisheries, (2) food from aquaculture, and (3) protection from coastal hazards such as storms and sea-level rise. Climate adaptation planning is just beginning for fisheries, aquaculture production, and risk mitigation for coastal erosion and inundation. A few examples are highlighted, showing the promise of considering multiple ecosystem services in developing approaches to adapt to sea-level rise, ocean acidification, and rising sea temperatures. Ecosystem-based adaptation in fisheries and along coastlines and changes in aquaculture practices can improve resilience of species and habitats to future environmental challenges. Opportunities to use market incentives - such as compensation for services or nutrient trading schemes - are relatively untested in marine systems. Relocation of communities in response to rising sea levels illustrates the urgent need to manage human activities and investments in ecosystems to provide a sustainable flow of benefits in the face of future climate change. (C) 2013 Elsevier Ltd. All rights reserved. C1 [Ruckelshaus, M.] Stanford Univ, Nat Capital Project, Stanford, CA 94305 USA. [Doney, S. C.] Woods Hole Oceanog Inst, Marine Chem & Geochem Dept, Woods Hole, MA 02543 USA. [Galindo, H. M.] Univ Washington, COMPASS, Seattle, WA 98195 USA. [Barry, J. P.] Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. [Chan, F.] Oregon State Univ, Corvallis, OR 97331 USA. [Duffy, J. E.] Virginia Inst Marine Sci, Gloucester Point, VA 23062 USA. [English, C. A.] COMPASS, Silver Spring, MD 20910 USA. [Gaines, S. D.] Univ Calif Santa Barbara, Santa Barbara, CA 93106 USA. [Grebmeier, J. M.] Univ Maryland, Ctr Environm Sci, Chesapeake Biol Lab, Solomons, MD 20688 USA. [Hollowed, A. B.] NOAA, Alaska Fisheries Sci Ctr, Natl Marine Fisheries Serv, Seattle, WA 98115 USA. [Knowlton, N.] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20013 USA. [Polovina, J.] NOAA, Pacific Isl Fisheries Sci Ctr, Honolulu, HI 96822 USA. [Rabalais, N. N.] Louisiana Univ Marine Consortium, Chauvin, LA 70344 USA. [Sydeman, W. J.] Farallon Inst, Petaluma, CA 94975 USA. [Talley, L. D.] Univ Calif San Diego, La Jolla, CA 92093 USA. RP Ruckelshaus, M (reprint author), 6828 51st Ave NE, Seattle, WA 98115 USA. EM mary.ruckelshaus@stanford.edu; sdoney@whoi.edu; hgalindo@compassonline.org; bany@mbari.org; chanft@science.oregonstate.edu; jeduffy@vims.edu; cenglish@compassonline.org; gaines@bren.ucsb.edu; jgrebmei@umces.edu; anne.hollowed@noaa.gov; knowlton@si.edu; jeffrey.polovina@noaa.gov; nrabalais@lumcon.edu; wsydeman@comcast.net; ltalley@ucsd.edu RI Grebmeier, Jacqueline/L-9805-2013 OI Grebmeier, Jacqueline/0000-0001-7624-3568 NR 136 TC 37 Z9 38 U1 9 U2 286 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0308-597X J9 MAR POLICY JI Mar. Pol. PD JUL PY 2013 VL 40 BP 154 EP 159 DI 10.1016/j.marpol.2013.01.009 PG 6 WC Environmental Studies; International Relations SC Environmental Sciences & Ecology; International Relations GA 125KR UT WOS:000317539200018 ER PT J AU Smith, P La Tierra, P Scott, N Cacciali, P Atkinson, K Pheasey, H AF Smith, Paul La Tierra, Para Scott, Norman Cacciali, Pier Atkinson, Karina Pheasey, Helen TI Confirmation of the presence of Philodryas nattereri STEINDACHNER, 1870, in Paraguay SO HERPETOZOA LA English DT Editorial Material DE Reptilia: Squamata: Serpentes: Colubridae: Dipsadinae; Philodryas nattereri; San Pedro; Para La Tierra; Reserva Natural de Laguna Blanca; Cerrado; new country record; Paraguay ID SNAKE ASSEMBLAGE; CERRADO; BRAZIL; COLUBRIDAE C1 [Smith, Paul; La Tierra, Para; Scott, Norman; Cacciali, Pier] Smithsonian Inst, Creston, CA 93432 USA. RP Smith, P (reprint author), Smithsonian Inst, POB 307, Creston, CA 93432 USA. EM faunaparaguay@gmail.com NR 36 TC 1 Z9 1 U1 0 U2 1 PU OSTERREICHISCHE GESELLSCHAFT HERPETOLOGIE E V PI VIENNA PA BURGRING 7, P O BOX 417, VIENNA, A-1014, AUSTRIA SN 1013-4425 J9 HERPETOZOA JI HERPETOZOA PD JUN 30 PY 2013 VL 26 IS 1-2 BP 91 EP 94 PG 4 WC Zoology SC Zoology GA 184HW UT WOS:000321881700009 ER PT J AU Barkley, MP De Smedt, I Van Roozendael, M Kurosu, TP Chance, K Arneth, A Hagberg, D Guenther, A Paulot, F Marais, E Mao, JQ AF Barkley, Michael P. De Smedt, Isabelle Van Roozendael, Michel Kurosu, Thomas P. Chance, Kelly Arneth, Almut Hagberg, Daniel Guenther, Alex Paulot, Fabien Marais, Eloise Mao, Jingqiu TI Top-down isoprene emissions over tropical South America inferred from SCIAMACHY and OMI formaldehyde columns SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE Amazon; isoprene; formaldehyde; SCIAMACHY; OMI; GEOS-Chem ID VOLATILE ORGANIC-COMPOUNDS; MAX-DOAS MEASUREMENTS; NITROGEN-DIOXIDE; ATMOSPHERIC CHEMISTRY; CROSS-SECTIONS; DRY DEPOSITION; BOUNDARY-LAYER; TRACE GASES; OXIDATION; MODEL AB We use formaldehyde (HCHO) vertical column measurements from the Scanning Imaging Absorption spectrometer for Atmospheric Chartography (SCIAMACHY) and Ozone Monitoring Instrument (OMI), and a nested-grid version of the GEOS-Chem chemistry transport model, to infer an ensemble of top-down isoprene emission estimates from tropical South America during 2006, using different model configurations and assumptions in the HCHO air-mass factor (AMF) calculation. Scenes affected by biomass burning are removed on a daily basis using fire count observations, and we use the local model sensitivity to identify locations where the impact of spatial smearing is small, though this comprises spatial coverage over the region. We find that the use of the HCHO column data more tightly constrains the ensemble isoprene emission range from 27-61TgC to 31-38TgC for SCIAMACHY, and 45-104TgC to 28-38TgC for OMI. Median uncertainties of the top-down emissions are about 60-260% for SCIAMACHY, and 10-90% for OMI. We find that the inferred emissions are most sensitive to uncertainties in cloud fraction and cloud top pressure (differences of +/- 10%), the a priori isoprene emissions (+/- 20%), and the HCHO vertical column retrieval (+/- 30%). Construction of continuous top-down emission maps generally improves GEOS-Chem's simulation of HCHO columns over the region, with respect to both the SCIAMACHY and OMI data. However, if local time top-down emissions are scaled to monthly mean values, the annual emission inferred from SCIAMACHY are nearly twice those from OMI. This difference cannot be explained by the different sampling of the sensors or uncertainties in the AMF calculation. C1 [Barkley, Michael P.] Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester LE1 7RH, Leics, England. [De Smedt, Isabelle; Van Roozendael, Michel] Belgian Inst Space Aeron BIRA IASB, Brussels, Belgium. [Kurosu, Thomas P.; Chance, Kelly] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Arneth, Almut; Hagberg, Daniel] Lund Univ, Dept Phys Geog & Ecosyst Anal, Geobiosphere Sci Ctr, Lund, Sweden. [Arneth, Almut] Karlsruhe Inst Technol, Atmospher Environm Res Inst Meteorol & Climate Re, D-76021 Karlsruhe, Germany. [Guenther, Alex] Natl Ctr Atmospher Res, Boulder, CO 80307 USA. [Paulot, Fabien; Marais, Eloise] Harvard Univ, Cambridge, MA 02138 USA. [Mao, Jingqiu] Princeton Univ, Geophys Fluid Dynam Lab, Princeton, NJ 08544 USA. RP Barkley, MP (reprint author), Univ Leicester, Dept Phys & Astron, EOS Grp, Leicester LE1 7RH, Leics, England. EM mpb14@le.ac.uk RI Mao, Jingqiu/F-2511-2010; Chem, GEOS/C-5595-2014; jingjing, cai/M-2687-2013; Guenther, Alex/B-1617-2008; OI Mao, Jingqiu/0000-0002-4774-9751; Guenther, Alex/0000-0001-6283-8288; Chance, Kelly/0000-0002-7339-7577; Marais, Eloise/0000-0001-5477-8051 FU Natural Environment Research Council [NE/GE013810/2]; Swedish Research Council Formas FX This work was supported by the Natural Environment Research Council (grant NE/GE013810/2). A.A. and D.H. acknowledge support from the Swedish Research Council Formas. NR 83 TC 20 Z9 20 U1 4 U2 41 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 27 PY 2013 VL 118 IS 12 BP 6849 EP 6868 DI 10.1002/jgrd.50552 PG 20 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 187OY UT WOS:000322129600069 ER PT J AU San Blas, G Davis, DR AF San Blas, German Davis, Donald R. TI Redescription of Dicranoses capsulifex Kieffer and Jorgensen (Lepidoptera: Cecidosidae) with description of the immature stages and biology SO ZOOTAXA LA English DT Article DE life cycle; immature stages; cecidogenic moth; plant gall; South America AB Dicranoses capsulifex Kieffer and Jorgensen (Lepidoptera: Cecidosidae) is a gall inducing moth associated with Schinus fasciculatus (Griseb.) (Anacardiaceae), with a known distribution restricted to Argentina. It undergoes a one year life cycle (univoltine), with leaf-like galls, and adult with only a half day life span. Male, female, pupa, and gall are redescribed, and the genitalia of both sexes, larva, and life cycle are described herein for the first time using light and scanning electron microscopy. The life cycle is documented from samples consisting of 15 larvae and/or pupae taken every 15 days during the year (from July, 2011, to July, 2012). C1 [San Blas, German] Consejo Nacl Invest Cient & Tecn, Entomol Lab, Inst Argentino Invest Zonas Aridas, RA-5500 Mendoza, Argentina. [Davis, Donald R.] Smithsonian Inst, Dept Entomol, Natl Museum Nat Hist, Washington, DC USA. RP San Blas, G (reprint author), Consejo Nacl Invest Cient & Tecn, Entomol Lab, Inst Argentino Invest Zonas Aridas, CC 507, RA-5500 Mendoza, Argentina. EM gsanblas@mendoza-conicet.gov.ar; davisd@si.edu OI San Blas, German/0000-0002-3119-590X 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 J9 ZOOTAXA JI Zootaxa PD JUN 27 PY 2013 VL 3682 IS 2 BP 371 EP 384 PG 14 WC Zoology SC Zoology GA 171IA UT WOS:000320917700009 PM 25243292 ER PT J AU Lehners, JL Steinhardt, PJ AF Lehners, Jean-Luc Steinhardt, Paul J. TI Planck 2013 results support the cyclic universe SO PHYSICAL REVIEW D LA English DT Article ID MODEL AB We show that results from the Planck satellite reported in 2013 are consistent with cyclic models of the Universe for natural parameter ranges (i.e. order unity dimensionless coefficients), assuming the standard entropic mechanism for generating curvature perturbations. With improved precision, forthcoming results from Planck and other experiments should be able to test the remaining parameter range and confirm or refute the core predictions, i.e. no observable primordial B-mode polarization and detectable local non-Gaussianity. A new prediction, given the Planck 2013 constraints on the bispectrum, is a sharp constraint on the local trispectrum parameter g(NL); namely, the currently best-understood models predict it is negative, with g(NL) less than or similar to -1700. C1 [Lehners, Jean-Luc] Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany. [Steinhardt, Paul J.] Harvard Univ, Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Steinhardt, Paul J.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. [Steinhardt, Paul J.] Princeton Univ, Joseph Henry Lab, Princeton, NJ 08544 USA. RP Lehners, JL (reprint author), Albert Einstein Inst, Max Planck Inst Gravitat Phys, D-14476 Potsdam, Germany. FU European Research Council [256994]; U.S. Department of Energy [DE-FG02-91ER40671] FX We would like to thank Bill Jones and David Spergel for reading the manuscript and for their valuable comments. J.L.L. gratefully acknowledges the support of the European Research Council via the Starting Grant No. 256994. This work was supported in part by the U.S. Department of Energy Grant No. DE-FG02-91ER40671 (P.J.S.). P.J.S. is grateful to the Simons Foundation and the Radcliffe Institute for providing support during his leave at Harvard and to the Institute for Theory and Computation at the Harvard-Smithsonian for hosting him during the period that this work was done. NR 36 TC 29 Z9 29 U1 1 U2 9 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 26 PY 2013 VL 87 IS 12 AR 123533 DI 10.1103/PhysRevD.87.123533 PG 5 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 172GF UT WOS:000320987600002 ER PT J AU Ijjas, A Steinhardt, PJ Loeb, A AF Ijjas, Anna Steinhardt, Paul J. Loeb, Abraham TI Inflationary paradigm in trouble after Planck2013 SO PHYSICS LETTERS B LA English DT Article ID EINSTEIN-HILBERT ACTION; SCALAR FIELD; ETERNAL INFLATION; COSMOLOGICAL MODELS; CHAOTIC INFLATION; HIGGS-BOSON; UNIVERSE; GENERALITY; FLATNESS; HORIZON AB Recent results from the Planck satellite combined with earlier observations from WMAP, ACT, SPT and other experiments eliminate a wide spectrum of more complex inflationary models and favor models with a single scalar field, as reported by the Planck Collaboration. More important, though, is that all the simplest inflaton models are disfavored statistically relative to those with plateau-like potentials. We discuss how a restriction to plateau-like models has three independent serious drawbacks: it exacerbates both the initial conditions problem and the multiverse-unpredictability problem and it creates a new difficulty that we call the inflationary "unlikeliness problem." Finally, we comment on problems reconciling inflation with a standard model Higgs, as suggested by recent LHC results. In sum, we find that recent experimental data disfavors all the best-motivated inflationary scenarios and introduces new, serious difficulties that cut to the core of the inflationary paradigm. Forthcoming searches for B-modes, non-Gaussianity and new particles should be decisive. (C) 2013 Elsevier B.V. All rights reserved. C1 [Ijjas, Anna; Steinhardt, Paul J.; Loeb, Abraham] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ijjas, Anna] Univ Observ Munich, D-81679 Munich, Germany. [Steinhardt, Paul J.] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. [Steinhardt, Paul J.] Princeton Univ, Princeton Ctr Theoret Sci, Princeton, NJ 08544 USA. RP Steinhardt, PJ (reprint author), Princeton Univ, Dept Phys, Princeton, NJ 08544 USA. EM aijjas@cfa.harvard.edu; steinh@princeton.edu; aloeb@cfa.harvard.edu FU US Department of Energy [DE-FG02-91ER40671]; NSF [AST-0907890]; NASA [NNX08AL43G, NNA09DB30A]; Fritz Thyssen Foundation; Simons Foundation; Radcliffe Institute FX We thank T. Baker, W. Jones, J. Kovac, J.-L. Lehners, D. Spergel, and B. Xue for helpful discussions. This work was supported in part by the US Department of Energy grant DE-FG02-91ER40671 (P.J.S.) and by NSF grant AST-0907890 and NASA grants NNX08AL43G and NNA09DB30A (A.L.). A.I. gratefully acknowledges the support of the Fritz Thyssen Foundation. P.J.S. is grateful to the Simons Foundation and the Radcliffe Institute for providing support during his leave at Harvard and to the Institute for Theory and Computation at the Harvard-Smithsonian for hosting him during the period that this work was done. NR 62 TC 98 Z9 98 U1 3 U2 10 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0370-2693 EI 1873-2445 J9 PHYS LETT B JI Phys. Lett. B PD JUN 25 PY 2013 VL 723 IS 4-5 BP 261 EP 266 DI 10.1016/j.physletb.2013.05.023 PG 6 WC Astronomy & Astrophysics; Physics, Nuclear; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 168ZB UT WOS:000320745400002 ER PT J AU Iono, D Saito, T Yun, MS Kawabe, R Espada, D Hagiwara, Y Imanishi, M Izumi, T Kohno, K Motohara, K Nakanishi, K Sugai, H Tateuchi, K Tamura, Y Ueda, J Yoshii, Y AF Iono, Daisuke Saito, Toshiki Yun, Min S. Kawabe, Ryohei Espada, Daniel Hagiwara, Yoshiaki Imanishi, Masatoshi Izumi, Takuma Kohno, Kotaro Motohara, Kentaro Nakanishi, Kouichiro Sugai, Hajime Tateuchi, Ken Tamura, Yoichi Ueda, Junko Yoshii, Yuzuru TI Active Galactic Nucleus and Extended Starbursts in a Midstage Merger VV 114 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: starburst; telescopes ID LUMINOUS INFRARED GALAXIES; DENSE MOLECULAR GAS; STAR-FORMATION; FAR-ULTRAVIOLET; EMISSION; VV-114; ENVIRONMENTS; HCN(1-0); HCO+ AB High-resolution (similar to 0 ''.4) Atacama Large Millimeter/submillimeter Array (ALMA) Cycle 0 observations of HCO+ (4-3) and HCN (4-3) toward a midstage infrared bright merger, VV 114, have revealed a compact nuclear (< 200 pc) and extended (similar to 3-4 kpc) dense gas distribution across the eastern part of the galaxy pair. We have found a significant enhancement of HCN (4-3) emission in an unresolved compact and broad (290 km s(-1)) component found in the eastern nucleus of VV 114, and suggest dense gas associated with the surrounding material around an Active Galactic Nucleus (AGN), with a mass upper limit of less than or similar to 4 x 10(8) M-circle dot. The extended dense gas is distributed along a filamentary structure with resolved dense gas concentrations (similar to 230 pc; similar to 10(6) M-circle dot) separated by a mean projected distance of similar to 600 pc, many of which are generally consistent with the location of star formation traced in Pace emission. Radiative-transfer calculations suggest moderately dense (n(H2) = 10(5)-10(6) cm(-3)) gas averaged over the entire emission region. These new ALMA observations demonstrate the strength of the dense gas tracers for identifying both the AGN and the star-formation activity in a galaxy merger, even in the most dust-enshrouded environment in the local universe. C1 [Iono, Daisuke; Saito, Toshiki; Kawabe, Ryohei; Espada, Daniel; Hagiwara, Yoshiaki; Imanishi, Masatoshi; Ueda, Junko] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan. [Iono, Daisuke; Hagiwara, Yoshiaki; Imanishi, Masatoshi; Nakanishi, Kouichiro] Grad Univ Adv Studies SOKENDAI, Mitaka, Tokyo 1810015, Japan. [Saito, Toshiki; Ueda, Junko] Univ Tokyo, Sch Sci, Dept Astron, Bunkyo Ku, Tokyo 1330033, Japan. [Yun, Min S.] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Kawabe, Ryohei; Espada, Daniel; Nakanishi, Kouichiro] Joint ALMA Observ, Santiago 7630355, Chile. [Izumi, Takuma; Kohno, Kotaro; Motohara, Kentaro; Tateuchi, Ken; Tamura, Yoichi; Yoshii, Yuzuru] Univ Tokyo, Inst Astron, Mitaka, Tokyo 1810015, Japan. [Kohno, Kotaro] Univ Tokyo, Res Ctr Early Univ, Bunkyo Ku, Tokyo 1130033, Japan. [Sugai, Hajime] Univ Tokyo, Kavli Inst Phys & Math Univ WPI, Kashiwa, Chiba 2778583, Japan. [Ueda, Junko] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Iono, D (reprint author), Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan. RI MOTOHARA, KENTARO/G-4905-2014 OI MOTOHARA, KENTARO/0000-0002-0724-9146 NR 27 TC 13 Z9 13 U1 0 U2 3 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 JUN 25 PY 2013 VL 65 IS 3 AR L7 DI 10.1093/pasj/65.3.L7 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 181PW UT WOS:000321682000005 ER PT J AU Suarez-Rubio, M Wilson, S Leimgruber, P Lookingbill, T AF Suarez-Rubio, Marcela Wilson, Scott Leimgruber, Peter Lookingbill, Todd TI Threshold Responses of Forest Birds to Landscape Changes around Exurban Development SO PLOS ONE LA English DT Article ID UNITED-STATES; HABITAT FRAGMENTATION; POPULATION-CHANGE; RESIDENTIAL DEVELOPMENT; RELATIVE IMPORTANCE; SPECIES RESPONSES; SPATIAL-PATTERN; TERRITORY SIZE; COMMUNITIES; CONSERVATION AB Low-density residential development (i.e., exurban development) is often embedded within a matrix of protected areas and natural amenities, raising concern about its ecological consequences. Forest-dependent species are particularly susceptible to human settlement even at low housing densities typical of exurban areas. However, few studies have examined the response of forest birds to this increasingly common form of land conversion. The aim of this study was to assess whether, how, and at what scale forest birds respond to changes in habitat due to exurban growth. We evaluated changes in habitat composition (amount) and configuration (arrangement) for forest and forest-edge species around North America Breeding Bird Survey (BBS) stops between 1986 and 2009. We used Threshold Indicator Taxa Analysis to detect change points in species occurrence at two spatial extents (400-m and 1-km radius buffer). Our results show that exurban development reduced forest cover and increased habitat fragmentation around BBS stops. Forest birds responded nonlinearly to most measures of habitat loss and fragmentation at both the local and landscape extents. However, the strength and even direction of the response changed with the extent for several of the metrics. The majority of forest birds' responses could be predicted by their habitat preferences indicating that management practices in exurban areas might target the maintenance of forested habitats, for example through easements or more focused management for birds within existing or new protected areas. C1 [Suarez-Rubio, Marcela] Univ Maryland, Ctr Environm Sci, Appalachian Lab, Frostburg, MD USA. [Wilson, Scott] Environm Canada, Canadian Wildlife Serv, Saskatoon, SK, Canada. [Leimgruber, Peter] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [Lookingbill, Todd] Univ Richmond, Dept Geog & Environm, Richmond, VA 23173 USA. RP Suarez-Rubio, M (reprint author), Univ Maryland, Ctr Environm Sci, Appalachian Lab, Frostburg, MD USA. EM marcela.suarezrubio@boku.ac.at RI Leimgruber, Peter/O-1304-2015; OI Leimgruber, Peter/0000-0002-3682-0153; Suarez-Rubio, Marcela/0000-0002-0596-2626 FU Appalachian Laboratory, University of Maryland Center for Environmental Science FX This work was supported by Appalachian Laboratory, University of Maryland Center for Environmental Science. The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript. NR 104 TC 13 Z9 13 U1 4 U2 67 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 JUN 24 PY 2013 VL 8 IS 6 AR e67593 DI 10.1371/journal.pone.0067593 PG 11 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 182JP UT WOS:000321738400161 PM 23826325 ER PT J AU Greenberg, R Danner, RM AF Greenberg, Russell Danner, Raymond M. TI Climate, ecological release and bill dimorphism in an island songbird SO BIOLOGY LETTERS LA English DT Article DE Allen's rule; sexual dimorphism; island rule; heat dissipation; song sparrows ID SEXUAL-DIMORPHISM; SIZE; CALIFORNIA; BIRDS; RULE AB Sexual size dimorphism is expected to be more pronounced in vertebrates on islands, particularly in trophic characters, as a response to decreased interspecific competition for food. We found (based on measurements of 1423 museum specimens) that bill size dimorphism was greater in island than mainland populations of song sparrows. However, dimorphism varied among islands and was positively correlated with high summer temperature and island size. Island song sparrow bills follow the overall positive temperature bill size relationship for California song sparrows, which includes larger bills on large, warmer islands. Large bills dissipate more heat and may be an adaptation to summer heat stress. Dimorphism increases because the slope for males is greater than females. Thus, the greater magnitude of bill dimorphism on islands with warmer summers may result from males experiencing greater thermal stress during territorial activity, creating different thermal optima. In contrast, bill dimorphism was unrelated to climate on the mainland. We hypothesize that reduced interspecific competition releases island populations from a constraint so that sex-specific physiological optima can be achieved, whereas mainland birds are constrained. C1 [Greenberg, Russell; Danner, Raymond M.] Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Washington, DC 20008 USA. RP Greenberg, R (reprint author), Smithsonian Conservat Biol Inst, Smithsonian Migratory Bird Ctr, Natl Zool Pk, Washington, DC 20008 USA. EM greenbergr@si.edu RI Danner, Raymond/J-8350-2013 OI Danner, Raymond/0000-0002-3999-8141 NR 20 TC 7 Z9 7 U1 1 U2 31 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 2013 VL 9 IS 3 AR 20130118 DI 10.1098/rsbl.2013.0118 PG 4 WC Biology; Ecology; Evolutionary Biology SC Life Sciences & Biomedicine - Other Topics; Environmental Sciences & Ecology; Evolutionary Biology GA 141YK UT WOS:000318762300030 PM 23616645 ER PT J AU Kantor, YI Harasewych, MG AF Kantor, Yuri I. Harasewych, M. G. TI Antarctica, where turrids and whelks converge: A revision of Falsimohnia Powell, 1951 (Neogastropoda: Buccinoidea) and a description of a new genus SO NAUTILUS LA English DT Article DE Gastropoda; Conoidea; Buccinoidea; Antarctic Convergence; biogeography; morphological convergence ID GASTROPODA; MOLLUSKS; SEA AB A study of the type material of Antarctic species of conoideans described by Herman Strebel revealed that four species, all originally described in the genus Bela Gray, 1847 (Mangeliidae), are referable to the superfamily Buccinoidea based on radular morphology. Three of the species: B. fluvi cans, B. minor, and B. anderssoni are transferred to the genus Falsimohnia, which is here reviewed. The new buccinoidean genus Strebela is proposed for the species originally described as Bela notophila. Of the five species of the conthologically similar genus Pareuthria Strebel, 1905 that have been recorded within the Antarctic Convergence, two, Pareuthria innocens (Smith, 1907) and P. hoshiaii Numanami, 1996, are transferred to the genus Falsimohnia based on radular morphology. The appropriate generic allocation of Pareuthria plicata Thiele, 1912 is not yet clear; however, major differences in radular morphology exclude it from the genus Pareuthria. The taxa Pareuthria valdiviae (Thiele, 1925) and Pareuthria turriformis Egorova, 1982 are presently known only from their shell morphology. We suggest that they will be referred to other genera when anatomical material becomes available, and that the genus Pareuthria will be limited to the Magellanic region. C1 [Kantor, Yuri I.] Russian Acad Sci, AN Severtzov Inst Ecol & Evolut, Moscow 119071, Russia. [Harasewych, M. G.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, Washington, DC 20013 USA. RP Harasewych, MG (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, MRC 163, POB 37012, Washington, DC 20013 USA. EM Harasewych@si.edu RI Kantor, Yuri/D-5259-2014 OI Kantor, Yuri/0000-0002-3209-4940 NR 29 TC 3 Z9 3 U1 0 U2 1 PU BAILEY-MATTHEWS SHELL MUSEUM PI SANIBEL PA C/O DR JOSE H LEAL, ASSOCIATE/MANAGING EDITOR, 3075 SANIBEL-CAPTIVA RD, SANIBEL, FL 33957 USA SN 0028-1344 J9 NAUTILUS JI Nautilus PD JUN 21 PY 2013 VL 127 IS 2 BP 43 EP 56 PG 14 WC Marine & Freshwater Biology; Zoology SC Marine & Freshwater Biology; Zoology GA 170ZD UT WOS:000320893000001 ER PT J AU Johnson, PD Bogan, AE Brown, KM Burkhead, NM Cordeiro, JR Garner, JT Hartfield, PD Lepitzki, DAW Mackie, GL Pip, E Tarpley, TA Tiemann, JS Whelan, NV Strong, EE AF Johnson, Paul D. Bogan, Arthur E. Brown, Kenneth M. Burkhead, Noel M. Cordeiro, James R. Garner, Jeffrey T. Hartfield, Paul D. Lepitzki, Dwayne A. W. Mackie, Gerry L. Pip, Eva Tarpley, Thomas A. Tiemann, Jeremy S. Whelan, Nathan V. Strong, Ellen E. TI Conservation Status of Freshwater Gastropods of Canada and the United States SO FISHERIES LA English DT Review ID SUBTROPICAL SNAILS PROSOBRANCHIA; LIFE-HISTORY; PHYLOGENETIC-RELATIONSHIPS; REPRODUCTIVE ISOLATION; PHYSIDAE GASTROPODA; MOLECULAR PHYLOGENY; EXTINCTION RATES; APPLE SNAIL; RIVER-BASIN; FISHES AB This is the first American Fisheries Society conservation assessment of freshwater gastropods (snails) from Canada and the United States by the Gastropod Subcommittee (Endangered Species Committee). This review covers 703 species representing 16 families and 93 genera, of which 67 species are considered extinct, or possibly extinct, 278 are endangered, 102 are threatened, 73 are vulnerable, 157 are currently stable, and 26 species have uncertain taxonomic status. Of the entire fauna, 74% of gastropods are imperiled (vulnerable, threatened, endangered) or extinct, which exceeds imperilment levels in fishes (39%) and crayfishes (48%) but is similar to that of mussels (72%). Comparison of modern to background extinction rates reveals that gastropods have the highest modern extinction rate yet observed, 9,539 times greater than background rates. Gastropods are highly susceptible to habitat loss and degradation, particularly narrow endemics restricted to a single spring or short stream reaches. Compilation of this review was hampered by a paucity of current distributional information and taxonomic uncertainties. Although research on several fronts including basic biology, physiology, conservation strategies, life history, and ecology are needed, systematics and curation of museum collections and databases coupled with comprehensive status surveys (geographic limits, threat identification) are priorities. C1 [Johnson, Paul D.; Tarpley, Thomas A.] Alabama Dept Conservat & Nat Resources, Alabama Aquat Biodivers Ctr, Marion, AL 36756 USA. [Bogan, Arthur E.] N Carolina State Museum Nat Sci, Raleigh, NC USA. [Brown, Kenneth M.] Louisiana State Univ, Baton Rouge, LA 70803 USA. [Burkhead, Noel M.] Southeast Ecol Sci Ctr, United States Geol Survey, Gainesville, FL USA. [Cordeiro, James R.] Univ Massachusetts, Boston, MA 02125 USA. [Garner, Jeffrey T.] Alabama Dept Conservat & Nat Resources, Florence, AL USA. [Hartfield, Paul D.] US Fish & Wildlife Serv, Jackson, MS USA. [Lepitzki, Dwayne A. W.] Wildlife Syst Res, Banff, AB, Canada. [Mackie, Gerry L.] Univ Guelph, Water Syst Analysts, Guelph, ON N1G 2W1, Canada. [Pip, Eva] Univ Winnipeg, Winnipeg, MB R3B 2E9, Canada. [Tiemann, Jeremy S.] Illinois Nat Hist Survey, Champaign, IL 61820 USA. [Whelan, Nathan V.] Univ Alabama, Tuscaloosa, AL USA. [Strong, Ellen E.] Smithsonian Inst, Dept Invertebrate Zool, Washington, DC 20560 USA. [Cordeiro, James R.] Nat Serve, Boston, MA USA. RP Johnson, PD (reprint author), Alabama Dept Conservat & Nat Resources, Alabama Aquat Biodivers Ctr, 2200 Highway 175, Marion, AL 36756 USA. EM paul.johnson@dcnr.alabama.gov RI Bogan, Arthur/G-7658-2016; OI Bogan, Arthur/0000-0003-4042-7706; Whelan, Nathan/0000-0002-3542-2102; Strong, Ellen/0000-0001-7181-4114 FU Alabama Department of Conservation and Natural Resources; Smithsonian Institution, North Carolina Museum of Natural Sciences; U.S. Fish and Wildlife Service FX We thank Jamie Smith, North Carolina Museum of Natural Sciences, for generating Figure 3. We are grateful to the numerous museum curators who provided access to the collections under their care during the preparation of this database. We also thank AFS Fisheries staff and especially Endangered Species Chair Howard Jelks for their assistance in publication. We thank Paul Callomon, Academy of Natural Sciences Philadelphia, for his technical assistance in photographing the micro planorbids. We thank Steve Ahlstedt for his assistance with the review process and his innumerable contributions to freshwater mollusk conservation over the years. Randall Haddock of the Cahaba River Society and Paul Freeman of the Nature Conservancy of Alabama contributed photographs. Thanks are extended to Buck Albert (Cherokee Nation Technology Solutions) and Howard Jelks (U.S. Geological Survey), Gainesville, Florida, for development of the website. We also gratefully acknowledge the contributions of two anonymous reviewers. Finally, a special thanks to Jim Williams, whose invaluable assistance facilitated completion of this assessment. This work was supported in part from various funding sources including the Alabama Department of Conservation and Natural Resources, the Smithsonian Institution, North Carolina Museum of Natural Sciences, and the U.S. Fish and Wildlife Service. Any use of trade, product, or firm names is for descriptive purposes only and does not imply endorsement by the U. S. Government. NR 135 TC 38 Z9 40 U1 5 U2 43 PU TAYLOR & FRANCIS INC PI PHILADELPHIA PA 325 CHESTNUT ST, SUITE 800, PHILADELPHIA, PA 19106 USA SN 0363-2415 J9 FISHERIES JI Fisheries PD JUN 21 PY 2013 VL 38 IS 6 BP 247 EP 282 DI 10.1080/03632415.2013.785396 PG 36 WC Fisheries SC Fisheries GA 163WW UT WOS:000320369800004 ER PT J AU Schmelz, JT Winebarger, AR Kimble, JA Pathak, S Golub, L Jenkins, BS Worley, BT AF Schmelz, J. T. Winebarger, A. R. Kimble, J. A. Pathak, S. Golub, L. Jenkins, B. S. Worley, B. T. TI BRIGHT POINTS: MULTITHERMAL ANALYSIS AS A TEST OF STEADY HEATING MODELS SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: fundamental parameters; Sun: UV radiation ID X-RAY TELESCOPE; EUV IMAGING SPECTROMETER; PLASMA FILLING FACTOR; ACTIVE-REGION CORE; ATOMIC DATA; DENSITY-MEASUREMENTS; RATE COEFFICIENTS; CORONAL-EXPLORER; EMISSION-MEASURE; MAGNETIC-FIELDS AB X-ray bright points are small, million-degree features in the solar atmosphere composed of short coronal loops. They are magnetically driven structures associated with photospheric magnetic bipoles. Their relatively small size and simple structure suggest they are ideal candidates for comparisons with coronal heating models. In this paper, we present the analysis of 12 bright points using data from the EUV Imaging Spectrometer on Hinode and the Michelson Doppler Imager on Solar and Heliospheric Observatory. Using the spectroscopy data, we construct differential emission measure (DEM) curves, calculate the electron density, and find DEM-weighted temperatures. In addition, we determine the most likely ionization balance. Using the magnetic field observations, we complete potential field extrapolations of the magnetograms and estimate the loop lengths. Using this information, we construct models assuming the bright points are formed of hundreds of strands, each heated steadily and uniformly. We formulate the models so that the observed emission measure distribution is matched within a few percent. We then compare the densities determined from the models, (1.4-5.0) x 10(9), to those calculated from spectral data, (0.6-2.0) x 10(9). We find the majority of bright points do not agree with steady uniform heating models; instead they are underdense relative to their expected density by a factor of 0.16-0.82. C1 [Schmelz, J. T.; Kimble, J. A.; Pathak, S.; Jenkins, B. S.; Worley, B. T.] Univ Memphis, Dept Phys, Memphis, TN 38152 USA. [Winebarger, A. R.] NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Golub, L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Schmelz, JT (reprint author), Univ Memphis, Dept Phys, Memphis, TN 38152 USA. EM jschmelz@memphis.edu FU Hinode subcontract from NASA/SAO; NSF [ATM-0402729] FX The authors would like to thank Steve Saar of CfA and Jim Klimchuk of GSFC for useful discussions on BPs. 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 the NSC (Norway). CHIANTI is a collaborative project involving the NRL (USA), the Universities of Florence (Italy) and Cambridge (UK), and George Mason University (USA). Solar physics research at the University of Memphis is supported by a Hinode subcontract from NASA/SAO as well as NSF ATM-0402729. NR 51 TC 2 Z9 2 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR 160 DI 10.1088/0004-637X/770/2/160 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AG2KE UT WOS:000335244400006 ER PT J AU Bracken-Grissom, HD Cannon, ME Cabezas, P Feldmann, RM Schweitzer, CE Ahyong, ST Felder, DL Lemaitre, R Crandall, KA AF Bracken-Grissom, Heather D. Cannon, Maren E. Cabezas, Patricia Feldmann, Rodney M. Schweitzer, Carrie E. Ahyong, Shane T. Felder, Darryl L. Lemaitre, Rafael Crandall, Keith A. TI A comprehensive and integrative reconstruction of evolutionary history for Anomura (Crustacea: Decapoda) SO BMC EVOLUTIONARY BIOLOGY LA English DT Article DE Anomura; Phylogeny; Divergence times; Diversification rates; Molecular; Morphology; Character evolution; Next-generation sequencing ID HERMIT-CRAB ANCESTORS; SOUTH-WEST PACIFIC; FAMILIES CHIROSTYLIDAE; ANNOTATED CHECKLIST; DIVERGENCE TIMES; MOLECULAR CLOCK; GALATHEOIDEA CRUSTACEA; MORPHOLOGICAL EVIDENCE; PHYLOGENETIC TREES; CLADISTIC-ANALYSIS AB Background: The infraorder Anomura has long captivated the attention of evolutionary biologists due to its impressive morphological diversity and ecological adaptations. To date, 2500 extant species have been described but phylogenetic relationships at high taxonomic levels remain unresolved. Here, we reconstruct the evolutionary history-phylogeny, divergence times, character evolution and diversification-of this speciose clade. For this purpose, we sequenced two mitochondrial (16S and 12S) and three nuclear (H3, 18S and 28S) markers for 19 of the 20 extant families, using traditional Sanger and next-generation 454 sequencing methods. Molecular data were combined with 156 morphological characters in order to estimate the largest anomuran phylogeny to date. The anomuran fossil record allowed us to incorporate 31 fossils for divergence time analyses. Results: Our best phylogenetic hypothesis (morphological + molecular data) supports most anomuran superfamilies and families as monophyletic. However, three families and eleven genera are recovered as para-and polyphyletic. Divergence time analysis dates the origin of Anomura to the Late Permian similar to 259 (224-296) MYA with many of the present day families radiating during the Jurassic and Early Cretaceous. Ancestral state reconstruction suggests that carcinization occurred independently 3 times within the group. The invasion of freshwater and terrestrial environments both occurred between the Late Cretaceous and Tertiary. Diversification analyses found the speciation rate to be low across Anomura, and we identify 2 major changes in the tempo of diversification; the most significant at the base of a clade that includes the squat-lobster family Chirostylidae. Conclusions: Our findings are compared against current classifications and previous hypotheses of anomuran relationships. Many families and genera appear to be poly-or paraphyletic suggesting a need for further taxonomic revisions at these levels. A divergence time analysis provides key insights into the origins of major lineages and events and the timing of morphological (body form) and ecological (habitat) transitions. Living anomuran biodiversity is the product of 2 major changes in the tempo of diversification; our initial insights suggest that the acquisition of a crab-like form did not act as a key innovation. C1 [Bracken-Grissom, Heather D.] Florida Int Univ, Dept Biol, North Miami, FL 33181 USA. [Cannon, Maren E.; Cabezas, Patricia] Brigham Young Univ, Dept Biol, Provo, UT 84602 USA. [Cabezas, Patricia; Crandall, Keith A.] George Washington Univ, Computat Biol Inst, Ashburn, VA 20147 USA. [Feldmann, Rodney M.] Kent State Univ, Dept Geol, Kent, OH 44242 USA. [Schweitzer, Carrie E.] Kent State Univ Stark, North Canton, OH 44720 USA. [Ahyong, Shane T.] Australian Museum, Sydney, NSW 2010, Australia. [Felder, Darryl L.] Univ Louisiana Lafayette, Dept Biol, Lafayette, LA 70504 USA. [Lemaitre, Rafael; Crandall, Keith A.] Smithsonian Inst, Natl Museum Nat Hist, Dept Invertebrate Zool, Suitland, MD 20746 USA. RP Bracken-Grissom, HD (reprint author), Florida Int Univ, Dept Biol, Biscayne Bay Campus, North Miami, FL 33181 USA. EM hbracken@fiu.edu OI Crandall, Keith/0000-0002-0836-3389; Ahyong, Shane/0000-0002-2820-4158 NR 130 TC 29 Z9 34 U1 3 U2 44 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 JUN 20 PY 2013 VL 13 AR 128 DI 10.1186/1471-2148-13-128 PG 28 WC Evolutionary Biology; Genetics & Heredity SC Evolutionary Biology; Genetics & Heredity GA 180GA UT WOS:000321580600001 PM 23786343 ER PT J AU Greenhill, LJ Goddi, C Chandler, CJ Matthews, LD Humphreys, EML AF Greenhill, L. J. Goddi, C. Chandler, C. J. Matthews, L. D. Humphreys, E. M. L. TI DYNAMICAL EVIDENCE FOR A MAGNETOCENTRIFUGAL WIND FROM A 20 M-circle dot BINARY YOUNG STELLAR OBJECT SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE ISM: individual objects (Orion BN/KL); ISM: jets and outflows; ISM: kinematics and dynamics; ISM: molecules; masers ID ORION SOURCE I; EMISSION; OUTFLOW; MASER; BN/KL; SHOCKS; DISK; KL AB In Orion BN/KL, proper motions of lambda 7 mm vibrationally excited SiO masers trace the rotation of a nearly edge-on disk and a bipolar wide-angle outflow 10-100 AU from radio source I, a binary young stellar object of similar to 20 M-circle dot. Here we map ground-state lambda 7 mm SiO emission with the Very Large Array and track proper motions over 9 yr. The innermost and strongest emission lies in two extended arcs bracketing Source I. The proper motions trace a northeast-southwest bipolar outflow 100-1000 AU from Source I with a median three-dimensional motion of similar to 18 km s(-1). An overlying distribution of lambda 1.3 cm H2O masers betrays similar flow characteristics. Gas dynamics and emission morphology traced by the masers suggest the presence of a magnetocentrifugal disk wind. Reinforcing evidence lies in the colinearity of the flow, apparent rotation across the flow parallel to the disk rotation, and recollimation that narrows the flow opening angle similar to 120 AU downstream. The arcs of ground-state SiO emission may mark the transition point to a shocked super-Alfvenic outflow. C1 [Greenhill, L. J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Goddi, C.; Humphreys, E. M. L.] Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. [Chandler, C. J.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Matthews, L. D.] MIT, Haystack Observ, Westford, MA 01886 USA. RP Greenhill, LJ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM greenhill@cfa.harvard.edu NR 16 TC 12 Z9 12 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 20 PY 2013 VL 770 IS 2 AR L32 DI 10.1088/2041-8205/770/2/L32 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168MJ UT WOS:000320709900016 ER PT J AU Meyer, KA Sabol, J Mackay, DH van Ballegooijen, AA AF Meyer, K. A. Sabol, J. Mackay, D. H. van Ballegooijen, A. A. TI THE STORAGE AND DISSIPATION OF MAGNETIC ENERGY IN THE QUIET SUN CORONA DETERMINED FROM SDO/HMI MAGNETOGRAMS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: corona; Sun: photosphere; Sun: surface magnetism ID CARPET; RECONNECTION; FIELDS; SUPERGRANULATION; DYNAMICS; EMERGENCE; ELEMENTS; POINTS; EVENTS; DRIVEN AB In recent years, higher cadence, higher resolution observations have revealed the quiet-Sun photosphere to be complex and rapidly evolving. Since magnetic fields anchored in the photosphere extend up into the solar corona, it is expected that the small-scale coronal magnetic field exhibits similar complexity. For the first time, the quiet-Sun coronal magnetic field is continuously evolved through a series of non-potential, quasi-static equilibria, deduced from magnetograms observed by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory, where the photospheric boundary condition which drives the coronal evolution exactly reproduces the observed magnetograms. The build-up, storage, and dissipation of magnetic energy within the simulations is studied. We find that the free magnetic energy built up and stored within the field is sufficient to explain small-scale, impulsive events such as nanoflares. On comparing with coronal images of the same region, the energy storage and dissipation visually reproduces many of the observed features. The results indicate that the complex small-scale magnetic evolution of a large number of magnetic features is a key element in explaining the nature of the solar corona. C1 [Meyer, K. A.; Sabol, J.; Mackay, D. H.] Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. [van Ballegooijen, A. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Meyer, KA (reprint author), Univ St Andrews, Sch Math & Stat, St Andrews KY16 9SS, Fife, Scotland. EM karen@mcs.st-and.ac.uk OI van Ballegooijen, Adriaan/0000-0002-5622-3540 FU Leverhulme Trust; STFC; EU under FP7; Royal Society of Edinburgh through the Cormack Vacation Scholarship; STFC/SRIF FX We thank the anonymous referee for constructive comments, which have improved the Letter. K.A.M. and D.H.M. acknowledge the support of the Leverhulme Trust, STFC, and the EU for their support under FP7. J.S. would like to thank The Royal Society of Edinburgh for their support through the Cormack Vacation Scholarship. We acknowledge the use of SDO/HMI and SDO/AIA data. Simulations were run using the STFC/SRIF funded UKMHD cluster. NR 33 TC 10 Z9 10 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 20 PY 2013 VL 770 IS 2 AR L18 DI 10.1088/2041-8205/770/2/L18 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168MJ UT WOS:000320709900002 ER PT J AU Milisavljevic, D Soderberg, AM Margutti, R Drout, MR Marion, H Sanders, NE Hsiao, EY Lunnan, R Chornock, R Fesen, RA Parrent, JT Levesque, EM Berger, E Foley, RJ Challis, P Kirshner, RP Dittmann, J Bieryla, A Kamble, A Chakraborti, S De Rosa, G Fausnaugh, M Hainline, KN Chen, CT Hickox, RC Morrell, N Phillips, MM Stritzinger, M AF Milisavljevic, Dan Soderberg, Alicia M. Margutti, Raffaella Drout, Maria R. Marion, Howie Sanders, Nathan E. Hsiao, Eric Y. Lunnan, Ragnhild Chornock, Ryan Fesen, Robert A. Parrent, Jerod T. Levesque, Emily M. Berger, Edo Foley, Ryan J. Challis, Pete Kirshner, Robert P. Dittmann, Jason Bieryla, Allyson Kamble, Atish Chakraborti, Sayan De Rosa, Gisella Fausnaugh, Michael Hainline, Kevin N. Chen, Chien-Ting Hickox, Ryan C. Morrell, Nidia Phillips, Mark M. Stritzinger, Maximilian TI SN 2012au: A GOLDEN LINK BETWEEN SUPERLUMINOUS SUPERNOVAE AND THEIR LOWER-LUMINOSITY COUNTERPARTS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE supernovae: general; supernovae: individual (SN 2012au) ID LIGHT CURVES; IB/C SUPERNOVAE; NEBULAR PHASE; HIGH-REDSHIFT; EXPLOSIONS; HYPERNOVA; GALAXIES; 1998BW; 1997EF; MODEL AB We present optical and near-infrared observations of SN 2012au, a slow-evolving supernova (SN) with properties that suggest a link between subsets of energetic and H-poor SNe and superluminous SNe. SN 2012au exhibited conspicuous Type-Ib-like He I lines and other absorption features at velocities reaching approximate to 2x10(4) km s(-1) in its early spectra, and a broad light curve that peaked at M-B = -18.1 mag. Models of these data indicate a large explosion kinetic energy of similar to 10(52) erg and Ni-56 mass ejection of M-Ni approximate to 0.3 M-circle dot on par with SN 1998bw. SN 2012au's spectra almost one year after explosion show a blend of persistent Fe II P-Cyg absorptions and nebular emissions originating from two distinct velocity regions. These late-time emissions include strong [Fe II], [Ca II], [O I], Mg I], and Na I lines at velocities greater than or similar to 4500 km s(-1), as well as O I and Mg I lines at noticeably smaller velocities less than or similar to 2000 km s(-1). Many of the late-time properties of SN 2012au are similar to the slow-evolving hypernovae SN 1997dq and SN 1997ef, and the superluminous SN 2007bi. Our observations suggest that a single explosion mechanism may unify all of these events that span -21 less than or similar to M-B less than or similar to -17 mag. The aspherical and possibly jetted explosion was most likely initiated by the core collapse of a massive progenitor star and created substantial high-density, low-velocity Ni-rich material. C1 [Milisavljevic, Dan; Soderberg, Alicia M.; Margutti, Raffaella; Drout, Maria R.; Marion, Howie; Sanders, Nathan E.; Lunnan, Ragnhild; Chornock, Ryan; Berger, Edo; Foley, Ryan J.; Challis, Pete; Kirshner, Robert P.; Dittmann, Jason; Bieryla, Allyson; Kamble, Atish; Chakraborti, Sayan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hsiao, Eric Y.; Morrell, Nidia; Phillips, Mark M.] Lab Campanas Observ, Carnegie Observ, Colina El Pino 601, Casilla, Chile. [Fesen, Robert A.; Parrent, Jerod T.; Hainline, Kevin N.; Chen, Chien-Ting; Hickox, Ryan C.] Dartmouth Coll, Dept Phys & Astron, Wilder Lab 6127, Hanover, NH 03755 USA. [Parrent, Jerod T.] Global Telescope Network, Las Cumbres Observ, Goleta, CA 93117 USA. [Levesque, Emily M.] Univ Colorado, Dept Astrophys Planetary & Atmospher Sci, CASA, Boulder, CO 80309 USA. [De Rosa, Gisella; Fausnaugh, Michael] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Stritzinger, Maximilian] Aarhus Univ, Dept Phys & Astron, DK-8000 Aarhus C, Denmark. RP Milisavljevic, D (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dmilisav@cfa.harvard.edu OI Lunnan, Ragnhild/0000-0001-9454-4639; stritzinger, maximilian/0000-0002-5571-1833 FU David and Lucile Packard Foundation; NSF [AST-0306969, AST-0607438, AST-1008343, AST-121196] FX We thank the anonymous referee for informed suggestions that improved the manuscript, and the Harvard College Observatory for supporting the Astronomy100 class, which was the first to classify SN 2012au. Support was provided by the David and Lucile Packard Foundation Fellowship for Science and Engineering awarded to A.M.S. Additional support is from the NSF under grants AST-0306969, AST-0607438, AST-1008343, and AST-121196. Observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona, as well as the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. NR 43 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 JUN 20 PY 2013 VL 770 IS 2 AR L38 DI 10.1088/2041-8205/770/2/L38 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168MJ UT WOS:000320709900022 ER PT J AU Mori, K Gotthelf, EV Zhang, S An, HJ Baganoff, FK Barriere, NM Beloborodov, AM Boggs, SE Christensen, FE Craig, WW Dufour, F Grefenstette, BW Hailey, CJ Harrison, FA Hong, J Kaspi, VM Kennea, JA Madsen, KK Markwardt, CB Nynka, M Stern, D Tomsick, JA Zhang, WW AF Mori, Kaya Gotthelf, Eric V. Zhang, Shuo An, Hongjun Baganoff, Frederick K. Barriere, Nicolas M. Beloborodov, Andrei M. Boggs, Steven E. Christensen, Finn E. Craig, William W. Dufour, Francois Grefenstette, Brian W. Hailey, Charles J. Harrison, Fiona A. Hong, Jaesub Kaspi, Victoria M. Kennea, Jamie A. Madsen, Kristin K. Markwardt, Craig B. Nynka, Melania Stern, Daniel Tomsick, John A. Zhang, William W. TI NuSTAR DISCOVERY OF A 3.76 s TRANSIENT MAGNETAR NEAR SAGITTARIUS A* SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Galaxy: center; pulsars: general; pulsars: individual (SGR J1745-29); stars: neutron ID X-RAY PULSARS; SOFT GAMMA-REPEATERS; GALACTIC-CENTER; NEUTRON-STARS; RADIO PULSATIONS; EMISSION; OUTBURST; TELESCOPE; MECHANISM; DISK AB We report the discovery of 3.76 s pulsations from a new burst source near Sgr A* observed by the NuSTAR observatory. The strong signal from SGR J1745-29 presents a complex pulse profile modulated with pulsed fraction 27% +/- 3% in the 3-10 keV band. Two observations spaced nine days apart yield a spin-down rate of (P) over dot = (6.5 +/- 1.4) x 10(-12). This implies a magnetic field B = 1.6 x 10(14) G, spin-down power (E) over dot = 5 x 10(33) erg s(-1), and characteristic age P/2(P) over dot = 9 x 10(3) yr for the rotating dipole model. However, the current (P) over dot may be erratic, especially during outburst. The flux and modulation remained steady during the observations and the 3-79 keV spectrum is well fitted by a combined blackbody plus power-law model with temperature kT(BB) = 0.96 +/- 0.02 keV and photon index Gamma = 1.5 +/- 0.4. The neutral hydrogen column density (N-H similar to 1.4 x 10(23) cm(-2)) measured by NuSTAR and Swift suggests that SGR J1745-29 is located at or near the Galactic center. The lack of an X-ray counterpart in the published Chandra survey catalog sets a quiescent 2-8 keV luminosity limit of Lx less than or similar to 10(32) erg s(-1). The bursting, timing, and spectral properties indicate a transient magnetar undergoing an outburst with 2-79 keV luminosity up to 3.5 x 10(35) erg s(-1) for a distance of 8 kpc. SGR J1745-29 joins a growing subclass of transient magnetars, indicating that many magnetars in quiescence remain undetected in the X-ray band or have been detected as high-B radio pulsars. The peculiar location of SGR J1745-29 has important implications for the formation and dynamics of neutron stars in the Galactic center region. C1 [Mori, Kaya; Gotthelf, Eric V.; Zhang, Shuo; Beloborodov, Andrei M.; Hailey, Charles J.; Nynka, Melania] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [An, Hongjun; Dufour, Francois; Kaspi, Victoria M.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Baganoff, Frederick K.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Barriere, Nicolas M.; Boggs, Steven E.; Craig, William W.; Tomsick, John A.] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.] Tech Univ Denmark, DTU Space Natl Space Inst, DK-2800 Lyngby, Denmark. [Grefenstette, Brian W.; Harrison, Fiona A.; Madsen, Kristin K.] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Hong, Jaesub] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Kennea, Jamie A.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Markwardt, Craig B.; Zhang, William W.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stern, Daniel] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mori, K (reprint author), Columbia Univ, Columbia Astrophys Lab, 538 W 120th St, New York, NY 10027 USA. EM kaya@astro.columbia.edu RI Boggs, Steven/E-4170-2015; OI Boggs, Steven/0000-0001-9567-4224; Madsen, Kristin/0000-0003-1252-4891 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration FX This work was supported under NASA Contract No. NNG08FD60C, and made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. The authors thank Arash Bodaghee and Clio Sleator for their assistance with data analysis and Brian Metzger for helpful discussions. NR 47 TC 68 Z9 69 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 20 PY 2013 VL 770 IS 2 AR L23 DI 10.1088/2041-8205/770/2/L23 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168MJ UT WOS:000320709900007 ER PT J AU Shen, KJ Guillochon, J Foley, RJ AF Shen, Ken J. Guillochon, James Foley, Ryan J. TI CIRCUMSTELLAR ABSORPTION IN DOUBLE DETONATION TYPE Ia SUPERNOVAE SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE binaries: close; novae, cataclysmic variables; nuclear reactions, nucleosynthesis, abundances; supernovae: general; white dwarfs ID ACCRETING WHITE-DWARFS; SODIUM-ABSORPTION; CLOSE BINARIES; MASS-TRANSFER; EVOLUTION; MERGERS; NOVAE; STARS; GAS; APPROXIMATIONS AB Upon formation, degenerate He core white dwarfs are surrounded by a radiative H-rich layer primarily supported by ideal gas pressure. In this Letter, we examine the effect of this H-rich layer on mass transfer in He+C/O double white dwarf binaries that will eventually merge and possibly yield a Type Ia supernova (SN Ia) in the double detonation scenario. Because its thermal profile and equation of state differ from the underlying He core, the H-rich layer is transferred stably onto the C/O white dwarf prior to the He core's tidal disruption. We find that this material is ejected from the binary system and sweeps up the surrounding interstellar medium hundreds to thousands of years before the SN Ia. The close match between the resulting circumstellar medium profiles and values inferred from recent observations of circumstellar absorption in SNe Ia gives further credence to the resurgent double detonation scenario. C1 [Shen, Ken J.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Shen, Ken J.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Shen, Ken J.] Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA. [Guillochon, James] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Foley, Ryan J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Shen, KJ (reprint author), Univ Calif Berkeley, Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA. EM kenshen@astro.berkeley.edu OI Guillochon, James/0000-0002-9809-8215 FU NASA through Einstein Postdoctoral Fellowship [PF1-120088]; Chandra X-ray Center; NASA [NAS8-03060] FX We thank Jason Dexter, Dan Kasen, Rodolfo Perez, Eliot Quataert, Cody Raskin, and Jeff Silverman for discussions. K.J.S. is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120088 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 46 TC 47 Z9 47 U1 1 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 JUN 20 PY 2013 VL 770 IS 2 AR L35 DI 10.1088/2041-8205/770/2/L35 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 168MJ UT WOS:000320709900019 ER PT J AU Fu, H Cooray, A Feruglio, C Ivison, RJ Riechers, DA Gurwell, M Bussmann, RS Harris, AI Altieri, B Aussel, H Baker, AJ Bock, J Boylan-Kolchin, M Bridge, C Calanog, JA Casey, CM Cava, A Chapman, SC Clements, DL Conley, A Cox, P Farrah, D Frayer, D Hopwood, R Jia, J Magdis, G Marsden, G Martinez-Navajas, P Negrello, M Neri, R Oliver, SJ Omont, A Page, MJ Perez-Fournon, I Schulz, B Scott, D Smith, A Vaccari, M Valtchanov, I Vieira, JD Viero, M Wang, L Wardlow, JL Zemcov, M AF Fu, Hai Cooray, Asantha Feruglio, C. Ivison, R. J. Riechers, D. A. Gurwell, M. Bussmann, R. S. Harris, A. I. Altieri, B. Aussel, H. Baker, A. J. Bock, J. Boylan-Kolchin, M. Bridge, C. Calanog, J. A. Casey, C. M. Cava, A. Chapman, S. C. Clements, D. L. Conley, A. Cox, P. Farrah, D. Frayer, D. Hopwood, R. Jia, J. Magdis, G. Marsden, G. Martinez-Navajas, P. Negrello, M. Neri, R. Oliver, S. J. Omont, A. Page, M. J. Perez-Fournon, I. Schulz, B. Scott, D. Smith, A. Vaccari, M. Valtchanov, I. Vieira, J. D. Viero, M. Wang, L. Wardlow, J. L. Zemcov, M. TI The rapid assembly of an elliptical galaxy of 400 billion solar masses at a redshift of 2.3 SO NATURE LA English DT Article ID STAR-FORMING GALAXIES; H-2 CONVERSION FACTOR; SUBMILLIMETER GALAXIES; MOLECULAR GAS; MODEL; SIMULATIONS; EMISSION; MERGERS; HERMES; GROWTH AB Stellar archaeology(1) shows that massive elliptical galaxies formed rapidly about ten billion years ago with star-formation rates of above several hundred solar masses per year. Their progenitors are probably the submillimetre bright galaxies(2) at redshifts z greater than 2. Although the mean molecular gas mass(3) (5 x 10(10) solar masses) of the submillimetre bright galaxies can explain the formation of typical elliptical galaxies, it is inadequate to form elliptical galaxies(4) that already have stellar masses above 2 x 10(11) solar masses at z approximate to 2. Here we report multi-wavelength high-resolution observations of a rare merger of two massive submillimetre bright galaxies at z approximate to 2.3. The system is seen to be forming stars at a rate of 2,000 solar masses per year. The star-formation efficiency is an order of magnitude greater than that of normal galaxies, so the gas reservoir will be exhausted and star formation will be quenched in only around 200 million years. At a projected separation of 19 kiloparsecs, the two massive starbursts are about to merge and form a passive elliptical galaxy with a stellar mass of about 4 x 10(11) solar masses. We conclude that gas-rich major galaxy mergers with intense star formation can form the most massive elliptical galaxies by z approximate to 1.5. C1 [Fu, Hai; Cooray, Asantha; Boylan-Kolchin, M.; Calanog, J. A.; Jia, J.; Wardlow, J. L.] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. [Feruglio, C.; Cox, P.; Neri, R.] Inst Radio Astron Millimetr, F-38406 St Martin Dheres, France. [Ivison, R. J.] Royal Observ, UK Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. [Riechers, D. A.] Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. [Gurwell, M.; Bussmann, R. S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Harris, A. I.] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Altieri, B.; Valtchanov, I.] European Space Astron Ctr, Herschel Sci Ctr, Madrid 28691, Spain. [Aussel, H.] Univ Paris Diderot, Lab AIM Paris Saclay, CEA Saclay, CEA,DSM,Irfu,SAp,CNRS, F-91191 Gif Sur Yvette, France. [Baker, A. J.] Rutgers State Univ, Dept Phys & Astron, Piscataway, NJ 08854 USA. [Bock, J.; Zemcov, M.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Bock, J.; Bridge, C.; Vieira, J. D.; Viero, M.] CALTECH, Pasadena, CA 91125 USA. [Casey, C. M.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Cava, A.] Univ Complutense Madrid, Fac Ciencias Fis, Dept Astrofis, E-28040 Madrid, Spain. [Chapman, S. C.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 4R2, Canada. [Clements, D. L.; Hopwood, R.] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England. [Conley, A.] Univ Colorado, Ctr Astrophys & Space Astron UCB 389, Boulder, CO 80309 USA. [Farrah, D.] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Frayer, D.] Natl Radio Astron Observ, Green Bank, WV 24944 USA. [Magdis, G.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Marsden, G.; Scott, D.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Martinez-Navajas, P.; Perez-Fournon, I.] Inst Astrofis Canarias, E-38200 Tenerife, Spain. [Martinez-Navajas, P.; Perez-Fournon, I.] Univ La Laguna, Dept Astrofis, E-38205 Tenerife, Spain. [Negrello, M.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Oliver, S. J.; Smith, A.; Wang, L.] Univ Sussex, Dept Phys & Astron, Ctr Astron, Brighton BN1 9QH, E Sussex, England. [Omont, A.] Univ Paris 06, CNRS, Inst Astrophys Paris, UMR 7095, F-75014 Paris, France. [Page, M. J.] Univ Coll London, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. [Schulz, B.] CALTECH, Jet Prop Lab, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Vaccari, M.] Univ Western Cape, Dept Phys, Astrophys Grp, ZA-7535 Cape Town, South Africa. RP Fu, H (reprint author), Univ Calif Irvine, Dept Phys & Astron, Irvine, CA 92697 USA. EM haif@uci.edu; acooray@uci.edu RI Magdis, Georgios/C-7295-2014; Wardlow, Julie/C-9903-2015; Ivison, R./G-4450-2011; Vaccari, Mattia/R-3431-2016; Cava, Antonio/C-5274-2017; OI Magdis, Georgios/0000-0002-4872-2294; Wardlow, Julie/0000-0003-2376-8971; Boylan-Kolchin, Michael/0000-0002-9604-343X; Ivison, R./0000-0001-5118-1313; Vaccari, Mattia/0000-0002-6748-0577; Cava, Antonio/0000-0002-4821-1275; Scott, Douglas/0000-0002-6878-9840; Casey, Caitlin/0000-0002-0930-6466; Altieri, Bruno/0000-0003-3936-0284 FU CSA (Canada); NAOC (China); CEA (France); CNES (France); CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); NASA (USA) FX Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. This research has made use of data from the HerMES project (http://hermes.sussex.ac.uk/). HerMES is a Herschel Key Programme using Guaranteed Time from the SPIRE instrument team, ESAC scientists and a mission scientist. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including the University of Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, the University of Sussex (UK); and Caltech/JPL, IPAC and the University of Colorado (USA). This development has been supported by the following national funding agencies: CSA (Canada); NAOC (China); CEA, CNES and CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). The data presented in this paper will be released through the HeDaM Database in Marseille at http://hedam.oamp.fr/HerMES. NR 30 TC 53 Z9 53 U1 1 U2 18 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 20 PY 2013 VL 498 IS 7454 BP 338 EP 341 DI 10.1038/nature12184 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 166XI UT WOS:000320592900034 PM 23698363 ER PT J AU Tang, KL Agnew, MK Hirt, MV Lumbantobing, DN Raley, ME Sado, T Teoh, VH Yang, L Bart, HL Harris, PM He, SP Miya, M Saitoh, K Simons, AM Wood, RM Mayden, RL AF Tang, Kevin L. Agnew, Mary K. Hirt, M. Vincent Lumbantobing, Daniel N. Raley, Morgan E. Sado, Tetsuya Teoh, View-Hune Yang, Lei Bart, Henry L. Harris, Phillip M. He, Shunping Miya, Masaki Saitoh, Kenji Simons, Andrew M. Wood, Robert M. Mayden, Richard L. TI Limits and phylogenetic relationships of East Asian fishes in the subfamily Oxygastrinae (Teleostei: Cypriniformes: Cyprinidae) SO ZOOTAXA LA English DT Article DE Cypriniformes; Cyprinidae; Oxygastrinae; phylogeny; systematics; taxonomy ID FRESH-WATER FISHES; CARP HYPOPHTHALMICHTHYS-NOBILIS; CYTOCHROME-B SEQUENCES; DNA CONTROL REGION; EUROPEAN CYPRINIDS; MOLECULAR SYSTEMATICS; SOUTH CHINA; GENE; CLADE; INTERRELATIONSHIPS AB The cyprinid subfamily Oxygastrinae is composed of a diverse group of fishes that has been taxonomically and phylogenetically problematic. Their great variation in appearance, life histories, and trophic diversity resulted in uncertainty regarding their relationships, which led to their historical classification across many disparate subfamilies. The phylogenetic relationships of Oxygastrinae are resolved based on sequence data from four loci: cytochrome b, cytochrome c oxidase I, opsin, and recombination activating gene 1. A combined data matrix consisting of 4114 bp for 144 taxa was compiled and analyzed using maximum likelihood and parsimony optimality criteria. The subfamily Oxygastrinae is recovered as a monophyletic group that includes Ancherythroculter, Aphyocypris, Candidia, Chanodichthys, Ctenopharyngodon, Culter, Distoechodon, Elopichthys, Hainania, Hemiculter, Hemiculterella, Hemigrammocypris, Hypophthalmichthys, Ischikauia, Macrochirichthys, Megalobrama, Metzia, Mylopharyngodon, Nicholsicypris, Nipponocypris, Ochetobius, Opsariichthys, Oxygaster, Parabramis, Parachela, Paralaubuca, Pararasbora, Parazacco, Plagiognathops, Pseudobrama, Pseudohemiculter, Pseudolaubuca, Sinibrama, Squaliobarbus, Toxabramis, Xenocyprioides, Xenocypris, Yaoshanicus, and Zacco. Of these genera, the following were found to be monophyletic: Aphyocypris, Distoechodon, Hypophthalmichthys, Nipponocypris, Opsariichthys, Parachela, Paralaubuca, Plagiognathops, Xenocyprioides, and Xenocypris. The following genera were not monophyletic: Metzia, Hemiculter, Toxabramis, Ancherythroculter, Chanodichthys, Culter, Megalobrama. The remainder are either monotypic or were represented by only a single species. Four genera not examined in this study are provisionally classified in Oxygastrinae: Anabarilius, Longiculter, Pogobrama, and Rasborichthys. C1 [Tang, Kevin L.] Univ Michigan, Dept Biol, Flint, MI 48502 USA. [Agnew, Mary K.; Yang, Lei; Wood, Robert M.; Mayden, Richard L.] St Louis Univ, Dept Biol, St Louis, MO 63103 USA. [Hirt, M. Vincent; Simons, Andrew M.] Univ Minnesota, Bell Museum Nat Hist, Minneapolis, MN 55455 USA. [Hirt, M. Vincent] Univ Minnesota, Grad Program Ecol Evolut & Behav, St Paul, MN 55108 USA. [Lumbantobing, Daniel N.] George Washington Univ, Dept Biol Sci, Washington, DC 20052 USA. [Lumbantobing, Daniel N.] Natl Museum Nat Hist, Smithsonian Inst, Div Fisheries, Washington, DC 20013 USA. [Raley, Morgan E.] North Carolina Museum Nat Sci, Natl Res Ctr, Raleigh, NC 27603 USA. [Sado, Tetsuya; Miya, Masaki] Nat Hist Museum & Inst, Dept Zool, Chiba 2608682, Japan. [Teoh, View-Hune] Univ Alabama, Dept Biol Sci, Tuscaloosa, AL 35487 USA. [Bart, Henry L.] Tulane Univ, Dept Ecol & Evolutionary Biol, New Orleans, LA 70118 USA. [Bart, Henry L.] Tulane Univ, Museum Nat Hist, Belle Chasse, LA 70037 USA. [He, Shunping] Chinese Acad Sci, Inst Hydrobiol, Wuhan 430072, Hubei, Peoples R China. [Saitoh, Kenji] Res Ctr Aquat Genom, Natl Res Inst Fisheries Sci, Yokohama, Kanagawa 2368648, Japan. [Simons, Andrew M.] Univ Minnesota, Dept Fisheries Wildlife & Conservat Biol, St Paul, MN 55108 USA. RP Tang, KL (reprint author), Univ Michigan, Dept Biol, Flint, MI 48502 USA. EM kltang@umflint.edu; agnewmk@slu.edu; hirt0021@umn.edu; dntobing@gwmail.gwu.edu; Morgan.Raley@naturalsciences.org; zacco_evolans@yahoo.co.jp; vteoh@bama.ua.edu; leiyangslu@gmail.com; hank@museum.tulane.edu; pharris@bama.ua.edu; clad@ihb.ac.cn; miya@chiba-muse.or.jp; ksaitoh@affrc.go.jp; asimons@umn.edu; wood2@slu.edu; maydenrl@slu.edu RI Bart, Henry/L-5354-2014 OI Bart, Henry/0000-0002-5662-9444 FU National Science Foundation (USA) [EF 0431326, EF 0431132, DEB 0431259] FX This research was supported by the National Science Foundation (USA) Assembling the Tree of Life grants EF 0431326 (Mayden/Wood), EF 0431132 (Simons), and DEB 0431259 (Bart). We are indebted to H. Takeuchi (Kinki University) who provided some key specimens for this study. The authors wish to acknowledge the Willi Hennig Society for making the TNT software freely available. Comments and suggestions from two anonymous reviewers greatly improved the final manuscript. NR 150 TC 4 Z9 4 U1 2 U2 25 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 20 PY 2013 VL 3681 IS 2 BP 101 EP 135 DI 10.11646/zootaxa.3681.2.1 PG 35 WC Zoology SC Zoology GA 166WX UT WOS:000320591500001 PM 25232592 ER PT J AU Aliu, E Archambault, S Arlen, T Aune, T Beilicke, M Benbow, W Bird, R Bouvier, A Bradbury, SM Buckley, JH Bugaev, V Byrum, K Cannon, A Cesarini, A Ciupik, L Collins-Hughes, E Connolly, MP Cui, W Dickherber, R Duke, C Dumm, J Dwarkadas, VV Errando, M Falcone, A Federici, S Feng, Q Finley, JP Finnegan, G Fortson, L Furniss, A Galante, N Gall, D Gillanders, GH Godambe, S Gotthelf, EV Griffin, S Grube, J Gyuk, G Hanna, D Holder, J Huan, H Hughes, G Humensky, TB Kaaret, P Karlsson, N Kertzman, M Khassen, Y Kieda, D Krawczynski, H Krennrich, F Lang, MJ Lee, K Madhavan, AS Maier, G Majumdar, P McArthur, S McCann, A Millis, J Moriarty, P Mukherjee, R Nelson, T de Bhroithe, AO Ong, RA Orr, M Otte, AN Pandel, D Park, N Perkins, JS Pohl, M Popkow, A Prokoph, H Quinn, J Ragan, K Reyes, LC Reynolds, PT Roache, E Rose, HJ Ruppel, J Saxon, DB Schroedter, M Sembroski, GH Senturk, GD Skole, C Telezhinsky, I Tesic, G Theiling, M Thibadeau, S Tsurusaki, K Tyler, J Varlotta, A Vassiliev, VV Vincent, S Wakely, SP Ward, JE Weekes, TC Weinstein, A Weisgarber, T Welsing, R Williams, DA Zitzer, B AF Aliu, E. Archambault, S. Arlen, T. Aune, T. Beilicke, M. Benbow, W. Bird, R. Bouvier, A. Bradbury, S. M. Buckley, J. H. Bugaev, V. Byrum, K. Cannon, A. Cesarini, A. Ciupik, L. Collins-Hughes, E. Connolly, M. P. Cui, W. Dickherber, R. Duke, C. Dumm, J. Dwarkadas, V. V. Errando, M. Falcone, A. Federici, S. Feng, Q. Finley, J. P. Finnegan, G. Fortson, L. Furniss, A. Galante, N. Gall, D. Gillanders, G. H. Godambe, S. Gotthelf, E. V. Griffin, S. Grube, J. Gyuk, G. Hanna, D. Holder, J. Huan, H. Hughes, G. Humensky, T. B. Kaaret, P. Karlsson, N. Kertzman, M. Khassen, Y. Kieda, D. Krawczynski, H. Krennrich, F. Lang, M. J. Lee, K. Madhavan, A. S. Maier, G. Majumdar, P. McArthur, S. McCann, A. Millis, J. Moriarty, P. Mukherjee, R. Nelson, T. de Bhroithe, A. O'Faolain Ong, R. A. Orr, M. Otte, A. N. Pandel, D. Park, N. Perkins, J. S. Pohl, M. Popkow, A. Prokoph, H. Quinn, J. Ragan, K. Reyes, L. C. Reynolds, P. T. Roache, E. Rose, H. J. Ruppel, J. Saxon, D. B. Schroedter, M. Sembroski, G. H. Sentuerk, G. D. Skole, C. Telezhinsky, I. Tesic, G. Theiling, M. Thibadeau, S. Tsurusaki, K. Tyler, J. Varlotta, A. Vassiliev, V. V. Vincent, S. Wakely, S. P. Ward, J. E. Weekes, T. C. Weinstein, A. Weisgarber, T. Welsing, R. Williams, D. A. Zitzer, B. TI DISCOVERY OF TeV GAMMA-RAY EMISSION TOWARD SUPERNOVA REMNANT SNR G78.2+2.1 SO ASTROPHYSICAL JOURNAL LA English DT Article DE acceleration of particles; cosmic rays; gamma rays: general; ISM: supernova remnants ID PARTICLE-ACCELERATION; FERMI; HESS; SEARCH; COUNTERPART; 2CG078+2; CATALOG; ORIGIN AB We report the discovery of an unidentified, extended source of very-high-energy gamma-ray emission, VER J2019+407, within the radio shell of the supernova remnant SNR G78.2+2.1, using 21.4 hr of data taken by the VERITAS gamma-ray observatory in 2009. These data confirm the preliminary indications of gamma-ray emission previously seen in a two-year (2007-2009) blind survey of the Cygnus region by VERITAS. VER J2019+407, which is detected at a post-trials significance of 7.5 standard deviations in the 2009 data, is localized to the northwestern rim of the remnant in a region of enhanced radio and X-ray emission. It has an intrinsic extent of 0 degrees.23 +/- 0 degrees.03(stat-0 degrees.02sys)(+0 degrees.04) and its spectrum is well-characterized by a differential power law (dN/dE = N-0 x (E/TeV)-Gamma) with a photon index of Gamma = 2.37 +/- 0.14(stat) +/- 0.20(sys) and a flux normalization of N-0 = 1.5 +/- 0.2(stat) +/- 0.4(sys) x 10(-12) photon TeV-1 cm(-2) s(-1). This yields an integral flux of 5.2 +/- 0.8(stat) +/- 1.4(sys) x 10(-12) photon cm(-2) s(-1) above 320 GeV, corresponding to 3.7% of the Crab Nebula flux. We consider the relationship of the TeV gamma-ray emission with the GeV gamma-ray emission seen from SNR G78.2+2.1 as well as that seen from a nearby cocoon of freshly accelerated cosmic rays. Multiple scenarios are considered as possible origins for the TeV gamma-ray emission, including hadronic particle acceleration at the SNR shock. C1 [Aliu, E.; Errando, M.; Mukherjee, R.] Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. [Archambault, S.; Griffin, S.; Hanna, D.; Ragan, K.; Tesic, G.; Tyler, J.] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Arlen, T.; Aune, T.; Majumdar, P.; Ong, R. A.; Popkow, A.; Vassiliev, V. V.] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. [Beilicke, M.; Buckley, J. H.; Bugaev, V.; Dickherber, R.; Krawczynski, H.; Lee, K.; Thibadeau, S.; Ward, J. E.] Washington Univ, Dept Phys, St Louis, MO 63130 USA. [Benbow, W.; Galante, N.; Roache, E.; Schroedter, M.; Weekes, T. C.] Harvard Smithsonian Ctr Astrophys, Fred Lawrence Whipple Observ, Amado, AZ 85645 USA. [Bird, R.; Cannon, A.; Collins-Hughes, E.; Khassen, Y.; de Bhroithe, A. O'Faolain; Quinn, J.] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Bouvier, A.; Furniss, A.; Williams, D. A.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Bradbury, S. M.; Rose, H. J.] Univ Leeds, Sch Phys & Astron, Leeds LS2 9JT, W Yorkshire, England. [Byrum, K.; Zitzer, B.] Argonne Natl Lab, Argonne, IL 60439 USA. [Cesarini, A.; Connolly, M. P.; Gillanders, G. H.; Lang, M. J.] Natl Univ Ireland Galway, Sch Phys, Galway, Ireland. [Ciupik, L.; Grube, J.; Gyuk, G.] Adler Planetarium & Astron Museum, Dept Astron, Chicago, IL 60605 USA. [Cui, W.; Feng, Q.; Finley, J. P.; Sembroski, G. H.; Theiling, M.; Varlotta, A.] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Duke, C.] Grinnell Coll, Dept Phys, Grinnell, IA 50112 USA. [Dumm, J.; Fortson, L.; Karlsson, N.; Nelson, T.] Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. [Dwarkadas, V. V.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Falcone, A.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Federici, S.; Hughes, G.; Maier, G.; Pohl, M.; Prokoph, H.; Ruppel, J.; Skole, C.; Telezhinsky, I.; Vincent, S.; Welsing, R.] DESY, D-15738 Zeuthen, Germany. [Federici, S.; Pohl, M.; Ruppel, J.; Telezhinsky, I.] Univ Potsdam, Inst Phys & Astron, D-14476 Potsdam, Germany. [Finnegan, G.; Godambe, S.; Kieda, D.] Univ Utah, Dept Phys & Astron, Salt Lake City, UT 84112 USA. [Gall, D.; Kaaret, P.; Tsurusaki, K.] Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. [Gotthelf, E. V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Holder, J.; Saxon, D. B.] Univ Delaware, Dept Phys & Astron, Newark, DE 19716 USA. [Holder, J.; Saxon, D. B.] Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. [Huan, H.; McArthur, S.; Park, N.; Wakely, S. P.; Weisgarber, T.] Univ Chicago, Enrico Fermi Inst, Chicago, IL 60637 USA. [Humensky, T. B.; Sentuerk, G. D.] Columbia Univ, Dept Phys, New York, NY 10027 USA. [Kertzman, M.] Depauw Univ, Dept Phys & Astron, Greencastle, IN 46135 USA. [Krennrich, F.; Madhavan, A. S.; Orr, M.; Weinstein, A.] Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. [Majumdar, P.] Saha Inst Nucl Phys, Kolkata 700064, India. [McCann, A.] Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA. [Millis, J.] Anderson Univ, Dept Phys, Anderson, IN 46012 USA. [Moriarty, P.] Galway Mayo Inst Technol, Dept Life & Phys Sci, Galway, Ireland. [Otte, A. N.] Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA. [Otte, A. N.] Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Pandel, D.] Grand Valley State Univ, Dept Phys, Allendale, MI 49401 USA. [Perkins, J. S.] NASA GSFC, CRESST, Greenbelt, MD 20771 USA. [Perkins, J. S.] NASA GSFC, Astroparticle Phys Lab, Greenbelt, MD 20771 USA. [Perkins, J. S.] Univ Maryland, Baltimore, MD 21250 USA. [Reyes, L. C.] Calif Polytech State Univ San Luis Obispo, Dept Phys, San Luis Obispo, CA 94307 USA. [Reynolds, P. T.] Cork Inst Technol, Dept Appl Phys & Instrumentat, Cork, Ireland. RP Aliu, E (reprint author), Columbia Univ Barnard Coll, Dept Phys & Astron, New York, NY 10027 USA. EM amandajw@iastate.edu RI Khassen, Yerbol/I-3806-2015; OI Khassen, Yerbol/0000-0002-7296-3100; Cui, Wei/0000-0002-6324-5772; Cesarini, Andrea/0000-0002-8611-8610; Ward, John E/0000-0003-1973-0794; Pandel, Dirk/0000-0003-2085-5586; Lang, Mark/0000-0003-4641-4201; Bird, Ralph/0000-0002-4596-8563 FU U.S. Department of Energy Office of Science; U.S. National Science Foundation; Smithsonian Institution; NSERC in Canada; Science Foundation Ireland [SFI 10/RFP/AST2748]; Science and Technology Facilities Council in the UK; NASA [NNX11A086G] FX This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, by the Science Foundation Ireland (SFI 10/RFP/AST2748) and by the Science and Technology Facilities Council in the UK. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. Dr. Weinstein and Dr. Dwarkadas' research was also supported in part by NASA grant NNX11A086G. NR 35 TC 17 Z9 17 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR 93 DI 10.1088/0004-637X/770/2/93 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200011 ER PT J AU Barnard, R Garcia, MR Murray, SS AF Barnard, R. Garcia, M. R. Murray, S. S. TI CHANDRA IDENTIFICATION OF 26 NEW BLACK HOLE CANDIDATES IN THE CENTRAL REGION OF M31 SO ASTROPHYSICAL JOURNAL LA English DT Article DE black hole physics; X-rays: binaries; X-rays: general ID X-RAY BINARIES; HUBBLE-SPACE-TELESCOPE; GLOBULAR-CLUSTERS; NEUTRON-STAR; XMM-NEWTON; SPECTRAL TRANSITIONS; UPDATED SURVEY; XTE J1701-462; ACCRETION; BRIGHT AB We have previously identified 10 M31 black hole candidates (BHCs) in M31 from their X-ray properties alone. They exhibit "hard state" emission spectra that are seen at luminosities less than or similar to 10% Eddington in X-ray binaries (XBs) containing a neutron star (NS) or black hole, at luminosities that significantly exceed the NS threshold. Nine of these are associated with globular clusters (GCs); hence, these are most likely low mass X-ray binaries; eight are included in this survey. We have recently discovered that analysis of the long term 0.5-4.5 keV variability of XBs via structure functions allows us to separate XBs from active galactic nuclei, even though the emission spectra are often similar; this has enabled us to search for BHCs outside of GCs. We have identified 26 new BHCs (12 strong, 14 plausible) within 20' of the M31 nucleus (M31*), using 152 Chandra observations spaced over similar to 13 yr; some of our classifications were enhanced with XMM-Newton observations. Of these, seven appear within 100 '' of M31*; this supports the theory suggesting that this region experiences enhanced XB production via dynamical processes similar to those seen in GCs. We have found a parameter space where our BHCs are separated from Galactic NS binaries: we show that modeling a simulated hard state spectrum with a disk blackbody + blackbody model yields parameters that lie outside the space occupied by NS binaries that are modeled this way. The probability that our BHCs all lie within the NS parameter space is similar to 3 x 10(-29). C1 [Barnard, R.; Garcia, M. R.; Murray, S. S.] Harvard Smithsonian Ctr Astrophys CFA, Cambridge, MA 02138 USA. [Murray, S. S.] Johns Hopkins Univ, Baltimore, MD USA. RP Barnard, R (reprint author), Harvard Smithsonian Ctr Astrophys CFA, Cambridge, MA 02138 USA. FU ESA member states; US (NASA); Chandra [GO0-11106X, GO1-12109X]; HST [GO-11833, GO-12014]; NASA [NAS8-03060] FX We thank the referee for their thoughtful comments. We thank Z. Li for merging the Chandra data. This research has made use of data obtained from the Chandra data archive and software provided by the Chandra X-ray Center (CXC). We also include analysis of data from XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA member states and the US (NASA). R.B. is funded by Chandra grants GO0-11106X and GO1-12109X, along with HST grants GO-11833 and GO-12014. M.R.G. and S.S.M. are partially supported by NASA contract NAS8-03060. NR 48 TC 11 Z9 11 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 20 PY 2013 VL 770 IS 2 AR UNSP 148 DI 10.1088/0004-637X/770/2/148 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200066 ER PT J AU Bowen, TA Testa, P Reeves, KK AF Bowen, Trevor A. Testa, Paola Reeves, Katharine K. TI MULTI-WAVELENGTH OBSERVATIONS OF SOLAR FLARES WITH A CONSTRAINED PEAK X-RAY FLUX SO ASTROPHYSICAL JOURNAL LA English DT Article DE Sun: corona; Sun: flares; Sun: UV radiation; Sun: X-rays, gamma rays ID STATISTICAL-ANALYSIS; EMISSION MEASURE; ATOMIC DATABASE; STELLAR FLARES; SCALING LAWS; LOOPS; DECAY; TEMPERATURE; ENERGETICS; DYNAMICS AB We present an analysis of soft X-ray (SXR) and extreme-ultraviolet (EUV) observations of solar flares with an approximate C8 Geostationary Operational Environmental Satellite (GOES) class. Our constraint on peak GOES SXR flux allows for the investigation of correlations between various flare parameters. We show that the duration of the decay phase of a flare is proportional to the duration of its rise phase. Additionally, we show significant correlations between the radiation emitted in the flare rise and decay phases. These results suggest that the total radiated energy of a given flare is proportional to the energy radiated during the rise phase alone. This partitioning of radiated energy between the rise and decay phases is observed in both SXR and EUV wavelengths. Though observations from the EUV Variability Experiment show significant variation in the behavior of individual EUV spectral lines during different C8 events, this work suggests that broadband EUV emission is well constrained. Furthermore, GOES and Atmospheric Imaging Assembly data allow us to determine several thermal parameters (e.g., temperature, volume, density, and emission measure) for the flares within our sample. Analysis of these parameters demonstrate that, within this constrained GOES class, the longer duration solar flares are cooler events with larger volumes capable of emitting vast amounts of radiation. The shortest C8 flares are typically the hottest events, smaller in physical size, and have lower associated total energies. These relationships are directly comparable with several scaling laws and flare loop models. C1 [Bowen, Trevor A.; Testa, Paola; Reeves, Katharine K.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Bowen, Trevor A.] Marlboro Coll, Marlboro, VT 05344 USA. RP Bowen, TA (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM tbowen@cfa.harvard.edu RI Reeves, Katharine/P-9163-2014 FU Lockheed-Martin [SP02H1701R]; NSF REU solar physics program at Harvard Smithsonian Center for Astrophysics [ATM-0851866]; NASA [NNM07AB07C] FX The authors would like to thank Ryan Milligan, John Raymond, and Phil Chamberlin for input which has greatly improved this paper. T.B., P.T., K.R., were supported by contract SP02H1701R from Lockheed-Martin to Smithsonian Astrophysical Observatory. T.B. was partially supported under the NSF REU solar physics program at Harvard Smithsonian Center for Astrophysics, grant number ATM-0851866. P.T. also acknowledges support by NASA contract NNM07AB07C to the Smithsonian Astrophysical Observatory. NR 36 TC 1 Z9 1 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR 126 DI 10.1088/0004-637X/770/2/126 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200044 ER PT J AU Brown, JM Pontoppidan, KM van Dishoeck, EF Herczeg, GJ Blake, GA Smette, A AF Brown, J. M. Pontoppidan, K. M. van Dishoeck, E. F. Herczeg, G. J. Blake, G. A. Smette, A. TI VLT-CRIRES SURVEY OF ROVIBRATIONAL CO EMISSION FROM PROTOPLANETARY DISKS SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: general; protoplanetary disks; stars: formation; stars: pre-main sequence; stars: protostars ID T-TAURI STARS; YOUNG CIRCUMSTELLAR DISKS; INTERMEDIATE-MASS STARS; PLANET-FORMING ZONES; R-CORONAE-AUSTRALIS; HERBIG AE/BE STARS; SPITZER C2D SURVEY; MOLECULAR CLOUD; SPECTROSCOPIC SURVEY; TRANSITIONAL DISKS AB We present a large, comprehensive survey of rovibrational CO line emission at 4.7 mu m from 69 protoplanetary disks, obtained with CRIRES on the ESO Very Large Telescope at the highest available spectral resolving power (R = 95,000, Delta v = 3.2 km s(-1)). The CO fundamental band (Delta v = 1) is a well-known tracer of warm gas in the inner, planet-forming regions of gas-rich disks around young stars, with the lines formed in the super-heated surfaces of the disks at radii of 0.1-10 AU. Consistent with earlier studies, the presence of 100-1000 K CO is found to be ubiquitous around young stars which still retain disks. Our high spectral resolution data provide new insight into the kinematics of the inner disk gas. The observed line profiles are complex and reveal several different components. Pure double-peaked Keplerian profiles are surprisingly uncommon in our sample, beyond the frequency expected based on disk inclination. The majority of the profiles are consistent with emission from a disk plus a slow (few km s(-1)) molecular disk wind. This is evidenced by analysis of different classes as well as an overall tendency for line profiles to have excess emission on their blue side. The data support the notion that thermal molecular winds are common for young disks. Thanks to the high spectral resolution, narrow absorption lines and weak emission lines from isotopologues and from vibrationally excited levels are readily detected. In general, (CO)-C-13 lines trace cooler gas than the bulk (CO)-C-12 emission and may arise from further out in the disk, as indicated by narrower line profiles. A high fraction of the sources show vibrationally excited emission (similar to 50%) which is correlated with accretion luminosity, consistent with ultraviolet fluorescent excitation. Disks around early-type Herbig AeBe stars have narrower line profiles, on average, than their lower-mass late-type counterparts, due to their increased luminosity. Evolutionary changes in CO are also seen. Removal of the protostellar envelope between class I and II results in the disappearance of the strong absorption lines and CO ice feature characteristic of class I spectra. However, CO emission from class I and II objects are similar in detection frequency, excitation, and line shape, indicating that inner disk characteristics are established early. C1 [Brown, J. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Brown, J. M.; van Dishoeck, E. F.] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Pontoppidan, K. M.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [van Dishoeck, E. F.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Herczeg, G. J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Blake, G. A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Smette, A.] ESO, Vitacura, Chile. RP Brown, JM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St,MS 78, Cambridge, MA 02138 USA. EM joannabrown@cfa.harvard.edu OI Herczeg, Gregory/0000-0002-7154-6065 FU Smithsonian Astrophysical Observatory; NASA [01201.01, NAS 5-26555]; Space Telescope Science Institute; Netherlands Organization for Scientific Research (NWO) [614.000.605]; Netherlands Research School for Astronomy (NOVA) FX The authors thank Colette Salyk, Jeanette Bast, Wing-Fai Thi, Bill Dent, and Kevin France for discussions and contributions to the program. We also thank the anonymous referee for comments which improved this paper. This work is based on observations collected at the European Southern Observatory Very Large Telescope under program ID 179.C-0151. J.M.B. acknowledges the Smithsonian Astrophysical Observatory for support from a SMA fellowship. Support for K.M.P. was provided by NASA through Hubble Fellowship grant no. 01201.01 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. Astrochemistry at Leiden is supported by a Spinoza grant from the Netherlands Organization for Scientific Research (NWO), by NWO grant 614.000.605, and by the Netherlands Research School for Astronomy (NOVA). NR 93 TC 31 Z9 31 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR UNSP 94 DI 10.1088/0004-637X/770/2/94 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200012 ER PT J AU Burkhart, B Lazarian, A Goodman, A Rosolowsky, E AF Burkhart, Blakesley Lazarian, A. Goodman, Alyssa Rosolowsky, Erik TI HIERARCHICAL STRUCTURE OF MAGNETOHYDRODYNAMIC TURBULENCE IN POSITION-POSITION-VELOCITY SPACE SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: structure; magnetohydrodynamics (MHD); turbulence ID SPECTRAL CORRELATION-FUNCTION; SMALL-MAGELLANIC-CLOUD; MOLECULAR CLOUDS; STAR-FORMATION; INTERSTELLAR TURBULENCE; POWER SPECTRUM; ASTROPHYSICAL IMPLICATIONS; COORDINATE SPECTRUM; ALFVENIC TURBULENCE; MAGNETIZED CLOUDS AB Magnetohydrodynamic turbulence is able to create hierarchical structures in the interstellar medium (ISM) that are correlated on a wide range of scales via the energy cascade. We use hierarchical tree diagrams known as dendrograms to characterize structures in synthetic position-position-velocity (PPV) emission cubes of isothermal magnetohydrodynamic turbulence. We show that the structures and degree of hierarchy observed in PPV space are related to the presence of self-gravity and the global sonic and Alfvenic Mach numbers. Simulations with higher Alfvenic Mach number, self-gravity and supersonic flows display enhanced hierarchical structure. We observe a strong dependency on the sonic and Alfvenic Mach numbers and self-gravity when we apply the statistical moments (i.e., mean, variance, skewness, kurtosis) to the leaf and node distribution of the dendrogram. Simulations with self-gravity, larger magnetic field and higher sonic Mach number have dendrogram distributions with higher statistical moments. Application of the dendrogram to three-dimensional density cubes, also known as position-position-position (PPP) cubes, reveals that the dominant emission contours in PPP and PPV are related for supersonic gas but not for subsonic. We also explore the effects of smoothing, thermal broadening, and velocity resolution on the dendrograms in order to make our study more applicable to observational data. These results all point to hierarchical tree diagrams as being a promising additional tool for studying ISM turbulence and star forming regions for obtaining information on the degree of self-gravity, the Mach numbers and the complicated relationship between PPV and PPP data. C1 [Burkhart, Blakesley; Lazarian, A.] Univ Wisconsin, Dept Astron, Madison, WI 53711 USA. [Goodman, Alyssa] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rosolowsky, Erik] Univ British Columbia, Kelowna, BC V1V 1V7, Canada. RP Burkhart, B (reprint author), Univ Wisconsin, Dept Astron, 475 N Charter St, Madison, WI 53711 USA. RI Goodman, Alyssa/A-6007-2010 OI Goodman, Alyssa/0000-0003-1312-0477 FU NSF Graduate Research Fellowship; NASA Wisconsin Space Grant Institution; NSF [AST 1212096, AST-0908159]; Center for Magnetic Self-Organization in Astrophysical and Laboratory Plasmas; Discovery Grant from NSERC of Canada FX The authors thank Professor Diego Falceta-Goncalves for the use of the self-gravitating simulation and useful discussions. B.B also thanks Professor Jungyeon Cho for helpful discussion. B.B. acknowledges support from the NSF Graduate Research Fellowship and the NASA Wisconsin Space Grant Institution. B.B. is thankful for valuable discussions and the use of the Dendrogui code via Chris Beaumont. A.L. thanks NSF grant AST 1212096 and A.L. and B.B. thank the Center for Magnetic Self-Organization in Astrophysical and Laboratory Plasmas for financial support. Most of the work was done during the stay of A.L. as Alexander-von-Humboldt-Preistrager at the RuhrUniversity Bochum. A.L. also thanks the International Institute of Physics in Natal for its hospitality at the final stages of editing the paper. A.G. acknowledges support from NSF Grant No. AST-0908159. E.R. is supported by a Discovery Grant from NSERC of Canada. NR 85 TC 12 Z9 12 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR 141 DI 10.1088/0004-637X/770/2/141 PG 16 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200059 ER PT J AU Green, JD Evans, NJ Jorgensen, JK Herczeg, GJ Kristensen, LE Lee, JE Dionatos, O Yildiz, UA Salyk, C Meeus, G Bouwman, J Visser, R Bergin, EA van Dishoeck, EF Rascati, MR Karska, A van Kempen, TA Dunham, MM Lindberg, JE Fedele, D AF Green, Joel D. Evans, Neal J., II Jorgensen, Jes K. Herczeg, Gregory J. Kristensen, Lars E. Lee, Jeong-Eun Dionatos, Odysseas Yildiz, Umut A. Salyk, Colette Meeus, Gwendolyn Bouwman, Jeroen Visser, Ruud Bergin, Edwin A. van Dishoeck, Ewine F. Rascati, Michelle R. Karska, Agata van Kempen, Tim A. Dunham, Michael M. Lindberg, Johan E. Fedele, Davide CA DIGIT Team TI EMBEDDED PROTOSTARS IN THE DUST, ICE, AND GAS IN TIME (DIGIT) HERSCHEL KEY PROGRAM: CONTINUUM SEDs, AND AN INVENTORY OF CHARACTERISTIC FAR-INFRARED LINES FROM PACS SPECTROSCOPY SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; stars: formation; stars: pre-main sequence; stars: winds, outflows; submillimeter: stars ID SPITZER-SPACE-TELESCOPE; LOW-MASS PROTOSTARS; YOUNG STELLAR OBJECTS; STAR-FORMING REGIONS; ISO-LWS OBSERVATIONS; OPHIUCHI MOLECULAR CLOUD; T-TAURI STARS; EVOLUTIONARY SIGNATURES; LEGACY CLOUDS; SHOCK-WAVES AB We present 50-210 mu m spectral scans of 30 Class 0/I protostellar sources, obtained with Herschel-PACS, and 0.5-1000 mu m spectral energy distributions, as part of the Dust, Ice, and Gas in Time Key Program. Some sources exhibit up to 75 H2O lines ranging in excitation energy from 100 to 2000 K, 12 transitions of OH, and CO rotational lines ranging from J = 14 -> 13 up to J = 40 -> 39. [O I] is detected in all but one source in the entire sample; among the sources with detectable [O I] are two very low luminosity objects. The mean 63/145 mu m [O I] flux ratio is 17.2 +/- 9.2. The [O I] 63 mu m line correlates with L-bol, but not with the time-averaged outflow rate derived from low-J CO maps. [C II] emission is in general not local to the source. The sample L-bol increased by 1.25 (1.06) and T-bol decreased to 0.96 (0.96) of mean (median) values with the inclusion of the Herschel data. Most CO rotational diagrams are characterized by two optically thin components (< N > = ( 0.70 +/- 1.12) x 10(49) total particles). N-CO correlates strongly with L-bol, but neither T-rot nor N-CO(warm)/N-CO(hot) correlates with L-bol, suggesting that the total excited gas is related to the current source luminosity, but that the excitation is primarily determined by the physics of the interaction (e.g., UV-heating/shocks). Rotational temperatures for H2O (< T-rot > = 194 +/- 85 K) and OH (< T-rot > = 183 +/- 117 K) are generally lower than for CO, and much of the scatter in the observations about the best fit is attributed to differences in excitation conditions and optical depths among the detected lines. C1 [Green, Joel D.; Evans, Neal J., II; Rascati, Michelle R.] Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. [Jorgensen, Jes K.; Dionatos, Odysseas; Lindberg, Johan E.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Jorgensen, Jes K.; Dionatos, Odysseas; Lindberg, Johan E.] Univ Copenhagen, Nat Hist Museum Denmark, Ctr Star & Planet Format, DK-1350 Copenhagen, Denmark. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Herczeg, Gregory J.; van Dishoeck, Ewine F.; Karska, Agata; Fedele, Davide] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. [Kristensen, Lars E.; Yildiz, Umut A.; van Dishoeck, Ewine F.; van Kempen, Tim A.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [Kristensen, Lars E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02183 USA. [Lee, Jeong-Eun] Kyung Hee Univ, Dept Astron & Space Sci, Gyeonggi 446701, South Korea. [Dionatos, Odysseas] Univ Vienna, Dept Astron, A-1180 Vienna, Austria. [Salyk, Colette] Natl Opt Astron Observ, Tucson, AZ 85719 USA. [Meeus, Gwendolyn] Univ Autonoma Madrid, Dpt Fis Teor, E-28049 Madrid, Spain. [Bouwman, Jeroen] Max Planck Inst Astron, D-69117 Heidelberg, Germany. [Visser, Ruud; Bergin, Edwin A.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [van Kempen, Tim A.] Joint ALMA Off, Santiago, Chile. [Dunham, Michael M.] Yale Univ, Dept Astron, New Haven, CT 06511 USA. RP Green, JD (reprint author), Univ Texas Austin, Dept Astron, 2515 Speedway,Stop C1400, Austin, TX 78712 USA. EM joel@astro.as.utexas.edu RI Fedele, Davide/L-8688-2013; Lee , Jeong-Eun/E-2387-2013; Yildiz, Umut/C-5257-2011; Kristensen, Lars/F-4774-2011; Karska, Agata/O-5311-2016; OI Herczeg, Gregory/0000-0002-7154-6065; Fedele, Davide/0000-0001-6156-0034; Yildiz, Umut/0000-0001-6197-2864; Kristensen, Lars/0000-0003-1159-3721; Karska, Agata/0000-0001-8913-925X; Lindberg, Johan/0000-0003-3811-4591; Dionatos, Odysseas/0000-0002-2689-8870 FU Herschel Open Time Key Project Program; NASA; Junior Group Leader Fellowship from the Lundbeck Foundation; Instrument Center for Danish Astrophysics; Danish National Research Foundation; University of Copenhagen's program of excellence; Basic Science Research Program through the National Research Foundation of Korea (NRF); Ministry of Education, Science and Technology [2012-0002330, 2012-044689] FX Support for this work, part of the Herschel Open Time Key Project Program, was provided by NASA through an award issued by the Jet Propulsion Laboratory, California Institute of Technology. The research of J.K.J., O.D., and J.L. was supported by a Junior Group Leader Fellowship from the Lundbeck Foundation and a grant from the Instrument Center for Danish Astrophysics. The research at the Centre for Star and Planet Formation is supported by the Danish National Research Foundation and the University of Copenhagen's program of excellence. The research of J.-E.L. is supported by Basic Science Research Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Education, Science and Technology (No. 2012-0002330 and No. 2012-044689). J.D.G. would like to acknowledge numerous helpful discussions with Isa Oliveira, Manoj Puravankara, Augusto Carballido, John Lacy, Dan Jaffe, Tom Megeath, Dan Watson, and Emma Yu. We thank the anonymous referee for extensive comments that greatly improved the manuscript. NR 96 TC 45 Z9 45 U1 0 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR 123 DI 10.1088/0004-637X/770/2/123 PG 45 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200041 ER PT J AU Harrison, FA Craig, WW Christensen, FE Hailey, CJ Zhang, WW Boggs, SE Stern, D Cook, WR Forster, K Giommi, P Grefenstette, BW Kim, Y Kitaguchi, T Koglin, JE Madsen, KK Mao, PH Miyasaka, H Mori, K Perri, M Pivovaroff, MJ Puccetti, S Rana, VR Westergaard, NJ Willis, J Zoglauer, A An, HJ Bachetti, M Barriere, NM Bellm, EC Bhalerao, V Brejnholt, NF Fuerst, F Liebe, CC Markwardt, CB Nynka, M Vogel, JK Walton, DJ Wik, DR Alexander, DM Cominsky, LR Hornschemeier, AE Hornstrup, A Kaspi, VM Madejski, GM Matt, G Molendi, S Smith, DM Tomsick, JA Ajello, M Ballantyne, DR Balokovic, M Barret, D Bauer, FE Blandford, RD Brandt, WN Brenneman, LW Chiang, J Chakrabarty, D Chenevez, J Comastri, A Dufour, F Elvis, M Fabian, AC Farrah, D Fryer, CL Gotthelf, EV Grindlay, JE Helfand, DJ Krivonos, R Meier, DL Miller, JM Natalucci, L Ogle, P Ofek, EO Ptak, A Reynolds, SP Rigby, JR Tagliaferri, G Thorsett, SE Treister, E Urry, CM AF Harrison, Fiona A. Craig, William W. Christensen, Finn E. Hailey, Charles J. Zhang, William W. Boggs, Steven E. Stern, Daniel Cook, W. Rick Forster, Karl Giommi, Paolo Grefenstette, Brian W. Kim, Yunjin Kitaguchi, Takao Koglin, Jason E. Madsen, Kristin K. Mao, Peter H. Miyasaka, Hiromasa Mori, Kaya Perri, Matteo Pivovaroff, Michael J. Puccetti, Simonetta Rana, Vikram R. Westergaard, Niels J. Willis, Jason Zoglauer, Andreas An, Hongjun Bachetti, Matteo Barriere, Nicolas M. Bellm, Eric C. Bhalerao, Varun Brejnholt, Nicolai F. Fuerst, Felix Liebe, Carl C. Markwardt, Craig B. Nynka, Melania Vogel, Julia K. Walton, Dominic J. Wik, Daniel R. Alexander, David M. Cominsky, Lynn R. Hornschemeier, Ann E. Hornstrup, Allan Kaspi, Victoria M. Madejski, Greg M. Matt, Giorgio Molendi, Silvano Smith, David M. Tomsick, John A. Ajello, Marco Ballantyne, David R. Balokovic, Mislav Barret, Didier Bauer, Franz E. Blandford, Roger D. Brandt, W. Niel Brenneman, Laura W. Chiang, James Chakrabarty, Deepto Chenevez, Jerome Comastri, Andrea Dufour, Francois Elvis, Martin Fabian, Andrew C. Farrah, Duncan Fryer, Chris L. Gotthelf, Eric V. Grindlay, Jonathan E. Helfand, David J. Krivonos, Roman Meier, David L. Miller, Jon M. Natalucci, Lorenzo Ogle, Patrick Ofek, Eran O. Ptak, Andrew Reynolds, Stephen P. Rigby, Jane R. Tagliaferri, Gianpiero Thorsett, Stephen E. Treister, Ezequiel Urry, C. Megan TI THE NUCLEAR SPECTROSCOPIC TELESCOPE ARRAY (NuSTAR) HIGH-ENERGY X-RAY MISSION SO ASTROPHYSICAL JOURNAL LA English DT Article DE space vehicles: instruments; X-rays: general ID ACTIVE GALACTIC NUCLEI; SUPERMASSIVE BLACK-HOLE; DEEP FIELD-SOUTH; SUPERNOVA REMNANT G1.9+0.3; SOFT GAMMA-REPEATERS; MS SOURCE CATALOGS; BROAD IRON LINES; XMM-NEWTON; ASCA OBSERVATIONS; NEUTRON-STAR AB The Nuclear Spectroscopic Telescope Array (NuSTAR) mission, launched on 2012 June 13, is the first focusing high-energy X-ray telescope in orbit. NuSTAR operates in the band from 3 to 79 keV, extending the sensitivity of focusing far beyond the similar to 10 keV high-energy cutoff achieved by all previous X-ray satellites. The inherently low background associated with concentrating the X-ray light enables NuSTAR to probe the hard X-ray sky with a more than 100-fold improvement in sensitivity over the collimated or coded mask instruments that have operated in this bandpass. Using its unprecedented combination of sensitivity and spatial and spectral resolution, NuSTAR will pursue five primary scientific objectives: (1) probe obscured active galactic nucleus (AGN) activity out to the peak epoch of galaxy assembly in the universe (at z less than or similar to 2) by surveying selected regions of the sky; (2) study the population of hard X-ray-emitting compact objects in the Galaxy by mapping the central regions of the Milky Way; (3) study the non-thermal radiation in young supernova remnants, both the hard X-ray continuum and the emission from the radioactive element Ti-44; (4) observe blazars contemporaneously with ground-based radio, optical, and TeV telescopes, as well as with Fermi and Swift, to constrain the structure of AGN jets; and (5) observe line and continuum emission from core-collapse supernovae in the Local Group, and from nearby Type Ia events, to constrain explosion models. During its baseline two-year mission, NuSTAR will also undertake a broad program of targeted observations. The observatory consists of two co-aligned grazing-incidence X-ray telescopes pointed at celestial targets by a three-axis stabilized spacecraft. Deployed into a 600 km, near-circular, 6 degrees inclination orbit, the observatory has now completed commissioning, and is performing consistent with pre-launch expectations. NuSTAR is now executing its primary science mission, and with an expected orbit lifetime of 10 yr, we anticipate proposing a guest investigator program, to begin in late 2014. C1 [Harrison, Fiona A.; Cook, W. Rick; Forster, Karl; Grefenstette, Brian W.; Madsen, Kristin K.; Mao, Peter H.; Miyasaka, Hiromasa; Rana, Vikram R.; Bellm, Eric C.; Bhalerao, Varun; Fuerst, Felix; Walton, Dominic J.; Balokovic, Mislav] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. [Craig, William W.; Pivovaroff, Michael J.; Vogel, Julia K.] Lawrence Livermore Natl Lab, Livermore, CA 94550 USA. [Craig, William W.; Boggs, Steven E.; Zoglauer, Andreas; Barriere, Nicolas M.; Tomsick, John A.; Ajello, Marco; Krivonos, Roman] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. [Christensen, Finn E.; Westergaard, Niels J.; Brejnholt, Nicolai F.; Hornstrup, Allan; Chenevez, Jerome] Tech Univ Denmark, DTU Space, Natl Space Inst, DK-2800 Lyngby, Denmark. [Hailey, Charles J.; Koglin, Jason E.; Mori, Kaya; Nynka, Melania; Gotthelf, Eric V.] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA. [Zhang, William W.; Markwardt, Craig B.; Wik, Daniel R.; Hornschemeier, Ann E.; Ptak, Andrew; Rigby, Jane R.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Stern, Daniel; Kim, Yunjin; Willis, Jason; Liebe, Carl C.; Meier, David L.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. [Giommi, Paolo; Perri, Matteo; Puccetti, Simonetta] ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy. [Kitaguchi, Takao] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy. [Koglin, Jason E.; Madejski, Greg M.] RIKEN, Wako, Saitama 3510198, Japan. [Perri, Matteo; Puccetti, Simonetta; Blandford, Roger D.; Chiang, James] SLAC Natl Accelerator Lab, Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [An, Hongjun; Kaspi, Victoria M.; Dufour, Francois] McGill Univ, Dept Phys, Montreal, PQ H3A 2T8, Canada. [Bachetti, Matteo; Barret, Didier] Univ Toulouse, IRAP, UPS OMP, Toulouse, France. [Bachetti, Matteo; Barret, Didier] CNRS, Inst Rech Astrophys & Planetol, F-31028 Toulouse 4, France. [Bhalerao, Varun] Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. [Alexander, David M.] Univ Durham, Dept Phys, Durham DH1 3LE, England. [Cominsky, Lynn R.] Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA. [Matt, Giorgio] Univ Roma Tre, Dipartimento Matemat & Fis, I-00146 Rome, Italy. [Molendi, Silvano] INAF, IASF Milano, I-20133 Milan, Italy. [Smith, David M.] Univ Calif Santa Cruz, Dept Phys, Santa Cruz, CA 95064 USA. [Smith, David M.] Univ Calif Santa Cruz, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA. [Ballantyne, David R.] Georgia Inst Technol, Sch Phys, Ctr Relativist Astrophys, Atlanta, GA 30332 USA. [Bauer, Franz E.] Pontificia Univ Catolica Chile, Dept Astron & Astrofis, Santiago 22, Chile. [Brandt, W. Niel] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Brandt, W. Niel] Penn State Univ, Inst Gravitat & Cosmos, University Pk, PA 16802 USA. [Brenneman, Laura W.; Elvis, Martin; Grindlay, Jonathan E.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Chakrabarty, Deepto] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Comastri, Andrea] INAF Osservatorio Astron Bologna, I-40127 Bologna, Italy. [Fabian, Andrew C.] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. [Farrah, Duncan] Virginia Tech, Dept Phys, Blacksburg, VA 24061 USA. [Fryer, Chris L.] Los Alamos Natl Lab, CCS 2, Los Alamos, NM 87545 USA. [Helfand, David J.] Quest Univ Canada, Squamish, BC V8B 0N8, Canada. [Miller, Jon M.] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Natalucci, Lorenzo] INAF, Ist Astrofis & Planetol Spaziali, I-00133 Rome, Italy. [Ogle, Patrick] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA. [Ofek, Eran O.] Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel. [Reynolds, Stephen P.] NC State Univ, Dept Phys, Raleigh, NC 27695 USA. [Tagliaferri, Gianpiero] INAF Osservatorio Astron Brera, I-23807 Merate, Italy. [Thorsett, Stephen E.] Willamette Univ, Dept Phys, Salem, OR 97301 USA. [Treister, Ezequiel] Univ Concepcion, Dept Astron, Concepcion, Chile. [Urry, C. Megan] Yale Univ, Dept Phys, New Haven, CT 06520 USA. [Urry, C. Megan] Yale Univ, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. RP Harrison, FA (reprint author), CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 USA. EM fiona@srl.caltech.edu RI Urry, Claudia/G-7381-2011; Rigby, Jane/D-4588-2012; Pivovaroff, Michael/M-7998-2014; Boggs, Steven/E-4170-2015; Brandt, William/N-2844-2015; Comastri, Andrea/O-9543-2015; OI Bachetti, Matteo/0000-0002-4576-9337; Rana, Vikram/0000-0003-1703-8796; Alexander, David/0000-0002-5896-6313; Molendi, Silvano/0000-0002-2483-278X; Tagliaferri, Gianpiero/0000-0003-0121-0723; Puccetti, Simonetta/0000-0002-2734-7835; Urry, Claudia/0000-0002-0745-9792; Rigby, Jane/0000-0002-7627-6551; Pivovaroff, Michael/0000-0001-6780-6816; Boggs, Steven/0000-0001-9567-4224; Brandt, William/0000-0002-0167-2453; Comastri, Andrea/0000-0003-3451-9970; Thorsett, Stephen/0000-0002-2025-9613; giommi, paolo/0000-0002-2265-5003; Bhalerao, Varun/0000-0002-6112-7609; Perri, Matteo/0000-0003-3613-4409 FU NASA [NNG08FD60C]; National Aeronautics and Space Administration; National Space Institute, Technical University of Denmark; Italian Space Agency (ASI); Centre National d'Etudes Spatiales (CNES); NASA Postdoctoral Program; Leverhulme Research Fellowship; U.S. DOE/LLNL; NSERC; CIFAR; FQRNT; Killam Research Fellowship; Science and Technology Facilities Council; NSF AST FX This work was supported under NASA No. NNG08FD60C and made use of data from the Nuclear Spectroscopic Telescope Array (NuSTAR) mission, a project led by Caltech, managed by the Jet Propulsion Laboratory, and funded by the National Aeronautics and Space Administration. Additional support for development was provided by the National Space Institute, Technical University of Denmark. The Malindi ground station is provided by the Italian Space Agency (ASI) and support for science software development by the ASI Science Data Center (ASDC). Science team members acknowledge support from Centre National d'Etudes Spatiales (CNES) (D.B., M.B.), the NASA Postdoctoral Program (D.R.W.), Leverhulme Research Fellowship and Science and Technology Facilities Council (D.M.A), NSF AST (D.R.B.), U.S. DOE/LLNL (W.W.C., M.P., J.V.), NSERC, CIFAR, FQRNT, and Killam Research Fellowship (V.K.). We thank David Burrows (PSU) for useful comments which improved the quality of the manuscript. NR 155 TC 427 Z9 427 U1 3 U2 52 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 2013 VL 770 IS 2 AR UNSP 103 DI 10.1088/0004-637X/770/2/103 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200021 ER PT J AU Ineson, J Croston, JH Hardcastle, MJ Kraft, RP Evans, DA Jarvis, M AF Ineson, J. Croston, J. H. Hardcastle, M. J. Kraft, R. P. Evans, D. A. Jarvis, M. TI RADIO-LOUD ACTIVE GALACTIC NUCLEUS: IS THERE A LINK BETWEEN LUMINOSITY AND CLUSTER ENVIRONMENT? SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies: active; galaxies: jets ID VIRTUALLY COMPLETE REDSHIFTS; MAGNETIC-FIELD STRENGTHS; X-RAY OBSERVATIONS; GALAXY CLUSTERS; XMM-NEWTON; UNIFIED MODELS; OPTICAL SPECTROSCOPY; CHANDRA OBSERVATION; COMPLETE SAMPLE; ABELL CLUSTERS AB We present here the first results from the Chandra ERA (Environments of Radio-loud AGN) Large Project, characterizing the cluster environments of a sample of 26 radio-loud active galactic nuclei (AGNs) at z similar to 0.5 that covers three decades of radio luminosity. This is the first systematic X-ray environmental study at a single epoch, and has allowed us to examine the relationship between radio luminosity and cluster environment without the problems of Malmquist bias. We have found a weak correlation between radio luminosity and host cluster X-ray luminosity, as well as tentative evidence that this correlation is driven by the subpopulation of low-excitation radio galaxies, with high-excitation radio galaxies showing no significant correlation. The considerable scatter in the environments may be indicative of complex relationships not currently included in feedback C1 [Ineson, J.; Croston, J. H.] Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. [Hardcastle, M. J.; Jarvis, M.] Univ Hertfordshire, Sch Phys Astron & Math, Hatfield AL10 9AB, Herts, England. [Kraft, R. P.; Evans, D. A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Jarvis, M.] Univ Oxford, Dept Phys, Oxford OX1 3RH, England. [Jarvis, M.] Univ Western Cape, Dept Phys, ZA-7535 Bellville, South Africa. RP Ineson, J (reprint author), Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. EM J.Croston@soton.ac.uk OI Hardcastle, Martin/0000-0003-4223-1117 FU South-East Physics Network (SEPnet); ESA Member States; NASA FX J.I. and J.C. acknowledge the support of the South-East Physics Network (SEPnet).; The scientific results reported in this article are based on observations made with the Chandra X-Ray Observatory and on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. This research has made use of software provided by the Chandra X-ray Center (CXC) in the application packages ciao and chips, and of the XMM-Newton Science Analysis Software (sas). NR 75 TC 10 Z9 10 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR UNSP 136 DI 10.1088/0004-637X/770/2/136 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200054 ER PT J AU Kipping, DM Hartman, J Buchhave, LA Schmitt, AR Bakos, GA Nesvorny, D AF Kipping, D. M. Hartman, J. Buchhave, L. A. Schmitt, A. R. Bakos, G. A. Nesvorny, D. TI THE HUNT FOR EXOMOONS WITH KEPLER (HEK). II. ANALYSIS OF SEVEN VIABLE SATELLITE-HOSTING PLANET CANDIDATES SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; stars: individual (KOI-174, KOI-303, KOI-365, KOI-722, KOI-1472, KOI-1857, KOI-1876); techniques: photometric ID EXTRASOLAR GIANT PLANETS; TRANSIT LIGHT-CURVE; PHOTOMETRY; STAR; SYSTEMS; MOON AB From the list of 2321 transiting planet candidates announced by the Kepler Mission, we select seven targets with favorable properties for the capacity to dynamically maintain an exomoon and present a detectable signal. These seven candidates were identified through our automatic target selection (TSA) algorithm and target selection prioritization (TSP) filtering, whereby we excluded systems exhibiting significant time-correlated noise and focused on those with a single transiting planet candidate of radius less than 6 R-circle plus. We find no compelling evidence for an exomoon around any of the seven Kepler Objects of Interest (KOIs) but constrain the satellite-to-planet mass ratios for each. For four of the seven KOIs, we estimate a 95% upper quantile of M-S/M-P < 0.04, which given the radii of the candidates, likely probes down to sub-Earth masses. We also derive precise transit times and durations for each candidate and find no evidence for dynamical variations in any of the KOIs. With just a few systems analyzed thus far in the ongoing "Hunt for Exomoons with Kepler" (HEK) project, projections on eta((sic)) would be premature, but a high frequency of large moons around Super-Earths/Mini-Neptunes would appear to be incommensurable with our results so far. C1 [Kipping, D. M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Hartman, J.; Bakos, G. A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Buchhave, L. A.] Univ Copenhagen, Niels Bohr Inst, DK-2100 Copenhagen, Denmark. [Buchhave, L. A.] Univ Copenhagen, Ctr Star & Planet Format, Nat Hist Museum Denmark, DK-1350 Copenhagen, Denmark. [Schmitt, A. R.] Citizen Sci, Cambridge, MA 02138 USA. [Nesvorny, D.] SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. RP Kipping, DM (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM dkipping@cfa.harvard.edu OI Buchhave, Lars A./0000-0003-1605-5666; Hartman, Joel/0000-0001-8732-6166 FU NSF [AST-1108686, AST-1008890]; NASA [NNX12AH91H] FX We would like to thank the anonymous reviewer for their thoughtful comments which improved the quality of our manuscript. This work made use of the Michael Dodds Computing Facility, for which we are grateful to Michael Dodds, Carl Allegretti, David Van Buren, Anthony Grange, Cameron Lehman, Ivan Longland, Dell Lunceford, Gregor Rothfuss, Matt Salzberg, Richard Sundvall, Graham Symmonds, Kenneth Takigawa, Marion Adam, Dour High Arch, Mike Barrett, Greg Cole, Sheena Dean, Steven Delong, Robert Goodman, Mark Greene, Stephen Kitt, Robert Leyland, Matthias Meier, Roy Mitsuoka, David Nicholson, Nicole Papas, Steven Purcell, Austen Redman, Michael Sheldon, Ronald Sonenthal, Nicholas Steinbrecher, Corbin Sydney, John Vajgrt, Louise Valmoria, Hunter Williams, Troy Winarski, and Nigel Wright. D.M.K. is funded by the NASA Carl Sagan Fellowships. J.H. and G.B. acknowledge partial support from NSF grant AST-1108686 and NASA grant NNX12AH91H. D.N. acknowledges support from NSF AST-1008890. Based on observations with the Apache Point Observatory 3.5 m telescope, which is owned and operated by the Astrophysical Research Consortium. We offer our thanks and praise to the extraordinary scientists, engineers, and individuals who have made the Kepler Mission possible. Without their continued efforts and contribution, our project would not be possible. NR 52 TC 36 Z9 36 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR UNSP 101 DI 10.1088/0004-637X/770/2/101 PG 30 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200019 ER PT J AU Lee, HG Moon, DS Koo, BC Rahman, M Eikenberry, SS Gruel, N Onaka, T Kim, HJ Chun, WS Raymond, J Raines, SN Guzman, R AF Lee, Ho-Gyu Moon, Dae-Sik Koo, Bon-Chul Rahman, Mubdi Eikenberry, Stephen S. Gruel, Nicolas Onaka, Takashi Kim, Hyun-Jeong Chun, Won-Seok Raymond, John Raines, S. Nicholas Guzman, Rafael TI WIDE INTEGRAL-FIELD INFRARED SPECTROSCOPY OF THE BRIGHT [Fe II] SHELL IN THE YOUNG SUPERNOVA REMNANT G11.2-0.3 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared: ISM; ISM: individual objects (G11.2-0.3); ISM: supernova remnants; shock waves ID X-RAY OBSERVATIONS; SHOCK-WAVES; STRENGTHS; WIND AB We present the results of wide integral-field near-infrared (1.0-1.8 mu m) spectroscopic observations of the southeastern shell of the young core-collapse supernova remnant (SNR) G11.2-0.3. We first construct [Fe II] 1.644 mu m line images of three bright clumps from the obtained spectral image cubes and compare them with those of other transitions such as [Fe II] 1.257, [Fe II] 1.534, and He I 1.083 mu m line images. This allows us to estimate the electron density (similar to 4700-9400 cm(-3)) and extinction (A(V) similar to 16-20 mag) of the shell, including a detailed two-dimensional distribution of the properties in the brightest clump, as well as the discovery of a faint high-velocity (similar to-440 km s(-1)) component in the clump. Our SNR shock model calculations estimate the pre-shock number density of similar to 250-500 cm(-3) and shock speed of similar to 80-250 km s(-1) in the [Fe II]-emitting region of the SNR. The comparison between the observed and modeled radial profiles of the line intensities and their ratios reveals that the shell is composed of multiple thin filaments which have been likely formed in episodic mass-loss processes of a progenitor star. The discovery of the faint high-velocity component supports the interpretation that the southeastern shell of G11.2-0.3 is mainly composed of circumstellar material with contamination by supernova ejecta and also that its ejected material was expelled primarily in the southeast-northwest direction. C1 [Lee, Ho-Gyu; Onaka, Takashi] Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan. [Lee, Ho-Gyu; Moon, Dae-Sik; Rahman, Mubdi] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Koo, Bon-Chul; Kim, Hyun-Jeong; Chun, Won-Seok] Seoul Natl Univ, Dept Phys & Astron, Seoul 151742, South Korea. [Rahman, Mubdi] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Eikenberry, Stephen S.; Gruel, Nicolas; Raines, S. Nicholas; Guzman, Rafael] Univ Florida, Dept Astron, Gainesville, FL 32611 USA. [Raymond, John] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Lee, HG (reprint author), Univ Tokyo, Grad Sch Sci, Dept Astron, Tokyo 1130033, Japan. EM hglee@astron.s.u-tokyo.ac.jp; moon@astro.utoronto.ca; koo@astro.snu.ac.kr; mubdi@pha.jhu.edu; eiken@astro.ufl.edu; onaka@astron.s.u-tokyo.ac.jp; hjkim@astro.snu.ac.kr; jraymond@cfa.harvard.edu; raines@astro.ufl.edu RI ONAKA, TAKASHI/G-5058-2014; OI Rahman, Mubdi/0000-0003-1842-6096; Gruel, Nicolas/0000-0001-8046-2536 FU Early Research Award; Ministry of Economic Development and Innovation (MEDI) of the Ontario Provincial Government in Canada; Natural Science and Engineering Research Council (NSERC) of Canada; Ministry of Education Science and Technology (MEST); Korean Federation of Science and Technology Societies (KOFST); National Research Foundation of Korea (NRF) [NRF-2010-616-C00020]; Florida Space Research Initiative; [23.01322] FX This work is supported by a Grant-in-Aid for Japan Society of Promotion of Science (JSPS) fellows (No. 23.01322). H.-G. L. was partly supported from Early Research Award to D.-S.M. by the Ministry of Economic Development and Innovation (MEDI) of the Ontario Provincial Government in Canada. D.-S.M. acknowledges support from the Natural Science and Engineering Research Council (NSERC) of Canada. This paper was studied with the support of the Ministry of Education Science and Technology (MEST) and the Korean Federation of Science and Technology Societies (KOFST). B.-C.K. was supported by the National Research Foundation of Korea (NRF) Grant (NRF-2010-616-C00020). FISICA was supported by the Florida Space Research Initiative. NR 25 TC 3 Z9 3 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 20 PY 2013 VL 770 IS 2 AR 143 DI 10.1088/0004-637X/770/2/143 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200061 ER PT J AU Lissauer, JJ Jontof-Hutter, D Rowe, JF Fabrycky, DC Lopez, ED Agol, E Marcy, GW Deck, KM Fischer, DA Fortney, JJ Howell, SB Isaacson, H Jenkins, JM Kolbl, R Sasselov, D Short, DR Welsh, WF AF Lissauer, Jack J. Jontof-Hutter, Daniel Rowe, Jason F. Fabrycky, Daniel C. Lopez, Eric D. Agol, Eric Marcy, Geoffrey W. Deck, Katherine M. Fischer, Debra A. Fortney, Jonathan J. Howell, Steve B. Isaacson, Howard Jenkins, Jon M. Kolbl, Rea Sasselov, Dimitar Short, Donald R. Welsh, William F. TI ALL SIX PLANETS KNOWN TO ORBIT KEPLER-11 HAVE LOW DENSITIES SO ASTROPHYSICAL JOURNAL LA English DT Article DE celestial mechanics; ephemerides; planets and satellites: composition; planets and satellites: dynamical evolution and stability; planets and satellites: fundamental parameters ID TRANSITING SUPER-EARTH; SUN-LIKE STAR; EXTRASOLAR PLANETS; THERMAL EVOLUTION; TIMING VARIATIONS; WARM-SPITZER; CANCRI E; LOW-MASS; SYSTEM; POPULATIONS AB The Kepler-11 planetary system contains six transiting planets ranging in size from 1.8 to 4.2 times the radius of Earth. Five of these planets orbit in a tightly packed configuration with periods between 10 and 47 days. We perform a dynamical analysis of the system based upon transit timing variations observed in more than three years of Kepler photometric data. Stellar parameters are derived using a combination of spectral classification and constraints on the star's density derived from transit profiles together with planetary eccentricity vectors provided by our dynamical study. Combining masses of the planets relative to the star from our dynamical study and radii of the planets relative to the star from transit depths together with deduced stellar properties yields measurements of the radii of all six planets, masses of the five inner planets, and an upper bound to the mass of the outermost planet, whose orbital period is 118 days. We find mass-radius combinations for all six planets that imply that substantial fractions of their volumes are occupied by constituents that are less dense than rock. Moreover, we examine the stability of these envelopes against photoevaporation and find that the compositions of at least the inner two planets have likely been significantly sculpted by mass loss. The Kepler-11 system contains the lowest mass exoplanets for which both mass and radius have been measured. C1 [Lissauer, Jack J.; Jontof-Hutter, Daniel; Rowe, Jason F.; Howell, Steve B.; Jenkins, Jon M.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rowe, Jason F.; Jenkins, Jon M.] NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. [Fabrycky, Daniel C.] Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. [Lopez, Eric D.; Fortney, Jonathan J.] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Marcy, Geoffrey W.; Isaacson, Howard; Kolbl, Rea] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. [Deck, Katherine M.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Deck, Katherine M.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. [Fischer, Debra A.] Yale Univ, Dept Astron, New Haven, CT 06520 USA. [Sasselov, Dimitar] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Short, Donald R.] San Diego State Univ, Dept Math, San Diego, CA 92182 USA. [Welsh, William F.] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Jack.Lissauer@nasa.gov OI Fortney, Jonathan/0000-0002-9843-4354; /0000-0002-0802-9145; Fabrycky, Daniel/0000-0003-3750-0183 FU NASA's Science Mission Directorate; NSF [AST-0645416, AST-1109928]; Kepler Participating Scientist Program via NASA [NNX12AD23G] FX Kepler was competitively selected as the tenth Discovery mission. Funding for this mission is provided by NASA's Science Mission Directorate. E.A.'s work was supported by NSF Career grant AST-0645416. W.F.W. gratefully acknowledges support from the Kepler Participating Scientist Program via NASA grant NNX12AD23G, and from the NSF via grant AST-1109928. D.J. gratefully acknowledges a Fellowship from the NASA Postdoctoral Program. We thank Jerome Orosz and Gur Windmiller for assistance in developing D.S.'s method for measuring transit times and Tony Dobrovolskis, Darin Ragozzine, and Billy Quarles for helpful comments on the manuscript. NR 36 TC 70 Z9 70 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 20 PY 2013 VL 770 IS 2 AR UNSP 131 DI 10.1088/0004-637X/770/2/131 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200049 ER PT J AU Neill, JL Wang, SY Bergin, EA Crockett, NR Favre, C Plume, R Melnick, GJ AF Neill, Justin L. Wang, Shiya Bergin, Edwin A. Crockett, Nathan R. Favre, Cecile Plume, Rene Melnick, Gary J. TI THE ABUNDANCE OF H2O AND HDO IN ORION KL FROM HERSCHEL/HIFI SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM: abundances; ISM: individual objects (Orion KL); ISM: molecules ID MAGNETOHYDRODYNAMIC SHOCK-WAVES; DENSE INTERSTELLAR CLOUDS; STAR-FORMING REGIONS; WATER-VAPOR EMISSION; MICROWAVE-SPECTRUM; MOLECULAR CLOUDS; DEUTERATED WATER; GROUND-STATE; LINE SURVEY; DEUTERIUM FRACTIONATION AB Using a broadband, high spectral resolution survey toward the Orion Kleinmann-Low nebula acquired with Herschel/HIFI as part of the Herschel Observations of Extra-Ordinary Sources key program, we derive the abundances of H2O and HDO in the different spatial/velocity components associated with this massive star-forming region: the Hot Core, Compact Ridge, and Plateau. A total of 20 transitions of (H2O)-O-18, 14 of (H2O)-O-17, 37 of (HDO)-O-16, 6 of (HDO)-O-18, and 6 of D2O are used in the analysis, spanning from ground state transitions to over 1200 K in upper-state energy. Low-excitation lines are detected in multiple components, but the highest-excitation lines (E-u > 500 K) are well modeled as emitting from a small (similar to 2 '') clump with a high abundance of H2O (chi = 6.5 x 10(-4) relative to H-2) and a HDO/H2O ratio of 0.003. Using high spatial resolution (1.'' 5 x 1.'' 1) images of two transitions of HDO measured by the Atacama Large Millimeter/Submillimeter Array as part of its science verification phase, we identify this component as located near, but not directly coincident with, known continuum sources in the Hot Core region. Significant HDO/H2O fractionation is also seen in the Compact Ridge and Plateau components. The outflowing gas, observed with both emission and absorption components, has a lower HDO/H2O ratio than the compact components in Orion Kleinmann-Low, which we propose could be due to modification by gas-phase shock chemistry. C1 [Neill, Justin L.; Wang, Shiya; Bergin, Edwin A.; Crockett, Nathan R.; Favre, Cecile] Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA. [Plume, Rene] Univ Calgary, Dept Phys & Astron, Calgary, AB T2N IN4, Canada. [Plume, Rene] Univ Calgary, Inst Space Imaging Sci, Calgary, AB T2N IN4, Canada. [Melnick, Gary J.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Neill, JL (reprint author), Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48109 USA. EM jneill@umich.edu FU NASA through an award issued by JPL/Caltech FX HIFI has been designed and built by a consortium of institutes and university departments from across Europe, Canada, and the United States under the leadership of SRON Netherlands Institute for Space Research, Groningen, The Netherlands and with major contributions from Germany, France, and the U.S. Consortium members are: Canada: CSA, U. Waterloo; France: CESR, LAB, LERMA, IRAM; Germany: KOSMA, MPIfR, MPS; Ireland: NUI Maynooth; Italy: ASI, IFSI-INAF, Osservatorio Astrofisico di Arcetri-INAF; Netherlands: SRON, TUD; Poland: CAMK, CBK; Spain: Observatorio Astronomico Nacional (IGN), Centro de Astrobiologia (CSIC-INTA); Sweden: Chalmers University of Technology-MC2, RSS and GARD, Onsala Space Observatory, Swedish National Space Board, Stockholm Observatory; Switzerland: ETH Zurich, FHNW; USA: Caltech, JPL, NHSC. Support for this work was provided by NASA through an award issued by JPL/Caltech. NR 88 TC 23 Z9 23 U1 0 U2 8 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR UNSP 142 DI 10.1088/0004-637X/770/2/142 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200060 ER PT J AU Todorov, KO Deming, D Knutson, HA Burrows, A Fortney, JJ Lewis, NK Cowan, NB Agol, E Desert, JM Sada, PV Charbonneau, D Laughlin, G Langton, J Showman, AP AF Todorov, Kamen O. Deming, Drake Knutson, Heather A. Burrows, Adam Fortney, Jonathan J. Lewis, Nikole K. Cowan, Nicolas B. Agol, Eric Desert, Jean-Michel Sada, Pedro V. Charbonneau, David Laughlin, Gregory Langton, Jonathan Showman, Adam P. TI WARM SPITZER PHOTOMETRY OF THREE HOT JUPITERS: HAT-P-3b, HAT-P-4b AND HAT-P-12b SO ASTROPHYSICAL JOURNAL LA English DT Article DE eclipses; planetary systems; techniques: photometric ID INFRARED-EMISSION SPECTRUM; SECONDARY ECLIPSE PHOTOMETRY; GIANT PLANET ATMOSPHERES; NEPTUNE-MASS PLANET; M-DWARF GJ-436; EXTRASOLAR PLANET; THERMAL EMISSION; HD 189733B; TEMPERATURE INVERSION; LIGHT CURVES AB We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 mu m bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of 0.112%(+0.015%)(-0.030%) (3.6 mu m) and 0.094%(+0.016%)(-0.009%) (4.5 mu m). The HAT-P-4b values are 0.142%(+0.014%)(-0.016%) (3.6 mu m) and 0.122%(+0.012%)(-0.014%) (4.5 mu m). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12b is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3 sigma upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: < 0.042% (3.6 mu m) and < 0.085% (4.5 mu m). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3 sigma upper limits on the vertical bar e cos omega vertical bar quantity (where e is eccentricity and omega is the argument of periapsis) for HAT-P-3b (< 0.0081) and HAT-P-4b (< 0.0042), based on the secondary eclipse timings. C1 [Todorov, Kamen O.] Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. [Todorov, Kamen O.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Todorov, Kamen O.; Deming, Drake] Univ Maryland, Dept Astron, College Pk, MD 20742 USA. [Knutson, Heather A.] CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. [Burrows, Adam] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Fortney, Jonathan J.; Laughlin, Gregory] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. [Lewis, Nikole K.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA 02139 USA. [Cowan, Nicolas B.] Northwestern Univ, Dept Phys & Astron, Evanston, IL 60208 USA. [Agol, Eric] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Desert, Jean-Michel] CALTECH, Dept Astron, Pasadena, CA 91125 USA. [Sada, Pedro V.] Univ Monterrey, Dept Math & Phys, Monterrey, Mexico. [Charbonneau, David] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Langton, Jonathan] Principia Coll, Dept Phys, Elsah, IL 62028 USA. [Showman, Adam P.] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. RP Todorov, KO (reprint author), Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA. OI Charbonneau, David/0000-0002-9003-484X; Fortney, Jonathan/0000-0002-9843-4354; Todorov, Kamen/0000-0002-9276-8118; /0000-0002-0802-9145 FU NASA; JPL/Caltech; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium FX We thank Jonathan Fraine for helpful discussions on "prayer bead" uncertainty estimation. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through an award issued by JPL/Caltech. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. We thank the anonymous referee for a careful review of this paper. NR 68 TC 24 Z9 24 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 20 PY 2013 VL 770 IS 2 AR UNSP 102 DI 10.1088/0004-637X/770/2/102 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200020 ER PT J AU van den Berg, M Verbunt, F Tagliaferri, G Belloni, T Bedin, LR Platais, I AF van den Berg, Maureen Verbunt, Frank Tagliaferri, Gianpiero Belloni, Tomaso Bedin, Luigi R. Platais, Imants TI A CHANDRA X-RAY STUDY OF THE INTERACTING BINARIES IN THE OLD OPEN CLUSTER NGC 6791 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: close; novae, cataclysmic variables; open clusters and associations: individual (NGC 6791); stars: activity; X-rays: binaries ID WIYN OPEN CLUSTER; SPACE-TELESCOPE COUNTERPARTS; CATACLYSMIC VARIABLE-STARS; DIGITAL SKY SURVEY; GLOBULAR-CLUSTERS; XMM-NEWTON; GLOBULAR-CLUSTER-47 TUCANAE; BOLOMETRIC CORRECTIONS; TIDAL CIRCULARIZATION; LUMINOSITY FUNCTION AB We present the first X-ray study of NGC 6791, one of the oldest open clusters known (8 Gyr). Our Chandra observation is aimed at uncovering the population of close interacting binaries down to L-X approximate to 1 x 10(30) erg s(-1) (0.3-7 keV). We detect 86 sources within 8' of the cluster center, including 59 inside the half-mass radius. We identify 20 sources with proper-motion cluster members, which are a mix of cataclysmic variables (CVs), active binaries (ABs), and binaries containing sub-subgiants. With follow-up optical spectroscopy, we confirm the nature of one CV. We discover one new, X-ray variable candidate CV with Balmer and He II emission lines in its optical spectrum; this is the first X-ray-selected CV in an open cluster. The number of CVs per unit mass is consistent with the field, suggesting that the 3-4 CVs observed in NGC 6791 are primordial. We compare the X-ray properties of NGC 6791 with those of a few old open (NGC 6819, M 67) and globular clusters (47 Tuc, NGC 6397). It is puzzling that the number of ABs brighter than 1 x 10(30) erg s(-1) normalized by cluster mass is lower in NGC 6791 than in M 67 by a factor similar to 3-7. CVs, ABs, and sub-subgiants brighter than 1 x 10(30) erg s(-1) are under-represented per unit mass in the globular clusters compared to the oldest open clusters, and this accounts for the lower total X-ray luminosity per unit mass of the former. This indicates that the net effect of dynamical encounters may be the destruction of even some of the hardest (i.e., X-ray-emitting) binaries. C1 [van den Berg, Maureen] Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 XH Amsterdam, Netherlands. [van den Berg, Maureen] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Verbunt, Frank] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands. [Verbunt, Frank] SRON Netherlands Inst Space Res, SRON, NL-3584 CA Utrecht, Netherlands. [Tagliaferri, Gianpiero; Belloni, Tomaso] Osserv Astron Brera, INAF, I-23807 Merate, LC, Italy. [Bedin, Luigi R.] Osserv Astron Padova, INAF, I-35122 Padua, Italy. [Platais, Imants] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. RP van den Berg, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands. EM M.C.vandenBerg@uva.nl OI bedin, luigi/0000-0003-4080-6466; Tagliaferri, Gianpiero/0000-0003-0121-0723 FU Chandra [GO0-11110X] FX The authors would like to thank J. Hong for providing the routines to compute energy quantiles, C. Heinke for comments on the manuscript, and K. Cudworth for providing a catalog of proper motions. This research was supported by Chandra grant GO0-11110X. Some of the observations reported here were obtained at the MMT Observatory, a joint facility of the Smithsonian Institution and the University of Arizona. NR 89 TC 8 Z9 8 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD JUN 20 PY 2013 VL 770 IS 2 AR UNSP 98 DI 10.1088/0004-637X/770/2/98 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200016 ER PT J AU Wright, JT Roy, A Mahadevan, S Wang, SX Ford, EB Payne, M Lee, BL Wang, J Crepp, JR Gaudi, BS Eastman, J Pepper, J Ge, J Fleming, SW Ghezzi, L Gonzalez-Hernandez, JI Cargile, P Stassun, KG Wisniewski, J Dutra-Ferreira, L de Mello, GFP Maia, MAG da Costa, LN Ogando, RLC Santiago, BX Schneider, DP Hearty, FR AF Wright, Jason T. Roy, Arpita Mahadevan, Suvrath Wang, Sharon X. Ford, Eric B. Payne, Matt Lee, Brian L. Wang, Ji Crepp, Justin R. Gaudi, B. Scott Eastman, Jason Pepper, Joshua Ge, Jian Fleming, Scott W. Ghezzi, Luan Gonzalez-Hernandez, Jonay I. Cargile, Phillip Stassun, Keivan G. Wisniewski, John Dutra-Ferreira, Leticia Porto de Mello, Gustavo F. Maia, Marcio A. G. da Costa, Luiz Nicolaci Ogando, Ricardo L. C. Santiago, Basilio X. Schneider, Donald P. Hearty, Fred R. TI MARVELS-1: A FACE-ON DOUBLE-LINED BINARY STAR MASQUERADING AS A RESONANT PLANETARY SYSTEM AND CONSIDERATION OF RARE FALSE POSITIVES IN RADIAL VELOCITY PLANET SEARCHES SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries: spectroscopic; brown dwarfs; stars: individual (TYC 1240-945-1); stars: low-mass ID HOBBY-EBERLY TELESCOPE; EXTRA-SOLAR PLANETS; CHAIN MONTE-CARLO; LOW-MASS STARS; SUBSTELLAR COMPANIONS; TRANSIT CANDIDATES; ACCURATE MASSES; CORALIE SURVEY; SHORT-PERIOD; STELLAR AB We have analyzed new and previously published radial velocity (RV) observations of MARVELS-1, known to have an ostensibly substellar companion in a similar to 6 day orbit. We find significant (similar to 100ms(-1)) residuals to the best-fit model for the companion, and these residuals are naively consistent with an interior giant planet with a P = 1.965 days in a nearly perfect 3: 1 period commensurability (vertical bar P-b/P-c - 3 vertical bar < 10(-4)). We have performed several tests for the reality of such a companion, including a dynamical analysis, a search for photometric variability, and a hunt for contaminating stellar spectra. We find many reasons to be critical of a planetary interpretation, including the fact that most of the three-body dynamical solutions are unstable. We find no evidence for transits, and no evidence of stellar photometric variability. We have discovered two apparent companions to MARVELS-1 with adaptive optics imaging at Keck; both are M dwarfs, one is likely bound, and the other is likely a foreground object. We explore false-alarm scenarios inspired by various curiosities in the data. Ultimately, a line profile and bisector analysis lead us to conclude that the similar to 100 m s(-1) residuals are an artifact of spectral contamination from a stellar companion contributing similar to 15%-30% of the optical light in the system. We conclude that origin of this contamination is the previously detected RV companion to MARVELS-1, which is not, as previously reported, a brown dwarf, but in fact a G dwarf in a face-on orbit. C1 [Wright, Jason T.; Roy, Arpita; Mahadevan, Suvrath; Wang, Sharon X.; Fleming, Scott W.; Schneider, Donald P.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. [Wright, Jason T.; Roy, Arpita; Mahadevan, Suvrath; Wang, Sharon X.; Fleming, Scott W.; Schneider, Donald P.] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA. [Ford, Eric B.; Payne, Matt; Lee, Brian L.; Ge, Jian] Univ Florida, Dept Astron, Bryant Space Sci Ctr 211, Gainesville, FL 32611 USA. [Payne, Matt] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Lee, Brian L.] Univ Washington, Dept Astron, Seattle, WA 98195 USA. [Wang, Ji] Yale Univ, Dept Astron, New Haven, CT 06511 USA. [Crepp, Justin R.] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 USA. [Gaudi, B. Scott; Eastman, Jason] Ohio State Univ, Dept Astron, Columbus, OH 43210 USA. [Pepper, Joshua; Cargile, Phillip; Stassun, Keivan G.] Vanderbilt Univ, Dept Phys & Astron, Nashville, TN 37235 USA. [Ghezzi, Luan; Maia, Marcio A. G.; da Costa, Luiz Nicolaci; Ogando, Ricardo L. C.] Observ Nacl, BR-20921400 Rio De Janeiro, RJ, Brazil. [Ghezzi, Luan; Dutra-Ferreira, Leticia; Porto de Mello, Gustavo F.; Maia, Marcio A. G.; da Costa, Luiz Nicolaci; Ogando, Ricardo L. C.; Santiago, Basilio X.] Lab Interinst E Astron LIneA, BR-20921400 Rio De Janeiro, RJ, Brazil. [Gonzalez-Hernandez, Jonay I.] Inst Astrofis Canarias, E-38200 San Cristobal la Laguna, Tenerife, Spain. [Gonzalez-Hernandez, Jonay I.] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain. [Stassun, Keivan G.] Fisk Univ, Dept Phys, Nashville, TN 37208 USA. [Wisniewski, John] Univ Oklahoma, HL Dodge Dept Phys & Astron, Norman, OK 73019 USA. [Dutra-Ferreira, Leticia; Porto de Mello, Gustavo F.] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio De Janeiro, RJ, Brazil. [Santiago, Basilio X.] Univ Fed Rio Grande do Sul, Inst Fis, BR-91501970 Porto Alegre, RS, Brazil. [Hearty, Fred R.] Univ Virginia, Dept Astron, Charlottesville, VA 22901 USA. RP Wright, JT (reprint author), Penn State Univ, Ctr Exoplanets & Habitable Worlds, Davey Lab 525, University Pk, PA 16802 USA. EM jtwright@astro.psu.edu RI Gonzalez Hernandez, Jonay I./L-3556-2014; Ogando, Ricardo/A-1747-2010; da Costa, Luiz Alberto/I-1326-2013; OI Gonzalez Hernandez, Jonay I./0000-0002-0264-7356; Ogando, Ricardo/0000-0003-2120-1154; da Costa, Luiz Alberto/0000-0002-7731-277X; Fleming, Scott/0000-0003-0556-027X; Eastman, Jason/0000-0003-3773-5142; Roy, Arpita/0000-0001-8127-5775; Wright, Jason/0000-0001-6160-5888; /0000-0001-6545-639X; Pepper, Joshua/0000-0002-3827-8417 FU Alfred P. Sloan Foundation; Participating Institutions; National Science Foundation; U.S. Department of Energy; Pennsylvania State University; Eberly College of Science; Pennsylvania Space Grant Consortium; NASA Astrobiology Institute through the Penn State Astrobiology Research Center [NNA09DA76A]; NASA Keck PI Data Award; W.M. Keck Foundation; NASA Origins of Solar Systems [NNX09AB35G]; NSF CAREER [AST-1056524]; Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics (VIDA); NSF Astronomy and Astrophysics Grant [AST-1109612]; Brazilian Participation Group; Ministerio de Ciencia e Tecnologia (MCT); Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ); Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq) [476909/2006-6, 474972/2009-7]; Financiadora de Estudos e Projetos (FINEP); FAPERJ [APQ1/26/170.687/2004]; PAPDRJ CAPES/FAPERJ Fellowship; CAPES/Brazil FX Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III Web site is http://www.sdss3.org/.; The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium.; This work was supported by the NASA Astrobiology Institute through the Penn State Astrobiology Research Center (grant NNA09DA76A).; We thank NASA and NExScI for providing Keck time in the 2011B semester for the study of multiplanet systems (NExScI ID40/Keck ID N141Hr, PIs Wright and Ford). This work was supported by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute. Data presented herein were obtained at the W.M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. We thank the California Planet Survey consortium, and especially Andrew Howard and Geoff Marcy, for managing the queue, undertaking the Keck radial velocity measurements and template observation, and the precise Doppler analysis.; E.B.F. and M.J.P. were supported by NASA Origins of Solar Systems Grant NNX09AB35G.; Work done by B.S.G. and J.E. was supported by NSF CAREER Grant AST-1056524.; J.P. and K.G.S. were supported by the Vanderbilt Office of the Provost through the Vanderbilt Initiative in Data-intensive Astrophysics (VIDA). The SME work at Vanderbilt was sponsored through the NSF Astronomy and Astrophysics Grant AST-1109612.; Funding for the Brazilian Participation Group has been provided by the Ministerio de Ciencia e Tecnologia (MCT), Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ), Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), and Financiadora de Estudos e Projetos (FINEP).; G.F.P.M. acknowledges financial support by CNPq (476909/2006-6 and 474972/2009-7) and FAPERJ (APQ1/26/170.687/2004) grants.; L.G. acknowledges financial support provided by the PAPDRJ CAPES/FAPERJ Fellowship. L.D.F. acknowledges a PhD scholarship from CAPES/Brazil. NR 72 TC 13 Z9 13 U1 1 U2 32 PU 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 2013 VL 770 IS 2 AR 119 DI 10.1088/0004-637X/770/2/119 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 160HZ UT WOS:000320111200037 ER PT J AU Lee, TE Gopalakrishnan, S Lukin, MD AF Lee, Tony E. Gopalakrishnan, Sarang Lukin, Mikhail D. TI Unconventional Magnetism via Optical Pumping of Interacting Spin Systems SO PHYSICAL REVIEW LETTERS LA English DT Article ID QUANTUM SIMULATION; PHASE-DIAGRAM; TRAPPED IONS; DRIVEN; ATOMS; FIELD; MODEL AB We consider strongly interacting systems of effective spins, subject to dissipative spin-flip processes associated with optical pumping. We predict the existence of novel magnetic phases in the steady state of this system, which emerge due to the competition between coherent and dissipative processes. Specifically, for strongly anisotropic spin-spin interactions, we find ferromagnetic, antiferromagnetic, spin-density-wave, and staggered-XY steady states, which are separated by nonequilibrium phase transitions meeting at a Lifshitz point. These transitions are accompanied by quantum correlations, resulting in spin squeezing. Experimental implementations in ultracold atoms and trapped ions are discussed. C1 [Lee, Tony E.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. [Gopalakrishnan, Sarang; Lukin, Mikhail D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. RP Lee, TE (reprint author), Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. FU NSF; Harvard Quantum Optics Center; Center for Ultracold Atoms; DARPA FX We thank Philipp Strack, Eric Kessler, Chris Laumann, Norman Yao, Hendrik Weimer, and Rajibul Islam for useful discussions. This work was supported by NSF through a grant to ITAMP, the Harvard Quantum Optics Center, the Center for Ultracold Atoms, and DARPA. NR 56 TC 37 Z9 37 U1 2 U2 27 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD JUN 19 PY 2013 VL 110 IS 25 AR 257204 DI 10.1103/PhysRevLett.110.257204 PG 5 WC Physics, Multidisciplinary SC Physics GA 169EU UT WOS:000320761800005 PM 23829757 ER PT J AU Lyson, TR Bever, GS Scheyer, TM Hsiang, AY Gauthier, JA AF Lyson, Tyler R. Bever, Gabe S. Scheyer, Torsten M. Hsiang, Allison Y. Gauthier, Jacques A. TI Evolutionary Origin of the Turtle Shell SO CURRENT BIOLOGY LA English DT Article ID BODY PLAN; CARAPACIAL RIDGE; PHYLOGENY; FOSSIL; INTERRELATIONSHIPS; DIVERSIFICATION; TRIONYCHIDAE; CALIBRATION; HOMOLOGIES; REPTILES AB The origin of the turtle shell has perplexed biologists for more than two centuries [1]. It was not until Odontochelys semitestacea [2] was discovered, however, that the fossil and developmental data [3-8] could be synthesized into a model [9] of shell assembly that makes predictions for the as-yet unestablished history of the turtle stem group. We build on this model by integrating novel data for Eunotosaurus africanus-a Late Guadalupian (similar to 260 mya) [10] Permian reptile inferred to be an early stem turtle [11]. Eunotosaurus expresses a number of relevant characters, including a reduced number of elongate trunk vertebrae (nine), nine pairs of T-shaped ribs, inferred loss of intercostal muscles, reorganization of respiratory muscles to the ventral side of the ribs, (sub)dermal outgrowth of bone from the developing perichondral collar of the ribs, and paired gastralia that lack both lateral and median elements. These features conform to the predicted sequence of character acquisition and provide further support that E. africanus, O. semitestacea, and Proganochelys quenstedti represent successive divergences from the turtle stem lineage. The initial transformations of the model thus occurred by the Middle Permian, which is congruent with molecular-based divergence estimates [12-15] for the lineage, and remain viable whether turtles originated inside or outside crown Diapsida. C1 [Lyson, Tyler R.; Hsiang, Allison Y.; Gauthier, Jacques A.] Yale Univ, Dept Geol & Geophys, New Haven, CT 06511 USA. [Lyson, Tyler R.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20560 USA. [Lyson, Tyler R.; Gauthier, Jacques A.] Yale Peabody Museum Nat Hist, Dept Vertebrate Paleontol, New Haven, CT 06511 USA. [Bever, Gabe S.] Coll Osteopath Med, New York Inst Technol, Old Westbury, NY 11568 USA. [Bever, Gabe S.] Amer Museum Nat Hist, Div Paleontol, New York, NY 10024 USA. [Scheyer, Torsten M.] Univ Zurich, Palaontol Inst & Museum, CH-8006 Zurich, Switzerland. RP Lyson, TR (reprint author), Yale Univ, Dept Geol & Geophys, 210 Whitney Ave, New Haven, CT 06511 USA. EM tyler.lyson@gmail.com FU NSF; Smithsonian Institution; Swiss National Science Foundation (SNSF) [31003A_127053] FX We thank the following institutions and their curators/staff for access to material under their care: Albany Museum (Grahamstown), Natural History Museum (London), Institute of Paleontology and Paleoanthropology (Beijing), Council for Geosciences (Pretoria), National Museum (Bloemfontein), Bernard Price Institute (Johannesburg), South African Museum (Cape Town), Staatliches Museum fur Naturkunde (Stuttgart), United States National Museum (Washington, D.C.), and Yale Peabody Museum of Natural History (New Haven). M. Fox (Yale Peabody Museum [YPM]) is thanked for her careful preparation of the fossil material. B. Roach (YPM) made the beautiful illustrations used herein. W. Joyce is thanked for his help with Figure 2. The vertebrate paleontology group at the PIMUZ is thanked for various assistances and discussions. K. deQueiroz, M.S.Y. Lee, M. Laurin, and an anonymous reviewer had useful comments that improved the manuscript. External funding for this project was provided by an NSF Graduate Research Fellowship and a Smithsonian Institution Peter Buck Fellowship to T.R.L. and a Swiss National Science Foundation grant (SNSF no. 31003A_127053) to T.M.S. NR 46 TC 31 Z9 31 U1 21 U2 110 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 17 PY 2013 VL 23 IS 12 BP 1113 EP 1119 DI 10.1016/j.cub.2013.05.003 PG 7 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 168CH UT WOS:000320682800027 PM 23727095 ER PT J AU Kelley, LZ Mandel, I Ramirez-Ruiz, E AF Kelley, Luke Zoltan Mandel, Ilya Ramirez-Ruiz, Enrico TI Electromagnetic transients as triggers in searches for gravitational waves from compact binary mergers SO PHYSICAL REVIEW D LA English DT Article ID GAMMA-RAY BURSTS; NEUTRON-STAR MERGERS; COOLED ACCRETION DISKS; BLACK-HOLE BINARIES; 28 FEBRUARY 1997; LIGHT CURVES; R-PROCESS; FORMATION HISTORY; TELESCOPE ARRAY; OBJECT MERGERS AB The detection of an electromagnetic transient which may originate from a binary neutron star merger can increase the probability that a given segment of data from the LIGO-Virgo ground-based gravitational-wave detector network contains a signal from a binary coalescence. Additional information contained in the electromagnetic signal, such as the sky location or distance to the source, can help rule out false alarms and thus lower the necessary threshold for a detection. Here, we develop a framework for determining how much sensitivity is added to a gravitational-wave search by triggering on an electromagnetic transient. We apply this framework to a variety of relevant electromagnetic transients, from short gamma-ray bursts (GRBs) to signatures of r-process heating to optical and radio orphan afterglows. We compute the expected rates of multimessenger observations in the advanced detector era and find that searches triggered on short GRBs-with current high-energy instruments, such as Fermi-and nucleo-synthetic "kilonovae"-with future optical surveys, like the Large Synoptic Survey Telescope-can boost the number of multimessenger detections by 15% and 40%, respectively, for a binary neutron star progenitor model. Short GRB triggers offer precise merger timing but suffer from detection rates decreased by beaming and the high a priori probability that the source is outside the LIGO-Virgo sensitive volume. Isotropic kilonovae, on the other hand, could be commonly observed within the LIGO-Virgo sensitive volume with an instrument roughly an order of magnitude more sensitive than current optical surveys. We propose that the most productive strategy for making multimessenger gravitational-wave observations is using triggers from future deep, optical all-sky surveys, with characteristics comparable to the Large Synoptic Survey Telescope, which could make as many as ten such coincident observations a year. C1 [Kelley, Luke Zoltan] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Mandel, Ilya] Univ Birmingham, Sch Phys & Astron, Edgbaston B15 2TT, W Midlands, England. [Ramirez-Ruiz, Enrico] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. RP Kelley, LZ (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM LKelley@cfa.harvard.edu OI Mandel, Ilya/0000-0002-6134-8946 FU David and Lucille Packard Foundation; NSF [AST-0847563] FX We are grateful to Hendrik van Eerten for making afterglow simulation data available online and for providing us with additional simulations for this project and to Luis Lehner, Edo Berger, Jolien Creighton, and especially Peter Shawhan for comments on the manuscript. Major portions of this review were written at the DARK Cosmology Centre, Copenhagen, the Theoretical Astrophysics Santa Cruz Institute, the Aspen Center for Physics and the Institute for Theory and Computation, Harvard. We thank the directors of these institutions for their generous hospitality. Financial support for this work was provided in part by the David and Lucille Packard Foundation and NSF (AST-0847563). NR 109 TC 33 Z9 33 U1 1 U2 8 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 JUN 17 PY 2013 VL 87 IS 12 AR 123004 DI 10.1103/PhysRevD.87.123004 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 167CW UT WOS:000320609200001 ER PT J AU van Donkelaar, A Martin, RV Spurr, RJD Drury, E Remer, LA Levy, RC Wang, J AF van Donkelaar, Aaron Martin, Randall V. Spurr, Robert J. D. Drury, Easan Remer, Lorraine A. Levy, Robert C. Wang, Jun TI Optimal estimation for global ground-level fine particulate matter concentrations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article DE PM2.5; AOD; Optimal Estimation; AERONET; CALIOP; MODIS ID AEROSOL OPTICAL DEPTH; UNITED-STATES; AIR-POLLUTION; SATELLITE RETRIEVALS; RADIATIVE-TRANSFER; ALGORITHM; PM2.5; REFLECTANCE; LONG; VISIBILITY AB We develop an optimal estimation (OE) algorithm based on top-of-atmosphere reflectances observed by the MODIS satellite instrument to retrieve near-surface fine particulate matter (PM2.5). The GEOS-Chem chemical transport model is used to provide prior information for the Aerosol Optical Depth (AOD) retrieval and to relate total column AOD to PM2.5. We adjust the shape of the GEOS-Chem relative vertical extinction profiles by comparison with lidar retrievals from the CALIOP satellite instrument. Surface reflectance relationships used in the OE algorithm are indexed by land type. Error quantities needed for this OE algorithm are inferred by comparison with AOD observations taken by a worldwide network of sun photometers (AERONET) and extended globally based upon aerosol speciation and cross correlation for simulated values, and upon land type for observational values. Significant agreement in PM2.5 is found over North America for 2005 (slope=0.89; r=0.82; 1-sigma error=1 mu g/m(3)+27%), with improved coverage and correlation relative to previous work for the same region and time period, although certain subregions, such as the San Joaquin Valley of California are better represented by previous estimates. Independently derived error estimates of the OE PM2.5 values at in situ locations over North America (of (2.5 mu g/m(3)+31%) and Europe of (3.5 mu g/m(3)+30%) are corroborated by comparison with in situ observations, although globally (error estimates of (3.0 mu g/m(3)+35%), may be underestimated. Global population-weighted PM2.5 at 50% relative humidity is estimated as 27.8 mu g/m(3) at 0.1 degrees x0.1 degrees resolution. C1 [van Donkelaar, Aaron; Martin, Randall V.] Dalhousie Univ, Dept Phys & Atmospher Sci, Halifax, NS B3H 3J5, Canada. [Martin, Randall V.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Spurr, Robert J. D.] RT Solut Inc, Cambridge, MA USA. [Drury, Easan] Natl Renewable Energy Lab, Golden, CO USA. [Remer, Lorraine A.] Univ Maryland, JCET, Baltimore, MD 21201 USA. [Levy, Robert C.] Inc Lanham, Sci Syst & Applicat, Greenbelt, MD USA. [Levy, Robert C.] NASA, Goddard Space Flight Ctr, Earth Sci Div, Greenbelt, MD 20771 USA. [Wang, Jun] Univ Nebraska, Dept Earth & Atmospher Sci, Lincoln, NE USA. RP van Donkelaar, A (reprint author), Dalhousie Univ, 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; Chem, GEOS/C-5595-2014; Wang, Jun/A-2977-2008 OI Levy, Robert/0000-0002-8933-5303; Martin, Randall/0000-0003-2632-8402; Wang, Jun/0000-0002-7334-0490 FU Health Canada; Natural Sciences and Engineering Research Council of Canada FX We are grateful to the CALIOP, AERONET, NAPS, and AQS teams for making available data used here. This work was funded by Health Canada and the Natural Sciences and Engineering Research Council of Canada. NR 63 TC 32 Z9 32 U1 7 U2 44 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD JUN 16 PY 2013 VL 118 IS 11 BP 5621 EP 5636 DI 10.1002/jgrd.50479 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 228TG UT WOS:000325212600030 ER PT J AU Krause, GH Cheesman, AW Winter, K Krause, B Virgo, A AF Heinrich Krause, G. Cheesman, Alexander W. Winter, Klaus Krause, Barbara Virgo, Aurelio TI Thermal tolerance, net CO2 exchange and growth of a tropical tree species, Ficus insipida, cultivated at elevated daytime and nighttime temperatures SO JOURNAL OF PLANT PHYSIOLOGY LA English DT Article DE Chlorophyll fluorescence; Respiration; Photosynthetic CO2 assimilation; Photosystem II; Heat acclimation ID RAIN-FOREST TREES; CLIMATE-CHANGE; CHLOROPHYLL FLUORESCENCE; DESERT PLANTS; CARBON LIMITATION; MOUNTAIN PASSES; PHOTOSYSTEM-II; HEAT TOLERANCE; PHOTOSYNTHESIS; SEEDLINGS AB Global warming and associated increases in the frequency and amplitude of extreme weather events, such as heat waves, may adversely affect tropical rainforest plants via significantly increased tissue temperatures. In this study, the response to two temperature regimes was assessed in seedlings of the neotropical pioneer tree species, Ficus insipida. Plants were cultivated in growth chambers at strongly elevated daytime temperature (39 degrees C), combined with either close to natural (22 degrees C) or elevated (32 degrees C) nighttime temperatures. Under both growth regimes, the critical temperature for irreversible leaf damage, determined by changes in chlorophyll a fluorescence, was approximately 51 degrees C. This is comparable to values found in F. insipida growing under natural ambient conditions and indicates a limited potential for heat tolerance acclimation of this tropical forest tree species. Yet, under high nighttime temperature, growth was strongly enhanced, accompanied by increased rates of net photosynthetic CO2 uptake and diminished temperature dependence of leaf-level dark respiration, consistent with thermal acclimation of these key physiological parameters. (c) 2013 Elsevier GmbH. All rights reserved. C1 [Heinrich Krause, G.; Cheesman, Alexander W.; Winter, Klaus; Krause, Barbara; Virgo, Aurelio] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Heinrich Krause, G.] Univ Dusseldorf, Inst Plant Biochem, D-40225 Dusseldorf, Germany. RP Krause, GH (reprint author), Univ Dusseldorf, Inst Plant Biochem, Univ Str 1, D-40225 Dusseldorf, Germany. EM ghkrause@uni-duesseldorf.de RI Cheesman, Alexander/H-5918-2013 OI Cheesman, Alexander/0000-0003-3931-5766 FU Smithsonian Tropical Research Institute through the Center for Tropical Forest Studies (CTFS) Smithsonian Institute Global Earth Observatory (SIGEO) FX The study was supported by the Smithsonian Tropical Research Institute through the Center for Tropical Forest Studies (CTFS) Smithsonian Institute Global Earth Observatory (SIGEO). NR 47 TC 11 Z9 11 U1 5 U2 75 PU ELSEVIER GMBH, URBAN & FISCHER VERLAG PI JENA PA OFFICE JENA, P O BOX 100537, 07705 JENA, GERMANY SN 0176-1617 J9 J PLANT PHYSIOL JI J. Plant Physiol. PD JUN 15 PY 2013 VL 170 IS 9 BP 822 EP 827 DI 10.1016/j.jplph.2013.01.005 PG 6 WC Plant Sciences SC Plant Sciences GA 168BS UT WOS:000320681300004 PM 23399405 ER PT J AU Leray, M Yang, JY Meyer, CP Mills, SC Agudelo, N Ranwez, V Boehm, JT Machida, RJ AF Leray, Matthieu Yang, Joy Y. Meyer, Christopher P. Mills, Suzanne C. Agudelo, Natalia Ranwez, Vincent Boehm, Joel T. Machida, Ryuji J. TI A new versatile primer set targeting a short fragment of the mitochondrial COI region for metabarcoding metazoan diversity: application for characterizing coral reef fish gut contents SO FRONTIERS IN ZOOLOGY LA English DT Article DE Second generation sequencing; DNA barcoding; Mini-barcode; Mitochondrial marker; Trophic interactions; Food web ID POLYMERASE-CHAIN-REACTION; BIODIVERSITY ASSESSMENT; DIET COMPOSITION; RIBOSOMAL-RNA; PREY DNA; AMPLIFICATION; SEQUENCES; PREDATORS; TAXONOMY; ECOLOGY AB Introduction: The PCR-based analysis of homologous genes has become one of the most powerful approaches for species detection and identification, particularly with the recent availability of Next Generation Sequencing platforms (NGS) making it possible to identify species composition from a broad range of environmental samples. Identifying species from these samples relies on the ability to match sequences with reference barcodes for taxonomic identification. Unfortunately, most studies of environmental samples have targeted ribosomal markers, despite the fact that the mitochondrial Cytochrome c Oxidase subunit I gene (COI) is by far the most widely available sequence region in public reference libraries. This is largely because the available versatile ("universal") COI primers target the 658 barcoding region, whose size is considered too large for many NGS applications. Moreover, traditional barcoding primers are known to be poorly conserved across some taxonomic groups. Results: We first design a new PCR primer within the highly variable mitochondrial COI region, the "mlCOIintF" primer. We then show that this newly designed forward primer combined with the "jgHCO2198" reverse primer to target a 313 bp fragment performs well across metazoan diversity, with higher success rates than versatile primer sets traditionally used for DNA barcoding (i.e. LCO1490/HCO2198). Finally, we demonstrate how the shorter COI fragment coupled with an efficient bioinformatics pipeline can be used to characterize species diversity from environmental samples by pyrosequencing. We examine the gut contents of three species of planktivorous and benthivorous coral reef fish (family: Apogonidae and Holocentridae). After the removal of dubious COI sequences, we obtained a total of 334 prey Operational Taxonomic Units (OTUs) belonging to 14 phyla from 16 fish guts. Of these, 52.5% matched a reference barcode (> 98% sequence similarity) and an additional 32% could be assigned to a higher taxonomic level using Bayesian assignment. Conclusions: The molecular analysis of gut contents targeting the 313 COI fragment using the newly designed mlCOIintF primer in combination with the jgHCO2198 primer offers enormous promise for metazoan metabarcoding studies. We believe that this primer set will be a valuable asset for a range of applications from large-scale biodiversity assessments to food web studies. C1 [Leray, Matthieu; Mills, Suzanne C.] Univ Perpignan, Lab Excellence CORAIL, USR CRIOBE CNRS EPHE 3278, F-66860 Perpignan, France. [Leray, Matthieu; Meyer, Christopher P.; Agudelo, Natalia] Smithsonian Inst, Dept Invertebrate Zool, Natl Museum Nat Hist, Washington, DC 20013 USA. [Yang, Joy Y.] NHGRI, NIH, Bethesda, MD 20892 USA. [Ranwez, Vincent] Montpellier SupAgro, UMR AGAP, Montpellier, France. [Boehm, Joel T.] CUNY City Coll, Dept Biol, New York, NY 10031 USA. [Boehm, Joel T.] CUNY, Grad Ctr, New York, NY 10016 USA. [Machida, Ryuji J.] Acad Sinica, Biodivers Res Ctr, Taipei 115, Taiwan. RP Leray, M (reprint author), Univ Perpignan, Lab Excellence CORAIL, USR CRIOBE CNRS EPHE 3278, F-66860 Perpignan, France. EM leray.upmc@gmail.com RI Mills, Suzanne/K-5538-2012 FU Gordon and Betty Moore Foundation; Smithsonian Institution; France American Cultural Exchange program (FACE - Partner University Fund); Live and Let Die [ANR-11-JSV7-012-01] FX We thank Gustav Paulay, Arthur Anker and the BIOCODE teams who collected and identified marine and terrestrial specimens, the "Centre de Recherche Insulaire et Observatoire de l'Environnement (CRIOBE) de Moorea" and the Richard B. Gump field station in Moorea for logistical support. We also greatly acknowledge the Gordon and Betty Moore Foundation, Smithsonian Institution Fellowship Program, France American Cultural Exchange program (FACE - Partner University Fund) and ANR-11-JSV7-012-01 Live and Let Die for financial support. Ehsan Kayal and Yvonne Linton provided constructive comments on an early draft of the manuscript. We are also grateful for insightful comments provided by Nancy Knowlton. This study was part of M. Leray PhD research program at Universite Pierre et Marie Curie (Paris VI) and Ecole Pratique des Hautes Etudes (EPHE) under the supervision of S.C. Mills. NR 68 TC 59 Z9 61 U1 20 U2 183 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 JUN 14 PY 2013 VL 10 AR UNSP 34 DI 10.1186/1742-9994-10-34 PG 14 WC Zoology SC Zoology GA 167FK UT WOS:000320616500001 PM 23767809 ER PT J AU Paszko, B Soreng, RJ AF Paszko, Beata Soreng, Robert J. TI Species delimitation and name application in Deyeuxia abnormis, Agrostis zenkeri, A. pleiophylla and related taxa (Poaceae: Agrostidinae) SO PHYTOTAXA LA English DT Article DE C. Mez; Calamagrostis; JD Hooker; NL Bor; new synonyms; nomenclature; revision; taxonomy; typification; South Asia ID TAXONOMIC REVISION; CHINA AB Historically tangled taxonomy and nomenclature of Deyeuxia abnormis, Agrostis zenkeri, A. pleiophylla and their allies is presented. Deyeuxia abnormis is recognized as a distinct species. Previous descriptions of this taxon were entangled with concepts of Agrostis zenkeri and Deyeuxia diffusa. The typification of Deyeuxia abnormis by Noltie is rejected in favor of the lectotype designated by Bor. The name Deyeuxia abnormis is applied to specimens of this species group with a tufted habit and callus hairs between 0.25 and 0.50 percent of their lemma in length. Specimens previously included in D. abnormis that are characterized by scrambling habit, simple or branched culms, and callus hairs between 0.6 and 1.0 percent of the lemma length, are assigned to D. diffusa. The taxonomy of Deyeuxia abnormis and its allies is clarified and new synonyms are provided, along with amended descriptions, and a key to the complex of D. abnormis and its allies. The distributions of Deyeuxia abnormis and D. diffusa in South Asia are updated. The previous typification of Agrostis pleiophylla is rejected and a new lectotype is selected. The names Anisachne gracilis (= Deyeuxia abnormis) and Agrostis continentalis (= Deyeuxia abnormis) are typified. C1 [Paszko, Beata] Polish Acad Sci, W Szafer Inst Bot, Dept Vasc Plant Systemat & Phytogeog, PL-31512 Krakow, Poland. [Soreng, Robert J.] Smithsonian Inst, Dept Bot, Natl Museum Nat Hist, Washington, DC 20013 USA. RP Paszko, B (reprint author), Polish Acad Sci, W Szafer Inst Bot, Dept Vasc Plant Systemat & Phytogeog, Lubicz 46, PL-31512 Krakow, Poland. EM b.paszko@botany.pl; sorengr@si.edu FU Institute of Botany of the Polish Academy of Sciences (Krakow, Poland); SYNTHESYS Project; European Community Research Infrastructure Action under the FP7 'Capacities' Program; Polish Academy of Sciences; Russian Academy of Sciences; Bilateral Exchange Programme FX The first author is grateful to the Curators of the following herbaria: B, BM, E, GOET, K, KRAM, L, LE, NY, P, TI, US, W and WU, for loans of, or access to, their collections and help during the study. This study is partly supported by the statutory funds of the Institute of Botany of the Polish Academy of Sciences (Krakow, Poland). The first author received support for this research from the SYNTHESYS Project which is financed by European Community Research Infrastructure Action under the FP7 'Capacities' Program. We thank the following people with help locating specimens (Wen-Li Chen from PE, Jochen Heinrichs from GOET, Eric Smets from L) and special thanks are due to Sylvia Phillips and Maria Vorontsova from Kew for valuable information. The research visit of Beata Paszko (2012) at LE (Saint Petersburg) was supported by Bilateral Exchange Programme between the Polish Academy of Sciences and the Russian Academy of Sciences. We would like to express our gratitude to Wojciech Paul from KRAM for his priceless help in translating the Latin diagnoses into English and to the anonymous reviewers and the editor for their helpful and constructive comments that greatly contributed to improving the manuscript. NR 58 TC 12 Z9 14 U1 1 U2 1 PU MAGNOLIA PRESS PI AUCKLAND PA PO BOX 41383, AUCKLAND, ST LUKES 1030, NEW ZEALAND SN 1179-3155 J9 PHYTOTAXA JI Phytotaxa PD JUN 14 PY 2013 VL 111 IS 1 BP 1 EP 26 PG 26 WC Plant Sciences SC Plant Sciences GA 164FK UT WOS:000320394200001 ER PT J AU Martinez-Garcia, R Calabrese, JM Mueller, T Olson, KA Lopez, C AF Martinez-Garcia, Ricardo Calabrese, Justin M. Mueller, Thomas Olson, Kirk A. Lopez, Cristobal TI Optimizing the Search for Resources by Sharing Information: Mongolian Gazelles as a Case Study SO PHYSICAL REVIEW LETTERS LA English DT Article ID PROCAPRA-GUTTUROSA PALLAS; COMMUNICATION; DISTANCE; BEHAVIOR; CONTEXT; MECHANISMS; BACTERIA; DENSITY; CALLS; SIZE AB We investigate the relationship between communication and search efficiency in a biological context by proposing a model of Brownian searchers with long-range pairwise interactions. After a general study of the properties of the model, we show an application to the particular case of acoustic communication among Mongolian gazelles, for which data are available, searching for good habitat areas. Using Monte Carlo simulations and density equations, our results point out that the search is optimal (i.e., the mean first hitting time among searchers is minimum) at intermediate scales of communication, showing that both an excess and a lack of information may worsen it. C1 [Martinez-Garcia, Ricardo; Lopez, Cristobal] Inst Fis Interdisciplinar & Sistemas Complejos CS, IFISC, E-07122 Palma De Mallorca, Spain. [Calabrese, Justin M.; Mueller, Thomas; Olson, Kirk A.] Natl Zool Pk, Smithsonian Conservat Biol Inst, Conservat Ecol Ctr, Front Royal, VA 22630 USA. [Mueller, Thomas] Univ Maryland, Behav Ecol Evolut & Systemat Program, College Pk, MD 20742 USA. RP Martinez-Garcia, R (reprint author), Inst Fis Interdisciplinar & Sistemas Complejos CS, IFISC, E-07122 Palma De Mallorca, Spain. RI Calabrese, Justin/B-9131-2012; Martinez-Garcia, Ricardo/J-4836-2013; OI Martinez-Garcia, Ricardo/0000-0003-2765-8147; Lopez, Cristobal/0000-0002-3445-4284 FU JAEPredoc program of CSIC; MICINN (Spain); FEDER (EU) [FIS2007-60327]; U.S. National Science Foundation [ABI 1062411] FX R. M.-G. is supported by the JAEPredoc program of CSIC. We thank C. H. Fleming for fruitful discussions and F. Vazquez for fruitful discussions and a critical reading of the manuscript. R. M.-G. and C. L. acknowledge support from MICINN (Spain) and FEDER (EU) through Grant No. FIS2007-60327 FISICOS. J. M. C. and T. M. were supported by a U.S. National Science Foundation grant (ABI 1062411). NR 41 TC 10 Z9 10 U1 3 U2 24 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 14 PY 2013 VL 110 IS 24 AR 248106 DI 10.1103/PhysRevLett.110.248106 PG 5 WC Physics, Multidisciplinary SC Physics GA 164FP UT WOS:000320394700020 PM 25165967 ER PT J AU Cottrell, E Kelley, KA AF Cottrell, Elizabeth Kelley, Katherine A. TI Redox Heterogeneity in Mid-Ocean Ridge Basalts as a Function of Mantle Source SO SCIENCE LA English DT Article ID EARTHS UPPER-MANTLE; OXIDATION-STATE; OXYGEN FUGACITY; CARBON-DIOXIDE; MORB GLASSES; MAGMAS; MELTS; INTERIOR; WATER; GPA AB The oxidation state of Earth's upper mantle both influences and records mantle evolution, but systematic fine-scale variations in upper mantle oxidation state have not previously been recognized in mantle-derived lavas from mid-ocean ridges. Through a global survey of mid-ocean ridge basalt glasses, we show that mantle oxidation state varies systematically as a function of mantle source composition. Negative correlations between Fe3+/Sigma Fe ratios and indices of mantle enrichment-such as Sr-87/Sr-86, Pb-208/Pb-204, Ba/La, and Nb/Zr ratios-reveal that enriched mantle is more reduced than depleted mantle. Because carbon may act to simultaneously reduce iron and generate melts that share geochemical traits with our reduced samples, we propose that carbon creates magmas at ridges that are reduced and enriched. C1 [Cottrell, Elizabeth] Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. [Kelley, Katherine A.] Univ Rhode Isl, Grad Sch Oceanog, Narragansett, RI 02882 USA. RP Cottrell, E (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Washington, DC 20560 USA. EM cottrelle@si.edu RI Kelley, Katherine/J-3728-2013 OI Kelley, Katherine/0000-0002-7516-2683 FU Deep Carbon Observatory; NSF [EAR-0841006, EAR-0841108]; U.S. Department of Energy [DE-AC02-98CH10886, DE-FG02-92ER14244] FX Data described in this paper are presented in the supplementary materials and are archived in the PetDB database (www.earthchem.org/petdb). We thank F. Davis for discussion and are grateful for support from the Deep Carbon Observatory and NSF awards EAR-0841006 (E. C.) and EAR-0841108 (K. A. K.). Use of the National Synchrotron Light Source was supported by U.S. Department of Energy under contracts DE-AC02-98CH10886 and DE-FG02-92ER14244. NR 30 TC 21 Z9 21 U1 4 U2 69 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 EI 1095-9203 J9 SCIENCE JI Science PD JUN 14 PY 2013 VL 340 IS 6138 BP 1314 EP 1317 DI 10.1126/science.1233299 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 163FC UT WOS:000320320200040 PM 23641060 ER PT J AU Yin, XY Blume, D AF Yin, X. Y. Blume, D. TI Small two-component Fermi gases in a cubic box with periodic boundary conditions SO PHYSICAL REVIEW A LA English DT Article ID ULTRACOLD GASES; SYSTEMS; STATES AB The properties of two-component Fermi gases become universal if the interspecies s-wave scattering length as and the average interparticle spacing are much larger than the range of the underlying two-body potential. Using an explicitly correlated Gaussian basis set expansion approach, we determine the eigenenergies of two-component Fermi gases in a cubic box with periodic boundary conditions as functions of the interspecies s-wave scattering length and the effective range of the two-body potential. The universal properties of systems consisting of up to four particles are determined by extrapolating the finite-range energies to the zero-range limit. We determine the eigenenergies of states with vanishing and finite momenta. In the weakly attractive BCS regime, we analyze the energy spectra and degeneracies using first-order degenerate perturbation theory. Excellent agreement between the perturbative energy shifts and the numerically determined energies is obtained. For the infinitely large scattering length case, we compare our results-where available-with those presented in the literature. C1 [Yin, X. Y.; Blume, D.] Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. [Blume, D.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom & Mol Phys, Cambridge, MA 02138 USA. RP Yin, XY (reprint author), Washington State Univ, Dept Phys & Astron, Pullman, WA 99164 USA. FU National Science Foundation (NSF) [PHY-1205443]; NSF [OCI-1053575]; WSU HPC; NSF FX Discussions with D. Kaplan, D. Lee, and K. Varga, which motivated this work, correspondence with O. Juillet, as well as support by the National Science Foundation (NSF) through Grant No. PHY-1205443 are gratefully acknowledged. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF Grant No. OCI-1053575, and the WSU HPC. This work was additionally supported by the NSF through a grant for the Institute for Theoretical Atomic, Molecular and Optical Physics at Harvard University and Smithsonian Astrophysical Observatory. NR 37 TC 0 Z9 0 U1 1 U2 4 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD JUN 10 PY 2013 VL 87 IS 6 AR 063609 DI 10.1103/PhysRevA.87.063609 PG 10 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 161AY UT WOS:000320163800010 ER PT J AU Liu, HB Ho, PTP Wright, MCH Su, YN Hsieh, PY Sun, AL Kim, SS Minh, YC AF Liu, Hauyu Baobab Ho, Paul T. P. Wright, Melvyn C. H. Su, Yu-Nung Hsieh, Pei-Ying Sun, Ai-Lei Kim, Sungsoo S. Minh, Young Chol TI INTERSTELLAR MEDIUM PROCESSING IN THE INNER 20 pc IN GALACTIC CENTER SO ASTROPHYSICAL JOURNAL LA English DT Article DE Galaxy: center; Galaxy: kinematics and dynamics; Galaxy: structure; ISM: clouds; stars: formation; techniques: interferometric ID MASSIVE STAR-FORMATION; LARGE ARRAY OBSERVATIONS; SUPERMASSIVE BLACK-HOLE; SAGITTARIUS A-ASTERISK; I METHANOL MASERS; CIRCUMNUCLEAR DISK; MOLECULAR CLOUDS; SGR-A; FORMING REGIONS; STELLAR ORBITS AB We present the Submillimeter Array 157 pointing mosaic in 0.86 mm dust continuum emission with 5 ''.1 x 4 ''.2 angular resolution, and the National Radio Astronomy Observatory Green Bank 100 m Telescope (GBT) observations of the CS/(CS)-S-34/(CS)-C-13 1-0 and SiO 1-0 emission with <= 20 '' x 18 '' angular resolution. The dust continuum image marginally resolves at least several tens of 10-10(2) M-circle dot dense clumps in the 5' field including the circumnuclear disk (CND) and the exterior gas streamers. There is very good agreement between the high resolution dust continuum map of the CND and all previous molecular line observations. As the dust emission is the most reliable optically thin tracer of the mass, free from most chemical and excitation effects, we demonstrate the reality of the abundant localized structures within the CND, and their connection to external gas structures. From the spectral line data, the velocity dispersions of the dense clumps and their parent molecular clouds are similar to 10-20 times higher than their virial velocity dispersions. This supports the idea that the CND and its immediate environment may not be stationary or stable structures. Some of the dense gas clumps are associated with 22 GHz water masers and 36.2 GHz and 44.1 GHz CH3OH masers. However, we do not find clumps that are bound by the gravity of the enclosed molecular gas. Hence, the CH3OH or H2O maser emission may be due to strong (proto) stellar feedback, which may be dispersing some of the gas clumps. C1 [Liu, Hauyu Baobab; Ho, Paul T. P.; Su, Yu-Nung; Hsieh, Pei-Ying] Acad Sinica, Inst Astron & Astrophys, Taipei 106, Taiwan. [Ho, Paul T. P.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Wright, Melvyn C. H.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Hsieh, Pei-Ying] Natl Cent Univ, Grad Inst Astron, Jhongli 32001, Taoyuan County, Taiwan. [Sun, Ai-Lei] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Kim, Sungsoo S.] Kyung Hee Univ, Dept Astron & Space Sci, Yongin 446701, Kyungki Do, South Korea. [Minh, Young Chol] Korea Astron & Space Sci Inst KASI, Taejon 305348, South Korea. RP Liu, HB (reprint author), Acad Sinica, Inst Astron & Astrophys, POB 23-141, Taipei 106, Taiwan. EM hyliu@asiaa.sinica.edu.tw RI Kim, Sungsoo/A-8601-2011 OI Kim, Sungsoo/0000-0002-5570-2160 FU ASIAA; Mid-career Research Program through the National Research Foundation (NRF) [2011-0016898]; Ministry of Education, Science and Technology (MEST) of Korea; Canadian Space Agency FX The GBT and SMA data are from projects GBT11B050, SMA2011AS085 and SMA2011BS040, which are parts of the integrated state-of-art imaging project KISS: Kinematic Processes of the Extremely Turbulent ISM around the Supermassive Black Holes. We acknowledge financial support from ASIAA. S.S.K. was supported by Mid-career Research Program (No. 2011-0016898) through the National Research Foundation (NRF) grant funded by the Ministry of Education, Science and Technology (MEST) of Korea. We thank Dr. Eric Feigelson for very useful suggestions. We thank Zhao Jun-Hui very much for his efforts in optimizing and upgrading MIRIAD for SMA, which made this project possible. We thank Toney Minter, Glen Langston, and David T. Frayer for assisting the GBT observations. We thank Glen Petitpas and Nimesh Patel for supporting the SMA observations. This research used the facilities of the Canadian Astronomy Data Centre operated by the National Research Council of Canada with the support of the Canadian Space Agency. NR 70 TC 18 Z9 18 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2013 VL 770 IS 1 AR 44 DI 10.1088/0004-637X/770/1/44 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158QD UT WOS:000319986400044 ER PT J AU Mann, AW Gaidos, E Kraus, A Hilton, EJ AF Mann, Andrew W. Gaidos, Eric Kraus, Adam Hilton, Eric J. TI TESTING THE METAL OF LATE-TYPE KEPLER PLANET HOSTS WITH IRON-CLAD METHODS SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems; planets and satellites: detection; planets and satellites: formation; stars: abundances; stars: late-type ID DIGITAL SKY SURVEY; LOW-MASS STARS; INFRARED TELESCOPE FACILITY; INTEGRAL-FIELD SPECTROGRAPH; K-BAND SPECTRA; M-DWARFS; PHOTOMETRIC CALIBRATION; EFFECTIVE TEMPERATURES; TARGET STARS; COOL STARS AB It has been shown that F, G, and early K dwarf hosts of Neptune-sized planets are not preferentially metal-rich. However, it is less clear whether the same holds for late K and M dwarf planet hosts. We report metallicities of Kepler targets and candidate transiting planet hosts with effective temperatures below 4500 K. We use new metallicity calibrations to determine [Fe/H] from visible and near-infrared spectra. We find that the metallicity distribution of late K and M dwarfs monitored by Kepler is consistent with that of the solar neighborhood. Further, we show that hosts of Earth- to Neptune-sized planets have metallicities consistent with those lacking detected planets and rule out a previously claimed 0.2 dex offset between the two distributions at 6 sigma confidence. We also demonstrate that the metallicities of late K and M dwarfs hosting multiple detected planets are consistent with those lacking detected planets. Our results indicate that multiple terrestrial and Neptune-sized planets can form around late K and M dwarfs with metallicities as low as 0.25 solar. The presence of Neptune-sized planets orbiting such low-metallicity M dwarfs suggests that accreting planets collect most or all of the solids from the disk and that the potential cores of giant planets can readily form around M dwarfs. The paucity of giant planets around M dwarfs compared to solar-type stars must be due to relatively rapid disk evaporation or a slower rate of planet accretion, rather than insufficient solids to form a core. C1 [Mann, Andrew W.; Hilton, Eric J.] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. [Gaidos, Eric] Univ Hawaii, Dept Geol & Geophys, Honolulu, HI 96822 USA. [Kraus, Adam] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Mann, AW (reprint author), Univ Hawaii, Inst Astron, 2680 Woodlawn Dr, Honolulu, HI 96822 USA. OI Mann, Andrew/0000-0003-3654-1602 FU NSF [AST-0908419]; NASA [NNX10AI90G, NNX11AC33G]; NASA Science Mission Directorate; University of Hawaii [NNX-08AE38A] FX We thank the anonymous reviewer for helping to make the manuscript significantly better. This work was supported by NSF grant AST-0908419, and NASA grants NNX10AI90G and NNX11AC33G (Origins of Solar Systems) to E.G.; This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission Directorate. SNIFS on the UH 2.2 m telescope is part of the Nearby Supernova Factory project, a scientific collaboration among the Centre de Recherche Astronomique de Lyon, Institut de Physique Nuclaire de Lyon, Laboratoire de Physique Nuclaire et des Hautes Energies, Lawrence Berkeley National Laboratory, Yale University, University of Bonn, Max Planck Institute for Astrophysics, Tsinghua Center for Astrophysics, and the Centre de Physique des Particules de Marseille. Based on data from the Infrared Telescope Facility, which is operated by the University of Hawaii under cooperative agreement No. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. NR 74 TC 26 Z9 26 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD JUN 10 PY 2013 VL 770 IS 1 AR 43 DI 10.1088/0004-637X/770/1/43 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158QD UT WOS:000319986400043 ER PT J AU Valencic, LA Smith, RK AF Valencic, Lynne A. Smith, Randall K. TI INTERSTELLAR ABUNDANCES TOWARD X Per, REVISITED SO ASTROPHYSICAL JOURNAL LA English DT Article DE ISM: abundances ID ABSORPTION-LINE OBSERVATIONS; RAY SPECTROSCOPY; CHEMICAL-COMPOSITION; GALACTIC DISK; TEMPERATURE-FLUCTUATIONS; PLANETARY-NEBULAE; FINE-STRUCTURE; STELLAR WINDS; NEUTRON-STAR; CRAB-NEBULA AB The nearby X-ray binary X Per (HD 24534) provides a useful beacon with which to examine dust grain types and measure elemental abundances in the local interstellar medium (ISM). The absorption features of O, Fe, Mg, and Si along this line of sight were measured using spectra from the Chandra X-Ray Observatory's LETG/ACIS-S and XMM-Newton's RGS instruments, and the Spex software package. The spectra were fit with dust analogs measured in the laboratory. The O, Mg, and Si abundances were compared to those from standard references, and the O abundance was compared to that along lines of sight toward other X-ray binaries. The results are as follows. First, it was found that a combination of MgSiO3 (enstatite) and Mg1.6Fe0.4SiO4 (olivine) provided the best fit to the O K edge, with N(MgSiO3)/N(Mg1.6Fe0.4SiO4) = 3.4. Second, the Fe L edge could be fit with models that included metallic iron, but it was not well described by the laboratory spectra currently available. Third, the total abundances of O, Mg, and Si were in very good agreement with that of recently re-analyzed B stars, suggesting that they are good indicators of abundances in the local ISM, and the depletions were also in agreement with expected values for the diffuse ISM. Finally, the O abundances found from X-ray binary absorption spectra show a similar correlation with Galactocentric distances as seen in other objects. C1 [Valencic, Lynne A.] Johns Hopkins Univ, Baltimore, MD 21218 USA. [Valencic, Lynne A.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Smith, Randall K.] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. RP Valencic, LA (reprint author), Johns Hopkins Univ, Baltimore, MD 21218 USA. FU Chandra Award [GO1-12052A] FX The authors are grateful to an anonymous referee, whose thoughtful comments improved this work. This work was supported by Chandra Award No. GO1-12052A. NR 96 TC 3 Z9 3 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 2013 VL 770 IS 1 AR 22 DI 10.1088/0004-637X/770/1/22 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 158QD UT WOS:000319986400022 ER PT J AU Testa, P De Pontieu, B Martinez-Sykora, J DeLuca, E Hansteen, V Cirtain, J Winebarger, A Golub, L Kobayashi, K Korreck, K Kuzin, S Walsh, R DeForest, C Title, A Weber, M AF Testa, Paola De Pontieu, Bart Martinez-Sykora, Juan DeLuca, Ed Hansteen, Viggo Cirtain, Jonathan Winebarger, Amy Golub, Leon Kobayashi, Ken Korreck, Kelly Kuzin, Sergey Walsh, Robert DeForest, Craig Title, Alan Weber, Mark TI OBSERVING CORONAL NANOFLARES IN ACTIVE REGION MOSS SO ASTROPHYSICAL JOURNAL LETTERS LA English DT Article DE Sun: activity; Sun: corona; Sun: magnetic topology; Sun: transition region; Sun: UV radiation ID X-RAY CORONA; TRANSITION REGION; HOT PLASMA; SOLAR CORONA; MAGNETIC RECONNECTION; IMAGING SPECTROMETER; LOOPS OBSERVATIONS; EMISSION; DYNAMICS; HINODE AB The High-resolution Coronal Imager (Hi-C) has provided Fe XII 193 angstrom images of the upper transition region moss at an unprecedented spatial (similar to 0 ''.3-0 ''.4) and temporal (5.5 s) resolution. The Hi-C observations show in some moss regions variability on timescales down to similar to 15 s, significantly shorter than the minute-scale variability typically found in previous observations of moss, therefore challenging the conclusion of moss being heated in a mostly steady manner. These rapid variability moss regions are located at the footpoints of bright hot coronal loops observed by the Solar Dynamics Observatory/Atmospheric Imaging Assembly in the 94 angstrom channel, and by the Hinode/X-Ray Telescope. The configuration of these loops is highly dynamic, and suggestive of slipping reconnection. We interpret these events as signatures of heating events associated with reconnection occurring in the overlying hot coronal loops, i.e., coronal nanoflares. We estimate the order of magnitude of the energy in these events to be of at least a few 10(23) erg, also supporting the nanoflare scenario. These Hi-C observations suggest that future observations at comparable high spatial and temporal resolution, with more extensive temperature coverage, are required to determine the exact characteristics of the heating mechanism(s). C1 [Testa, Paola; DeLuca, Ed; Golub, Leon; Korreck, Kelly; Weber, Mark] Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [De Pontieu, Bart; Martinez-Sykora, Juan; Title, Alan] Lockheed Martin Solar & Astrophys Lab, Palo Alto, CA 94304 USA. [Martinez-Sykora, Juan] Bay Area Environm Res Inst, Sonoma, CA 95476 USA. [Hansteen, Viggo] Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. [Cirtain, Jonathan; Winebarger, Amy; Kobayashi, Ken] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. [Kuzin, Sergey] Russian Acad Sci, PN Lebedev Phys Inst, Moscow 119991, Russia. [Walsh, Robert] Univ Cent Lancashire, Preston PR1 2HE, Lancs, England. [DeForest, Craig] Southwest Res Inst, Boulder, CO 80302 USA. RP Testa, P (reprint author), Smithsonian Astrophys Observ, 60 Garden St,MS 58, Cambridge, MA 02138 USA. EM ptesta@cfa.harvard.edu RI Kuzin, Sergey/M-3435-2015; DeLuca, Edward/L-7534-2013; OI DeLuca, Edward/0000-0001-7416-2895; Golub, Leon/0000-0001-9638-3082 FU Lockheed-Martin [SP02H1701R]; NASA [NNM07AB07C, NNX08BA99G, NNX08AH45G, NNX11AN98G] FX We thank the referees for their useful comments which greatly helped to improve the Letter. P.T. was supported by contract SP02H1701R from Lockheed-Martin, and NASA contract NNM07AB07C to SAO. B.D.P. was supported through NASA grants NNX08BA99G, NNX08AH45G, and NNX11AN98G. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ, NASA, and STFC (UK) as partners, and operated by these agencies in cooperation with ESA and NSC (Norway). NR 50 TC 39 Z9 39 U1 0 U2 6 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 2041-8205 EI 2041-8213 J9 ASTROPHYS J LETT JI Astrophys. J. Lett. PD JUN 10 PY 2013 VL 770 IS 1 AR UNSP L1 DI 10.1088/2041-8205/770/1/L1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 155CR UT WOS:000319723500001 ER PT J AU van der Marel, N van Dishoeck, EF Bruderer, S Birnstiel, T Pinilla, P Dullemond, CP van Kempen, TA Schmalzl, M Brown, JM Herczeg, GJ Mathews, GS Geers, V AF van der Marel, Nienke van Dishoeck, Ewine F. Bruderer, Simon Birnstiel, Til Pinilla, Paola Dullemond, Cornelis P. van Kempen, Tim A. Schmalzl, Markus Brown, Joanna M. Herczeg, Gregory J. Mathews, Geoffrey S. Geers, Vincent TI A Major Asymmetric Dust Trap in a Transition Disk SO SCIENCE LA English DT Article ID PROTOPLANETARY DISKS; ACCRETION DISKS; GIANT PLANET; VORTICES; YOUNG; IMAGES; GAP AB The statistics of discovered exoplanets suggest that planets form efficiently. However, there are fundamental unsolved problems, such as excessive inward drift of particles in protoplanetary disks during planet formation. Recent theories invoke dust traps to overcome this problem. We report the detection of a dust trap in the disk around the star Oph IRS 48 using observations from the Atacama Large Millimeter/submillimeter Array (ALMA). The 0.44-millimeter-wavelength continuum map shows high-contrast crescent-shaped emission on one side of the star, originating from millimeter-sized grains, whereas both the mid-infrared image (micrometer-sized dust) and the gas traced by the carbon monoxide 6-5 rotational line suggest rings centered on the star. The difference in distribution of big grains versus small grains/gas can be modeled with a vortex-shaped dust trap triggered by a companion. C1 [van der Marel, Nienke; van Dishoeck, Ewine F.; van Kempen, Tim A.; Schmalzl, Markus; Mathews, Geoffrey S.] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Dishoeck, Ewine F.; Bruderer, Simon] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Birnstiel, Til; Brown, Joanna M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Pinilla, Paola; Dullemond, Cornelis P.] Heidelberg Univ, Ctr Astron, Inst Theoret Astrophys, D-69120 Heidelberg, Germany. [van Kempen, Tim A.] Joint Atacama Large Millimeter Submillimeter Arra, Santiago, Chile. [Herczeg, Gregory J.] Peking Univ, Kavli Inst Astron & Astrophys, Beijing 100871, Peoples R China. [Geers, Vincent] Dublin Inst Adv Studies, Dublin 2, Ireland. RP van der Marel, N (reprint author), Leiden Univ, Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM nmarel@strw.leidenuniv.nl OI Dullemond, Cornelis/0000-0002-7078-5910; Birnstiel, Tilman/0000-0002-1899-8783 NR 29 TC 170 Z9 170 U1 2 U2 26 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD JUN 7 PY 2013 VL 340 IS 6137 BP 1199 EP 1202 DI 10.1126/science.1236770 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 158LP UT WOS:000319972800040 PM 23744942 ER PT J AU Thompson, JD Tiecke, TG de Leon, NP Feist, J Akimov, AV Gullans, M Zibrov, AS Vuletic, V Lukin, MD AF Thompson, J. D. Tiecke, T. G. de Leon, N. P. Feist, J. Akimov, A. V. Gullans, M. Zibrov, A. S. Vuletic, V. Lukin, M. D. TI Coupling a Single Trapped Atom to a Nanoscale Optical Cavity SO SCIENCE LA English DT Article ID QUANTUM-DOT AB Hybrid quantum devices, in which dissimilar quantum systems are combined in order to attain qualities not available with either system alone, may enable far-reaching control in quantum measurement, sensing, and information processing. A paradigmatic example is trapped ultracold atoms, which offer excellent quantum coherent properties, coupled to nanoscale solid-state systems, which allow for strong interactions. We demonstrate a deterministic interface between a single trapped rubidium atom and a nanoscale photonic crystal cavity. Precise control over the atom's position allows us to probe the cavity near-field with a resolution below the diffraction limit and to observe large atom-photon coupling. This approach may enable the realization of integrated, strongly coupled quantum nano-optical circuits. C1 [Thompson, J. D.; Tiecke, T. G.; de Leon, N. P.; Feist, J.; Akimov, A. V.; Gullans, M.; Zibrov, A. S.; Lukin, M. D.] Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. [Tiecke, T. G.; Vuletic, V.] Massachusetts Inst Technol MIT Harvard Ctr Ultrac, Dept Phys, Cambridge, MA 02139 USA. [Tiecke, T. G.; Vuletic, V.] MIT, Elect Res Lab, Cambridge, MA 02139 USA. [de Leon, N. P.] Harvard Univ, Dept Chem & Chem Biol, Cambridge, MA 02138 USA. [Feist, J.] Harvard Smithsonian Ctr Astrophys, Inst Theoret Atom Mol & Opt Phys ITAMP, Cambridge, MA 02138 USA. [Akimov, A. V.] Russian Quantum Ctr, Skolkovo 143025, Moscow Region, Russia. RP Lukin, MD (reprint author), Harvard Univ, Dept Phys, Cambridge, MA 02138 USA. EM lukin@physics.harvard.edu RI Feist, Johannes/J-7394-2012; Akimov, Alexey/J-6385-2015; Zibrov, Alexander/G-7419-2014; OI Feist, Johannes/0000-0002-7972-0646; Akimov, Alexey/0000-0002-4167-5085; Gullans, Michael/0000-0003-3974-2987 FU NSF [ECS-0335765]; Center for Ultracold Atoms; Defense Advanced Research Projects Agency (QUASAR program); Air Force Office of Scientific Research Multidisciplinary University Research Initiative; European Union project AQUTE; Packard Foundation; Fannie and John Hertz Foundation; NSF Graduate Research Fellowship Program; NSF through ITAMP FX We acknowledge helpful discussions with O. Painter, D. Chang, M. Loncar, Q. Quan, E. Kuznetsova, S. Yelin, H. Park, and M. Greiner. Financial support was provided by the NSF, the Center for Ultracold Atoms, the Defense Advanced Research Projects Agency (QUASAR program), the Air Force Office of Scientific Research Multidisciplinary University Research Initiative, European Union project AQUTE, and the Packard Foundation. J.D.T. acknowledges support from the Fannie and John Hertz Foundation and the NSF Graduate Research Fellowship Program, N.P.d.L. acknowledges an Element Six postdoctoral fellowship, and J.F. acknowledges a grant from the NSF through ITAMP. This work was performed in part at the Center for Nanoscale Systems (CNS), a member of the National Nanotechnology Infrastructure Network, which is supported by NSF award ECS-0335765. CNS is part of Harvard University. NR 30 TC 123 Z9 124 U1 10 U2 151 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 7 PY 2013 VL 340 IS 6137 BP 1202 EP 1205 DI 10.1126/science.1237125 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 158LP UT WOS:000319972800041 PM 23618764 ER PT J AU Thomas, DB McGoverin, CM McGraw, KJ James, HF Madden, O AF Thomas, Daniel B. McGoverin, Cushla M. McGraw, Kevin J. James, Helen F. Madden, Odile TI Vibrational spectroscopic analyses of unique yellow feather pigments (spheniscins) in penguins SO JOURNAL OF THE ROYAL SOCIETY INTERFACE LA English DT Article DE plumage; Raman; spectroscopy; Sphenisciformes; spheniscin ID SURFACE-ENHANCED RAMAN; RESONANCE RAMAN; KING PENGUINS; FT-RAMAN; APTENODYTES-PATAGONICUS; CAROTENOID-PIGMENTS; CYTOCHROME-C; SPECTRA; PLUMAGE; COLOR AB Many animals extract, synthesize and refine chemicals for colour display, where a range of compounds and structures can produce a diverse colour palette. Feather colours, for example, span the visible spectrum and mostly result from pigments in five chemical classes (carotenoids, melanins, porphyrins, psittacofulvins and metal oxides). However, the pigment that generates the yellow colour of penguin feathers appears to represent a sixth, poorly characterized class of feather pigments. This pigment class, here termed 'spheniscin', is displayed by half of the living penguin genera; the larger and richer colour displays of the pigment are highly attractive. Using Raman and mid-infrared spectroscopies, we analysed yellow feathers from two penguin species (king penguin, Aptenodytes patagonicus; macaroni penguin, Eudyptes chrysolophus) to further characterize spheniscin pigments. The Raman spectrum of spheniscin is distinct from spectra of other feather pigments and exhibits 17 distinctive spectral bands between 300 and 1700 cm(-1). Spectral bands from the yellow pigment are assigned to aromatically bound carbon atoms, and to skeletal modes in an aromatic, heterocyclic ring. It has been suggested that the penguin pigment is a pterin compound; Raman spectra from yellow penguin feathers are broadly consistent with previously reported pterin spectra, although we have not matched it to any known compound. Raman spectroscopy can provide a rapid and non-destructive method for surveying the distribution of different classes of feather pigments in the avian family tree, and for correlating the chemistry of spheniscin with compounds analysed elsewhere. We suggest that the sixth class of feather pigments may have evolved in a stem-lineage penguin and endowed modern penguins with a costly plumage trait that appears to be chemically unique among birds. C1 [Thomas, Daniel B.; James, Helen F.] Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. [Thomas, Daniel B.; Madden, Odile] Smithsonian Inst, Museum Conservat Inst, Suitland, MD 20746 USA. [McGoverin, Cushla M.] Temple Univ, Dept Bioengn, Philadelphia, PA 19122 USA. [McGraw, Kevin J.] Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. RP Thomas, DB (reprint author), Smithsonian Inst, Natl Museum Nat Hist, Dept Vertebrate Zool, Washington, DC 20013 USA. EM thomas@si.edu RI Madden, Odile/N-9909-2015 OI Madden, Odile/0000-0003-2322-2522 FU Peter Buck Fellowship FX We gratefully acknowledge Christopher Milensky (Division of Birds, NMNH) for help with specimen access, Matthew Carrano (Paleobiology Department), Daniel Ksepka (North Carolina State University), Jennifer Giaccai and Molly McGath (Museum Conservation Institute) for technical assistance and helpful comment, and Peter Buck for generously funding postdoctoral research. We are also grateful for the comments and improvements from Dr Tim Holt and four anonymous referees. D. B. T. is funded by a Peter Buck Fellowship administered by the Smithsonian Institution. NR 84 TC 10 Z9 11 U1 1 U2 42 PU ROYAL SOC PI LONDON PA 6-9 CARLTON HOUSE TERRACE, LONDON SW1Y 5AG, ENGLAND SN 1742-5689 J9 J R SOC INTERFACE JI J. R. Soc. Interface PD JUN 6 PY 2013 VL 10 IS 83 AR 20121065 DI 10.1098/rsif.2012.1065 PG 9 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 131QN UT WOS:000318009300003 PM 23516063 ER PT J AU Clarin, TMA Ruczynski, I Page, RA Siemers, BM AF Clarin, Theresa M. A. Ruczynski, Ireneusz Page, Rachel A. Siemers, Bjoern M. TI Foraging Ecology Predicts Learning Performance in Insectivorous Bats SO PLOS ONE LA English DT Article ID MYOTIS-CAPACCINII BONAPARTE; LONG-FINGERED BAT; MOUSE-EARED BATS; MACROPHYLLUM-MACROPHYLLUM; ECHOLOCATION BEHAVIOR; EXPLORATORY-BEHAVIOR; HABITAT SELECTION; HUNTING BEHAVIOR; PREY DETECTION; TRAWLING BATS AB Bats are unusual among mammals in showing great ecological diversity even among closely related species and are thus well suited for studies of adaptation to the ecological background. Here we investigate whether behavioral flexibility and simple- and complex-rule learning performance can be predicted by foraging ecology. We predict faster learning and higher flexibility in animals hunting in more complex, variable environments than in animals hunting in more simple, stable environments. To test this hypothesis, we studied three closely related insectivorous European bat species of the genus Myotis that belong to three different functional groups based on foraging habitats: M. capaccinii, an open water forager, M. myotis, a passive listening gleaner, and M. emarginatus, a clutter specialist. We predicted that M. capaccinii would show the least flexibility and slowest learning reflecting its relatively unstructured foraging habitat and the stereotypy of its natural foraging behavior, while the other two species would show greater flexibility and more rapid learning reflecting the complexity of their natural foraging tasks. We used a purposefully unnatural and thus species-fair crawling maze to test simple- and complex-rule learning, flexibility and re-learning performance. We found that M. capaccinii learned a simple rule as fast as the other species, but was slower in complex rule learning and was less flexible in response to changes in reward location. We found no differences in re-learning ability among species. Our results corroborate the hypothesis that animals' cognitive skills reflect the demands of their ecological niche. C1 [Clarin, Theresa M. A.; Ruczynski, Ireneusz; Siemers, Bjoern M.] Max Planck Inst Ornithol, Sensory Ecol Grp, Seewiesen, Germany. [Ruczynski, Ireneusz] Mammal Res Inst PAS, Bialowieza, Poland. [Page, Rachel A.] Smithonian Trop Res Inst, Panama City, Panama. RP Clarin, TMA (reprint author), Max Planck Inst Ornithol, Sensory Ecol Grp, Seewiesen, Germany. EM tclarin@orn.mpg.de FU Polish Ministry of Science and Higher Education; Tabachka Bat Research Station Team FX The study was undertaken with the budget of the Max Planck Society (www.mpg.de). IR was supported by the Polish Ministry of Science and Higher Education (http://www.nauka.gov.pl). Program: "Support for International Mobility of Scientists". The funders had no role in study design, data collection and analysis, decision to publish, or preparation of the manuscript.; We acknowledge Angela Clarin and Katharina Clarin for help with the logistic flow of the experiment, Renate Heckel and Leonie Baier for drawing the bats in figure 1 and 2, the Tabachka Bat Research Station Team 2010 for support, and John Ratcliffe and Irmgard Teschke for helpful comments on the manuscript. Our work was supported by the International Max Planck Research School (IMPRS) for Organismal Biology. Sadly, PD Dr. Bjorn Siemers, head of the Sensory Ecology Group in Seewiesen, Germany, passed away in May 2012. We are deeply thankful for his support, friendship, and inspiration. NR 67 TC 6 Z9 6 U1 4 U2 80 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 JUN 5 PY 2013 VL 8 IS 6 AR e64823 DI 10.1371/journal.pone.0064823 PG 12 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 166TB UT WOS:000320579400026 PM 23755146 ER PT J AU Graham, AM Aiken, GR Gilmour, CC AF Graham, Andrew M. Aiken, George R. Gilmour, Cynthia C. TI Effect of Dissolved Organic Matter Source and Character on Microbial Hg Methylation in Hg-S-DOM Solutions SO ENVIRONMENTAL SCIENCE & TECHNOLOGY LA English DT Article ID DESULFOBULBUS-PROPIONICUS 1PR3; AQUATIC HUMIC SUBSTANCES; METHYLMERCURY PRODUCTION; FLORIDA EVERGLADES; MERCURY METHYLATION; SULFIDE NANOPARTICLES; ESTUARINE SEDIMENT; PURE CULTURES; BINDING; BIOAVAILABILITY AB Dissolved organic matter (DOM) is a key component of fate and transport models for most metals, including mercury (Hg). Utilizing a suite of diverse DOM isolates, we demonstrated that DOM character, in addition to concentration, influences inorganic Hg (Hg(II)(i)) bioavailability to Hg-rnethylating bacteria. Using a model Hg-methylating bacterium, Desulfovibrio desulfuricans ND132, we evaluated Hg-DOM-sulfide bioavailability in washed-cell assays at environmentally relevant Hg/DOM ratios (similar to 1-8 ng Hg/mg C) and sulfide concentrations (1-1000 mu M). All tested DOM isolates significantly enhanced Hg methylation above DOM-free controls (from similar to 2 to >20-fold for 20 mg C/L DOM solutions), but high molecular weight/highly aromatic DOM isolates and/or those with high sulfur content were particularly effective at enhancing Hg methylation. Because these experiments were conducted under conditions of predicted supersaturation with respect to metacinnabar (beta-HgS(s)), we attribute the DOM-dependent enhancement of Hg(II)(i) bioavailability to steric and specific chemical (e.g., DOM thiols) inhibition of beta-HgS(s) growth and aggregation by DOM. Experiments examining the role of DOM across a wide sulfide, gradient revealed that DOM only enhances Hg methylation under fairly low sulfide conditions (less than or similar to 30 mu M), conditions that favor HgS nanoparticle/cluster formation relative to dissolved HgS species. C1 [Graham, Andrew M.] Grinnell Coll, Noyce Sci Ctr, Dept Chem, Grinnell, IA 50112 USA. [Graham, Andrew M.; Gilmour, Cynthia C.] Smithsonian Environm Res Ctr, Edgewater, MD 21037 USA. [Aiken, George R.] US Geol Survey, Boulder, CO 80303 USA. RP Graham, AM (reprint author), Grinnell Coll, Noyce Sci Ctr, Dept Chem, 1116 8th Ave, Grinnell, IA 50112 USA. EM grahaman@grinnell.edu RI Gilmour, Cynthia/G-1784-2010 OI Gilmour, Cynthia/0000-0002-1720-9498 FU U.S. Department of Energy under the Subsurface Biogeochemical Research Program; Office of Science, through the Mercury Science Focus Area Program at Oak Ridge National Laboratory; U.S. National Science Foundation [DEB0351050]; U.S. Geological Survey Priority Ecosystems and Toxics Substances Hydrology Programs FX We thank A. Bullock, A. Maizel, G. Riedel, Tyler Bell (SERC), K. Butler and B. Poulin (USGS) for laboratory assistance. This paper benefited from the instructive comments of Jeff Jeremiason and three anonymous reviewers. This work was supported by the U.S. Department of Energy under the Subsurface Biogeochemical Research Program, Office of Science, through the Mercury Science Focus Area Program at Oak Ridge National Laboratory, by U.S. National Science Foundation grant DEB0351050 to A. Heyes and C.C.G., and by the U.S. Geological Survey Priority Ecosystems and Toxics Substances Hydrology Programs. Any use of trade, firm, or product names is for descriptive purposes only and does not imply endorsement by the U.S. government. NR 59 TC 22 Z9 23 U1 9 U2 125 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0013-936X EI 1520-5851 J9 ENVIRON SCI TECHNOL JI Environ. Sci. Technol. PD JUN 4 PY 2013 VL 47 IS 11 BP 5746 EP 5754 DI 10.1021/es400414a PG 9 WC Engineering, Environmental; Environmental Sciences SC Engineering; Environmental Sciences & Ecology GA 160DO UT WOS:000320097400031 PM 23634978 ER PT J AU Beky, B Holman, MJ Gilliland, RL Bakos, GA Winn, JN Noyes, RW Sasselov, DD AF Beky, Bence Holman, Matthew J. Gilliland, Ronald L. Bakos, Gaspar A. Winn, Joshua N. Noyes, Robert W. Sasselov, Dimitar D. TI RELATIVE PHOTOMETRY OF HAT-P-1b OCCULTATIONS SO ASTRONOMICAL JOURNAL LA English DT Article DE stars: individual (ADS 16402 A, ADS 16402 B); techniques: photometric ID EXOPLANET HD 189733B; EMISSION-SPECTRUM; PLANET; 209458B; SPECTROSCOPY; INVERSION; BINARY; ALBEDO; XO-2B; STIS AB We present Hubble Space Telescope (HST) Space Telescope Imaging Spectrograph observations of two occultations of the transiting exoplanet HAT-P-1b. By measuring the planet to star flux ratio near opposition, we constrain the geometric albedo of the planet, which is strongly linked to its atmospheric temperature gradient. An advantage of HAT-P-1 as a target is its binary companion ADS 16402 A, which provides an excellent photometric reference, simplifying the usual steps in removing instrumental artifacts from HST time-series photometry. We find that without this reference star, we would need to detrend the lightcurve with the time of the exposures as well as the first three powers of HST orbital phase, and this would introduce a strong bias in the results for the albedo. However, with this reference star, we only need to detrend the data with the time of the exposures to achieve the same per-point scatter, therefore we can avoid most of the bias associated with detrending. Our final result is a 2 sigma upper limit of 0.64 for the geometric albedo of HAT-P-1b between 577 and 947 nm. C1 [Beky, Bence; Holman, Matthew J.; Noyes, Robert W.; Sasselov, Dimitar D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Gilliland, Ronald L.] Penn State Univ, Ctr Exoplanets & Habitable Worlds, University Pk, PA 16802 USA. [Bakos, Gaspar A.] Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. [Winn, Joshua N.] MIT, Dept Phys, Cambridge, MA 02139 USA. [Winn, Joshua N.] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Beky, B (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA. EM bbeky@cfa.harvard.edu FU NASA [NNX09AB33G, NNX12AH91H]; NSF [AST-1108686] FX M.J.H. and J.N.W. gratefully acknowledge support from NASA Origins grant NNX09AB33G. G.A.B. acknowledges support from NSF grant AST-1108686 and NASA grant NNX12AH91H. NR 26 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2013 VL 145 IS 6 AR 166 DI 10.1088/0004-6256/145/6/166 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD6DH UT WOS:000333343700009 ER PT J AU Ruiz-Rodriguez, D Prato, L Torres, G Wasserman, LH Neuhauser, R AF Ruiz-Rodriguez, Dary Prato, L. Torres, Guillermo Wasserman, L. H. Neuhaeuser, Ralph TI RX J0513.1+0851 AND RX J0539.9+0956: TWO YOUNG, RAPIDLY ROTATING SPECTROSCOPIC BINARY STARS SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries: spectroscopic; stars: pre-main sequence; techniques: radial velocities ID T-TAURI STARS; LOW-MASS STARS; MAIN-SEQUENCE STARS; KECK II TELESCOPE; RADIAL-VELOCITIES; ECHELLE SPECTROGRAPH; SPATIAL-DISTRIBUTION; DYNAMICAL MASS; ORION; WEAK AB RX J0513.1+0851 and RX J0539.9+0956 were previously identified as young, low-mass, single-lined spectroscopic binary systems and classified as weak-lined T Tauri stars at visible wavelengths. Here we present radial velocities, spectral types, nu sin i values, and flux ratios for the components in these systems resulting from two-dimensional cross-correlation analysis. These results are based on high-resolution, near-infrared spectroscopy taken with the Keck II telescope to provide a first characterization of these systems as double-lined rather than single-lined. It applies the power of infrared spectroscopy to the detection of cool secondaries; the flux scales as a less steep function of mass in the infrared than in the visible, thus enabling an identification of low-mass secondaries. We found that the RX J0513.1+0851 and RX J0539.9+0956 primary stars are fast rotators, 60 km s(-1) and 80 km s-1, respectively; this introduces extra difficulty in the detection of the secondary component as a result of the quite broad absorption lines. To date, these are the highest rotational velocities measured for a pre-main sequence spectroscopic binary. The orbital parameters and mass ratios were determined by combining new visible light spectroscopy with our infrared data for both systems. For RX J0513.1+0851, we derived a period of similar to 4 days and a mass ratio of q = 0.46 +/- 0.01 and for RX J0539.9+0956, a period of similar to 1117 days and a mass ratio of q = 0.66 +/- 0.01. Based on our derived properties for the stellar components, we estimate the luminosities and hence distances to these binaries at 220 pc and 90 pc. They appear to be significantly closer than previously estimated. C1 [Ruiz-Rodriguez, Dary; Prato, L.; Wasserman, L. H.] Lowell Observ, Flagstaff, AZ 86001 USA. [Torres, Guillermo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Neuhaeuser, Ralph] Inst Astrophys, D-07745 Jena, Germany. [Neuhaeuser, Ralph] Univ Sternwarte, FSU Jena, D-07745 Jena, Germany. RP Ruiz-Rodriguez, D (reprint author), Lowell Observ, 1400 W Mars Hill Rd, Flagstaff, AZ 86001 USA. EM dar@lowell.edu FU NASA Keck PI Data Award; NSF [AST-0444017, AST-1009136, AST-1007992]; NOAO, through the Telescope System Instrumentation Program (TSIP); W. M. Keck Foundation; National Aeronautics and Space Administration; National Science Foundation FX We thank the Keck staff for their support of this science, in particular T. Stickel, J. Rivera, S. Magee, G. Puniwai, C. Wilburn, G. Hill, and B. Schaefer. We are also grateful to P. Berlind, M. Calkins, J. Caruso, R. Davis, D. Latham, A. Milone, R. Stefanik, and J. Zajac for their assistance in obtaining the spectroscopic observations with the CfA facilities, and to R. Davis for maintaining the database of echelle observations. We thank R. Mathieu for permission to reproduce Figure 7. We thank the referee for detailed comments which have improved the presentation of this manuscript. This research was funded in part by a NASA Keck PI Data Award, administered by the NASA Exoplanet Science Institute, and NSF Grants AST-0444017 and AST-1009136 (to L.P.). G.T. acknowledges partial support from the NSF through grant AST-1007992. Some of the data described herein were taken on the Keck II telescope with time granted by NOAO, through the Telescope System Instrumentation Program (TSIP). TSIP is funded by NSF. Some data presented herein were obtained at the W. M. Keck Observatory from telescope time allocated to the National Aeronautics and Space Administration through the agency's scientific partnership with the California Institute of Technology and the University of California. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. This work made use of the SIMBAD reference database, the NASA Astrophysics Data System, and the data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. We recognize and acknowledge the significant cultural role that the summit of Mauna Kea plays within the indigenous Hawaiian community and are grateful for the opportunity to conduct observations from this special mountain. NR 53 TC 1 Z9 1 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6256 EI 1538-3881 J9 ASTRON J JI Astron. J. PD JUN PY 2013 VL 145 IS 6 AR 162 DI 10.1088/0004-6256/145/6/162 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA AD6DH UT WOS:000333343700005 ER PT J AU Galametz, A Grazian, A Fontana, A Ferguson, HC Ashby, MLN Barro, G Castellano, M Dahlen, T Donley, JL Faber, SM Grogin, N Guo, Y Huang, KH Kocevski, DD Koekemoer, AM Lee, KS McGrath, EJ Peth, M Willner, SP Almaini, O Cooper, M Cooray, A Conselice, CJ Dickinson, M Dunlop, JS Fazio, GG Foucaud, S Gardner, JP Giavalisco, M Hathi, NP Hartley, WG Koo, DC Lai, K de Mello, DF McLure, RJ Lucas, RA Paris, D Pentericci, L Santini, P Simpson, C Sommariva, V Targett, T Weiner, BJ Wuyts, S AF Galametz, Audrey Grazian, Andrea Fontana, Adriano Ferguson, Henry C. Ashby, M. L. N. Barro, Guillermo Castellano, Marco Dahlen, Tomas Donley, Jennifer L. Faber, Sandy M. Grogin, Norman Guo, Yicheng Huang, Kuang-Han Kocevski, Dale D. Koekemoer, Anton M. Lee, Kyoung-Soo McGrath, Elizabeth J. Peth, Michael Willner, S. P. Almaini, Omar Cooper, Michael Cooray, Asantha Conselice, Christopher J. Dickinson, Mark Dunlop, James S. Fazio, G. G. Foucaud, Sebastien Gardner, Jonathan P. Giavalisco, Mauro Hathi, N. P. Hartley, Will G. Koo, David C. Lai, Kamson de Mello, Duilia F. McLure, Ross J. Lucas, Ray A. Paris, Diego Pentericci, Laura Santini, Paola Simpson, Chris Sommariva, Veronica Targett, Thomas Weiner, Benjamin J. Wuyts, Stijn CA CANDELS Team TI CANDELS MULTIWAVELENGTH CATALOGS: SOURCE IDENTIFICATION AND PHOTOMETRY IN THE CANDELS UKIDSS ULTRA-DEEP SURVEY FIELD SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE galaxies: photometry; methods: data analysis; techniques: image processing ID EXTRAGALACTIC LEGACY SURVEY; GALAXY LUMINOSITY FUNCTION; SPITZER-SPACE-TELESCOPE; ACTIVE GALACTIC NUCLEI; EARLY DATA RELEASE; IMAGE SUBTRACTION; EVOLUTION SURVEY; SURVEY SXDS; SELECTION; CLUSTER AB We present the multiwavelength-ultraviolet to mid-infrared-catalog of the UKIRT Infrared Deep Sky Survey (UKIDSS) Ultra-Deep Survey field observed as part of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS). Based on publicly available data, the catalog includes the CANDELS data from the Hubble Space Telescope (near-infrared WFC3 F125W and F160W data and visible ACS F606W and F814W data); u-band data from CFHT/Megacam; B, V, R-c, i', and z' band data from Subaru/Suprime-Cam; Y and K-s band data from VLT/HAWK-I; J, H, and K band data from UKIDSS (Data Release 8); and Spitzer/IRAC data (3.6, 4.5 mu m from SEDS; 5.8 and 8.0 mu m from SpUDS). The present catalog is F160W-selected and contains 35, 932 sources over an area of 201.7 arcmin(2) and includes radio-and X-ray-detected sources and spectroscopic redshifts available for 210 sources. C1 [Galametz, Audrey; Grazian, Andrea; Fontana, Adriano; Castellano, Marco; Paris, Diego; Pentericci, Laura; Santini, Paola; Sommariva, Veronica] INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. [Ferguson, Henry C.; Dahlen, Tomas; Grogin, Norman; Huang, Kuang-Han; Koekemoer, Anton M.; Lai, Kamson; Lucas, Ray A.] Space Telescope Sci Inst, Baltimore, MD 21218 USA. [Ashby, M. L. N.; Willner, S. P.; Fazio, G. G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Barro, Guillermo; Faber, Sandy M.; Guo, Yicheng; Koo, David C.] Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. [Donley, Jennifer L.] Los Alamos Natl Lab, Los Alamos, NM USA. [Guo, Yicheng; Giavalisco, Mauro] Univ Massachusetts, Dept Astron, Amherst, MA 01003 USA. [Huang, Kuang-Han; Peth, Michael] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Kocevski, Dale D.] Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. [Lee, Kyoung-Soo] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [McGrath, Elizabeth J.] Colby Coll, Dept Phys & Astron, Waterville, ME 04901 USA. [Almaini, Omar; Conselice, Christopher J.; Hartley, Will G.] Univ Nottingham, Sch Phys & Astron, Nottingham NG7 2RD, England. [Cooper, Michael; Cooray, Asantha] Univ Calif Irvine, Dept Phys & Astron, Irvine, CA USA. [Dickinson, Mark] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Dunlop, James S.; McLure, Ross J.; Targett, Thomas] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh, Midlothian, Scotland. [Foucaud, Sebastien] Natl Taiwan Normal Univ, Taipei, Taiwan. [Gardner, Jonathan P.] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Observat Cosmol Lab, Greenbelt, MD 20771 USA. [Hathi, N. P.] Observ Carnegie Inst Sci, Pasadena, CA USA. [de Mello, Duilia F.] Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. [Simpson, Chris] Liverpool John Moores Univ, Astrophys Res Inst, Birkenhead, Merseyside, England. [Weiner, Benjamin J.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Wuyts, Stijn] Max Planck Inst Extraterr Phys, D-85741 Garching, Germany. RP Galametz, A (reprint author), INAF Osservatorio Roma, I-00040 Monte Porzio Catone, Italy. EM audrey.galametz@oa-roma.inaf.it RI Hathi, Nimish/J-7092-2014; OI Hathi, Nimish/0000-0001-6145-5090; Castellano, Marco/0000-0001-9875-8263; Weiner, Benjamin/0000-0001-6065-7483; Santini, Paola/0000-0002-9334-8705; Koekemoer, Anton/0000-0002-6610-2048; fontana, adriano/0000-0003-3820-2823 NR 54 TC 73 Z9 73 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 JUN PY 2013 VL 206 IS 2 AR UNSP 10 DI 10.1088/0067-0049/206/2/10 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 234OX UT WOS:000325654800001 ER PT J AU Maselli, A Massaro, F Cusumano, G D'Abrusco, R La Parola, V Paggi, A Segreto, A Smith, HA Tosti, G AF Maselli, A. Massaro, F. Cusumano, G. D'Abrusco, R. La Parola, V. Paggi, A. Segreto, A. Smith, Howard A. Tosti, G. TI SEARCHING FOR NEW gamma-RAY BLAZAR CANDIDATES IN THE THIRD PALERMO BAT HARD X-RAY CATALOG WITH WISE SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE BL Lacertae objects: general; galaxies: active; radiation mechanisms: non; thermal; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; LARGE-AREA TELESCOPE; BL LACERTAE OBJECTS; SKY SURVEY; DATA RELEASE; SAMPLE; MISSION; IDENTIFICATION; EVOLUTION; IMAGER AB We searched for gamma-ray blazar candidates among the 382 unidentified hard X-ray sources of the third Palermo BAT Catalog (3PBC) obtained from the analysis of 66 months of Swift Burst Alert Telescope (BAT) survey data and listing 1586 sources. We adopted a recently developed association method based on the peculiar infrared colors that characterize the. gamma-ray blazars included in the second catalog of active galactic nuclei detected by the Fermi Large Area Telescope. We used this method exploiting the data of the all-sky survey performed by the Wide-field Infrared Survey Explorer (WISE) to establish correspondences between unidentified 3PBC sources and WISE. -ray blazar candidates located within the BAT positional uncertainty region at a 99% confidence level. We obtained a preliminary list of candidates for which we analyzed all the available data in the Swift archive to complement the information in the literature and in the radio, infrared, and optical catalogs with the information on their optical-UV and soft X-ray emission. Requiring the presence of radio and soft X-ray counterparts consistent with the infrared positions of the selected WISE sources, as well as a blazar-like radio morphology, we finally obtained a list of 24 gamma-ray blazar candidates. C1 [Maselli, A.; Cusumano, G.; La Parola, V.; Segreto, A.] INAF IASF Palermo, I-90146 Palermo, Italy. [Massaro, F.] SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA. [Massaro, F.] Kavli Inst Particle Astrophys & Cosmol, Menlo Pk, CA 94025 USA. [D'Abrusco, R.; Paggi, A.; Smith, Howard A.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Tosti, G.] Univ Perugia, Dipartimento Fis, I-06123 Perugia, Italy. [Tosti, G.] Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy. RP Maselli, A (reprint author), INAF IASF Palermo, Via U La Malfa 153, I-90146 Palermo, Italy. RI D'Abrusco, Raffaele/L-2767-2016; Massaro, Francesco/L-9102-2016; Paggi, Alessandro/C-1219-2017; OI D'Abrusco, Raffaele/0000-0003-3073-0605; Massaro, Francesco/0000-0002-1704-9850; Paggi, Alessandro/0000-0002-5646-2410; Segreto, Alberto/0000-0001-7341-6603; Cusumano, Giancarlo/0000-0002-8151-1990 NR 67 TC 8 Z9 8 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 JUN PY 2013 VL 206 IS 2 AR UNSP 17 DI 10.1088/0067-0049/206/2/17 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 234OX UT WOS:000325654800008 ER PT J AU Zeri, M Hussain, MZ Anderson-Teixeira, KJ DeLucia, E Bernacchi, CJ AF Zeri, Marcelo Hussain, Mir Zaman Anderson-Teixeira, Kristina J. DeLucia, Evan Bernacchi, Carl J. TI Water use efficiency of perennial and annual bioenergy crops in central Illinois SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article DE Water Use Efficiency; biofuels; Carbon balance; Agriculture ID MISCANTHUS X GIGANTEUS; LAND-USE CHANGE; BIOFUEL CROPS; ECOSYSTEM RESPIRATION; CARBON SEQUESTRATION; TEMPERATE CLIMATE; HYDROLOGIC-CYCLE; UNITED-STATES; SOIL CARBON; EXCHANGE AB Sustainable bioenergy production depends upon the efficiency with which crops use available water to produce biomass and store carbon belowground. Therefore, water use efficiency (WUE; productivity vs. annual evapotranspiration, ET) is a key metric of bioenergy crop performance. We evaluate WUE of three potential perennial grass bioenergy crops, Miscanthusxgiganteus (miscanthus), Panicum virgatum (switchgrass), and an assemblage of prairie species (28 species), and Zea mays-Glycine max rotation, during the establishment phase in Illinois. Ecosystem WUE (EWUE; net ecosystem productivity vs. ET) was highest in miscanthus, reaching a maximum value of 12.80.3kgha(-1)mm(-1) in the third year, followed by switchgrass (7.50.3kgha(-1)mm(-1)) and prairie (3.90.3kgha(-1)mm(-1)); the row crop was the lowest. Besides EWUE, harvest-WUE (HWUE, harvested biomass vs. ET) and net biome productivity-WUE (BWUE, calculated as net ecosystem production - harvest vs. ET) were also estimated for all crops and years. After three years of establishment, HWUE and BWUE were highest in miscanthus (9.02 and 3.8 +/- 2.9kgha(-1)mm(-1), respectively) providing a net benefit to the carbon balance, while the row crops had a negative carbon balance and a negative BWUE. BWUE for maize/soybean indicate that this ecosystem would deplete the soil carbon stocks while using the water resources. Switchgrass had the second highest BWUE, while prairie was almost neutral indicating that long-term carbon sequestration for this agro-ecosystem would be sensitive to harvest timing with an early harvest removing more biomass, and thus carbon, from the field. C1 [Zeri, Marcelo; Hussain, Mir Zaman; Anderson-Teixeira, Kristina J.; DeLucia, Evan; Bernacchi, Carl J.] Univ Illinois, Energy Biosci Inst, Urbana, IL 61801 USA. [Zeri, Marcelo] Inst Nacl Pesquisas Espaciais, Ctr Ciencia Sistema Terr, BR-12630000 Cachoeira Paulista, SP, Brazil. [Anderson-Teixeira, Kristina J.] Smithsonian Inst Global Earth Observ, Ctr Trop Forest Sci, Front Royal, VA USA. [Anderson-Teixeira, Kristina J.] Smithsonian Conservat Biol Inst, Front Royal, VA USA. [DeLucia, Evan; Bernacchi, Carl J.] Univ Illinois, Dept Plant Biol, Urbana, IL 61801 USA. [DeLucia, Evan] Univ Illinois, Inst Genom Biol, Urbana, IL 61801 USA. [Bernacchi, Carl J.] ARS, Global Change & Photosynth Res Unit, USDA, Urbana, IL USA. RP Bernacchi, CJ (reprint author), Univ Illinois, Dept Plant Biol, 1201 West Gregory Dr,Room 193, Urbana, IL 61801 USA. EM bernacch@illinois.edu FU Energy Biosciences Institute; FAPESP [2011/04101-0] FX The authors are grateful to the helpful comments and suggestions of three anonymous reviewers. Climate data provided by the Illinois State Water Survey (ISWS) located in Champaign, Illinois, and on the web at www.isws.illinois.edu. This work was funded by the Energy Biosciences Institute. M. Zeri would like to thank FAPESP (process 2011/04101-0) for the support during the preparation of this manuscript. NR 54 TC 17 Z9 18 U1 1 U2 33 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-8953 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD JUN PY 2013 VL 118 IS 2 BP 581 EP 589 DI 10.1002/jgrg.20052 PG 9 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 224TU UT WOS:000324913100016 ER PT J AU Hauck, SA Margot, JL Solomon, SC Phillips, RJ Johnson, CL Lemoine, FG Mazarico, E McCoy, TJ Padovan, S Peale, SJ Perry, ME Smith, DE Zuber, MT AF Hauck, Steven A., II Margot, Jean-Luc Solomon, Sean C. Phillips, Roger J. Johnson, Catherine L. Lemoine, Frank G. Mazarico, Erwan McCoy, Timothy J. Padovan, Sebastiano Peale, Stanton J. Perry, Mark E. Smith, David E. Zuber, Maria T. TI The curious case of Mercury's internal structure SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article DE Mercury; Internal Structure; MESSENGER ID EQUATION-OF-STATE; FE-RICH PORTION; HIGH-PRESSURE; MAGNETIC-FIELD; GRAVITY-FIELD; EARTHS CORE; MELTING RELATIONS; HIGH-TEMPERATURE; PLANETARY CORES; PHASE-RELATIONS AB The recent determination of the gravity field of Mercury and new Earth-based radar observations of the planet's spin state afford the opportunity to explore Mercury's internal structure. These observations provide estimates of two measures of the radial mass distribution of Mercury: the normalized polar moment of inertia and the fractional polar moment of inertia of the solid portion of the planet overlying the liquid core. Employing Monte Carlo techniques, we calculate several million models of the radial density structure of Mercury consistent with its radius and bulk density and constrained by these moment of inertia parameters. We estimate that the top of the liquid core is at a radius of 202030km, the mean density above this boundary is 3380200kgm(-3), and the density below the boundary is 6980280kgm(-3). We find that these internal structure parameters are robust across a broad range of compositional models for the core and planet as a whole. Geochemical observations of Mercury's surface by MESSENGER indicate a chemically reducing environment that would favor the partitioning of silicon or both silicon and sulfur into the metallic core during core-mantle differentiation. For a core composed of Fe-S-Si materials, the thermodynamic properties at elevated pressures and temperatures suggest that an FeS-rich layer could form at the top of the core and that a portion of it may be presently solid. C1 [Hauck, Steven A., II] Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. [Margot, Jean-Luc] Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA USA. [Margot, Jean-Luc; Padovan, Sebastiano] Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90024 USA. [Solomon, Sean C.] Carnegie Inst Sci, Dept Terr Magnetism, Washington, DC USA. [Solomon, Sean C.] Columbia Univ, Lamont Doherty Earth Observ, Palisades, NY USA. [Phillips, Roger J.] SW Res Inst, Planetary Sci Directorate, Boulder, CO USA. [Johnson, Catherine L.] Univ British Columbia, Dept Earth Ocean & Atmospher Sci, Vancouver, BC V5Z 1M9, Canada. [Johnson, Catherine L.] Planetary Sci Inst, Tucson, AZ USA. [Lemoine, Frank G.] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Mazarico, Erwan; Smith, David E.; Zuber, Maria T.] MIT, Dept Earth Atmospher & Planetary Sci, Cambridge, MA USA. [McCoy, Timothy J.] Smithsonian Inst, Dept Mineral Sci, Natl Museum Nat Hist, Washington, DC 20560 USA. [Peale, Stanton J.] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. [Perry, Mark E.] Johns Hopkins Appl Phys Lab, Space Dept, Laurel, MD USA. RP Hauck, SA (reprint author), Case Western Reserve Univ, Dept Earth Environm & Planetary Sci, Cleveland, OH 44106 USA. EM hauck@case.edu RI Hauck, Steven/A-7865-2008; Margot, Jean-Luc/A-6154-2012; Lemoine, Frank/D-1215-2013; Mazarico, Erwan/N-6034-2014; Perry, Mark/B-8870-2016 OI Hauck, Steven/0000-0001-8245-146X; Margot, Jean-Luc/0000-0001-9798-1797; Mazarico, Erwan/0000-0003-3456-427X; Perry, Mark/0000-0003-1600-6856 FU NASA MESSENGER [NNX07AR77G]; NASA [NASW-00002, NAS5-97271] FX We thank the entire MESSENGER team for the development and operation of the mission and the acquisition of the data from the first spacecraft to orbit Mercury. Discussions with Larry Nittler and Nathalie Michel on an early draft are greatly appreciated. Comments by Frank Sohl and an anonymous reviewer helped sharpen the manuscript. This work is supported by NASA MESSENGER Participating Scientist grant NNX07AR77G to S. A. H. The MESSENGER project is supported by the NASA Discovery Program under contracts NASW-00002 to the Carnegie Institution of Washington and NAS5-97271 to The Johns Hopkins University Applied Physics Laboratory. This work made use of the High Performance Computing Resource in the Core Facility for Advanced Research Computing at Case Western Reserve University. NR 73 TC 52 Z9 52 U1 3 U2 40 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD JUN PY 2013 VL 118 IS 6 BP 1204 EP 1220 DI 10.1002/jgre.20091 PG 17 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 224TI UT WOS:000324911900004 ER PT J AU Joyce, CJ Schwadron, NA Wilson, JK Spence, HE Kasper, JC Golightly, M Blake, JB Mazur, J Townsend, LW Case, AW Semones, E Smith, S Zeitlin, CJ AF Joyce, C. J. Schwadron, N. A. Wilson, J. K. Spence, H. E. Kasper, J. C. Golightly, M. Blake, J. B. Mazur, J. Townsend, L. W. Case, A. W. Semones, E. Smith, S. Zeitlin, C. J. TI Validation of PREDICCS using LRO/CRaTER observations during three major solar events in 2012 SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radiation model; doserate; modulation potential AB PREDICCS (Predictions of Radiation from Release, EMMREM, and Data Incorporating the CRaTER, COSTEP and other SEP measurements, prediccs.sr.unh.edu) is an online system designed to provide a near real-time characterization of the radiation environment of the inner heliosphere. PREDICCS utilizes data from various satellites in conjunction with numerical models such as the Earth-Moon-Mars Radiation Environment Module (EMMREM) to produce dose rate and particle flux data at the Earth, Moon and Mars. The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument launched aboard the Lunar Reconnaissance Orbiter (LRO) spacecraft in 2009 and designed to measure energetic particle radiation, offers an opportunity to test the capability of PREDICCS to accurately describe the lunar radiation environment. We provide comparisons between dose rates produced by PREDICCS with those measured by CRaTER during three major solar energetic particle (SEP) events that occurred in 2012. In addition, using EMMREM data products together with our archive of measured CRaTER dose rates, we compute the modulation potential at the Moon throughout the LRO mission and, using this, compute the background GCR dose rate during each event. We demonstrate reasonable agreement between PREDICCS and CRaTER dose rates and come to the conclusion that PREDICCS provides credible characterization of the lunar radiation environment. This study represents the first multi-event validation, via in situ measurement, of radiation models such as EMMREM, which should prove to be valuable in future efforts in risk assessment and in the study of radiation in the inner heliosphere. C1 [Joyce, C. J.; Schwadron, N. A.; Wilson, J. K.; Spence, H. E.; Golightly, M.; Smith, S.] Univ New Hampshire, Dept Phys, Ctr Space Sci, Durham, NH 03824 USA. [Kasper, J. C.; Case, A. W.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Blake, J. B.] Aerosp Corp, Los Angeles, CA 90009 USA. [Mazur, J.] Aerosp Corp, Space Sci Dept Chantilly, Chantilly, VA USA. [Townsend, L. W.] Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. [Semones, E.] NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. [Zeitlin, C. J.] SW Res Inst, Boulder, CO USA. RP Joyce, CJ (reprint author), Univ New Hampshire, Dept Phys, Ctr Space Sci, 39 Coll Rd, Durham, NH 03824 USA. EM cjl46@unh.edu OI Spence, Harlan/0000-0002-2526-2205 FU NASA LRO/CRaTER/PREDICCS Project [NNG11PA03C]; NSF/FESD Sun-to-Ice Project [AGS1135432]; NASA/LWS/NSF EMMREM Project [NNX11AC06G] FX This work is supported by NASA LRO/CRaTER/PREDICCS Project (Contract NNG11PA03C), the NSF/FESD Sun-to-Ice Project (Grant AGS1135432), and the NASA/LWS/NSF EMMREM Project (Grant NNX11AC06G). We thank the ACE SIS instrument team and the ACE Science Center for providing the ACE data used here. NR 10 TC 9 Z9 9 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2013 VL 11 IS 6 BP 350 EP 360 DI 10.1002/swe.20059 PG 11 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 231OI UT WOS:000325426100007 ER PT J AU Case, AW Kasper, JC Spence, HE Zeitlin, CJ Looper, MD Golightly, MJ Schwadron, NA Townsend, LW Mazur, JE Blake, JB Iwata, Y AF Case, A. W. Kasper, J. C. Spence, H. E. Zeitlin, C. J. Looper, M. D. Golightly, M. J. Schwadron, N. A. Townsend, L. W. Mazur, J. E. Blake, J. B. Iwata, Y. TI The deep space galactic cosmic ray lineal energy spectrum at solar minimum SO SPACE WEATHER-THE INTERNATIONAL JOURNAL OF RESEARCH AND APPLICATIONS LA English DT Article DE radiation; galactic cosmic rays AB The Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument is an energetic particle telescope on board the Lunar Reconnaissance Orbiter spacecraft. CRaTER measures energetic charged particles that have sufficient energy to penetrate the outer shielding of the instrument (about 12MeV/nucleon). Galactic cosmic rays (GCR) with these energies are the primary radiation concern for spacecraft and astronauts outside of the Earth's magnetosphere during times of minimal solar activity. These particles can easily penetrate typical shielding and damage electronics, causing increased electronics failure rates and single event upsets. When this radiation impacts biological cells, it causes an increased risk of cancer. The CRaTER instrument was built to characterize the radiation dose and lineal energy with unprecedented time and energy resolution and was fortuitously flown during a period of time that coincided with the highest GCR fluxes in the modern space age. We report here this worst-case GCR lineal energy spectrum. Observations are made behind a thin aluminum window and different thicknesses of tissue-equivalent plastic. These measurements provide important observational data points to compare with current model predictions of the dose deposited by energetic particles within a tissue-like material. C1 [Case, A. W.; Kasper, J. C.] Smithsonian Astrophys Observ, Cambridge, MA USA. [Spence, H. E.; Golightly, M. J.; Schwadron, N. A.] Univ New Hampshire, Inst Earth Ocean & Space Sci, Durham, NH 03824 USA. [Zeitlin, C. J.] SW Res Inst, Boulder, CO USA. [Looper, M. D.; Blake, J. B.] Aerosp Corp, El Segundo, CA 90245 USA. [Townsend, L. W.] Univ Tennessee, Knoxville, TN USA. [Mazur, J. E.] Aerosp Corp, Chantilly, VA USA. [Iwata, Y.] Natl Inst Radiol Sci, Chiba 260, Japan. RP Case, AW (reprint author), Harvard Smithsonian Ctr Astrophys, 60 Garden St MS 58, Cambridge, MA 02138 USA. EM tonycase@cfa.harvard.edu OI Spence, Harlan/0000-0002-2526-2205 FU NASA CRaTER [NNG11PA03C] FX This work is supported by NASA CRaTER contract NNG11PA03C. We wish to thank the LRO spacecraft team for their excellence in designing, building, and operating the spacecraft. We thank the team at the NASA Space Radiation Laboratory (NSRL) at Brookhaven National Laboratory for providing ion beams for instrument characterization. We also thank the staff at the HIMAC facility for providing ion beams for instrument characterization. NR 20 TC 9 Z9 9 U1 1 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 1542-7390 J9 SPACE WEATHER JI Space Weather PD JUN PY 2013 VL 11 IS 6 BP 361 EP 368 DI 10.1002/swe.20051 PG 8 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 231OI UT WOS:000325426100008 ER PT J AU Wendler, I Huber, BT MacLeod, KG Wendler, JE AF Wendler, Ines Huber, Brian T. MacLeod, Kenneth G. Wendler, Jens E. TI Stable oxygen and carbon isotope systematics of exquisitely preserved Turonian foraminifera from Tanzania - Understanding isotopic signatures in fossils SO MARINE MICROPALEONTOLOGY LA English DT Article DE foraminifera; Turonian stable isotopes; isotopic covariance; vital effect; Tanzania ID SEA BENTHIC FORAMINIFERA; CRETACEOUS-TERTIARY BOUNDARY; DEEP-WATER CIRCULATION; LIVING PLANKTONIC-FORAMINIFERA; WESTERN MEDITERRANEAN SEA; JURASSIC PREBETIC ZONE; NORTHERN ADRIATIC SEA; OCEANIC ANOXIC EVENT; PACIFIC-OCEAN; INDIAN-OCEAN AB The interpretation of delta O-18 and delta C-13 analyses of extinct foraminifera is hampered by insufficient knowledge on the contribution of environmental versus biological factors on the measured values. We present single-species stable isotope data for 18 benthic and 11 planktic foraminiferal species and one calcareous dinoflagellate cyst species from a Turonian equatorial record measured on samples collected in SE Tanzania. All microfossils analyzed were excellently preserved and results are compared to isotopic measurements from bulk sediment of the same material. Remarkably low intra-specific variability (standard deviations <0.2 parts per thousand) across the studied interval and consistently large benthic/planktic offsets in delta O-18 (similar to 2.8 parts per thousand.) and delta C-13 (similar to 1.5 parts per thousand) indicate absence of major long-term environmental fluctuations and presence of a well stratified water column. Stratigraphic isotopic trends show small shifts that are parallel in all studied benthic species (with the exception of the delta C-13 record of Lenticulina species), but within-sample inter-specific offsets reflect a combination of habitat differences and species-specific isotopic disequilibrium fractionation. Among planktic taxa closely related taxa tend to have similar isotopic values. Biserial taxa have the lowest delta O-18 values (similar to-4.7 parts per thousand) but also have relatively low delta C-13 values (similar to 1.6 parts per thousand) indicating that, for the assumption of a surface water habitat, additional metabolic effects need to be involved, which supports the concept of their opportunistic lifestyle. Among trochospiral planktics the keeled taxa with compressed chambers have slightly higher delta O-18 (similar to-4.2 parts per thousand) and lower delta C-13 (similar to 2.3 parts per thousand) values than taxa with globular chambers (similar to-4.4 parts per thousand and similar to 2.4 parts per thousand, respectively), suggesting differences in habitat or in peak seasonal abundance. Benthic taxa are subdivided into three isotopically distinct groups with differences reflecting mineralogy, life strategy and habitat; Group I: aragonitic taxa (Epistomina, Colomia africana), Group II: calcitic trochospiral taxa with isotopic values seemingly close to equilibrium (Berthelina berthelini, Oridorsalis umbonatus, Lingulogavelinella globosa, Lingulogavelinella convexa) and Group III: calcitic taxa with low delta O-18 values and large scatter in delta C-13 values (Lenticulina). Four other benthic species show values between Groups II and III. The wealth and consistency of data, especially for benthic taxa, permit refined conclusions. The five studied species of Epistomina have a similar isotopic signature and are inferred to form their aragonitic shells with close to equilibrium values. Small isotopic offsets are seen among species that differ in orientation of the septal foramen, but no offsets are seen that seem to co-vary with test shape or ornamentation. The conical species C africana has delta O-18 values similar to 0.2 parts per thousand lower and delta C-13 values degrees 0.7 parts per thousand lower than species of Epistomina. The latter offset probably reflects an infaunal habitat for C. africana. Epistomina and Group II species are recommended for paleoenviromental studies. Mono-specific Lenticulina delta O-18 values may be used if increased by correction factors of 0.4 parts per thousand to 0.9 parts per thousand, but this taxon's low and variable delta C-13 values are interpreted to reflect incorporation of respiratory CO2, possibly combined with fast growth rates related to opportunism, rather than equilibrium with benthic dissolved inorganic carbon. The observed stability of inter-specific isotopic offsets suggests disequilibrium isotopic effects are relatively consistent for many taxa in this section, and correction factors are proposed that may help to generate more robust Upper Cretaceous foraminiferal isotopic records. However, delta O-18/delta C-13 covariance in some benthic inter-specific comparisons suggests offsets might vary with changes in temperature, food supply or other factors so the appropriateness of the correction factors should be confirmed before being applied at different sites. Similarities between the observed single-species isotopic patterns from this and other studies are used to present a summarizing scheme of influences on the stable isotopic composition in foraminiferal tests. By applying the new insights from our study to data from other Cretaceous studies we demonstrate that the selection of species for isotopic analysis and understanding these signals are critical to the outcome of paleoceanographic interpretations. (C) 2013 Elsevier B.V. All rights reserved. C1 [Wendler, Ines; Huber, Brian T.; Wendler, Jens E.] Smithsonian Museum Nat Hist, Dept Paleobiol, Washington, DC 20013 USA. [Wendler, Ines; Wendler, Jens E.] Univ Bremen, Dept Geol Sci, D-28334 Bremen, Germany. [MacLeod, Kenneth G.] Univ Missouri, Dept Geol Sci, Columbia, MO 65211 USA. RP Wendler, I (reprint author), Univ Bremen, Dept Geol Sci, POB 330 440, D-28334 Bremen, Germany. EM flatter@uni-bremen.de RI MacLeod, Kenneth/C-4042-2017 OI MacLeod, Kenneth/0000-0002-6016-0837 FU National Science Foundation [NSF EAR 0641956]; Smithsonian Institution Scholarly Studies Program; German Science Foundation (DFG) [WE 4587/1-1] FX Logistical and field support from the Tanzania Petroleum Development Corporation was critical to the success of the Tanzania Drilling Program; we are particularly grateful for the generous assistance of TPDC staff including Joyce Singano, Michael Kereme, Ephrem Mchana, Amina Mweneinda, Emma Msaki, and Frank Mayagilo. For assistance with sample preparation and foraminifer picking we thank Shannon Haynes, Carlos Rodriguez-Russo, Sarah Ehlinger, Joshua Johnson, John Vincent, Erin Jacobs and Loren Petruny. Comments and suggestions by L Alegret, O. Friedrich, an anonymous third reviewer and by F. Jorissen are highly acknowledged. This study was funded by the National Science Foundation (NSF EAR 0641956), the Smithsonian Institution Scholarly Studies Program and the German Science Foundation (DFG, WE 4587/1-1). NR 237 TC 23 Z9 23 U1 0 U2 34 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0377-8398 EI 1872-6186 J9 MAR MICROPALEONTOL JI Mar. Micropaleontol. PD JUN PY 2013 VL 102 BP 1 EP 33 DI 10.1016/j.marmicro.2013.04.003 PG 33 WC Paleontology SC Paleontology GA 211NB UT WOS:000323913800001 ER PT J AU de Stapf, MNS Silva, TD AF Sanchez de Stapf, Maria Natividad Silva, Tania dos Santos TI Typifications in Cordia (Cordiaceae), with an assessment of the status of Cordia blanchetii SO KEW BULLETIN LA English DT Article DE Brazil; lectotype; neotype; nomenclatural synonyms; Patagonula; synonym ID BORAGINALES AB Typifications are proposed to facilitate ongoing studies in Cordiaceae and to maintain current usage. Lectotypes are designated for the following 13 names: Cordia ecalyculata, C. digyna, C. diospyrifolia, C. exaltata var. melanoneura, C. magnoliifolia, C. obscura var. tomentosa, C. obscura var. magnifolia, C. salicifolia, C. sellowiana, C. silvestris, C. ulei, C. ucayaliensis, and Patagonula glaziovii. Two new synonyms are proposed: C. crenatifolia Rizzini to C. glazioviana (Taub.) Gottschling & J. S. Mill. and C. araripensis Rizzini to C. bicolor A. DC. Additionally, nomenclatural notes on C. blanchetii are provided. C1 [Sanchez de Stapf, Maria Natividad; Silva, Tania dos Santos] Univ Estadual Feira de Santana, Dept Ciencias Biol, BR-44036900 Feira De Santana, BA, Brazil. [Sanchez de Stapf, Maria Natividad] Smithsonian Trop Res Inst, Balboa, Panama. RP de Stapf, MNS (reprint author), Univ Estadual Feira de Santana, Dept Ciencias Biol, Av Transnordestina Sn, BR-44036900 Feira De Santana, BA, Brazil. EM stapfm@si.edu FU Organization American States (OAS); Secretaria Nacional de Ciencia y Tecnologia (SENACYT) of Panama; Kew Latin America Research Fellowship Programme (KLARF); CNPq FX Financial support for this research was provided by Organization American States (OAS) and Secretaria Nacional de Ciencia y Tecnologia (SENACYT) of Panama as PhD fellowship for the first author, who also received support of Kew Latin America Research Fellowship Programme (KLARF), to visit of European herbaria. T. R. S. Silva was supported by CNPq. We are grateful to the herbarium curators who provided loans or access to their collections. NR 28 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER LONDON LTD PI LONDON PA 236 GRAYS INN RD, 6TH FLOOR, LONDON WC1X 8HL, ENGLAND SN 0075-5974 EI 1874-933X J9 KEW BULL JI Kew Bull. PD JUN PY 2013 VL 68 IS 2 BP 355 EP 359 DI 10.1007/S12225-013-9439-Z PG 5 WC Plant Sciences SC Plant Sciences GA 211HL UT WOS:000323897100019 ER PT J AU Giannios, D Sironi, L AF Giannios, Dimitrios Sironi, Lorenzo TI The S2 star as a probe of the accretion disc of Sgr A* SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE accretion; accretion discs; black hole physics; radiation mechanisms: thermal; shock waves; stars: winds; outflows; galaxies: active ID SUPERMASSIVE BLACK-HOLE; GALACTIC-CENTER; SAGITTARIUS-A; DOMINATED ACCRETION; GRMHD SIMULATIONS; CLOUD G2; FLOWS; MODELS; EMISSION; WINDS AB How accretion proceeds around the massive black hole in the Galactic Centre and other highly sub-Eddington accretors remains poorly understood. The orbit of the S2 star in the Galactic Centre passes through the accretion disc of the massive black hole and any observational signature from such interaction may be used as an accretion probe. Because of its early stellar type, S2 is expected to posses a fairly powerful wind. We show here that the ram pressure of the accretion disc shocks the stellar wind fairly close to the star. The shocked fluid reaches a temperature of similar to 1 keV and cools efficiently through optically thin, thermal bremsstrahlung emission. The radiation from the shocked wind peaks around the epoch of the pericentre passage of the star at a luminosity potentially comparable to the quiescent emission detected from Sgr A*. Detection of shocked wind radiation can constrain the density of the accretion disc at a distance of several thousands of gravitational radii from the black hole. C1 [Giannios, Dimitrios] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA. [Sironi, Lorenzo] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Giannios, D (reprint author), Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 USA. EM dgiannio@purdue.edu FU NASA through Einstein Postdoctoral Fellowship [PF1-120090]; Chandra X-ray Center FX LS is supported by NASA through Einstein Postdoctoral Fellowship grant number PF1-120090 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. NR 30 TC 5 Z9 5 U1 1 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 433 IS 1 BP L25 EP L29 DI 10.1093/mnrasl/slt051 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208VE UT WOS:000323708300006 ER PT J AU Laporte, CFP Walker, MG Penarrubia, J AF Laporte, Chervin F. P. Walker, Matthew G. Penarrubia, Jorge TI Measuring the slopes of mass profiles for dwarf spheroidals in triaxial cold dark matter potentials SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: kinematics and dynamics; galaxies: structure ID DENSITY PROFILE; FORNAX DWARF; LOCAL GROUP; GALAXIES; MODELS; HALOES; KINEMATICS; EVOLUTION; CLUSTERS; PROJECT AB We generate stellar distribution functions (DFs) in triaxial haloes in order to examine the reliability of slopes Gamma equivalent to delta log M/delta log r inferred by applying mass estimators of the form M proportional to R-e Sigma(2) (i.e. assuming spherical symmetry, where R-e and Sigma are luminous effective radius and global velocity dispersion, respectively) to two stellar subpopulations independently tracing the same gravitational potential. The DFs take the form f(E), are dynamically stable and are generated within triaxial potentials corresponding directly to subhaloes formed in cosmological dark-matter-only simulations of Milky Way and galaxy cluster haloes. Additionally, we consider the effect of different tracer number density profiles (cuspy and cored) on the inferred slopes of mass profiles. For the isotropic DFs considered here, we find that halo triaxiality tends to introduce an anticorrelation between R-e and Sigma when estimated for a variety of viewing angles. The net effect is a negligible contribution to the systematic error associated with the slope of the mass profile, which continues to be dominated by a bias towards greater overestimation of masses for more concentrated tracer populations. We demonstrate that simple mass estimates for two distinct tracer populations can give reliable lower limits for Gamma, irrespective of the degree of triaxiality or shape of the tracer number density profile. C1 [Laporte, Chervin F. P.] Max Planck Inst Astrophys, D-85740 Garching, Germany. [Walker, Matthew G.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Penarrubia, Jorge] Univ Edinburgh, Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Midlothian, Scotland. [Penarrubia, Jorge] CSIC, Inst Astrofis Andalucia, E-18008 Granada, Spain. RP Laporte, CFP (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM cfpl2@mpa-garching.mpg.de RI Walker, Matthew/P-1777-2014 OI Walker, Matthew/0000-0003-2496-1925 FU Marie Curie Initial Training Network CosmoComp [PITN-GA-2009-238356]; NASA [HST-HF-51283.01-A, NAS5-26555]; Space Telescope Science Institute FX CFPL thanks Simon White for useful discussions, Mark Gieles and the IoA where early discussions began. MGW and JGP thank the MPA for its hospitality during their visit. The authors thank the Virgo Consortium for making their data available for this study. CFPL is supported by the Marie Curie Initial Training Network CosmoComp (PITN-GA-2009-238356). MGW is supported by NASA through Hubble Fellowship grant HST-HF-51283.01-A, awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. NR 31 TC 7 Z9 7 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 433 IS 1 BP L54 EP L58 DI 10.1093/mnrasl/slt057 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208VE UT WOS:000323708300012 ER PT J AU Patton, DR Torrey, P Ellison, SL Mendel, JT Scudder, JM AF Patton, David R. Torrey, Paul Ellison, Sara L. Mendel, J. Trevor Scudder, Jillian M. TI Galaxy pairs in the Sloan Digital Sky Survey - VI. The orbital extent of enhanced star formation in interacting galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE galaxies: evolution; galaxies: interactions; galaxies: star formation ID ACTIVE GALACTIC NUCLEI; METALLICITY EVOLUTION; REDSHIFT SURVEY; MERGER RATE; SIMULATIONS; GASDYNAMICS; CONNECTION; STARBURSTS; DEPENDENCE; UNIVERSE AB We use pair and environmental classifications of similar to 211 000 star-forming galaxies from the Sloan Digital Sky Survey, along with a suite of merger simulations, to investigate the enhancement of star formation as a function of separation in galaxy pairs. Using a new technique for distinguishing between the influence of nearby neighbours and larger scale environment, we find a clear enhancement in star formation out to projected separations of similar to 150 kpc, beyond which there is no net enhancement. We find the strongest enhancements at the smallest separations (especially < 20 kpc), consistent with earlier work. Similar trends are seen in the simulations, which indicate that the strongest enhancements are produced in highly disturbed systems approaching final coalescence, whereas the more modest enhancements seen at wider separations are the result of starburst activity triggered at first pericentre passage, which persists as the galaxies move to larger separations. The absence of any net enhancement beyond 150 kpc provides reassurance that the detected enhancements are due to galaxy-galaxy interactions, rather than larger scale environmental effects or potential pair selection biases. A rough census indicates that 66 per cent of the enhanced star formation in our pair sample occurs at separations > 30 kpc. We conclude that significant interaction-induced star formation is not restricted to merger remnants or galaxies with close companions; instead, a larger population of wider separation pairs exhibit enhanced star formation due to recent close encounters. C1 [Patton, David R.] Trent Univ, Dept Phys & Astron, Peterborough, ON K9J 7B8, Canada. [Torrey, Paul] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Ellison, Sara L.; Mendel, J. Trevor; Scudder, Jillian M.] Univ Victoria, Dept Phys & Astron, Victoria, BC V8P 1A1, Canada. RP Patton, DR (reprint author), Trent Univ, Dept Phys & Astron, 1600 West Bank Dr, Peterborough, ON K9J 7B8, Canada. EM dpatton@trentu.ca OI Scudder, Jillian/0000-0002-8798-3972; Torrey, Paul/0000-0002-5653-0786 NR 38 TC 48 Z9 48 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 PY 2013 VL 433 IS 1 BP L59 EP L63 DI 10.1093/mnrasl/slt058 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 208VE UT WOS:000323708300013 ER PT J AU Wendler, JE Bown, P AF Wendler, Jens E. Bown, Paul TI Exceptionally well-preserved Cretaceous microfossils reveal new biomineralization styles SO NATURE COMMUNICATIONS LA English DT Article ID CALCAREOUS DINOFLAGELLATE CYSTS; RECONSTRUCTION; PALEOECOLOGY; CALCISPHERES; SEA AB Calcareous microplankton shells form the dominant components of ancient and modern pelagic sea-floor carbonates and are widely used in palaeoenvironmental reconstructions. The efficacy of these applications, however, is dependent upon minimal geochemical alteration during diagenesis, but these modifying processes are poorly understood. Here we report on new biomineralization architectures of previously unsuspected complexity in calcareous cell-wall coverings of extinct dinoflagellates (pithonellids) from a Tanzanian microfossil-lagerstatte. These Cretaceous 'calcispheres' have previously been considered biomineralogically unremarkable but our new observations show that the true nature of these tests has been masked by recrystallization. The pristine Tanzanian fossils are formed from fibre-like crystallites and show archeopyles and exquisitely constructed opercula, demonstrating the dinoflagellate affinity of pithonellids, which has long been uncertain. The interwoven fibre-like structures provide strength and flexibility enhancing the protective function of these tests. The low-density wall fabrics may represent specific adaptation for oceanic encystment life cycles, preventing the cells from rapid sinking. C1 [Wendler, Jens E.] Smithsonian Inst, Dept Paleobiol, Washington, DC 20560 USA. [Wendler, Jens E.] Univ Bremen, Dept Geosci, D-28334 Bremen, Germany. [Bown, Paul] UCL, Dept Earth Sci, London WC1E 6BT, England. RP Wendler, JE (reprint author), Smithsonian Inst, Dept Paleobiol, MRC-121,10th & Constitut Ave, Washington, DC 20560 USA. EM wendler@uni-bremen.de OI Bown, Paul/0000-0001-6777-4463 FU DFG [WE 4587/1-1]; Natural Environment Research Council FX This research was supported by DFG fund WE 4587/1-1 (Wendler) and the Natural Environment Research Council (Bown). Ines Wendler, Sebastian Meier, Gerard Versteegh, Jeremy Young, Helmut Willems, Laurie Gower and Brian Huber are kindly thanked for conversations and comments on the manuscript. We thank Monika Kirsch for discussion on extant calcareous dinoflagellates and providing culture material. We acknowledge the Tanzania Petroleum Development Corporation, and particularly Dr Joyce Singano, for logistical support and the Tanzania Commission for Science and Technology for permission to drill. NR 19 TC 5 Z9 5 U1 1 U2 18 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 2041-1723 J9 NAT COMMUN JI Nat. Commun. PD JUN PY 2013 VL 4 AR 2052 DI 10.1038/ncomms3052 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 207TL UT WOS:000323626700006 PM 23774480 ER PT J AU Garcia, K Shaffer, JP Sarmiento, C Zalamea, PC Dalling, JW Davis, A Baltrus, DA Gallery, RE Arnold, AE AF Garcia, K. Shaffer, J. P. Sarmiento, C. Zalamea, P. C. Dalling, J. W. Davis, A. Baltrus, D. A. Gallery, R. E. Arnold, A. E. TI Diversity and evolutionary relationships of bacteria affiliated with tropical seeds and seed-associated fungi SO PHYTOPATHOLOGY LA English DT Meeting Abstract CT APS-MSA Joint Meeting CY AUG 10-14, 2013 CL Austin, TX SP APS, MSA C1 [Garcia, K.; Shaffer, J. P.; Baltrus, D. A.; Gallery, R. E.; Arnold, A. E.] Univ Arizona, Tucson, AZ USA. [Sarmiento, C.; Zalamea, P. C.] Smithsonian Trop Res Inst, Balboa, Ancon, Panama. [Dalling, J. W.] Univ Illinois, Urbana, IL USA. [Davis, A.] USDA ARS, Urbana, IL USA. NR 0 TC 0 Z9 0 U1 1 U2 4 PU AMER PHYTOPATHOLOGICAL SOC PI ST PAUL PA 3340 PILOT KNOB ROAD, ST PAUL, MN 55121 USA SN 0031-949X J9 PHYTOPATHOLOGY JI Phytopathology PD JUN PY 2013 VL 103 IS 6 SU 2 BP 48 EP 48 PG 1 WC Plant Sciences SC Plant Sciences GA 196TM UT WOS:000322799500261 ER PT J AU Demissew, S Funk, V AF Demissew, Sebsebe Funk, Vicki TI INSTITUTIONAL VOTES FOR THE 2017 NOMENCLATURE SECTION SO TAXON LA English DT Editorial Material C1 [Demissew, Sebsebe] Univ Addis Ababa, Fac Sci, Dept Biol, Natl Herbarium, Addis Ababa, Ethiopia. [Funk, Vicki] Smithsonian Inst, US Natl Herbarium, Dept Bot, NMNH,MRC 166, Washington, DC 20013 USA. RP Demissew, S (reprint author), Univ Addis Ababa, Fac Sci, Dept Biol, Natl Herbarium, POB 3434, Addis Ababa, Ethiopia. EM s_demissew@yahoo.com; funkv@si.edu NR 1 TC 1 Z9 1 U1 0 U2 1 PU INT ASSOC PLANT TAXONOMY-IAPT PI BRATISLAVA PA C/O INST BOTANY, SLOVAK ACAD SCIENCES DUBRAVSKA CESTA 9, SK-845 23 BRATISLAVA, SLOVAKIA SN 0040-0262 J9 TAXON JI Taxon PD JUN PY 2013 VL 62 IS 3 BP 648 EP 649 PG 2 WC Plant Sciences; Evolutionary Biology SC Plant Sciences; Evolutionary Biology GA 196CN UT WOS:000322751100031 ER PT J AU Jerzykiewicz, M Lehmann, H Niemczura, E Molenda-Zakowicz, J Dymitrov, W Fagas, M Guenther, DB Hartmann, M Hrudkova, M Kaminski, K Moffat, AFJ Kuschnig, R Leto, G Matthews, JM Rowe, JF Rucinski, SM Sasselov, D Weiss, WW AF Jerzykiewicz, M. Lehmann, H. Niemczura, E. Molenda-Zakowicz, J. Dymitrov, W. Fagas, M. Guenther, D. B. Hartmann, M. Hrudkova, M. Kaminski, K. Moffat, A. F. J. Kuschnig, R. Leto, G. Matthews, J. M. Rowe, J. F. Rucinski, S. M. Sasselov, D. Weiss, W. W. TI mu Eridani from MOST star and from the ground: an orbit, the SPB component's fundamental parameters and the SPB frequencies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE binaries: eclipsing; binaries: spectroscopic; stars: early-type; stars: individual: mu Eridani; stars: oscillations ID B-TYPE STARS; EMPIRICAL EFFECTIVE TEMPERATURES; SOLAR MODEL PROBLEM; BOLOMETRIC CORRECTIONS; RADIAL-VELOCITIES; ECLIPSING BINARIES; BETA PHOTOMETRY; SURFACE GRAVITY; NU-ERIDANI; F-STARS AB MOST time series photometry of mu Eri, an SB1 eclipsing binary with a rapidly rotating SPB primary, is reported and analysed. The analysis yields a number of sinusoidal terms, mainly due to the intrinsic variation of the primary, and the eclipse light curve. New radial-velocity observations are presented and used to compute parameters of a spectroscopic orbit. Frequency analysis of the radial-velocity residuals from the spectroscopic orbital solution fails to uncover periodic variations with amplitudes greater than 2 km s (1). A Rossiter-McLaughlin anomaly is detected from observations covering ingress. From archival photometric indices and the revised Hipparcos parallax, we derive the primary's effective temperature, surface gravity, bolometric correction and the luminosity. An analysis of a high signal-to-noise spectrogram yields the effective temperature and surface gravity in good agreement with the photometric values. From the same spectrogram, we determine the abundance of He, C, N, O, Ne, Mg, Al, Si, P, S, Cl and Fe. The eclipse light curve is solved by means of EBOP. For a range of mass of the primary, a value of mean density, very nearly independent of assumed mass, is computed from the parameters of the system. Contrary to a recent report, this value is approximately equal to the mean density obtained from the star's effective temperature and luminosity. Despite limited frequency resolution of the MOST data, we were able to recover the closely spaced SPB frequency quadruplet discovered from the ground in 2002-2004. The other two SPB terms seen from the ground were also recovered. Moreover, our analysis of the MOST data adds 15 low-amplitude SPB terms with frequencies ranging from 0.109 to 2.786 d(-1). C1 [Jerzykiewicz, M.; Niemczura, E.; Molenda-Zakowicz, J.] Uniwersytetu Wroclawskiego, Inst Astron, PL-51622 Wroclaw, Poland. [Lehmann, H.; Hartmann, M.; Hrudkova, M.] Thuringer Landessternwarte Tautenburg, D-07778 Tautenburg, Germany. [Dymitrov, W.; Fagas, M.; Kaminski, K.] Adam Mickiewicz Univ, Astron Observ Inst, Fac Phys, PL-60286 Poznan, Poland. [Guenther, D. B.; Weiss, W. W.] St Marys Univ, Dept Phys & Astron, Halifax, NS B3H 3C3, Canada. [Hrudkova, M.] Isaac Newton Grp Telescopes, E-38700 Santa Cruz De La Palma, Canary Islands, Spain. [Moffat, A. F. J.] Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. [Kuschnig, R.] Univ Vienna, Inst Astron, A-1180 Vienna, Austria. [Kuschnig, R.; Matthews, J. M.] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. [Leto, G.] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy. [Rowe, J. F.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Rucinski, S. M.] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H4, Canada. [Sasselov, D.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. RP Jerzykiewicz, M (reprint author), Uniwersytetu Wroclawskiego, Inst Astron, Kopernika 11, PL-51622 Wroclaw, Poland. EM mjerz@astro.uni.wroc.pl RI Leto, Giuseppe/N-3355-2015 OI Leto, Giuseppe/0000-0002-0040-5011 FU MNiSW grant [N N203 405139]; NCN grant [2011/01/B/St9/05448]; Wroclaw Centre for Networking and Supercomputing [214]; DFG [HA 3279/5-1]; Natural Sciences and Engineering Research Council (NSERC) of Canada; Fonds de recherche du Quebec (FQNRT) FX We are indebted to Dr Paul B. Etzel for providing the source code of his computer program EBOP and explanations and to Dr Jadwiga Daszynska-Daszkiewicz for computing the evolutionary tracks used in Section 8. MJ, EN and JM-.Z acknowledge support from MNiSW grant N N203 405139. EN acknowledges support from NCN grant 2011/01/B/St9/05448. Calculations have been partially carried out at the Wroclaw Centre for Networking and Supercomputing under grant No. 214. MHr acknowledges support from DFG grant HA 3279/5-1. WD thanks his students, Karolina Bakowska, Adrian Kruszewski, Krystian Kurzawa and Anna Przybyszewska for assisting in observations. DBG, JMM, AFJM and SMR acknowledge funding support of the Natural Sciences and Engineering Research Council (NSERC) of Canada. AFJM is also grateful for financial assistance from Fonds de recherche du Quebec (FQNRT). In this research, we have used the Aladin service, operated at CDS, Strasbourg, France, and the SAO/NASA Astrophysics Data System Abstract Service. NR 59 TC 2 Z9 2 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1032 EP 1045 DI 10.1093/mnras/stt522 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300015 ER PT J AU Hong, T Staveley-Smith, L Masters, KL Springob, CM Macri, LM Koribalski, BS Jones, DH Jarrett, TH Crook, AC AF Hong, Tao Staveley-Smith, Lister Masters, Karen L. Springob, Christopher M. Macri, Lucas M. Koribalski, Baerbel S. Jones, D. Heath Jarrett, Tom H. Crook, Aidan C. TI 2MTF-II. New Parkes 21-cm observations of 303 southern galaxies SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE catalogues; surveys; galaxies: distances and redshifts; galaxies: spiral; radio lines: galaxies ID TULLY-FISHER RELATION; 2MASS REDSHIFT SURVEY; FAST ALPHA SURVEY; ALL-SKY SURVEY; LOCAL UNIVERSE; LINE MEASUREMENTS; SOURCE CATALOG; SC GALAXIES; BAND; CALIBRATION AB We present new 21-cm neutral hydrogen (H i) observations of spiral galaxies for the 2MASS Tully-Fisher (2MTF) survey. Using the 64-m Parkes radio telescope multibeam system we obtain 152 high signal-to-noise ratio H i spectra from which we extract 148 high-accuracy (< 5 per cent error) velocity widths and derive reliable rotation velocities. The observed sample consists of 303 southern (delta < -40 degrees) galaxies selected from the 2MASS Redshift Survey with K-s < 11.25 mag, cz < 10 000 km s(-1) and axis ratio b/a < 0.5. The H i observations reported in this paper will be combined with new H i spectra from the Green Bank and Arecibo telescopes, together producing the most uniform Tully-Fisher survey ever constructed (in terms of sky coverage). In particular, due to its near-infrared selection, 2MTF will be significantly more complete at low Galactic latitude (vertical bar b vertical bar < 15 degrees) and will provide a more reliable map of peculiar velocities in the local Universe. C1 [Hong, Tao] Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. [Hong, Tao; Staveley-Smith, Lister; Springob, Christopher M.] Univ Western Australia, Int Ctr Radio Astron Res, Crawley, WA 6009, Australia. [Masters, Karen L.] Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England. [Masters, Karen L.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Springob, Christopher M.] Australian Astron Observ, N Ryde, NSW 1670, Australia. [Macri, Lucas M.] Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, Dept Phys & Astron, College Stn, TX 77843 USA. [Koribalski, Baerbel S.] Australia Telescope Natl Facil, CSIRO Astron & Space Sci, Epping, NSW 1710, Australia. [Jones, D. Heath] Monash Univ, Sch Phys, Clayton, Vic 3800, Australia. [Jarrett, Tom H.] Univ Cape Town, Dept Astron, ZA-7701 Rondebosch, South Africa. [Crook, Aidan C.] Microsoft Corp, Redmond, WA 98052 USA. RP Hong, T (reprint author), Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China. EM bartonhongtao@gmail.com RI Staveley-Smith, Lister/A-1683-2011; OI Staveley-Smith, Lister/0000-0002-8057-0294; Macri, Lucas/0000-0002-1775-4859 FU Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]; National Natural Science Foundation (NNSF) of China [10833003, 11103032]; NSF [AST-0406906]; Peter and Patricia Gruber Foundation; Leverhulme Trust; NASA, Space Telescope Science Institute [HST-HF-01153]; NSF through National Optical Astronomy Observatory FX Parts of this research were conducted by the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through project number CE110001020. TH was supported by the National Natural Science Foundation (NNSF) of China (10833003 and 11103032). KLM was supported by NSF grant AST-0406906, the Peter and Patricia Gruber Foundation and the Leverhulme Trust. LMM was supported by NASA through Hubble Fellowship grant HST-HF-01153 from the Space Telescope Science Institute and by the NSF through a Goldberg Fellowship from the National Optical Astronomy Observatory. ACC was supported by NSF grant AST-0406906. NR 33 TC 13 Z9 13 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1178 EP 1188 DI 10.1093/mnras/stt555 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300023 ER PT J AU Stefan, II Carilli, CL Green, DA Ali, Z Aguirre, JE Bradley, RF DeBoer, D Dexter, M Gugliucci, NE Harris, DE Jacobs, DC Klima, P MacMahon, D Manley, J Moore, DF Parsons, AR Pober, JC Walbrugh, WP AF Stefan, Irina I. Carilli, Chris L. Green, David A. Ali, Zaki Aguirre, James E. Bradley, Richard F. DeBoer, David Dexter, Matthew Gugliucci, Nicole E. Harris, D. E. Jacobs, Daniel C. Klima, Pat MacMahon, David Manley, Jason Moore, David F. Parsons, Aaron R. Pober, Jonathan C. Walbrugh, William P. TI Imaging on PAPER: Centaurus A at 148 MHz SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation: interferometers; galaxies: active; galaxies: individual: Centaurus A; galaxies: structure; X-rays: galaxies ID ACTIVE GALACTIC NUCLEI; ENERGY COSMIC-RAYS; NGC 5128 CENTAURUS; RADIO-SOURCES; SCALE STRUCTURE; EMISSION; GALAXY; LOBES; REIONIZATION; NGC-5128 AB We present observations taken with the Precision Array for Probing the Epoch of Reionization (PAPER) of the Centaurus A field in the frequency range 114-188 MHz. The resulting image has a 25 arcmin resolution, a dynamic range of 3500 and an rms of 0.5 Jy beam(-1) (for a beam size of 25 arcmin x 23 arcmin). A spectral index map of Cen A is produced across the full band. The spectral index distribution is qualitatively consistent with electron reacceleration in regions of excess turbulence in the radio lobes, as previously identified morphologically. Hence, there appears to be an association of 'severe weather' in radio lobes with energy input into the relativistic electron population. We compare the PAPER large-scale radio image with the X-ray image from the ROSAT All Sky Survey. There is a tentative correlation between radio and X-ray features at the end of the southern lobe, some 200 kpc from the nucleus, as might be expected from inverse Compton (IC) scattering of the cosmic microwave background by the relativistic electrons also responsible for the radio synchrotron emission. The magnetic fields derived from the (possible) IC and radio emission are of similar magnitude to fields derived under the minimum pressure assumptions, similar to 1 mu G. However, the X-ray field is complex, with large-scale gradients and features possibly unrelated to Cen A. If these X-ray features are unrelated to Cen A, then these fields are lower limits. C1 [Stefan, Irina I.; Green, David A.] Univ Cambridge, Cavendish Lab, Cambridge CB3 0HE, England. [Carilli, Chris L.] Natl Radio Astron Observ, Socorro, NM 87801 USA. [Ali, Zaki; DeBoer, David; Dexter, Matthew; MacMahon, David; Parsons, Aaron R.] Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. [Aguirre, James E.; Moore, David F.] Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA. [Bradley, Richard F.] Univ Virginia, Dept Elect & Comp Engn, Charlottesville, VA 22904 USA. [Bradley, Richard F.] Natl Radio Astron Observ, Charlottesville, VA 22903 USA. [Bradley, Richard F.; Gugliucci, Nicole E.; Klima, Pat] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. [Harris, D. E.] Harvard Smithsonian Ctr Astrophys, Smithsonian Astrophys Observ, Cambridge, MA 02138 USA. [Jacobs, Daniel C.] Arizona State Univ, Sch Earth & Space Explorat, Tempe, AZ 85287 USA. [Manley, Jason; Walbrugh, William P.] Sq Kilometre Array South Africa Project, ZA-7405 Pinelands, South Africa. [Parsons, Aaron R.; Pober, Jonathan C.] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. RP Stefan, II (reprint author), Univ Cambridge, Cavendish Lab, 19 JJ Thomson Ave, Cambridge CB3 0HE, England. EM iis21@cam.ac.uk RI Green, David/E-9609-2010 OI Green, David/0000-0003-3189-9998 FU NSF-AST programme [0804508, 1129258, 1125558]; Mt Cuba Astronomical Foundation FX We thank the SKA project office in South Africa for their efforts in ensuring the smooth running of PAPER. The PAPER project is supported through the NSF-AST programme (awards 0804508, 1129258 and 1125558), and by significant efforts by staff at NRAO's Green Bank and Charlottesville sites. We acknowledge grant support from the Mt Cuba Astronomical Foundation. We have made use of the ROSAT Data Archive of the Max-Planck-Institut fur extraterrestrische Physik (MPE) at Garching, Germany. We thank the referee for helpful comments. NR 48 TC 10 Z9 10 U1 1 U2 3 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 PY 2013 VL 432 IS 2 BP 1285 EP 1293 DI 10.1093/mnras/stt548 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300032 ER PT J AU LaMassa, SM Urry, CM Glikman, E Cappelluti, N Civano, F Comastri, A Treister, E Arifin Bohringer, H Cardamone, C Chon, GY Kephart, M Murray, SS Richards, G Ross, NP Rozner, JS Schawinski, K AF LaMassa, Stephanie M. Urry, C. Megan Glikman, Eilat Cappelluti, Nico Civano, Francesca Comastri, Andrea Treister, Ezequiel Arifin Boehringer, Hans Cardamone, Carie Chon, Gayoung Kephart, Miranda Murray, Stephen S. Richards, Gordon Ross, Nicholas P. Rozner, Joshua S. Schawinski, Kevin TI Finding rare AGN: X-ray number counts of Chandra sources in Stripe 82 SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE surveys; galaxies: active; quasars: general; X-rays: galaxies; X-rays: general ID DIGITAL-SKY-SURVEY; ACTIVE GALACTIC NUCLEI; POINT-SOURCE CATALOG; WIDE-FIELD SURVEY; QUASAR LUMINOSITY FUNCTION; YALE-CHILE MUSYC; MULTIWAVELENGTH PROJECT; COSMOS FIELD; DATA RELEASE; SURVEY DESIGN AB We present the first results of a wide-area X-ray survey within the Sloan Digital Sky Survey Stripe 82, a 300 deg(2) region of the sky with a substantial investment in multiwavelength coverage. We analysed archival Chandra observations that cover 6.2 deg(2) within Stripe 82 ('Stripe 82 ACX'), reaching 4.5 Sigma flux limits of 1.2 x 10(-15), 5.4 x 10(-15) and 2.9 x 10(-15) erg s(-1) cm(-2) in the soft (0.5-2 keV), hard (2-7 keV) and full (0.5-7 keV) bands, to find 480, 137 and 705 X-ray sources, respectively. 214 sources are detected only in the full band and 4 sources are detected solely in the soft band. Utilizing data products from the Chandra Source Catalog, we construct independent log N-log S relationships, detailing the number density of X-ray sources as a function of flux. The soft and full bands show general agreement with previous Chandra surveys; the hard band number counts agree among Stripe 82 ACX, XBootes and XDEEP2, but all three are somewhat systematically lower than the counts derived from Chandra Multiwavelength Project. We compare the luminosity distribution of Stripe 82 ACX with the smaller, deeper Chandra Deep Field-South, Extended Chandra Deep Field-South and Chandra-COSMOS surveys to illustrate the benefit of wide-area surveys in locating high-luminosity and/or high-redshift active galactic nuclei (AGN). Finally, we compare the identified AGN with predictions from population synthesis models, noting that prior to any spectroscopic follow-up campaign, we have already located roughly half the high-luminosity quasars at high redshift expected to lie within the survey area. However, our data also suggest that refinements to population synthesis models will be required. C1 [LaMassa, Stephanie M.; Urry, C. Megan; Glikman, Eilat; Kephart, Miranda; Rozner, Joshua S.] Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, New Haven, CT 06520 USA. [Cappelluti, Nico; Comastri, Andrea] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Cappelluti, Nico] Univ Maryland, Baltimore Coll, Ctr Space Sci & Technol, Dept Phys, Baltimore, MD 21250 USA. [Civano, Francesca; Murray, Stephen S.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Civano, Francesca] Dartmouth Coll, Dept Phys & Astron, Wilder Lab, Hanover, NH 03755 USA. [Treister, Ezequiel] Univ Concepcion, Concepcion, Chile. [Arifin] Natl Univ Singapore, Singapore 119077, Singapore. [Boehringer, Hans; Chon, Gayoung] Max Planck Inst Extraterr Phys, D-85748 Garching, Germany. [Cardamone, Carie] Brown Univ, Harriet W Sheridan Ctr Teaching & Learning, Providence, RI 02912 USA. [Murray, Stephen S.] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. [Richards, Gordon] Drexel Univ, Dept Phys, Philadelphia, PA 19104 USA. [Ross, Nicholas P.] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Berkeley, CA 94720 USA. [Schawinski, Kevin] ETH, Dept Phys, Inst Astron, CH-8093 Zurich, Switzerland. RP LaMassa, SM (reprint author), Yale Univ, Dept Phys, Yale Ctr Astron & Astrophys, POB 208120, New Haven, CT 06520 USA. EM stephanie.lamassa@yale.edu RI Urry, Claudia/G-7381-2011; Comastri, Andrea/O-9543-2015; OI Urry, Claudia/0000-0002-0745-9792; Comastri, Andrea/0000-0003-3451-9970; Cappelluti, Nico/0000-0002-1697-186X; Schawinski, Kevin/0000-0001-5464-0888 FU Swiss National Science Foundation [PP00P2\_138979/1] FX We thank the referee for insightful critiques and comments that improved this manuscript. This research has made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. We also thank Frank Primini and Nina Bonaventura for answering many CSC-related questions. We thank Bret Lehmer and Andy Goulding for thoughtful discussions. We also thank Bret Lehmer, Andy Goulding and Minsun Kim for access to their logN-logS data. KS gratefully acknowledges support from Swiss National Science Foundation Grant PP00P2\_138979/1. NR 47 TC 10 Z9 10 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD JUN PY 2013 VL 432 IS 2 BP 1351 EP 1360 DI 10.1093/mnras/stt553 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 156OP UT WOS:000319832300039 ER EF